研究者詳細 - 田村　陽一

論文 - 田村　陽一

分割表示 >> ／全件表示 143 件中 1 - 143 件目

Bound star clusters observed in a lensed galaxy 460 Myr after the Big Bang 査読有り国際共著国際誌 Open Access

Adamo, A; Bradley, LD; Vanzella, E; Claeyssens, A; Welch, B; Diego, JM; Mahler, G; Oguri, M; Sharon, K; Abdurro'uf; Hsiao, TYY; Xu, XF; Messa, M; Lassen, AE; Zackrisson, E; Brammer, G; Coe, D; Kokorev, V; Ricotti, M; Zitrin, A; Fujimoto, S; Inoue, AK; Resseguier, T; Rigby, JR; Jiménez-Teja, Y; Windhorst, RA; Hashimoto, T; Tamura, Y

NATURE 632 巻 ( 8025 ) 頁： 513 - 516 2024年8月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Nature

The Cosmic Gems arc is among the brightest and highly magnified galaxies observed at redshift z ≈ 10.2 (ref. 1). However, it is an intrinsically ultraviolet faint galaxy, in the range of those now thought to drive the reionization of the Universe2–4. Hitherto the smallest features resolved in a galaxy at a comparable redshift are between a few hundreds and a few tens of parsecs (pc)5,6. Here we report JWST observations of the Cosmic Gems. The light of the galaxy is resolved into five star clusters located in a region smaller than 70 pc. They exhibit minimal dust attenuation and low metallicity, ages younger than 50 Myr and intrinsic masses of about 106M⊙. Their lensing-corrected sizes are approximately 1 pc, resulting in stellar surface densities near 105M⊙ pc−2, three orders of magnitude higher than typical young star clusters in the local Universe7. Despite the uncertainties inherent to the lensing model, they are consistent with being gravitationally bound stellar systems, that is, proto-globular clusters. We conclude that star cluster formation and feedback likely contributed to shaping the properties of galaxies during the epoch of reionization.

DOI： 10.1038/s41586-024-07703-7

FINER: Far-Infrared Nebular Emission Receiver for the Large Millimeter Telescope 国際共著国際誌 Open Access

Tamura, Y; Sakai, T; Kawabe, R; Kojima, T; Taniguchi, A; Takekoshi, T; Kang, HR; Shan, WL; Hagimoto, M; Okauchi, N; Tetsuka, A; Inoue, AK; Kohno, K; Tanaka, K; Bakx, TJLC; Fudamoto, Y; Fujita, K; Harikane, Y; Hashimoto, T; Hatsukade, B; Hughes, DH; Iino, T; Kimura, Y; Maezawa, H; Matsuda, Y; Mawatari, K; Nakajima, T; Nakatsubo, S; Oshima, T; Sagawa, H; Schloerb, FP; Takahashi, S; Taniguchi, K; Tsujita, A; Umehata, H; Yonetsu, T; Yun, MS

MILLIMETER, SUBMILLIMETER, AND FAR-INFRARED DETECTORS AND INSTRUMENTATION FOR ASTRONOMY XII, PT 1 13102 巻 2024年

担当区分：筆頭著者,　責任著者記述言語：英語掲載種別：研究論文（国際会議プロシーディングス）出版者・発行元：Proceedings of SPIE - The International Society for Optical Engineering

Unveiling the emergence and prevalence of massive/bright galaxies during the epoch of reionization and beyond, within the first 600 million years of the Universe, stands as a pivotal pursuit in astronomy. Remarkable progress has been made by JWST in identifying an immense population of bright galaxies, which hints at exceptionally efficient galaxy assembly processes. However, the underlying physical mechanisms propelling their rapid growth remain unclear. With this in mind, millimeter and submillimeter-wave spectroscopic observations of redshifted far-infrared spectral lines, particularly the [O iii] 88 µm and [C ii] 158 µm lines, offers a crucial pathway to address this fundamental query. To this end, we develop a dual-polarization sideband-separating superconductor-insulator-superconductor (SIS) mixer receiver, FINER, for the Large Millimeter Telescope (LMT) situated in Mexico. Harnessing advancements from ALMA's wideband sensitivity upgrade (WSU) technology, FINER covers radio frequencies spanning 120-360 GHz, delivering an instantaneous intermediate frequency (IF) of 3-21 GHz per sideband per polarization, which is followed by a set of 10.24 GHz-wide digital spectrometers. At 40% of ALMA's light-collecting area, the LMT's similar atmospheric transmittance and FINER's 5 times wider bandwidth compared to ALMA culminate in an unparalleled spectral scanning capability in the northern hemisphere, paving the way for finer spectral-resolution detection of distant galaxies.

DOI： 10.1117/12.3017788

Reionization and the ISM/Stellar Origins with JWST and ALMA (RIOJA): The Core of the Highest-redshift Galaxy Overdensity at <i>z</i>=7.88 Confirmed by NIRSpec/JWST 査読有り国際共著国際誌 Open Access

Hashimoto, T; Alvarez-Márquez, J; Fudamoto, Y; Colina, L; Inoue, AK; Nakazato, Y; Ceverino, D; Yoshida, N; Costantin, L; Sugahara, Y; Gómez, AC; Blanco-Prieto, C; Mawatari, K; Arribas, S; Marques-Chaves, R; Pereira-Santaella, M; Bakx, TJLC; Hagimoto, M; Hashigaya, T; Matsuo, H; Tamura, Y; Usui, M; Ren, YW

ASTROPHYSICAL JOURNAL LETTERS 955 巻 ( 1 ) 頁： L2 2023年9月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal Letters

The protoclusters in the epoch of reionization, traced by galaxy overdensity regions, are ideal laboratories for studying the process of stellar assembly and cosmic reionization. We present the spectroscopic confirmation of the core of the most distant protocluster at z = 7.88, A2744-z7p9OD, with the James Webb Space Telescope NIRSpec integral field unit spectroscopy. The core region includes as many as four galaxies detected in [O iii] 4960 and 5008 Å in a small area of ∼3″ × 3″, corresponding to ∼11 × 11 kpc, after the lensing magnification correction. Three member galaxies are also tentatively detected in dust continuum in Atacama Large Millimeter/submillimeter Array Band 6, which is consistent with their red ultraviolet continuum slopes, β ∼ −1.3. The member galaxies have stellar masses in the range of log(M */M ⊙) ∼7.6-9.2 and star formation rates of ∼3-50 M ⊙ yr−1, showing a diversity in their properties. FirstLight cosmological simulations reproduce the physical properties of the member galaxies including the stellar mass, [O iii] luminosity, and dust-to-stellar mass ratio, and predict that the member galaxies are on the verge of merging in a few to several tens of Myr to become a large galaxy with M * ∼ 6 × 109 M ⊙. The presence of a multiple merger and evolved galaxies in the core region of A2744-z7p9OD indicates that environmental effects are already at work 650 Myr after the Big Bang.

DOI： 10.3847/2041-8213/acf57c

The 300 pc Resolution Imaging of a <i>z</i>=8.31 Galaxy: Turbulent Ionized Gas and Potential Stellar Feedback 600 Million Years after the Big Bang 査読有り国際共著国際誌 Open Access

Tamura, Y; Bakx, TJLC; Inoue, AK; Hashimoto, T; Tokuoka, T; Imamura, C; Hatsukade, B; Lee, MM; Moriwaki, K; Okamoto, T; Ota, K; Umehata, H; Yoshida, N; Zackrisson, E; Hagimoto, M; Matsuo, H; Shimizu, I; Sugahara, Y; Takeuchi, TT

ASTROPHYSICAL JOURNAL 952 巻 ( 1 ) 頁： 9 2023年7月

担当区分：筆頭著者,　責任著者記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present the results of 300 pc resolution Atacama Large Millimeter/submillimeter Array imaging of the [O iii] 88 μm line and dust continuum emission from a z = 8.312 Lyman-break galaxy MACS0416_Y1. The velocity-integrated [O iii] emission has three peaks that are likely associated with three young stellar clumps of MACS0416_Y1, while the channel map shows a complicated velocity structure with little indication of a global velocity gradient unlike what was found in [C ii] 158 μm at a larger scale, suggesting random bulk motion of ionized gas clouds inside the galaxy. In contrast, dust emission appears as two individual clumps apparently separating or bridging the [O iii]/stellar clumps. The cross-correlation coefficient between dust and ultraviolet-related emission (i.e., [O iii] and ultraviolet continuum) is unity on a galactic scale, while it drops at <1 kpc, suggesting well-mixed geometry of multiphase interstellar media on subkiloparsec scales. If the cutoff scale characterizes different stages of star formation, the cutoff scale can be explained by gravitational instability of turbulent gas. We also report on a kiloparsec-scale off-center cavity embedded in the dust continuum image. This could be a superbubble producing galactic-scale outflows, since the energy injection from the 4 Myr starburst suggested by a spectral energy distribution analysis is large enough to push the surrounding media creating a kiloparsec-scale cavity.

DOI： 10.3847/1538-4357/acd637

The bright extragalactic ALMA redshift survey (BEARS) - II. Millimetre photometry of gravitational lens candidates 国際共著 Open Access

Bendo, GJ; Urquhart, SA; Serjeant, S; Bakx, T; Hagimoto, M; Cox, P; Neri, R; Lehnert, MD; Dannerbauer, H; Amvrosiadis, A; Andreani, P; Baker, AJ; Beelen, A; Berta, S; Borsato, E; Buat, ; Butler, KM; Cooray, A; De Zotti, G; Dunne, L; Dye, S; Eales, S; Enia, A; Fan, L; Gavazzi, R; González-Nuevo, J; Harris, A; Herrera, CN; Hughes, DH; Ismail, D; Jones, BM; Kohno, K; Krips, M; Lagache, G; Marchetti, L; Massardi, M; Messias, H; Negrello, M; Omont, A; Pérez-Fournon, ; Riechers, DA; Scott, D; Smith, MWL; Stanley, F; Tamura, Y; Temi, P; van der Werf, P; Verma, A; Vlahakis, C; Weiss, A; Yang, C; Young, AJ

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 522 巻 ( 2 ) 頁： 2995 - 3017 2023年4月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society

We present 101- and 151-GHz ALMA continuum images for 85 fields selected from Herschel observations that have 500-μm flux densities >80 mJy and 250–500-μm colours consistent with z > 2, most of which are expected to be gravitationally lensed or hyperluminous infrared galaxies. Approximately half of the Herschel 500-μm sources were resolved into multiple ALMA sources, but 11 of the 15 brightest 500-μm Herschel sources correspond to individual ALMA sources. For the 37 fields containing either a single source with a spectroscopic redshift or two sources with the same spectroscopic redshift, we examined the colour temperatures and dust emissivity indices. The colour temperatures only vary weakly with redshift and are statistically consistent with no redshift-dependent temperature variations, which generally corresponds to results from other samples selected in far-infrared, submillimetre, or millimetre bands but not to results from samples selected in optical or near-infrared bands. The dust emissivity indices, with very few exceptions, are largely consistent with a value of 2. We also compared spectroscopic redshifts to photometric redshifts based on spectral energy distribution templates designed for infrared-bright high-redshift galaxies. While the templates systematically underestimate the redshifts by ∼15 per cent, the inclusion of ALMA data decreases the scatter in the predicted redshifts by a factor of ∼2, illustrating the potential usefulness of these millimetre data for estimating photometric redshifts.

DOI： 10.1093/mnras/stac3771

Possible Systematic Rotation in the Mature Stellar Population of a z = 9.1 Galaxy

Tokuoka, T; Inoue, AK; Hashimoto, T; Ellis, RS; Laporte, N; Sugahara, Y; Matsuo, H; Tamura, Y; Fudamoto, Y; Moriwaki, K; Roberts-Borsani, G; Shimizu, I; Yamanaka, S; Yoshida, N; Zackrisson, E; Zheng, W

ASTROPHYSICAL JOURNAL LETTERS 944 巻 ( 2 ) 頁： 19 2023年2月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal Letters

In Section 4, dynamical modeling, we erroneously omit the redshift dependence of the gravitational lensing effect. For the source redshift of z = 9.1096, the lensing magnification factor predicted by the glafic model (Kawamata et al. 2016) is 17.4 instead of 4.7 in the published article. We have redone the dynamical modeling with the correct lensing effect for the source redshift. The correct results are summarized in the revised Table 1. Figure 2 bottom panel and Figures 3 and 4 are also revised with the correct treatment of the gravitational lensing effect. The conclusion does not change, while the numbers of the best-fit model and their uncertainties have changed.

DOI： 10.3847/2041-8213/acb935

Data science based efficient and automated spectroscopy for submillimeter single-dish telescopes

Taniguchi A., Tamura Y., Ikeda S., Takekoshi T., Kawabe R., Kohno K., Sakai T.

2023 35th General Assembly and Scientific Symposium of the International Union of Radio Science, URSI GASS 2023 2023年

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：2023 35th General Assembly and Scientific Symposium of the International Union of Radio Science, URSI GASS 2023

In this paper, we present a new data scientific approach for efficient and automated spectroscopy with millimeter and submillimeter single-dish telescopes. The proposed approach avoids direct subtraction between two noisy spectra (i.e. on-source and off-source spectra) that is common in the current data reduction: It then offers us to improve the observation sensitivity by a factor of 2 and reduce artificial baseline ripples in parallel with developing observational instruments. We demonstrate such upgrades in the real observed spectra taken by existing large millimeter single-dish telescopes. We finally discuss the application of the proposed approach for the future large submillimeter single-dish telescopes that will yield petabytes of data resulting from sensitive, wide field (1°2), and wide band (>100 GHz) imaging spectroscopy.

DOI： 10.23919/URSIGASS57860.2023.10265475

Wavefront sensor for millimeter/submillimeter-wave adaptive optics based on aperture-plane interferometry

Tamura Yoichi, Kawabe Ryohei, Fukasaku Yuhei, Kimura Kimihiro, Ueda Tetsutaro, Taniguchi Akio, Okada Nozomi, Ogawa Hideo, Hashimoto Ikumi, Minamidani Tetsuhiro, Kawaguchi Noriyuki, Kuno Nario, Togami Yohei, Hagimoto Masato, Nakano Satoya, Matsuda Keiichi, Okumura Sachiko K., Nakamura Tomoko, Kurita Mikio, Takekoshi Tatsuya, Oshima Tai, Onishi Toshikazu, Kohno Kotaro

GROUND-BASED AND AIRBORNE TELESCOPES VIII 11445 巻頁： 114451N 2020年

担当区分：筆頭著者,　責任著者記述言語：英語掲載種別：研究論文（国際会議プロシーディングス）出版者・発行元：Proceedings of SPIE - The International Society for Optical Engineering

We present a concept of a millimeter wavefront sensor that allows real-time sensing of the surface of a groundbased millimeter/submillimeter telescope. It is becoming important for ground-based millimeter/submillimeter astronomy to make telescopes larger with keeping their surface accurate. To establish 'millimetric adaptive optics (MAO)' that instantaneously corrects the wavefront degradation induced by deformation of telescope optics, our wavefront sensor based on radio interferometry measures changes in excess path lengths from characteristic positions on the primary mirror surface to the focal plane. This plays a fundamental role in planed 50-m class submillimeter telescopes such as LST and AtLAST.

DOI： 10.1117/12.2561885

ALMA twenty-six arcmin<sup>2</sup>survey of GOODS-S at one millimeter (ASAGAO) Open Access

Hatsukade B., Kohno K., Yamaguchi Y., Umehata H., Ao Y., Aretxaga I., Caputi K.I., Dunlop J.S., Egami E., Espada D., Fujimoto S., Hayatsu N., Hughes D.H., Ikarashi S., Iono D., Ivison R.J., Kawabe R., Kodama T., Lee M., Matsuda Y., Nakanishi K., Ohta K., Ouchi M., Rujopakarn W., Suzuki T., Tamura Y., Ueda Y., Wang T., Wang W.H., Wilson G.W., Yoshimura Y., Yun M.S.

Proceedings of the International Astronomical Union 頁： 239 - 240 2020年

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Proceedings of the International Astronomical Union

The ALMA twenty-six arcmin2 survey of GOODS-S at one millimeter (ASAGAO) is a deep (1σ ∼61μJy/beam) and wide area (26 arcmin2) survey on a contiguous field at 1.2 mm. By combining with archival data, we obtained a deeper map in the same region (1σ ∼30μJy/beam-1, synthesized beam size 0.59″ × 0.53″), providing the largest sample of sources (25 sources at 5σ, 45 sources at 4.5σ) among ALMA blank-field surveys. The median redshift of the 4.5σ sources is 2.4. The number counts shows that 52% of the extragalactic background light at 1.2 mm is resolved into discrete sources. We create IR luminosity functions (LFs) at z = 1-3, and constrain the faintest luminosity of the LF at 2 < z < 3. The LFs are consistent with previous results based on other ALMA and SCUBA-2 observations, which suggests a positive luminosity evolution and negative density evolution.

DOI： 10.1017/S1743921319009542

First light demonstration of the integrated superconducting spectrometer 査読有り

Endo Akira, Karatsu Kenichi, Tamura Yoichi, Oshima Tai, Taniguchi Akio, Takekoshi Tatsuya, Asayama Shin'ichiro, Bakx Tom J. L. C., Bosma Sjoerd, Bueno Juan, Chin Kah Wuy, Fujii Yasunori, Fujita Kazuyuki, Huiting Robert, Ikarashi Soh, Ishida Tsuyoshi, Ishii Shun, Kawabe Ryohei, Klapwijk Teun M., Kohno Kotaro, Kouchi Akira, Llombart Nuria, Maekawa Jun, Murugesan Vignesh, Nakatsubo Shunichi, Naruse Masato, Ohtawara Kazushige, Laguna Alejandro Pascual, Suzuki Junya, Suzuki Koyo, Thoen David J., Tsukagoshi Takashi, Ueda Tetsutaro, de Visser Pieter J., van der Werf Paul P., Yates Stephen J. C., Yoshimura Yuki, Yurduseven Ozan, Baselmans Jochem J. A.

NATURE ASTRONOMY 3 巻 ( 11 ) 頁： 989 - 996 2019年11月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Nature Astronomy

Ultra-wideband, three-dimensional (3D) imaging spectrometry in the millimeter–submillimeter (mm–submm) band is an essential tool for uncovering the dust-enshrouded portion of the cosmic history of star formation and galaxy evolution1–3. However, it is challenging to scale up conventional coherent heterodyne receivers4 or free-space diffraction techniques5 to sufficient bandwidths (≥1 octave) and numbers of spatial pixels2,3 (>102). Here, we present the design and astronomical spectra of an intrinsically scalable, integrated superconducting spectrometer6, which covers 332–377 GHz with a spectral resolution of F/ΔF ~ 380. It combines the multiplexing advantage of microwave kinetic inductance detectors (MKIDs)7 with planar superconducting filters for dispersing the signal in a single, small superconducting integrated circuit. We demonstrate the two key applications for an instrument of this type: as an efficient redshift machine and as a fast multi-line spectral mapper of extended areas. The line detection sensitivity is in excellent agreement with the instrument design and laboratory performance, reaching the atmospheric foreground photon noise limit on-sky. The design can be scaled to bandwidths in excess of an octave, spectral resolution up to a few thousand and frequencies up to ~1.1 THz. The miniature chip footprint of a few cm2 allows for compact multi-pixel spectral imagers, which would enable spectroscopic direct imaging and large-volume spectroscopic surveys that are several orders of magnitude faster than what is currently possible1–3.

DOI： 10.1038/s41550-019-0850-8

Gas filaments of the cosmic web located around active galaxies in a protocluster 査読有り

Umehata H., Fumagalli M., Smail I., Matsuda Y., Swinbank A. M., Cantalupo S., Sykes C., Ivison R. J., Steidel C. C., Shapley A. E., Vernet J., Yamada T., Tamura Y., Kubo M., Nakanishi K., Kajisawa M., Hatsukade B., Kohno K.

SCIENCE 366 巻 ( 6461 ) 頁： 97 - + 2019年10月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Science

Cosmological simulations predict that the Universe contains a network of intergalactic gas filaments, within which galaxies form and evolve. However, the faintness of any emission from these filaments has limited tests of this prediction. We report the detection of rest-frame ultraviolet Lyman-a radiation from multiple filaments extending more than one megaparsec between galaxies within the SSA22 protocluster at a redshift of 3.1. Intense star formation and supermassive black-hole activity is occurring within the galaxies embedded in these structures, which are the likely sources of the elevated ionizing radiation powering the observed Lyman-a emission. Our observations map the gas in filamentary structures of the type thought to fuel the growth of galaxies and black holes in massive protoclusters.

DOI： 10.1126/science.aaw5949

Big Three Dragons: A z=7.15 Lyman-break galaxy detected in [O III] 88 μm, [C II] 158 μm, and dust continuum with ALMA 査読有り

Hashimoto Takuya, Inoue Akio K., Mawatari Ken, Tamura Yoichi, Matsuo Hiroshi, Furusawa Hisanori, Harikane Yuichi, Shibuya Takatoshi, Knudsen Kirsten K., Kohno Kotaro, Ono Yoshiaki, Zackrisson Erik, Okamoto Takashi, Kashikawa Nobunari, Oesch Pascal A., Ouchi Masami, Ota Kazuaki, Shimizu Ikkoh, Taniguchi Yoshiaki, Umehata Hideki, Watson Darach

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 71 巻 ( 4 ) 2019年8月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

We present new ALMA observations and physical properties of a Lyman break galaxy at z = 7.15. Our target, B14-65666, has a bright ultra-violet (UV) absolute magnitude, MUV ≈ -22.4, and has been spectroscopically identified in Lyα with a small rest-frame equivalent width of ≈4 Å. A previous Hubble Space TElescope (HST) image has shown that the target is composed of two spatially separated clumps in the rest-frame UV. With ALMA, we have newly detected spatially resolved [O iii] 88 μm, [C ii] 158 μm, and their underlying dust continuum emission. In the whole system of B14-65666, the [O iii] and [C ii] lines have consistent redshifts of 7.1520 ± 0.0003, and the [O iii] luminosity, (34.4 ± 4.1) × 108 Lo, is about three times higher than the [C ii] luminosity, (11.0 ± 1.4) × 108 Lo. With our two continuum flux densities, the dust temperature is constrained to be Td ≈ 50-60 K under the assumption of a dust emissivity index of βd = 2.0-1.5, leading to a large total infrared luminosity of LTIR ≈ 1 × 1012 Lo. Owing to our high spatial resolution data, we show that the [O iii] and [C ii] emission can be spatially decomposed into two clumps associated with the two rest-frame UV clumps whose spectra are kinematically separated by ≈200 km s-1. We also find these two clumps have comparable UV, infrared, [O iii], and [C ii] luminosities. Based on these results, we argue that B14-65666 is a starburst galaxy induced by a major merger. The merger interpretation is also supported by the large specific star formation rate (defined as the star formation rate per unit stellar mass), sSFR = 260+119-57:Gyr-1, inferred from our SED fitting. Probably, a strong UV radiation field caused by intense star formation contributes to its high dust temperature and the [O iii]-to-[C ii] luminosity ratio.

DOI： 10.1093/pasj/psz049

The onset of star formation 250 million years after the Big Bang 査読有り

Hashimoto Takuya, Laporte Nicolas, Mawatari Ken, Ellis Richard S., Inoue Akio K., Zackrisson Erik, Roberts-Borsani Guido, Zheng Wei, Tamura Yoichi, Bauer Franz E., Fletcher Thomas, Harikane Yuichi, Hatsukade Bunyo, Hayatsu Natsuki H., Matsuda Yuichi, Matsuo Hiroshi, Okamoto Takashi, Ouchi Masami, Pello Roser, Rydberg Claes-Erik, Shimizu Ikkoh, Taniguchi Yoshiaki, Umehata Hideki, Yoshida Naoki

NATURE 557 巻 ( 7705 ) 頁： 392 - + 2018年5月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Nature

A fundamental quest of modern astronomy is to locate the earliest galaxies and study how they influenced the intergalactic medium a few hundred million years after the Big Bang 1-3 . The abundance of star-forming galaxies is known to decline 4,5 from redshifts of about 6 to 10, but a key question is the extent of star formation at even earlier times, corresponding to the period when the first galaxies might have emerged. Here we report spectroscopic observations of MACS1149-JD1 6, a gravitationally lensed galaxy observed when the Universe was less than four per cent of its present age. We detect an emission line of doubly ionized oxygen at a redshift of 9.1096 ± 0.0006, with an uncertainty of one standard deviation. This precisely determined redshift indicates that the red rest-frame optical colour arises from a dominant stellar component that formed about 250 million years after the Big Bang, corresponding to a redshift of about 15. Our results indicate that it may be possible to detect such early episodes of star formation in similar galaxies with future telescopes.

DOI： 10.1038/s41586-018-0117-z

ADF22-WEB: A giant barred spiral starburst galaxy in the z=3.1 SSA22 protocluster core Open Access

Umehata, H; Steidel, CC; Smail, I; Swinbank, M; Monson, EB; Rosario, D; Lehmer, BD; Nakanishi, K; Kubo, M; Iono, D; Alexander, DM; Kohno, K; Tamura, Y; Ivison, RJ; Saito, T; Mitsuhashi, I; Huang, S; Matsuda, Y

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 2025年3月

RIOJA. Complex Dusty Starbursts in a Major Merger B14-65666 at <i>z</i>=7.15 Open Access

Sugahara, Y; Alvarez-Márquez, J; Hashimoto, T; Colina, L; Inoue, AK; Costantin, L; Fudamoto, Y; Mawatari, K; Ren, YW; Arribas, S; Bakx, TJLC; Blanco-Prieto, C; Ceverino, D; Gómez, AC; Hagimoto, M; Hashigaya, T; Marques-Chaves, R; Matsuo, H; Nakazato, Y; Pereira-Santaella, M; Tamura, Y; Usui, M; Yoshida, N

ASTROPHYSICAL JOURNAL 981 巻 ( 2 ) 2025年3月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present JWST NIRCam imaging of B14-65666 (“Big Three Dragons”), a bright Lyman-break galaxy system (MUV = −22.5 mag) at z = 7.15. The high angular resolution of NIRCam reveals the complex morphology of two galaxy components: galaxy E has a compact core (E-core), surrounded by diffuse, extended, rest-frame optical emission, which is likely to be tidal tails; and galaxy W has a clumpy and elongated morphology with a blue UV slope (βUV = −2.2 ± 0.1). The flux excess, F356W − F444W, peaks at the E-core ( 1.0 5 − 0.09 + 0.08 mag), tracing the presence of strong [O iii] λλ4960,5008 emission. Atacama Large Millimeter/submillimeter Array archival data show that the bluer galaxy W is brighter in dust continua than the redder galaxy E, while the tails are bright in [O iii] 88 μm. The UV/optical and submillimeter spectral energy distribution (SED) fitting confirms that B14-65666 is a major merger in a starburst phase as derived from the stellar mass ratio (3:1 to 2:1) and the star formation rate, ≃1 dex higher than the star formation main sequence at the same redshift. Galaxy E is a dusty (AV = 1.2 ± 0.1 mag) starburst with a possible high dust temperature (≥63-68 K). Galaxy W would have a low dust temperature (≤27-33 K) or patchy stellar-and-dust geometry, as suggested by the IR excess and βUV diagram. The high optical-to-far-IR [O iii] line ratio of the E-core shows its lower gas-phase metallicity (≃0.2-0.4 Z⊙) than galaxy W. These results agree with a scenario where major mergers disturb morphology and induce nuclear dusty starbursts triggered by less-enriched inflows. B14-65666 shows a picture of complex stellar buildup processes during major mergers in the epoch of reionization.

DOI： 10.3847/1538-4357/adb02a

Large Molecular and Dust Reservoir of a Gravitationally Lensed Submillimeter Galaxy behind the Lupus I Molecular Cloud Open Access

Tamura, Y; Taniguchi, A; Bakx, TJLC; De Gregorio-Monsalvo, I; Hagimoto, M; Ikarashi, S; Kawabe, R; Kohno, K; Nakanishi, K; Takekoshi, T; Shimajiri, Y; Tsukagoshi, T; Hatsukade, B; Iono, D; Matsuhara, H; Saigo, K; Saito, M

ASTROPHYSICAL JOURNAL 981 巻 ( 1 ) 2025年3月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We report the Australian Telescope Compact Array and Nobeyama 45 m telescope detection of a remarkably bright (S1.1mm = 44 mJy) submillimeter galaxy MM J154506.4−344318 in emission lines at 48.5 and 97.0 GHz, respectively. We also identify part of an emission line at ≈218.3 GHz using the Atacama Large Millimeter/submillimeter Array (ALMA). Together with photometric redshift estimates and the ratio between the line and infrared luminosities, we conclude that the emission lines are most likely to be the J = 2-1, 4-3, and 9-8 transitions of 12CO at redshift z = 3.753 ± 0.001. ALMA 1.3 mm continuum imaging reveals an arc and a spot separated by an angular distance of 1 . ″ 6 , indicative of a strongly lensed dusty star-forming galaxy with respective molecular and dust masses of log M mol / M ⊙ ≈ 11.5 and log M dust / M ⊙ ≈ 9.4 after being corrected for ≈6.6× gravitational magnification. The inferred dust-to-gas mass ratio is found to be high (≈0.0083) among coeval dusty star-forming galaxies, implying the presence of a massive, chemically enriched reservoir of cool interstellar medium at z ≈ 4, or 1.6 Gyr after the Big Bang.

DOI： 10.3847/1538-4357/adb1b9

JWST, ALMA, and Keck Spectroscopic Constraints on the UV Luminosity Functions at <i>z</i> ∼ 7-14: Clumpiness and Compactness of the Brightest Galaxies in the Early Universe Open Access

Harikane, Y; Inoue, AK; Ellis, RS; Ouchi, M; Nakazato, Y; Yoshida, N; Ono, Y; Sun, FW; Sato, RA; Ferrami, G; Fujimoto, S; Kashikawa, N; Mcleod, DJ; Pérez-González, PG; Sawicki, M; Sugahara, Y; Xu, Y; Yamanaka, S; Carnall, AC; Cullen, F; Dunlop, JS; Egami, E; Grogin, N; Isobe, Y; Koekemoer, AM; Laporte, N; Lee, CH; Magee, D; Matsuo, H; Matsuoka, Y; Mawatari, K; Nakajima, K; Nakane, M; Tamura, Y; Umeda, H; Yanagisawa, H

ASTROPHYSICAL JOURNAL 980 巻 ( 1 ) 2025年2月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present the number densities and physical properties of the bright galaxies spectroscopically confirmed at z ∼ 7-14. Our sample is composed of 60 galaxies at zspec ∼ 7-14, including recently confirmed galaxies at zspec = 12.34-14.18 with JWST, as well as new confirmations at zspec = 6.583-7.643 with −24 < MUV < −21 mag using ALMA and Keck. Our JWST/NIRSpec observations have also revealed that very bright galaxy candidates at z ∼ 10-13 identified from ground-based telescope images before JWST are passive galaxies at z ∼ 3-4, emphasizing the necessity of strict screening and spectroscopy in the selection of the brightest galaxies at z > 10. The UV luminosity functions derived from these spectroscopic results are consistent with a double power-law function, showing tensions with theoretical models at the bright end. To understand the origin of the overabundance of bright galaxies, we investigate their morphologies using JWST/NIRCam high-resolution images obtained in various surveys, including PRIMER and COSMOS-Web. We find that ∼70% of the bright galaxies at z ∼ 7 exhibit clumpy morphologies with multiple subcomponents, suggesting merger-induced starburst activity, which is consistent with SED fitting results showing bursty star formation histories. At z ≳ 10, bright galaxies are classified into two types of galaxies: extended ones with weak high-ionization emission lines, and compact ones with strong high-ionization lines including N iv]λ1486, indicating that at least two different processes (e.g., merger-induced starburst and compact star formation/AGN) are shaping the physical properties of the brightest galaxies at z ≳ 10 and are responsible for their overabundance.

DOI： 10.3847/1538-4357/ad9b2c

Detection of the [O i] 63 μm emission line from the z=6.04 quasar J2054-0005 Open Access

Ishii, N; Hashimoto, T; Ferkinhoff, C; Rybak, M; Inoue, AK; Michiyama, T; Donevski, D; Fujimoto, S; Salak, D; Kuno, N; Matsuo, H; Mawatari, K; Tamura, Y; Izumi, T; Nagao, T; Nakazato, Y; Osone, W; Sugahara, Y; Usui, M; Wakasugi, K; Yajima, H; Bakx, TJLC; Fudamoto, Y; Meyer, RA; Walter, F; Yoshida, N

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 77 巻 ( 1 ) 頁： 139 - 148 2024年12月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

We report the highest-redshift detection of [O i] 63 m from a luminous quasar, J20540005, at based on the Atacama Large Millimeter/sub-millimeter Array (ALMA) Band 9 observations. The [O i] 63 m line luminosity is, corresponding to the [O i] 63 m-to-far-infrared luminosity ratio of 6.7, which is consistent with the value obtained in the local Universe. Remarkably, [O i] 63 m is as bright as [C ii] 158 m, resulting in the [O i]-to-[C ii] line luminosity ratio of. Based on a careful comparison of the luminosity ratios of [O i] 63 m, [C ii] 158 m, and dust continuum emission to models of photodissociation regions, we find that J20540005 has a gas density and an incident far-ultraviolet radiation field of, showing that [O i] 63 m serves as an important coolant of the dense and warm gas in J20540005. A close examination of the [O i] and [C ii] line profiles suggests that the [O i] line may be partially self-absorbed; however, deeper observations are needed to verify this conclusion. Regardless, the gas density and incident radiation field are in broad agreement with the values obtained in nearby star-forming galaxies and objects with [O i] 63 m observations at -3 with the Herschel Space Observatory. These results demonstrate the power of ALMA high-frequency observations targeting [O i] 63 m to examine the properties of photodissociation regions in high-redshift galaxies.

DOI： 10.1093/pasj/psae105

A novel high-z submm galaxy efficient line survey in ALMA Bands 3 through 8-an ANGELS pilot Open Access

Bakx, TJLC; Amvrosiadis, A; Bendo, GJ; Algera, HSB; Serjeant, S; Bonavera, L; Borsato, E; Chen, X; Cox, P; Gonzalez-Nuevo, J; Hagimoto, M; Harrington, KC; Ivison, RJ; Kamieneski, P; Marchetti, L; Riechers, DA; Tsukui, T; van der Werf, PP; Yang, C; Zavala, JA; Andreani, P; Berta, S; Cooray, AR; De Zotti, G; Eales, S; Ikeda, R; Knudsen, KK; Mitsuhashi, ; Negrello, M; Neri, R; Omont, A; Scott, D; Tamura, Y; Temi, P; Urquhart, SA

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 535 巻 ( 2 ) 頁： 1533 - 1574 2024年11月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society

We use the Atacama Large sub/Millimetre Array (ALMA) to efficiently observe spectral lines across Bands 3, 4, 5, 6, 7, and 8 at high-resolution (0.5–0.1 arcsec) for 16 bright southern Herschel sources at 1.5 < z < 4.2. With only six and a half hours of observations, we reveal 66 spectral lines in 17 galaxies. These observations detect emission from CO (3−2) to CO(18−17), as well as atomic ([C I](1−0), (2−1), [O I] 145 μm and [N II] 205 μm) lines. Additional molecular lines are seen in emission (H2O and H2O+) and absorption (OH+ and CH+). The morphologies based on dust continuum ranges from extended sources to strong lensed galaxies with magnifications between 2 and 30. CO line transitions indicate a diverse set of excitation conditions with a fraction of the sources (∼ 35 per cent) showcasing dense, warm gas. The resolved gas to star formation surface densities vary strongly per source, and suggest that the observed diversity of dusty star-forming galaxies could be a combination of lensed, compact dusty starbursts and extended, potentially merging galaxies. The predicted gas depletion time-scales are consistent with 100 Myr to 1 Gyr, but require efficient fuelling from the extended gas reservoirs onto the more central starbursts, in line with the Doppler-shifted absorption lines that indicate inflowing gas for two out of six sources. This pilot paper explores a successful new method of observing spectral lines in large samples of galaxies, supports future studies of larger samples, and finds that the efficiency of this new observational method will be further improved with the planned ALMA Wideband Sensitivity Upgrade.

DOI： 10.1093/mnras/stae2409

JWST/NIRSpec spectroscopy of intermediate-mass quiescent galaxies at z ∼ 3-4 Open Access

Sato, RA; Inoue, AK; Harikane, Y; Shimakawa, R; Sugahara, Y; Tamura, Y; Hashimoto, T; Ito, K; Yamanaka, S; Mawatari, K; Fudamoto, Y; Ren, YW

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 534 巻 ( 4 ) 頁： 3552 - 3564 2024年10月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society

We present the analysis of three intermediate-mass quiescent galaxies (QGs) with stellar masses of ∼1010 M at redshifts z ∼ 3–4 using NIRSpec low-resolution spectroscopy. Utilizing the spectral energy distribution fitting code BAGPIPES, we confirm these target galaxies are consistent with quiescent population, with their specific star formation rates falling below 2 dex the star-forming main sequence at the same redshifts. Additionally, we identify these QGs to be less massive than those discovered in previous works, particularly prior to the JWST era. Two of our target galaxies exhibit the potentially blended H α + [N II] emission line within their spectra with signal-to-noise ratio >5. We discuss whether this feature comes from an active galactic nucleus (AGN) or star formation, although future high-resolution spectroscopy is required to reach a conclusion. One of the target galaxies is covered by JWST/NIRCam imaging of the Public Release IMaging for Extragalactic Research survey. Using the 2D profile fitting code GALFIT, we examine its morphology, revealing a disc-like profile with a Sérsic index of n = 1.1 ± 0.1. On the size–mass relation, we find a potential distinction between less massive (log10 (M∗/M) < 10.3) and massive (log10 (M∗/M) > 10.3) QGs in their evolutionary pathways. The derived quenching time-scales for our targets are less than 1 Gyr. This may result from these galaxies being quenched by AGN feedback, supporting the AGN scenario of the emission line features.

DOI： 10.1093/mnras/stae2300

Gas conditions of a star-formation selected sample in the first billion years 査読有り国際共著国際誌 Open Access

Bakx, TJLC; Algera, HSB; Venemans, B; Sommovigo, L; Fujimoto, S; Carniani, S; Hagimoto, M; Hashimoto, T; Inoue, AK; Salak, D; Serjeant, S; Vallini, L; Eales, S; Ferrara, A; Fudamoto, Y; Imamura, C; Inoue, S; Knudsen, KK; Matsuo, H; Sugahara, Y; Tamura, Y; Taniguchi, A; Yamanaka, S

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 532 巻 ( 2 ) 頁： 2270 - 2288 2024年7月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society

We present Atacama Large Millimetre/submillimetre Array (ALMA) observations of the [O iii] 88 emission of a sample of thirteen galaxies at to 7.6 selected as [C ii]-emitting companion sources of quasars. To disentangle the origins of the luminous Oxygen line in the Universe, we looked at emission-line galaxies that are selected through an excellent star-formation tracer [C ii] with star-formation rates between 9 and 162. Direct observations reveal [O iii] emission in just a single galaxy (), and a stacked image shows no [O iii] detection, providing deep upper limits on the ratios in the Universe (at). While the fidelity of this sample is high, no obvious optical/near-infrared counterpart is seen in the JWST imaging available for four galaxies. Additionally accounting for low-z CO emitters, line stacking shows that our sample-wide result remains robust: The enhanced reported in the first billion years of the Universe is likely due to the selection towards bright, blue Lyman-break galaxies with high surface star-formation rates or young stellar populations. The deep upper limit on the rest-frame 90 μm continuum emission (Jy at), implies a low average dust temperature (K) and high-dust mass (). As more normal galaxies are explored in the early Universe, synergy between JWST and ALMA is fundamental to further investigate the ISM properties of the a broad range of samples of high-z galaxies.

DOI： 10.1093/mnras/stae1613

A dusty protocluster surrounding the binary galaxy HerBS-70 at z=2.3 査読有り国際共著国際誌 Open Access

Bakx, TJLC; Berta, S; Dannerbauer, H; Cox, P; Butler, KM; Hagimoto, M; Hughes, DH; Riechers, DA; van der Werf, PP; Yang, C; Baker, AJ; Beelen, A; Bendo, GJ; Borsato, E; Buat, ; Cooray, AR; Dunne, L; Dye, S; Eales, S; Gavazzi, R; Harris, A; Ismail, D; Ivison, RJ; Jones, B; Krips, M; Lehnert, MD; Marchetti, L; Messias, H; Negrello, M; Neri, R; Omont, A; Perez-Fournon, ; Nanni, A; Chartab, N; Serjeant, S; Stanley, F; Tamura, Y; Urquhart, SA; Vlahakis, C; Weiss, A; Young, AJ

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 530 巻 ( 4 ) 頁： 4578 - 4596 2024年5月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society

We report on deep SCUBA-2 observations at 850 μm and NOrthern Extended Millimetre Array (NOEMA) spectroscopic measurements at 2 mm of the environment surrounding the luminous, massive (M∗ ≈ 2 × 1011 M☉) Herschel-selected source HerBS-70. This source was revealed by previous NOEMA observations to be a binary system of dusty star-forming galaxies at z = 2.3, with the east component (HerBS-70E) hosting an active galactic nucleus. The SCUBA-2 observations detected, in addition to the binary system, 21 sources at >3.5σ over an area of ∼25 square comoving Mpc with a sensitivity of 1σ850 = 0.75 mJy. The surface density of continuum sources around HerBS-70 is three times higher than for field galaxies. The NOEMA spectroscopic measurements confirm the protocluster membership of three of the nine brightest sources through their CO(4–3) line emission, yielding a volume density 36 times higher than for field galaxies. All five confirmed sub-mm galaxies in the HerBS-70 system have relatively short gas depletion times (80−500 Myr), indicating the onset of quenching for this protocluster core due to the depletion of gas. The dark matter halo mass of the HerBS-70 system is estimated around 5 × 1013 M☉, with a projected current-day mass of 1015 M☉, similar to the local Virgo and Coma clusters. These observations support the claim that DSFGs, in particular the ones with observed multiplicity, can trace cosmic overdensities.

DOI： 10.1093/mnras/stae1155

JWST and ALMA Multiple-line Study in and around a Galaxy at <i>z</i>=8.496: Optical to Far-Infrared Line Ratios and the Onset of an Outflow Promoting Ionizing Photon Escape 査読有り国際共著国際誌 Open Access

Fujimoto, S; Ouchi, M; Nakajima, K; Harikane, Y; Isobe, Y; Brammer, G; Oguri, M; Giménez-Arteaga, C; Heintz, KE; Kokorev, V; Bauer, FE; Ferrara, A; Kojima, T; Lagos, CD; Laura, S; Schaerer, D; Shimasaku, K; Hatsukade, B; Kohno, K; Sun, FW; Valentino, F; Watson, D; Fudamoto, Y; Inoue, AK; González-López, J; Koekemoer, AM; Knudsen, K; Lee, MM; Magdis, GE; Richard, J; Strait, VB; Sugahara, Y; Tamura, Y; Toft, S; Umehata, H; Walth, G

ASTROPHYSICAL JOURNAL 964 巻 ( 2 ) 頁： 146 2024年4月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：American Astronomical Society

<jats:title>Abstract</jats:title>
<jats:p>We present Atacama Large Millimeter/submillimeter Array (ALMA) deep spectroscopy for a lensed galaxy at <jats:italic>z</jats:italic>
<jats:sub>spec</jats:sub> = 8.496 with <jats:inline-formula>
<jats:tex-math>

</jats:tex-math>
<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll">
<mml:mi>log</mml:mi>
<mml:mo stretchy="false">(</mml:mo>
<mml:msub>
<mml:mrow>
<mml:mi>M</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>star</mml:mi>
</mml:mrow>
</mml:msub>
<mml:mrow>
<mml:mo stretchy="true">/</mml:mo>
</mml:mrow>
<mml:msub>
<mml:mrow>
<mml:mi>M</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mo>⊙</mml:mo>
</mml:mrow>
</mml:msub>
<mml:mo stretchy="false">)</mml:mo>
<mml:mo>∼</mml:mo>
<mml:mn>7.8</mml:mn>
</mml:math>
</jats:inline-formula> whose optical nebular lines and stellar continuum are detected by JWST/NIRSpec and NIRCam Early Release Observations in the field of SMACS J0723.3–7327. Our ALMA spectrum shows [O <jats:sc>iii</jats:sc>] 88 <jats:italic>μ</jats:italic>m and [C <jats:sc>ii</jats:sc>] 158 <jats:italic>μ</jats:italic>m line detections at 4.0<jats:italic>σ</jats:italic> and 4.5<jats:italic>σ</jats:italic>, respectively. The redshift and position of the [O <jats:sc>iii</jats:sc>] line coincide with those of the JWST source, while the [C <jats:sc>ii</jats:sc>] line is blueshifted by 90 km s<jats:sup>−1</jats:sup> with a spatial offset of 0.″5 (≈0.5 kpc in the source plane) from the centroid of the JWST source. The NIRCam F444W image, including [O <jats:sc>iii</jats:sc>] <jats:italic>λ</jats:italic>5007 and H<jats:italic>β</jats:italic> line emission, spatially extends beyond the stellar components by a factor of >8. This indicates that the <jats:italic>z</jats:italic> = 8.5 galaxy has already experienced strong outflows as traced by extended [O <jats:sc>iii</jats:sc>] <jats:italic>λ</jats:italic>5007 and offset [C <jats:sc>ii</jats:sc>] emission, which would promote ionizing photon escape and facilitate reionization. With careful slit-loss corrections and the removal of emission spatially outside the galaxy, we evaluate the [O <jats:sc>iii</jats:sc>] 88 <jats:italic>μ</jats:italic>m/<jats:italic>λ</jats:italic>5007 line ratio, and derive the electron density <jats:italic>n</jats:italic>
<jats:sub>e</jats:sub> by photoionization modeling to be <jats:inline-formula>
<jats:tex-math>

</jats:tex-math>
<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll">
<mml:msubsup>
<mml:mrow>
<mml:mn>220</mml:mn>
</mml:mrow>
<mml:mrow>
<mml:mo>−</mml:mo>
<mml:mn>130</mml:mn>
</mml:mrow>
<mml:mrow>
<mml:mo>+</mml:mo>
<mml:mn>230</mml:mn>
</mml:mrow>
</mml:msubsup>
</mml:math>
</jats:inline-formula> cm<jats:sup>−3</jats:sup>, which is comparable with those of <jats:italic>z</jats:italic> ∼ 2–3 galaxies. We estimate an [O <jats:sc>iii</jats:sc>] 88 <jats:italic>μ</jats:italic>m/[C <jats:sc>ii</jats:sc>] 158 <jats:italic>μ</jats:italic>m line ratio in the galaxy of >4, as high as those of known <jats:italic>z</jats:italic> ∼ 6–9 galaxies. This high [O <jats:sc>iii</jats:sc>] 88 <jats:italic>μ</jats:italic>m/[C <jats:sc>ii</jats:sc>] 158 <jats:italic>μ</jats:italic>m line ratio is generally explained by the high <jats:italic>n</jats:italic>
<jats:sub>e</jats:sub> as well as the low metallicity (<jats:inline-formula>
<jats:tex-math>

</jats:tex-math>
<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll">
<mml:msub>
<mml:mrow>
<mml:mi>Z</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>gas</mml:mi>
</mml:mrow>
...

DOI： 10.3847/1538-4357/ad235c

Large-scale Mapping Observations of DCN and DCO+ toward Orion KL 査読有り国際共著

Taniguchi K., Rayalacheruvu P., Yonetsu T., Takekoshi T., Hatsukade B., Kohno K., Oshima T., Tamura Y., Yoshimura Y., Gómez-Rivera V., Rojas-García S., Gómez-Ruiz A.I., Hughes D.H., Schloerb F.P., Majumdar L., Saito M., Rodríguez-Montoya I., Sánchez-Arguelles D., Kawabe R.

The Astrophysical Journal 963 巻 ( 1 ) 頁： 12 - 12 2024年2月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present emission maps ( 1 .′ 5 × 1 .′ 5 scale, corresponding to 0.18 pc) of the DCN (J = 2 − 1) and DCO+ (J = 2 − 1) lines in the 2 mm band toward the Orion KL region obtained with the 2 mm receiver system named B4R installed on the Large Millimeter Telescope. The DCN emission shows a peak at the Orion KL hot core position, whereas no DCO+ emission has been detected there. The DCO+ emission shows enhancement at the west side of the hot core, which is well shielded from the UV radiation from OB massive stars in the Trapezium cluster. We have derived the abundance ratio of DCN/DCO+ at three representative positions where both species have been detected. The gas components with V LSR ≈ 7.5-8.7 km s−1 are associated with low abundance ratios of ∼4-6, whereas much higher abundance ratios (∼22-30) are derived for the gas components with V LSR ≈ 9.2-11.6 km s−1. We have compared the observed abundance ratio to our chemical models and found that the observed differences in the DCN/DCO+ abundance ratios are explained by different densities.

DOI： 10.3847/1538-4357/ad1e5a

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/ad1e5a/pdf

Molecular Outflow in the Reionization-epoch Quasar J2054-0005 Revealed by OH 119 μm Observations 査読有り国際共著

Salak, D; Hashimoto, T; Inoue, AK; Bakx, TJLC; Donevski, D; Tamura, Y; Sugahara, Y; Kuno, N; Miyamoto, Y; Fujimoto, S; Suphapolthaworn, S

The Astrophysical Journal 962 巻 ( 1 ) 2024年2月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

Molecular outflows are expected to play a key role in galaxy evolution at high redshift. To study the impact of outflows on star formation at the epoch of reionization, we performed sensitive Atacama Large Millimeter/submillimeter Array observations of OH 119 μm toward J2054-0005, a luminous quasar at z = 6.04. The OH line is detected and exhibits a P-Cygni profile that can be fitted with a broad blueshifted absorption component, providing unambiguous evidence of an outflow, and an emission component at near-systemic velocity. The mean and terminal outflow velocities are estimated to be v out ≈ 670 and 1500 km s−1, respectively, making the molecular outflow in this quasar one of the fastest at the epoch of reionization. The OH line is marginally spatially resolved for the first time in a quasar at z > 6, revealing that the outflow extends over the central 2 kpc region. The mass outflow rate is comparable to the star formation rate ( M ̇ out / SFR ∼ 2 ), indicating rapid (∼107 yr) quenching of star formation. The mass outflow rate in a sample of star-forming galaxies and quasars at 4 < z < 6.4 exhibits a positive correlation with the total infrared luminosity, although the scatter is large. Owing to the high outflow velocity, a large fraction (up to ∼50%) of the outflowing molecular gas may be able to escape from the host galaxy into the intergalactic medium.

DOI： 10.3847/1538-4357/ad0df5

The Extended [C <sc>ii</sc>] under Construction? Observation of the Brightest High-<i>z</i> Lensed Star-forming Galaxy at <i>z</i>=6.2 査読有り国際共著国際誌 Open Access

Fudamoto, Y; Inoue, AK; Coe, D; Welch, B; Acebron, A; Ricotti, M; Mandelker, N; Windhorst, RA; Xu, XF; Sugahara, Y; Bauer, FE; Bradac, M; Bradley, LD; Diego, JM; Florian, M; Frye, B; Fujimoto, S; Hashimoto, T; Henry, A; Mahler, G; Oesch, PA; Ravindranath, S; Rigby, J; Sharon, K; Strait, V; Tamura, Y; Trenti, M; Vanzella, E; Zackrisson, E; Zitrin, A

ASTROPHYSICAL JOURNAL 961 巻 ( 1 ) 頁： 71 2024年1月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present results of [C II] 158 μm emission line observations, and report the spectroscopic redshift confirmation of a strongly lensed (μ ∼ 20) star-forming galaxy, MACS0308-zD1 at z = 6.2078 ± 0.0002. The [C II] emission line is detected with a signal-to-noise ratio >6 within the rest-frame UV-bright clump of the lensed galaxy (zD1.1) and exhibits multiple velocity components; the narrow [C II] has a velocity full width half maximum (FWHM) of 110 ± 20 km s−1, while broader [C II] is seen with an FWHM of 230 ± 50 km s−1. The broader [C II] component is blueshifted (−80 ± 20 km s−1) with respect to the narrow [C II] component, and has a morphology that extends beyond the UV-bright clump. We find that, while the narrow [C II] emission is most likely associated with zD1.1, the broader component is possibly associated with a physically distinct gas component from zD1.1 (e.g., outflowing or inflowing gas). Based on the nondetection of λ158μm dust continuum, we find that MACS0308-zDl's star formation activity occurs in a dust-free environment indicated by a strong upper limit of infrared luminosity ≲9 × 108 Le. Targeting this strongly lensed faint galaxy for follow-up Atacama Large Millimeter/submillimeter Array and JWST observations will be crucial to characterize the details of typical galaxy growth in the early Universe.

DOI： 10.3847/1538-4357/ad0f95

Development Status of Wideband Millimeter-Wave Receivers for LMT-FINER 国際共著国際誌 Open Access

Kang, H; Kojima, T; Sakai, T; Tamura, Y; Tetsuka, A; Masui, S; Takekoshi, T

MILLIMETER, SUBMILLIMETER, AND FAR-INFRARED DETECTORS AND INSTRUMENTATION FOR ASTRONOMY XII, PT 1 13102 巻 2024年

記述言語：英語掲載種別：研究論文（国際会議プロシーディングス）出版者・発行元：Proceedings of SPIE - The International Society for Optical Engineering

Spectroscopic observations of the far-infrared [O iii] 88 µm and [C ii] 158 µm lines present a pathway to explore the mechanisms of the emergence of massive galaxies in the epoch of reionization and beyond, which is one of the most fundamental questions in astronomy. To address this question, the Far-Infrared Nebular Emission Receiver (FINER) project is developing two wideband dual-polarization sideband-separating heterodyne receivers at 120-210 GHz and 210-360 GHz for the Large Millimeter Telescope (LMT) in Mexico. Compared with Atacama Large Millimeter/submillimeter Array (ALMA), LMT provides 40% of ALMA's light-collecting area and a similar atmospheric transmittance, but FINER plans to have an instantaneous intermediate frequency (IF) of 3-21 GHz per sideband per polarization which is five times wider than current ALMA's bandwidth. Therefore, FINER is going to offer cutting-edge spectral scanning capability in the next several years. The project is currently in an active development phase. In this proceeding, the latest development status for FINER, including the optics, wideband waveguide components as well as low-noise superconductor-insulator-superconductor (SIS) mixers is reported.

DOI： 10.1117/12.3018190

A 10.24-GHz-wide digital spectrometer array system for LMT-FINER: system design and laboratory performance verification 国際共著国際誌 Open Access

Hagimoto, M; Taniguchi, A; Tamura, Y; Okauchi, N; Kawamoto, H; Nakajima, T; Hikosaka, T; Harada, K; Taniguchi, T; Kamazaki, T; Sakai, T; Tanaka, K; Kawabe, R

MILLIMETER, SUBMILLIMETER, AND FAR-INFRARED DETECTORS AND INSTRUMENTATION FOR ASTRONOMY XII, PT 1 13102 巻 2024年

記述言語：英語掲載種別：研究論文（国際会議プロシーディングス）出版者・発行元：Proceedings of SPIE - The International Society for Optical Engineering

For efficient spectroscopic redshift identification of early galaxies in the northern hemisphere, we aim to combine the Large Millimeter Telescope (LMT) with a wide-band heterodyne receiver, FINER, which will cover radio frequencies of 120-360 GHz and offer a 3-21 GHz intermediate frequency (IF) per sideband and polarization. To take full advantage of such wide IFs, we present a novel 10.24-GHz-wide digital spectrometer, DRS4 (Elecs Industry Co., Ltd.). It incorporates 20.48 Gsps samplers with an FPGA-based digital signal processing module. To mitigate the noise contamination from the image sideband, it is equipped with a digital sideband separation function to improve the sideband rejection up to 25 dB. Laboratory performance evaluations show that it exhibits an Allan time of at least ∼ 100 s and a total power dynamic range of at least 7 dB. These results demonstrate its capability of instantaneously wide-band spectroscopy toward high-redshift galaxies with position-switching observations.

DOI： 10.1117/12.3018296

J0107a: A Barred Spiral Dusty Star-forming Galaxy at z = 2.467 査読有り国際共著

Huang, S; Kawabe, R; Kohno, K; Saito, T; Mizukoshi, S; Iono, D; Michiyama, T; Tamura, Y; Hayward, CC; Umehata, H

The Astrophysical Journal Letters 958 巻 ( 2 ) 2023年12月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal Letters

Dusty star-forming galaxies (DSFGs) are among the most massive and active star-forming galaxies during the cosmic noon. Theoretical studies have proposed various formation mechanisms of DSFGs, including major merger-driven starbursts and secular star-forming disks. Here, we report J0107a, a bright (∼8 mJy at observed-frame 888 μm) DSFG at z = 2.467 that appears to be a gas-rich massive disk and might be an extreme case of the secular disk scenario. J0107a has a stellar mass M ⋆ ∼ 5 × 1011 M ⊙, molecular gas mass M mol ≳ 1011 M ⊙, and a star formation rate of ∼500M ⊙ yr−1. J0107a does not have a gas-rich companion. The rest-frame 1.28 μm JWST NIRCam image of J0107a shows a grand-design spiral with a prominent stellar bar extending ∼15 kpc. The Atacama Large Millimeter/submillimeter Array Band 7 continuum map reveals that the dust emission originates from both the central starburst and the stellar bar. 3D disk modeling of the CO(4-3) emission line indicates a dynamically cold disk with rotation-to-dispersion ratio V max / σ ∼ 8 . The results suggest a bright DSFG may have a nonmerger origin, and its vigorous star formation may be triggered by the bar and/or rapid gas inflow.

DOI： 10.3847/2041-8213/acff63

Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA 査読有り国際共著国際誌 Open Access

Nakajima, T; Takano, S; Tosaki, T; Taniguchi, A; Harada, N; Saito, T; Imanishi, M; Nishimura, Y; Izumi, T; Tamura, Y; Kohno, K; Herbst, E

ASTROPHYSICAL JOURNAL 955 巻 ( 1 ) 頁： 27 - 27 2023年9月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present an imaging molecular line survey in the 3 mm band (85-114 GHz) focused on one of the nearest galaxies with an active galactic nucleus (AGN), NGC 1068, based on observations taken with the Atacama Large Millimeter/submillimeter Array. Distributions of 23 molecular transitions are obtained in the central ∼3 kpc region, including both the circumnuclear disk (CND) and starburst ring (SBR) with 60 and 350 pc resolution. The column densities and relative abundances of all the detected molecules are estimated under the assumption of local thermodynamic equilibrium in the CND and SBR. Then, we discuss the physical and chemical effects of the AGN on molecular abundance corresponding to the observation scale. We found that H13CN, SiO, HCN, and H13CO+ are abundant in the CND relative to the SBR. In contrast, 13CO is more abundant in the SBR. Based on the calculated column density ratios of N(HCN)/N(HCO+), N(HCN)/N(CN), and other molecular distributions, we conclude that the enhancement of HCN in the CND may be due to high-temperature environments resulting from strong shocks, which are traced by the SiO emission. Moreover, the abundance of CN in the CND is significantly lower than the expected value of the model calculations in the region affected by strong radiation. The expected strong X-ray irradiation from the AGN has a relatively lower impact on the molecular abundance in the CND than mechanical feedback.

DOI： 10.3847/1538-4357/ace4c7

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/ace4c7/pdf

Characterizing CO Emitters in the SSA22-AzTEC26 Field 査読有り国際共著国際誌 Open Access

Huang, S; Umehata, H; Kawabe, R; Kohno, K; Lee, M; Tamura, Y; Hatsukade, B; Mawatari, K

ASTROPHYSICAL JOURNAL 953 巻 ( 1 ) 頁： 75 2023年8月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We report the physical characterization of four CO emitters detected near the bright submillimeter galaxy (SMG) SSA22-AzTEC26. We analyze the data from Atacama Large Millimeter/submillimeter Array band 3, 4, and 7 observations of the SSA22-AzTEC26 field. In addition to the targeted SMG, we detect four line emitters with signal-to-noise ratio >5.2 in the cube smoothed with a 300 km s−1 FWHM Gaussian filter. All four sources have NIR counterparts within 1″. We perform UV-to-FIR spectral energy distribution modeling to derive the photometric redshifts and physical properties. Based on the photometric redshifts, we reveal that two of them are CO(2-1) at redshifts of 1.113 and 1.146 and one is CO(3-2) at z = 2.124. The three sources are massive galaxies with a stellar mass ≳1010.5 M ⊙, but have different levels of star formation. Two lie within the scatter of the main sequence (MS) of star-forming galaxies at z ∼ 1-2, and the most massive galaxy lies significantly below the MS. However, all three sources have a gas fraction within the scatter of the MS scaling relation. This shows that a blind CO line search can detect massive galaxies with low specific star formation rates that still host large gas reservoirs and that it also complements targeted surveys, suggesting later gas acquisition and the need for other mechanisms in addition to gas consumption to suppress star formation.

DOI： 10.3847/1538-4357/ace0c0

Big Three Dragons: Molecular Gas in a Bright Lyman-break Galaxy at <i>z</i>=7.15 査読有り国際共著国際誌 Open Access

Hashimoto, T; Inoue, AK; Sugahara, Y; Fudamoto, Y; Fujimoto, S; Knudsen, KK; Matsuo, H; Tamura, Y; Yamanaka, S; Harikane, Y; Kuno, N; Ono, Y; Salak, D; Ishii, N

ASTROPHYSICAL JOURNAL 952 巻 ( 1 ) 2023年7月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We report Atacama Large Millimeter/submillimeter Array Band 3 observations of CO(6−5), CO(7−6), and [C i](2−1) in B14-65666 (“Big Three Dragons”), one of the brightest Lyman-break galaxies at z > 7 in the rest-frame ultraviolet continuum, far-infrared continuum, and emission lines of [O iii] 88 μm and [C ii] 158 μm. CO(6−5), CO(7−6), and [C i](2−1), whose 3σ upper limits on the luminosities are approximately 40 times fainter than the [C ii] luminosity, are all not detected. The L [C II]/L CO(6-5) and L [C II]/L CO(7-6) ratios are higher than the typical ratios obtained in dusty star-forming galaxies or quasar host galaxies at similar redshifts, and they may suggest a lower gas density in the photodissociated region in B14-65666. By using the (1) [C ii] luminosity, (2) dust mass-to-gas mass ratio, and (3) a dynamical mass estimate, we find that the molecular gas mass (M mol) is (0.05-11) × 1010 M ⊙. This value is consistent with the upper limit inferred from the nondetection of mid-J CO and [C i](2−1). Despite the large uncertainty in M mol, we estimate a molecular gas-to-stellar mass ratio (μ gas) of 0.65-140 and a gas depletion time (τ dep) of 2.5-550 Myr; these values are broadly consistent with those of other high-redshift galaxies. B14-65666 could be an ancestor of a passive galaxy at z ≳ 4 if no gas is fueled from outside the galaxy.

DOI： 10.3847/1538-4357/acdd5c

Detections of [C ii] 158 <i>μ</i>m and [O iii] 88 <i>μ</i>m in a Local Lyman Continuum Emitter, Mrk 54, and Its Implications to High-redshift ALMA Studies* 査読有り国際共著国際誌 Open Access

Ura, R; Hashimoto, T; Inoue, AK; Fadda, D; Hayes, M; Puschnig, J; Zackrisson, E; Tamura, Y; Matsuo, H; Mawatari, K; Fudamoto, Y; Hagimoto, M; Kuno, N; Sugahara, Y; Yamanaka, S; Bakx, TJLC; Nakazato, Y; Usui, M; Yajima, H; Yoshida, N

ASTROPHYSICAL JOURNAL 948 巻 ( 1 ) 頁： 3 2023年5月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present integral field, far-infrared (FIR) spectroscopy of Mrk 54, a local Lyman continuum emitter, obtained with FIFI-LS on the Stratospheric Observatory for Infrared Astronomy. This is only the second time, after Haro 11, that [C ii] 158 μm and [O iii] 88 μm spectroscopy of the known LCEs have been obtained. We find that Mrk 54 has a strong [C ii] emission that accounts for ∼1% of the total FIR luminosity, whereas it has only moderate [O iii] emission, resulting in the low [O iii]/[C ii] luminosity ratio of 0.22 ± 0.06. In order to investigate whether [O iii]/[C ii] is a useful tracer of f esc (LyC escape fraction), we examine the correlations of [O iii]/[C ii] and (i) the optical line ratio of O32 ≡ [O iii] 5007 Å/[O ii] 3727 Å, (ii) specific star formation rate, (iii) [O iii] 88 μm/[O i] 63 μm ratio, (iv) gas-phase metallicity, and (v) dust temperature based on a combined sample of Mrk 54 and the literature data from the Herschel Dwarf Galaxy Survey and the LITTLE THINGS Survey. We find that galaxies with high [O iii]/[C ii] luminosity ratios could be the result of high ionization (traced by O32), bursty star formation, high ionized-to-neutral gas volume filling factors (traced by [O iii] 88 μm/[O i] 63 μm), and low gas-phase metallicities, which is in agreement with theoretical predictions. We present an empirical relation between the [O iii]/[C ii] ratio and f esc based on the combination of the [O iii]/[C ii] and O32 correlation, and the known relation between O32 and f esc. The relation implies that high-redshift galaxies with high [O iii]/[C ii] ratios revealed by the Atacama Large Millimeter/submillimeter Array may have f esc ≳ 0.1, significantly contributing to the cosmic reionization.

DOI： 10.3847/1538-4357/acc530

The SSA22 H i Tomography Survey (SSA22-HIT). I. Data Set and Compiled Redshift Catalog 査読有り国際共著国際誌 Open Access

Mawatari, K; Inoue, AK; Yamada, T; Hayashino, T; Prochaska, JX; Lee, KG; Tejos, N; Kashikawa, N; Otsuka, T; Yamanaka, S; Schlegel, DJ; Matsuda, Y; Hennawi, JF; Iwata, I; Umehata, H; Mukae, S; Ouchi, M; Sugahara, Y; Tamura, Y

ASTRONOMICAL JOURNAL 165 巻 ( 5 ) 頁： 208 2023年5月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astronomical Journal

We conducted a deep spectroscopic survey, named SSA22-HIT, in the SSA22 field with the DEep Imaging MultiObject Spectrograph (DEIMOS) on the Keck telescope, designed to tomographically map high-z H i gas through analysis of Lyα absorption in background galaxies’ spectra. In total, 198 galaxies were spectroscopically confirmed at 2.5 < z < 6 with a few low-z exceptions in the 26 × 15 arcmin2 area, of which 148 were newly determined in this study. Our redshift measurements were merged with previously confirmed redshifts available in the 34 × 27 arcmin2 area of the SSA22 field. This compiled catalog containing 730 galaxies of various types at z > 2 is useful for various applications, and it is made publicly available. Our SSA22-HIT survey has increased by approximately twice the number of spectroscopic redshifts of sources at z > 3.2 in the observed field. From a comparison with publicly available redshift catalogs, we show that our compiled redshift catalog in the SSA22 field is comparable to those among major extragalactic survey fields in terms of a combination of wide area and high surface number density of objects at z > 2. About 40% of the spectroscopically confirmed objects in SSA22-HIT show reasonable quality of spectra in the wavelengths shorter than Lyα when a sufficient amount of smoothing is adopted. Our data set enables us to make the H i tomographic map at z ≳ 3, which we present in a parallel study.

DOI： 10.3847/1538-3881/acb707

Bright extragalactic ALMA redshift survey (BEARS) III: detailed study of emission lines from 71 Herschel targets

Hagimoto, M; Bakx, TJLC; Serjeant, S; Bendo, GJ; Urquhart, SA; Eales, S; Harrington, KC; Tamura, Y; Umehata, H; Berta, S; Cooray, AR; Cox, P; De Zotti, G; Lehnert, MD; Riechers, DA; Scott, D; Temi, P; van der Werf, PP; Yang, C; Amvrosiadis, A; Andreani, PM; Baker, AJ; Beelen, A; Borsato, E; Buat, V; Butler, KM; Dannerbauer, H; Dunne, L; Dye, S; Enia, AFM; Fan, L; Gavazzi, R; González-Nuevo, J; Harris, AI; Herrera, CN; Hughes, DH; Ismail, D; Ivison, RJ; Jones, B; Kohno, K; Krips, M; Lagache, G; Marchetti, L; Massardi, M; Messias, H; Negrello, M; Neri, R; Omont, A; Perez-Fournon, I; Sedgwick, C; Smith, MWL; Stanley, F; Verma, A; Vlahakis, C; Ward, B; Weiner, C; Weiss, A; Young, AJ

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 521 巻 ( 4 ) 頁： 5508 - 5535 2023年3月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society

We analyse the molecular and atomic emission lines of 71 bright Herschel-selected galaxies between redshifts 1.4 and 4.6 detected by the Atacama Large Millimeter/submillimeter Array. These lines include a total of 156 CO, [C i], and H2O emission lines. For 46 galaxies, we detect two transitions of CO lines, and for these galaxies we find gas properties similar to those of other dusty star-forming galaxy (DSFG) samples. A comparison to photodissociation models suggests that most of Herschel-selected galaxies have similar interstellar medium conditions as local infrared-luminous galaxies and high-redshift DSFGs, although with denser gas and more intense far-ultraviolet radiation fields than normal star-forming galaxies. The line luminosities agree with the luminosity scaling relations across five orders of magnitude, although the star formation and gas surface density distributions (i.e. Schmidt-Kennicutt relation) suggest a different star formation phase in our galaxies (and other DSFGs) compared to local and low-redshift gas-rich, normal star-forming systems. The gas-to-dust ratios of these galaxies are similar to Milky Way values, with no apparent redshift evolution. Four of 46 sources appear to have CO line ratios in excess of the expected maximum (thermalized) profile, suggesting a rare phase in the evolution of DSFGs. Finally, we create a deep stacked spectrum over a wide rest-frame frequency (220-890 GHz) that reveals faint transitions from HCN and CH, in line with previous stacking experiments.

DOI： 10.1093/mnras/stad784

Updated Measurements of [O iii] 88 <i>μ</i>m, [C ii] 158 <i>μ</i>m, and Dust Continuum Emission from a <i>z</i>=7.2 Galaxy 査読有り国際共著国際誌 Open Access

Ren, YW; Fudamoto, Y; Inoue, AK; Sugahara, Y; Tokuoka, T; Tamura, Y; Matsuo, H; Kohno, K; Umehata, H; Hashimoto, T; Bouwens, RJ; Smit, R; Kashikawa, N; Okamoto, T; Shibuya, T; Shimizu, I

ASTROPHYSICAL JOURNAL 945 巻 ( 1 ) 頁： 69 2023年3月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present updated measurements of the [O iii] 88 μm, [C ii] 158 μm, and dust continuum emission from a star-forming galaxy at z = 7.212, SXDF-NB1006-2, by utilizing Atacama Large Millimeter/submillimeter Array (ALMA) archival data sets analysed in previous studies and data sets that have not been analysed before. The follow-up ALMA observations with higher angular resolution and sensitivity reveal a clumpy structure of the [O iii] emission on a scale of 0.32-0.85 kpc. We also combined all the ALMA [O iii] ([C ii]) data sets and updated the [O iii] ([C ii]) detection to 5.9σ (3.6σ-4.5σ). The non-detection of [C ii] with data from the REBELS large program implies the incompleteness of spectral-scan surveys using [C ii] to detect galaxies with high star formation rates (SFRs) but marginal [C ii] emission at high-z. The dust continuum at 90 and 160 μm remains undetected, indicating little dust content of <3.9 × 106 M ⊙ (3σ), and we obtained a more stringent constraint on the total infrared luminosity. We updated the [O iii]/[C ii] luminosity ratios to 10.2 ± 4.7 (6.1 ± 3.5) and 20 ± 12 (9.6 ± 6.1) for the 4.5σ and 3.6σ [C ii] detections, respectively, where the ratios in the parentheses are corrected for the surface brightness dimming effect on the extended [C ii] emission. We also found a strong [C ii] deficit (0.6-1.3 dex) between SXDF-NB1006-2 and the mean L [C II]−SFR relation of galaxies at 0 < z < 9.

DOI： 10.3847/1538-4357/acb8ab

Bright Extragalactic ALMA Redshift Survey (BEARS) III: Detailed study of emission lines from 71 Herschel targets 査読有り

Hagimoto, M, Bakx, T. J. L. C, Serjeant, S, Bendo, G. J, Urquhart, S. A, Eales, S, Harrington, K. C, Tamura, Y, Umehata, H, Berta, S, Cooray, A. R, Cox, P, De Zotti, G, Lehnert, M. D, Riechers, D. A, Scott, D, Temi, P, van der Werf, P. P, Yang, C, Amvrosiadis, A, Andreani, P. M, Baker, A. J, Beelen, A, Borsato, E, Buat, V, Butler, K. M, Dannerbauer, H, Dunne, L, Dye, S, Enia, A. F. M, Fan, L, Gavazzi, R, Gonzalez-Nuevo, J, Harris, A. I, Herrera, C. N, Hughes, D. H, Ismail, D, Ivison, R. J, Jones, B, Kohno, K, Krips, M, Lagache, G, Marchetti, L, Massardi, M, Messias, H, Negrello, M, Neri, R, Omont, A, Perez-Fournon, I, Sedgwick, C, Smith, M. W. L, Stanley, F, Verma, A, Vlahakis, C, Ward, B, Weiner, C, Weiss, A, Young, A. J

Monthly Notices of the Royal Astronomical Society 2023年3月

The SCUBA-2 Large eXtragalactic Survey: 850μm map, catalogue and the bright-end number counts of the XMM-LSS field 査読有り国際誌 Open Access

Garratt, TK; Geach, JE; Tamura, Y; Coppin, KEK; Franco, M; Ao, Y; Chen, CC; Cheng, C; Clements, DL; Dai, YS; Dannerbauer, H; Greve, TR; Hatsukade, B; Hwang, HS; Jiang, L; Kohno, K; Koprowski, MP; Michalowski, MJ; Sawicki, M; Scott, D; Shim, H; Takeuchi, TT; Wang, WH; Xue, YQ; Yang, C

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 520 巻 ( 3 ) 頁： 3669 - 3687 2023年2月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society

We present 850 μm imaging of the XMM-LSS field observed for 170 h as part of the James Clerk Maxwell Telescope SCUBA-2 Large eXtragalactic Survey (S2LXS). S2LXS XMM-LSS maps an area of 9 deg2, reaching a moderate depth of 1σ 4 mJy beam−1. This is the largest contiguous area of extragalactic sky mapped by James Clerk Maxwell Telescope (JCMT) at 850 μm to date. The wide area of the S2LXS XMM-LSS survey allows us to probe the ultra-bright (S850μm 15 mJy), yet rare submillimetre population. We present the S2LXS XMM-LSS catalogue, which comprises 40 sources detected at >5σ significance, with deboosted flux densities in the range of 7–48 mJy. We robustly measure the bright-end of the 850 μm number counts at flux densities >7 mJy, reducing the Poisson errors compared to existing measurements. The S2LXS XMM-LSS observed number counts show the characteristic upturn at bright fluxes, expected to be motivated by local sources of submillimetre emission and high-redshift strongly lensed galaxies. We find that the observed 850 μm number counts are best reproduced by model predictions that include either strong lensing or source blending from a 15-arcsec beam, indicating that both may make an important contribution to the observed overabundance of bright single dish 850 μm selected sources. We make the S2LXS XMM-LSS 850 μm map and >5σ catalogue presented here publicly available.

DOI： 10.1093/mnras/stad307

Deep ALMA redshift search of a z ∼ 12 GLASS-JWST galaxy candidate 査読有り国際誌 Open Access

Bakx, TJLC; Zavala, JA; Mitsuhashi, I; Treu, T; Fontana, A; Tadaki, KI; Casey, CM; Castellano, M; Glazebrook, K; Hagimoto, M; Ikeda, R; Jones, T; Leethochawalit, N; Mason, C; Morishita, T; Nanayakkara, T; Pentericci, L; Roberts-Borsani, G; Santini, P; Serjeant, S; Tamura, Y; Trenti, M; Vanzella, E

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 519 巻 ( 4 ) 頁： 5076 - 5085 2023年1月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society

The JWST has discovered a surprising abundance of bright galaxy candidates in the very early universe (≤500 Myr after the Big Bang), calling into question current galaxy formation models. Spectroscopy is needed to confirm the primeval nature of these candidates, as well as to understand how the first galaxies form stars and grow. Here we present deep spectroscopic and continuum ALMA observations towards GHZ2/GLASS-z12, one of the brightest and most robust candidates at z > 10, identified in the GLASS-JWST Early Release Science Program. We detect a 5.8σ line, offset 0″.5 from the JWST position of GHZ2/GLASS-z12, that associating it with the [O iii] 88 μm transition, implies a spectroscopic redshift of z = 12.117 ± 0.001. We verify the detection using extensive statistical tests. The oxygen line luminosity places GHZ2/GLASS-z12 above the [O iii]-SFR relation for metal-poor galaxies, implying an enhancement of [O iii] emission in this system while the JWST-observed emission is likely a lower-metallicity region. The lack of dust emission seen by these observations is consistent with the blue UV slope observed by JWST, which suggest little dust attenuation in galaxies at this early epoch. Further observations will unambiguously confirm the redshift and shed light on the origins of the wide and offset line and physical properties of this early galaxy. This work illustrates the synergy between JWST and ALMA, and paves the way for future spectroscopic surveys of z > 10 galaxy candidates.

DOI： 10.1093/mnras/stac3723

DOI： 10.48550/arXiv.2208.13642

ALMA Observations of CO Emission from Luminous Lyman-break Galaxies at <i>z</i>=6.0293-6.2037 査読有り

Ono Yoshiaki, Fujimoto Seiji, Harikane Yuichi, Ouchi Masami, Vallini Livia, Ferrara Andrea, Shibuya Takatoshi, Pallottini Andrea, Inoue Akio K., Imanishi Masatoshi, Shimasaku Kazuhiro, Hashimoto Takuya, Lee Chien-Hsiu, Sugahara Yuma, Tamura Yoichi, Kohno Kotaro, Schramm Malte

ASTROPHYSICAL JOURNAL 941 巻 ( 1 ) 頁： 74 - 74 2022年12月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present our new Atacama Large Millimeter/submillimeter Array (ALMA) observations targeting CO(6–5) emission from three luminous Lyman-break galaxies (LBGs) at zspec = 6.0293–6.2037 found in the Subaru/Hyper Suprime-Cam survey, whose [O III] 88 μm and [C II] 158 μm emissions have been detected with ALMA. We find a marginal detection of the CO(6–5) line from one of our LBGs, J0235–0532, at the;4σ significance level and obtain upper limits for the other two LBGs, J1211–0118 and J0217–0208. Our z = 6 luminous LBGs are consistent with the previously found correlation between the CO luminosity and the infrared luminosity. The unique ensemble of the multiple far-infrared emission lines and underlying continuum fed to a photodissociation region model reveals that J0235–0532 has a relatively high density of hydrogen nuclei nH that is comparable to those of low-z (U)LIRGs, quasars, and Galactic star-forming regions with high nH values, while the other two LBGs have lower nH consistent with local star-forming galaxies. By carefully taking account of various uncertainties, we obtain constraints on total gas mass and gas surface density from their CO luminosity measurements. We find that J0235–0532 is located below the Kennicutt–Schmidt (KS) relation, comparable to the z = 5.7 LBG, HZ10, previously detected with CO(2–1). Combined with previous results for dusty starbursts at similar redshifts, the KS relation at z = 5–6 is on average consistent with the local one.

DOI： 10.3847/1538-4357/ac9ea6

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/ac9ea6/pdf

Central concentration of warm and dense molecular gas in a strongly lensed submillimeter galaxy at <i>z</i>=6 査読有り

Tsujita Akiyoshi, Tadaki Ken-ichi, Kohno Kotaro, Hatsukade Bunyo, Egusa Fumi, Tamura Yoichi, Nishimura Yuri, Zavala Jorge, Saito Toshiki, Umehata Hideki, Lee Minju M.

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 74 巻 ( 6 ) 頁： 1429 - 1440 2022年12月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

We report the detection of the CO(12–11) line emission toward G09-83808 (or H-ATLAS J090045.4+004125), a strongly-lensed submillimeter galaxy at z = 6.02, with Atacama Large Millimeter/submillimeter Array observations. Combining previously detected [O III] 88 μm, [N II] 205 μm, and dust continuum at 0.6 mm and 1.5 mm, we investigate the physical properties of the multi-phase interstellar medium in G09-83808. A source-plane reconstruction reveals that the region of the CO(12–11) emission is compact (Re,CO = 0.49+−002919 kpc) and roughly coincides with that of the dust continuum. Non-local thermodynamic equilibrium radiative transfer modeling of CO spectral-line energy distribution reveals that most of the CO(12–11) emission comes from a warm (kinetic temperature of Tkin = 320 ± 170 K) and dense [log (nH2/cm−3) = 5.4 ± 0.6] gas, indicating that the warm and dense molecular gas is concentrated in the central 0.5 kpc region. The luminosity ratio in G09-83808 is estimated to be LCO(12-11)/LCO(6-5) = 1.1 ± 0.2. The high ratio is consistent with those in local active galactic nuclei (AGNs) and 6 < z < 7 quasars, the fact of which implies that G09-83808 would be a good target to explore dust-obscured AGNs in the epoch of reionization. In the reconstructed [O III] 88 μm and [N II] 205 μm cubes, we also find that a monotonic velocity gradient is extending over the central starburst region by a factor of 2 and that star-forming sub-components exist. High-resolution observations of bright [C II] 158 μm line emissions will enable us to characterize the kinematics of a possible rotating disk and the nature of the sub-components.

DOI： 10.1093/pasj/psac082

Deshima 2.0: Rapid Redshift Surveys and Multi-line Spectroscopy of Dusty Galaxies 査読有り

Rybak M., Bakx T., Baselmans J., Karatsu K., Kohno K., Takekoshi T., Tamura Y., Taniguchi A., van der Werf P., Endo A.

JOURNAL OF LOW TEMPERATURE PHYSICS 209 巻 ( 5-6 ) 頁： 766 - 778 2022年12月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Journal of Low Temperature Physics

We present a feasibility study for the high-redshift galaxy part of the Science Verification Campaign with the 220–440 GHz deshima 2.0 integrated superconducting spectrometer on the ASTE telescope. The first version of the deshima 2.0 chip has been recently manufactured and tested in the lab. Based on these realistic performance measurements, we evaluate potential target samples and prospects for detecting the [CII] and CO emission lines. The planned observations comprise two distinct, but complementary objectives: (1) acquiring spectroscopic redshifts for dusty galaxies selected in far-infrared/mm-wave surveys; (2) multi-line observations to infer physical conditions in dusty galaxies.

DOI： 10.1007/s10909-022-02730-y

DESHIMA 2.0: Development of an Integrated Superconducting Spectrometer for Science-Grade Astronomical Observations 査読有り

Taniguchi Akio, Bakx Tom J. L. C., Baselmans Jochem J. A., Huiting Robert, Karatsu Kenichi, Llombart Nuria, Rybak Matus, Takekoshi Tatsuya, Tamura Yoichi, Akamatsu Hiroki, Brackenhoff Stefanie, Bueno Juan, Buijtendorp Bruno T., Dabironezare Shahab O., Doing Anne-Kee, Fujii Yasunori, Fujita Kazuyuki, Gouwerok Matthijs, Hahnle Sebastian, Ishida Tsuyoshi, Ishii Shun, Kawabe Ryohei, Kitayama Tetsu, Kohno Kotaro, Kouchi Akira, Maekawa Jun, Matsuda Keiichi, Murugesan Vignesh, Nakatsubo Shunichi, Oshima Tai, Laguna Alejandro Pascual, Thoen David J., van der Werf Paul P., Yates Stephen J. C., Endo Akira

JOURNAL OF LOW TEMPERATURE PHYSICS 209 巻 ( 3-4 ) 頁： 278 - 286 2022年11月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Journal of Low Temperature Physics

Integrated superconducting spectrometer (ISS) technology will enable ultra-wideband, integral-field spectroscopy for (sub)millimeter-wave astronomy, in particular, for uncovering the dust-obscured cosmic star formation and galaxy evolution over cosmic time. Here, we present the development of DESHIMA 2.0, an ISS for ultra-wideband spectroscopy toward high-redshift galaxies. DESHIMA 2.0 is designed to observe the 220–440 GHz band in a single shot, corresponding to a redshift range of z = 3.3–7.6 for the ionized carbon emission ([C II] 158 μ m). The first-light experiment of DESHIMA 1.0, using the 332–377 GHz band, has shown an excellent agreement among the on-sky measurements, the laboratory measurements, and the design. As a successor to DESHIMA 1.0, we plan the commissioning and the scientific observation campaign of DESHIMA 2.0 on the ASTE 10-m telescope in 2023. Ongoing upgrades for the full octave-bandwidth system include the wideband 347-channel chip design and the wideband quasi-optical system. For efficient measurements, we also develop the observation strategy using the mechanical fast sky-position chopper and the sky-noise removal technique based on a novel data-scientific approach. In the paper, we show the recent status of the upgrades and the plans for the scientific observation campaign.

DOI： 10.1007/s10909-022-02888-5

Characterization of sensitivity and responses of a 2-element prototype wavefront sensor for millimeter-wave adaptive optics attached to the Nobeyama 45 m telescope

Satoya Nakano, Yoichi Tamura, Akio Taniguchi, Sachiko K. Okumura, Ryohei Kawabe, Nozomi Okada, Tomoko Nakamura, Yuhei Fukasaku

Proceedings of the SPIE 12185 巻頁： 121856Z 2022年8月

Development status of TAO/MIMIZUKU: performance test of the near-infrared channel 招待有り

Takafumi Kamizuka, Takashi Miyata, Shigeyuki Sako, Ryou Ohsawa, Kentaro Asano, Atsushi Nishimura, Kengo Tachibana, Tsubasa Michifuji, Hirokazu Iida, Akira C. Naruse, Mizuho Uchiyama, Itsuki Sakon, Takashi Onaka, Hirokazu Kataza, Sunao Hasegawa, Fumihiko Usui, Naruhisa Takato, Noboru Ebizuka, Takuya Hosobata, Tsutomu Aoki, Mamoru Doi, Fumi Egusa, Bunyo Hatsukade, Natsuko Kato, Kotaro Kohno, Masahiro Konishi, Shintaro Koshida, Shuhei Koyama, Takeo Minezaki, Tomoki Morokuma, Kentaro Motohara, Mizuki Numata, Hiroaki Sameshima, Hidenori Takahashi, Yoichi Tamura, Toshihiko Tanabe, Masuo Tanaka, Kosuke Kushibiki, Nuo Chen, Shogo Homan, Yuzuru Yoshii

Proceedings of the SPIE 12184 巻頁： 121845J 2022年8月

An AGN with an Ionized Gas Outflow in a Massive Quiescent Galaxy in a Protocluster at z=3.09 査読有り

Kubo Mariko, Umehata Hideki, Matsuda Yuichi, Kajisawa Masaru, Steidel Charles C., Yamada Toru, Tanaka Ichi, Hatsukade Bunyo, Tamura Yoichi, Nakanishi Kouichiro, Kohno Kotaro, Lee Kianhong, Matsuda Keiichi, Ao Yiping, Nagao Tohru, Yun Min S.

ASTROPHYSICAL JOURNAL 935 巻 ( 2 ) 頁： 89 - 89 2022年8月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We report the detection of an ionized gas outflow from an X-ray active galactic nucleus hosted in a massive quiescent galaxy in a protocluster at z = 3.09 (J221737.29+001823.4). It is a type-2 QSO with broad (W 80 > 1000 km s-1) and strong ( log(L[OIII] /erg s-1) ≈ 43.4) [O iii]λ λ 4959,5007 emission lines detected by slit spectroscopy in three-position angles using Multi-Object Infra-Red Camera and Spectrograph (MOIRCS) on the Subaru telescope and the Multi-Object Spectrometer For Infra-Red Exploration (MOSFIRE) on the Keck-I telescope. In the all slit directions, [O iii] emission is extended to ∼15 physical kpc and indicates a powerful outflow spreading over the host galaxy. The inferred ionized gas mass outflow rate is 22 ± 3 M ⊙ yr-1. Although it is a radio source, according to the line diagnostics using Hβ, [O ii], and [O iii], photoionization by the central QSO is likely the dominant ionization mechanism rather than shocks caused by radio jets. On the other hand, the spectral energy distribution of the host galaxy is well characterized as a quiescent galaxy that has shut down star formation several hundred Myr ago. Our results suggest a scenario that QSOs are powered after the shutdown of the star formation and help complete the quenching of massive quiescent galaxies at high redshift.

DOI： 10.3847/1538-4357/ac7f2d

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/ac7f2d/pdf

ALMA Reveals Extended Cool Gas and Hot Ionized Outflows in a Typical Star-forming Galaxy at <i>Z</i>=7.13 査読有り

Akins Hollis B., Fujimoto Seiji, Finlator Kristian, Watson Darach, Knudsen Kirsten K., Richard Johan, Bakx Tom J. L. C., Hashimoto Takuya, Inoue Akio K., Matsuo Hiroshi, Michalowski Michal J., Tamura Yoichi

ASTROPHYSICAL JOURNAL 934 巻 ( 1 ) 頁： 64 2022年7月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present spatially resolved morphological properties of [C II] 158 μm, [O III] 88 μm, dust, and rest-frame ultraviolet (UV) continuum emission for A1689-zD1, a strongly lensed, sub-L* galaxy at z = 7.13, by utilizing deep Atacama Large Millimeter/submillimeter Array (ALMA) and Hubble Space Telescope (HST) observations. While the [O III] line and UV continuum are compact, the [C II] line is extended up to a radius of r ∼ 12 kpc. Using multi-band rest-frame far-infrared continuum data ranging from 52 to 400 μm, we find an average dust temperature and emissivity index of T dust = 41 − 14 + 17 K and β = 1.7 − 0.7 + 1.1 , respectively, across the galaxy. We find slight differences in the dust continuum profiles at different wavelengths, which may indicate that the dust temperature decreases with distance. We map the star formation rate (SFR) via IR and UV luminosities and determine a total SFR of 37 ± 1M ⊙yr−1 with an obscured fraction of 87%. While the [O III] line is a good tracer of the SFR, the [C II] line shows deviation from the local L [C II]-SFR relations in the outskirts of the galaxy. Finally, we observe a clear difference in the line profile between [C II] and [O III], with significant residuals (∼5σ) in the [O III] line spectrum after subtracting a single Gaussian model. This suggests a possible origin of the extended [C II] structure from the cooling of hot ionized outflows. The extended [C II] and high-velocity [O III] emission may both contribute in part to the high L [O III]/L [C II] ratios recently reported in z > 6 galaxies.

DOI： 10.3847/1538-4357/ac795b

High-resolution ALMA Study of CO J=2-1 Line and Dust Continuum Emissions in Cluster Galaxies at z=1.46 査読有り

Ikeda Ryota, Tadaki Ken-ichi, Iono Daisuke, Kodama Tadayuki, Chan Jeffrey C. C., Hatsukade Bunyo, Hayashi Masao, Izumi Takuma, Kohno Kotaro, Koyama Yusei, Shimakawa Rhythm, Suzuki Tomoko L., Tamura Yoichi, Tanaka Ichi

ASTROPHYSICAL JOURNAL 933 巻 ( 1 ) 頁： 11 - 11 2022年7月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present new Atacama Large Millimeter/submillimeter Array (ALMA) results obtained from spatially resolved CO J = 2-1 line (0.″4 resolution) and 870 μm continuum (0.″2 resolution) observations of cluster galaxies in XMMXCS J2215.9-1738 at z = 1.46. Our sample comprises 17 galaxies within ∼0.5 Mpc (0.6R 200) of the cluster center, all of which have previously been detected in the CO J = 2-1 line at a lower resolution. The effective radii of both the CO J = 2-1 line and 870 μm dust continuum emissions are robustly measured for nine galaxies by modeling the visibilities. We find that the CO J = 2-1 line emission in all of the nine galaxies is more extended than the dust continuum emission by a factor of 2.8 ± 1.4. We investigate the spatially resolved Kennicutt-Schmidt (KS) relation in two regions within the interstellar medium of the galaxies. The relation for our sample reveals that the central region (0 < r < R e,870μm) of galaxies tends to have a shorter gas depletion timescale, i.e., a higher star formation efficiency, compared to the extended region (R e,870μm < r < R e,CO). Overall, our result suggests that star formation activities are concentrated inside the extended gas reservoir, possibly resulting in the formation of a bulge structure. We find consistency between the ALMA 870 μm radii of star-forming members and the Hubble Space Telescope/1.6 μm radii of passive members in a mass-size distribution, which suggests a transition from star-forming to passive members within ∼0.5 Gyr. In addition, no clear differences in the KS relation nor in the sizes are found between galaxies with and without a close companion.

DOI： 10.3847/1538-4357/ac6cdc

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/ac6cdc/pdf

Possible Systematic Rotation in the Mature Stellar Population of a <i>z</i>=9.1 Galaxy

Tokuoka Tsuyoshi, Inoue Akio K., Hashimoto Takuya, Ellis Richard S., Laporte Nicolas, Sugahara Yuma, Matsuo Hiroshi, Tamura Yoichi, Fudamoto Yoshinobu, Moriwaki Kana, Roberts-Borsani Guido, Shimizu Ikkoh, Yamanaka Satoshi, Yoshida Naoki, Zackrisson Erik, Zheng Wei

ASTROPHYSICAL JOURNAL LETTERS 933 巻 ( 1 ) 2022年7月

Detection of nitrogen and oxygen in a galaxy at the end of reionization 査読有り

Tadaki Ken-ichi, Tsujita Akiyoshi, Tamura Yoichi, Kohno Kotaro, Hatsukade Bunyo, Iono Daisuke, Lee Minju M., Matsuda Yuichi, Michiyama Tomonari, Nagao Tohru, Nakanishi Kouichiro, Nishimura Yuri, Saito Toshiki, Umehata Hideki, Zavala Jorge

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 74 巻 ( 3 ) 頁： L9 - L16 2022年6月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

We present observations of [N II] 205 μm, [O III] 88 μm, and dust emission in a strongly-lensed, submillimeter galaxy (SMG) at z = 6.0, G09.83808, with the Atacama Large Millimeter/submillimeter Array (ALMA). Both [N II] and [O III] line emissions are detected at >12σ in the 0.″8-resolution maps. Lens modeling indicates that the spatial distribution of the dust continuum emission is well characterized by a compact disk with an effective radius of 0.64 ± 0.02 kpc and a high infrared surface brightness of ΣIR = (1.8 ± 0.3) × 1012 L⊙ kpc-2. This result supports that G09.83808 is the progenitor of compact quiescent galaxies at z ∼4, where the majority of its stars are expected to be formed through a strong and short burst of star formation. G09.83808 and other lensed SMGs show a decreasing trend in the [N II] line to infrared luminosity ratio with increasing continuum flux density ratio between 63 and 158 μm, as seen in local luminous infrared galaxies (LIRGs). The decreasing trend can be reproduced by photoionization models with increasing ionization parameters. Furthermore, by combining the [N II]/[O III] luminosity ratio with far-infrared continuum flux density ratio in G09.83808, we infer that the gas phase metallicity is already Z ≈ 0.5-0.7 Z⊙. G09.83808 is likely one of the earliest galaxies that has been chemically enriched at the end of reionization.

DOI： 10.1093/pasj/psac018

Properties of molecular gas in galaxies in early and mid stages of Interaction. III. Resolved Kennicutt–Schmidt law 招待有り査読有り

Publications of the Astronomical Society of Japan 74 巻 ( 2 ) 頁： 343 - 363 2022年4月

The bright extragalactic ALMA redshift survey (BEARS) I: Redshifts of bright gravitationally lensed galaxies from the Herschel ATLAS

Urquhart S.A., Bendo G.J., Serjeant S., Bakx T., Hagimoto M., Cox P., Neri R., Lehnert M., Sedgwick C., Weiner C., Dannerbauer H., Amvrosiadis A., Andreani P., Baker A.J., Beelen A., Berta S., Borsato E., Buat V., Butler K.M., Cooray A., De Zotti G., Dunne L., Dye S., Eales S., Enia A., Fan L., Gavazzi R., González-Nuevo J., Harris A.I., Herrera C.N., Hughes D., Ismail D., Ivison R., Jin S., Jones B., Kohno K., Krips M., Lagache G., Marchetti L., Massardi M., Messias H., Negrello M., Omont A., Perez-Fournon I., Riechers D.A., Scott D., Smith M.W.L., Stanley F., Tamura Y., Temi P., Vlahakis C., Weiß A., Van Der Werf P., Verma A., Yang C., Young A.J.

Monthly Notices of the Royal Astronomical Society 511 巻 ( 2 ) 頁： 3017 - 3033 2022年4月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society

We present spectroscopic measurements for 71 galaxies associated with 62 of the brightest high-redshift submillimetre sources from the Southern fields of the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS), while targeting 85 sources which resolved into 142. We have obtained robust redshift measurements for all sources using the 12-m Array and an efficient tuning of ALMA to optimize its use as a redshift hunter, with 73 per cent of the sources having a robust redshift identification. Nine of these redshift identifications also rely on observations from the Atacama Compact Array. The spectroscopic redshifts span a range 1.41 < z < 4.53 with a mean value of 2.75, and the CO emission line full-width at half-maxima range between 110, km, s-1 < FWHM < 1290, km, s-1 with a mean value of ∼500 km s-1, in line with other high-z samples. The derived CO(1-0) luminosity is significantly elevated relative to line-width to CO(1-0) luminosity scaling relation, which is suggestive of lensing magnification across our sources. In fact, the distribution of magnification factors inferred from the CO equivalent widths is consistent with expectations from galaxy-galaxy lensing models, though there is a hint of an excess at large magnifications that may be attributable to the additional lensing optical depth from galaxy groups or clusters.

DOI： 10.1093/mnras/stac150

A Search for <i>H</i>-Dropout Lyman Break Galaxies at <i>z</i> ∼ 12-16 査読有り

Harikane Yuichi, Inoue Akio K., Mawatari Ken, Hashimoto Takuya, Yamanaka Satoshi, Fudamoto Yoshinobu, Matsuo Hiroshi, Tamura Yoichi, Dayal Pratika, Yung L. Y. Aaron, Hutter Anne, Pacucci Fabio, Sugahara Yuma, Koekemoer Anton M.

ASTROPHYSICAL JOURNAL 929 巻 ( 1 ) 頁： 1 - 1 2022年4月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present two bright galaxy candidates at z ∼12-13 identified in our H-dropout Lyman break selection with 2.3 deg2 near-infrared deep imaging data. These galaxy candidates, selected after careful screening of foreground interlopers, have spectral energy distributions showing a sharp discontinuity around 1.7 μm, a flat continuum at 2-5 μm, and nondetections at <1.2 μm in the available photometric data sets, all of which are consistent with a z > 12 galaxy. An ALMA program targeting one of the candidates shows a tentative 4σ [O iii] 88 μm line at z = 13.27, in agreement with its photometric redshift estimate. The number density of the z ∼12-13 candidates is comparable to that of bright z ∼10 galaxies and is consistent with a recently proposed double-power-law luminosity function rather than the Schechter function, indicating little evolution in the abundance of bright galaxies from z ∼4 to 13. Comparisons with theoretical models show that the models cannot reproduce the bright end of rest-frame ultraviolet luminosity functions at z ∼10-13. Combined with recent studies reporting similarly bright galaxies at z ∼9-11 and mature stellar populations at z ∼6-9, our results indicate the existence of a number of star-forming galaxies at z > 10, which will be detected with upcoming space missions such as the James Webb Space Telescope, Nancy Grace Roman Space Telescope, and GREX-PLUS.

DOI： 10.3847/1538-4357/ac53a9

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/ac53a9/pdf

TiEMPO: open-source time-dependent end-to-end model for simulating ground-based submillimeter astronomical observations

Huijten Esmee, Roelvink Yannick, Brackenhoff Stefanie A., Taniguchi Akio, Bakx Tom J. L. C., Marthi Kaushal B., Zaalberg Stan, Doing Anne-Kee, Baselmans Jochem J. A., Chin Kah Wuy, Huiting Robert, Karatsu Kenichi, Laguna Alejandro Pascual, Tamura Yoichi, Takekoshi Tatsuya, Yates Stephen J. C., van Hoven Maarten, Endo Akira

JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS 8 巻 ( 2 ) 2022年4月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Journal of Astronomical Telescopes, Instruments, and Systems

The next technological breakthrough in millimeter–submillimeter astronomy is three-dimensional imaging spectrometry with wide instantaneous spectral bandwidths and wide fields of view. The total optimization of the focal-plane instrument, the telescope, the observing strategy, and the signal-processing software must enable efficient removal of foreground emission from the Earth’s atmosphere, which is time-dependent and highly nonlinear in frequency. Here, we present Time-dependent End-to-end Model for Post-process Optimization (TiEMPO) of the DEep Spectroscopic HIgh-redshift MApper (DESHIMA) spectrometer. TiEMPO utilizes a dynamical model of the atmosphere and parameterized models of the astronomical source, the telescope, the instrument, and the detector. The output of TiEMPO is a time stream of sky brightness temperature and detected power, which can be analyzed by standard signal-processing software. We first compare TiEMPO simulations with an on-sky measurement by the wideband DESHIMA spectrometer, and find good agreement in the noise and sensitivity. We then use TiEMPO to simulate the detection of the line emission spectrum of a high-redshift galaxy using the DESHIMA 2.0 spectrometer in development. The TiEMPO model is open source. Its modular and parametrized design enables users to adapt it to optimize the end-to-end performance of spectroscopic and photometric instruments on existing and future telescopes

DOI： 10.1117/1.JATIS.8.2.028005

The Kiloparsec-scale Neutral Atomic Carbon Outflow in the Nearby Type 2 Seyfert Galaxy NGC 1068: Evidence for Negative AGN Feedback 査読有り

Toshiki Saito, Shuro Takano, Nanase Harada, Taku Nakajima, Eva Schinnerer, Daizhong Liu, Akio Taniguchi, Takuma Izumi, Yumi Watanabe, Kazuharu Bamba, Eric Herbst, Kotaro Kohno, Yuri Nishimura, Sophia Stuber, Yoichi Tamura, Tomoka Tosaki

The Astrophysical Journal Letters 927 巻 ( 2 ) 頁： L32 - L32 2022年3月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：American Astronomical Society

Abstract

Active galactic nucleus (AGN) feedback is postulated as a key mechanism for regulating star formation within galaxies. Studying the physical properties of the outflowing gas from AGNs is thus crucial for understanding the coevolution of galaxies and supermassive black holes. Here we report 55 pc resolution ALMA neutral atomic carbon [C i] <sup>3</sup>P<sub>1</sub>−<sup>3</sup>P<sub>0</sub> observations toward the central 1 kpc of the nearby Type 2 Seyfert galaxy NGC 1068, supplemented by 55 pc resolution CO(J = 1−0) observations. We find that [C i] emission within the central kiloparsec is strongly enhanced by a factor of >5 compared to the typical [C i]/CO intensity ratio of ∼0.2 for nearby starburst galaxies (in units of brightness temperature). The most [C i]-enhanced gas (ratio > 1) exhibits a kiloparsec-scale elongated structure centered at the AGN that matches the known biconical ionized gas outflow entraining molecular gas in the disk. A truncated, decelerating bicone model explains well the kinematics of the elongated structure, indicating that the [C i] enhancement is predominantly driven by the interaction between the ISM in the disk and the highly inclined ionized gas outflow (which is likely driven by the radio jet). Our results strongly favor the “CO dissociation scenario” rather than the “in situ C formation” one, which prefers a perfect bicone geometry. We suggest that the high-[C i]/CO intensity ratio gas in NGC 1068 directly traces ISM in the disk that is currently dissociated and entrained by the jet and the outflow, i.e., the “negative” effect of the AGN feedback.

DOI： 10.3847/2041-8213/ac59ae

その他リンク： https://iopscience.iop.org/article/10.3847/2041-8213/ac59ae/pdf

Properties of molecular gas in galaxies in early and mid stages of Interaction. III. Resolved Kennicutt-Schmidt law

Kaneko Hiroyuki, Kuno Nario, Iono Daisuke, Tamura Yoichi, Tosaki Tomoka, Nakanishi Kouichiro, Sawada Tsuyoshi

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 2022年2月

Characterization of sensitivity and responses of a 2-element prototype wavefront sensor for millimeter-wave adaptive optics attached to the Nobeyama 45 m telescope

Nakano Satoya, Tamura Yoichi, Taniguchi Akio, Okumura Sachiko, Kawabe Ryohei, Okada Nozomi, Nakamura Tomoko, Fukasaku Yuhei

ADAPTIVE OPTICS SYSTEMS VIII 12185 巻頁： 121856Z 2022年

Development status of TAO/MIMIZUKU: Performance test of the near-infrared channel

Kamizuka Takafumi, Miyata Takashi, Sako Shigeyuki, Ohsawa Ryou, Asano Kentaro, Nishimura Atsushi, Tachibana Kengo, Michifuji Tsubasa, Iida Hirokazu, Naruse Akira C., Uchiyama Mizuho, Sakon Itsuki, Onaka Takashi, Kataza Hirokazu, Hasegawa Sunao, Usui Fumihiko, Takato Naruhisa, Ebizuka Noboru, Hosobata Takuya, Aoki Tsutomu, Doi Mamoru, Egusa Fumi, Hatsukade Bunyo, Kato Natsuko, Kohno Kotaro, Konishi Masahiro, Koshida Shintaro, Koyama Shuhei, Minezaki Takeo, Morokuma Tomoki, Motohara Kentaro, Numata Mizuki, Sameshima Hiroaki, Takahashi Hidenori, Tamura Yoichi, Tanabe Toshihiko, Tanaka Masuo, Kushibiki Kosuke, Chen Nuo, Homan Shogo, Yoshii Yuzuru

GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY IX 12184 巻 2022年

The Kiloparsec-scale Neutral Atomic Carbon Outflow in the Nearby Type 2 Seyfert Galaxy NGC 1068 : Evidence for Negative AGN Feedback 査読有り

927 巻 ( L32 ) 2022年

Big Three Dragons: A [N II] 122 mu m Constraint and New Dust-continuum Detection of a z=7.15 Bright Lyman-break Galaxy with ALMA

Sugahara Yuma, Inoue Akio K., Hashimoto Takuya, Yamanaka Satoshi, Fujimoto Seiji, Tamura Yoichi, Matsuo Hiroshi, Binggeli Christian, Zackrisson Erik

ASTROPHYSICAL JOURNAL 923 巻 ( 1 ) 2021年12月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present new Atacama Large Millimeter/submillimeter Array Band 7 observational results of a Lyman-break galaxy at z = 7.15, B14-65666 ("Big Three Dragons"), which is an object detected in [O iii] 88 μm, [C ii] 158 μm, and dust continuum emission during the epoch of reionization. Our targets are the [N ii] 122 μm fine-structure emission line and the underlying 120 μm dust continuum. The dust continuum is detected with a ∼19σ significance. From far-infrared spectral energy distribution sampled at 90, 120, and 160 μm, we obtain a best-fit dust temperature of 40 K (79 K) and an infrared luminosity of (12.1) at the emissivity index β = 2.0 (1.0). The [N ii] 122 μm line is not detected. The 3σ upper limit of the [N ii] luminosity is 8.1 × 107 L o˙. From the [N ii], [O iii], and [C ii] line luminosities, we use the Cloudy photoionization code to estimate nebular parameters as functions of metallicity. If the metallicity of the galaxy is high (Z > 0.4 Z o˙), the ionization parameter and hydrogen density are log10 U ≃ -2.7 ± 0.1 and n H ≃ 50-250 cm-3, respectively, which are comparable to those measured in low-redshift galaxies. The nitrogen-to-oxygen abundance ratio, N/O, is constrained to be subsolar. At Z < 0.4 Z o˙, the allowed U drastically increases as the assumed metallicity decreases. For high ionization parameters, the N/O constraint becomes weak. Finally, our Cloudy models predict the location of B14-65666 on the BPT diagram, thereby allowing a comparison with low-redshift galaxies.

DOI： 10.3847/1538-4357/ac2a36

A VLA Survey of Late-time Radio Emission from Superluminous Supernovae and the Host Galaxies

Hatsukade Bunyo, Tominaga Nozomu, Morokuma Tomoki, Morokuma-Matsui Kana, Matsuda Yuichi, Tamura Yoichi, Niinuma Kotaro, Motogi Kazuhiro

ASTROPHYSICAL JOURNAL 922 巻 ( 1 ) 2021年11月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present the results of 3 GHz radio continuum observations of 23 superluminous supernovae (SLSNe) and their host galaxies by using the Karl G. Jansky Very Large Array conducted 5-21 yr after the explosions. The sample consists of 15 Type I and 8 Type II SLSNe at z < 0.3, providing one of the largest samples of SLSNe with late-time radio data. We detected radio emission from one SLSN (PTF10hgi) and five hosts with a significance of >5σ. No time variability is found in late-time radio light curves of the radio-detected sources in a timescale of years except for PTF10hgi, whose variability is reported in a separate study. Comparison of star formation rates (SFRs) derived from the 3 GHz flux densities with those derived from SED modeling based on UV-NIR data shows that four hosts have an excess of radio SFRs, suggesting obscured star formation. Upper limits for undetected hosts and stacked results show that the majority of the SLSN hosts do not have a significant obscured star formation. By using the 3 GHz upper limits, we constrain the parameters for afterglows arising from interaction between initially off-axis jets and circumstellar medium (CSM). We found that the models with higher energies (Eiso ≳ several × 1053 erg) and CSM densities (n ≳ 0.01 cm-3) are excluded, but lower energies or CSM densities are not excluded with the current data. We also constrained the models of pulsar wind nebulae powered by a newly born magnetar for a subsample of SLSNe with model predictions in the literature.

DOI： 10.3847/1538-4357/ac20d5

Accurate dust temperature determination in a z=7.13 galaxy

Bakx Tom J. L. C., Sommovigo Laura, Carniani Stefano, Ferrara Andrea, Akins Hollis B., Fujimoto Seiji, Hagimoto Masato, Knudsen Kirsten K., Pallottini Andrea, Tamura Yoichi, Watson Darach

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 508 巻 ( 1 ) 頁： L58 - L63 2021年11月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society: Letters

We report ALMA Band 9 continuum observations of the normal, dusty star-forming galaxy A1689-zD1 at z = 7.13, resulting in a ∼4.6 σ detection at 702 GHz. For the first time, these observations probe the far-infrared spectrum shortward of the emission peak of a galaxy in the Epoch of Reionization (EoR). Together with ancillary data from earlier works, we derive the dust temperature, Td, and mass, Md, of A1689-zD1 using both traditional modified blackbody spectral energy density fitting, and a new method that relies only on the [C ii] 158 μm line and underlying continuum data. The two methods give Td = (42+13-7, 40+13-) K, and Md} = (1.7+1.3-0.7, 2.0+1.8-1.0), ×, 107, M⊙. Band 9 observations improve the accuracy of the dust temperature (mass) estimate by ∼50 per cent (6 times). The derived temperatures confirm the reported increasing Td-redshift trend between z = 0 and 8; the dust mass is consistent with a supernova origin. Although A1689-zD1 is a normal UV-selected galaxy, our results, implying that ∼85 per cent of its star-formation rate is obscured, underline the non-negligible effects of dust in EoR galaxies.

DOI： 10.1093/mnrasl/slab104

Accurate dust temperature determination in a z = 7.13 galaxy

Bakx Tom J L C, Sommovigo Laura, Carniani Stefano, Ferrara Andrea, Akins Hollis B, Fujimoto Seiji, Hagimoto Masato, Knudsen Kirsten K, Pallottini Andrea, Tamura Yoichi, Watson Darach

Monthly Notices of the Royal Astronomical Society: Letters 508 巻 ( 1 ) 頁： L58 - L63 2021年11月

記述言語：英語掲載種別：研究論文（学術雑誌）

We report ALMA Band 9 continuum observations of the normal, dusty star-forming galaxy A1689-zD1 at z = 7.13, resulting in a ∼4.6 σ detection at 702 GHz. For the first time, these observations probe the far-infrared spectrum shortward of the emission peak of a galaxy in the Epoch of Reionization (EoR). Together with ancillary data from earlier works, we derive the dust temperature, Td, and mass, Md, of A1689-zD1 using both traditional modified blackbody spectral energy density fitting, and a new method that relies only on the [C ii] 158 μm line and underlying continuum data. The two methods give Td=(42^+13−7,40^+13−7⁠) K, and Md=(1.7^+1.3−0.7,2.0^+1.8−1.0)×10^7M⊙⁠. Band 9 observations improve the accuracy of the dust temperature (mass) estimate by ∼50 per cent (6 times). The derived temperatures confirm the reported increasing Td-redshift trend between z = 0 and 8; the dust mass is consistent with a supernova origin. Although A1689-zD1 is a normal UV-selected galaxy, our results, implying that ∼85 per cent of its star-formation rate is obscured, underline the non-negligible effects of dust in EoR galaxies.

ALMA Observations of Ly alpha Blob 1: Multiple Major Mergers and Widely Distributed Interstellar Media

Umehata Hideki, Smail Ian, Steidel Charles C., Hayes Matthew, Scott Douglas, Swinbank A. M., Ivison R. J., Nagao Toru, Kubo Mariko, Nakanishi Kouichiro, Matsuda Yuichi, Ikarashi Soh, Tamura Yoichi, Geach J. E.

ASTROPHYSICAL JOURNAL 918 巻 ( 2 ) 2021年9月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present observations of a giant Lyα blob (LAB) in the SSA22 protocluster at z = 3.1, SSA22-LAB1, taken with the Atacama Large Millimeter/submillimeter Array. Dust continuum, along with [C II] 158 μm and CO(4–3) line emission have been detected in LAB1, showing complex morphology and kinematics across a ∼100 kpc central region. Seven galaxies at z = 3.0987–3.1016 in the surroundings are identified in [C II] and dust continuum emission, with two of them potential companions or tidal structures associated with the most massive galaxies. Spatially resolved [C II] and infrared luminosity ratios for the widely distributed media (L[CII]/LIR ≈ 10-2-10-3) suggest that the observed extended interstellar media are likely to have originated from star formation activity and the contribution from shocked gas is probably not dominant. LAB1 is found to harbor a total molecular gas mass Mmol = (8.7 ± 2.0) × 1010 Me, concentrated in the core region of the Lyα-emitting area. While (primarily obscured) star formation activity in the LAB1 core is one of the most plausible power sources for the Lyα emission, multiple major mergers found in the core may also play a role in making LAB1 exceptionally bright and extended in Lyα as a result of cooling radiation induced by gravitational interactions.

DOI： 10.3847/1538-4357/ac1106

A Massive Quiescent Galaxy Confirmed in a Protocluster at z=3.09

Kubo Mariko, Umehata Hideki, Matsuda Yuichi, Kajisawa Masaru, Steidel Charles C., Yamada Toru, Tanaka Ichi, Hatsukade Bunyo, Tamura Yoichi, Nakanishi Kouichiro, Kohno Kotaro, Lee Kianhong, Matsuda Keiichi

ASTROPHYSICAL JOURNAL 919 巻 ( 1 ) 頁： 6 - 6 2021年9月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We report a massive quiescent galaxy at zspec= -3.0922+0.008-0.004 spectroscopically confirmed at a protocluster in the SSA22 field by detecting the Balmer and Ca II absorption features with the multi-object spectrometer for infrared exploration on the Keck I telescope. This is the most distant quiescent galaxy confirmed in a protocluster to date. We fit the optical to mid-infrared photometry and spectrum simultaneously with spectral energy distribution (SED) models of parametric and nonparametric star formation histories (SFHs). Both models fit the observed SED well and confirm that this object is a massive quiescent galaxy with a stellar mass of log (M∗/M⊙=11.26+0.03-0.04 and 11.54+0.03-0.00 and a star formation rate of SFR/M⊙ yr-1 < 0.3 and = -0.01+0.03-0.01 for parametric and nonparametric models, respectively. The SFH from the former modeling is described as an instantaneous starburst whereas that of the latter modeling is longer-lived, but both models agree with a sudden quenching of the star formation at ~0.6 Gyr ago. This massive quiescent galaxy is confirmed in an extremely dense group of galaxies predicted as a progenitor of a brightest cluster galaxy formed via multiple mergers in cosmological numerical simulations. We discover three new plausible [O III]λ5007 emitters at 3.0791 ≤ zspec ≤ 3.0833 serendipitously detected around the target. Two of them just between the target and its nearest massive galaxy are possible evidence of their interactions. They suggest the future great size and stellar mass evolution of this massive quiescent galaxy via mergers.

DOI： 10.3847/1538-4357/ac0cf8

A Data-scientific Noise-removal Method for Efficient Submillimeter Spectroscopy With Single-dish Telescopes

Taniguchi Akio, Tamura Yoichi, Ikeda Shiro, Takekoshi Tatsuya, Kawabe Ryohei

ASTRONOMICAL JOURNAL 162 巻 ( 3 ) 2021年9月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astronomical Journal

For submillimeter spectroscopy with ground-based single-dish telescopes, removing the noise contribution from the Earth's atmosphere and the instrument is essential. For this purpose, here we propose a new method based on a data-scientific approach. The key technique is statistical matrix decomposition that automatically separates the signals of astronomical emission lines from the drift noise components in the fast-sampled (1-10 Hz) time-series spectra obtained by a position-switching (PSW) observation. Because the proposed method does not apply subtraction between two sets of noisy data (i.e., on-source and off-source spectra), it improves the observation sensitivity by a factor of 2 . It also reduces artificial signals such as baseline ripples on a spectrum, which may also help to improve the effective sensitivity. We demonstrate this improvement by using the spectroscopic data of emission lines toward a high-redshift galaxy observed with a 2 mm receiver on the 50 m Large Millimeter Telescope. Since the proposed method is carried out offline and no additional measurements are required, it offers an instant improvement on the spectra reduced so far with the conventional method. It also enables efficient deep spectroscopy driven by the future 50 m class large submillimeter single-dish telescopes, where fast PSW observations by mechanical antenna or mirror drive are difficult to achieve.

DOI： 10.3847/1538-3881/ac11f7

Physical Characterization of Serendipitously Uncovered Millimeter-wave Line-emitting Galaxies at z similar to 2.5 behind the Local Luminous Infrared Galaxy VV 114

Mizukoshi Shoichiro, Kohno Kotaro, Egusa Fumi, Hatsukade Bunyo, Minezaki Takeo, Saito Toshiki, Tamura Yoichi, Iono Daisuke, Ueda Junko, Matsuda Yuichi, Kawabe Ryohei, Lee Minju M., Yun Min S., Espada Daniel

ASTROPHYSICAL JOURNAL 917 巻 ( 2 ) 2021年8月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present a detailed investigation of millimeter-wave line emitters ALMA J010748.3-173028 (ALMA-J0107a) and ALMA J010747.0-173010 (ALMA-J0107b), which were serendipitously uncovered in the background of the nearby galaxy VV 114 with spectral scan observations at λ = 2-3 mm. Via Atacama Large Millimeter/submillimeter Array (ALMA) detection of CO(4-3), CO(3-2), and [C i](1-0) lines for both sources, their spectroscopic redshifts are unambiguously determined to be z = 2.4666 0.0002 and z = 2.3100 0.0002, respectively. We obtain the apparent molecular gas masses M gas of these two line emitters from [C i] line fluxes as (11.2 3.1) 1010 M o˙ and (4.2 1.2) 1010 M o˙, respectively. The observed CO(4-3) velocity field of ALMA-J0107a exhibits a clear velocity gradient across the CO disk, and we find that ALMA-J0107a is characterized by an inclined rotating disk with a significant turbulence, that is, a deprojected maximum rotation velocity to velocity dispersion ratio of 1.3 0.3. We find that the dynamical mass of ALMA-J0107a within the CO-emitting disk computed from the derived kinetic parameters, (1.1 0.2) 1010 M o˙, is an order of magnitude smaller than the molecular gas mass derived from dust continuum emission, (3.2 1.6) 1011 M o˙. We suggest this source is magnified by a gravitational lens with a magnification of μ ⪆ 10, which is consistent with the measured offset from the empirical correlation between CO-line luminosity and width.

DOI： 10.3847/1538-4357/ac01cc

J-GEM optical and near-infrared follow-up of gravitational wave events during LIGO's and Virgo's third observing run

Sasada Mahito, Utsumi Yousuke, Itoh Ryosuke, Tominaga Nozomu, Tanaka Masaomi, Morokuma Tomoki, Yanagisawa Kenshi, Kawabata Koji S., Ohgami Takayuki, Yoshida Michitoshi, Abe Fumio, Adachi Ryo, Akitaya Hiroshi, Chong Yang, Daikuhara Kazuki, Hamasaki Ryo, Honda Satoshi, Hosokawa Ryohei, Iida Kota, Imazato Fumiya, Ishioka Chihiro, Iwasaki Takumi, Jian Mingjie, Kamei Yuhei, Kanai Takahiro, Kaneda Hidehiro, Kaneko Ayane, Katoh Noriyuki, Kawai Nobuyuki, Kubota Keiichiro, Kubota Yuma, Mamiya Hideo, Matsubayashi Kazuya, Morihana Kumiko, Murata Katsuhiro L., Nagayama Takahiro, Nakamura Noriatsu, Nakaoka Tatsuya, Niino Yuu, Nishinaka Yuki, Niwano Masafumi, Nogami Daisaku, Oasa Yumiko, Oeda Miki, Ogawa Futa, Ohsawa Ryou, Ohta Kouji, Oide Kohei, Onozato Hiroki, Sako Shigeyuki, Saito Tomoki, Sekiguchi Yuichiro, Shigeyama Toshikazu, Shigeyoshi Takumi, Shikauchi Minori, Shiraishi Kazuki, Suzuki Daisuke, Takagi Kengo, Takahashi Jun, Takarada Takuya, Takayama Masaki, Takeuchi Himeka, Tamura Yasuki, Tanaka Ryoya, Toma Sayaka, Tozuka Miyako, Uchida Nagomi, Uzawa Yoshinori, Yamanaka Masayuki, Yasuda Moeno, Yatsu Yoichi

PROGRESS OF THEORETICAL AND EXPERIMENTAL PHYSICS 2021 巻 ( 5 ) 2021年5月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Progress of Theoretical and Experimental Physics

The Laser Interferometer Gravitational-wave Observatory Scientific Collaboration and Virgo Collaboration (LVC) sent out 56 gravitational-wave (GW) notices during the third observing run (O3). The Japanese Collaboration for Gravitational wave ElectroMagnetic follow-up (J-GEM) performed optical and near-infrared observations to identify and observe an electromagnetic (EM) counterpart. We constructed a web-based system that enabled us to obtain and share information on candidate host galaxies for the counterpart, and the status of our observations. Candidate host galaxies were selected from the GLADE catalog with a weight based on the 3D GW localization map provided by LVC. We conducted galaxy-targeted and wide-field blind surveys, real-time data analysis, and visual inspection of observed galaxies. We performed galaxy-targeted follow-ups to 23 GW events during O3, and the maximum probability covered by our observations reached 9.8%. Among these, we successfully started observations for 10 GW events within 0.5 days after the detection. This result demonstrates that our follow-up observation has the potential to constrain EM radiation models for a merger of binary neutron stars at a distance of up to ∼100 Mpc with a probability area of ≤ 500 deg 2.

DOI： 10.1093/ptep/ptab007

Variability of Late-time Radio Emission in the Superluminous Supernova PTF10hgi

Hatsukade Bunyo, Tominaga Nozomu, Morokuma Tomoki, Morokuma-Matsui Kana, Tamura Yoichi, Niinuma Kotaro, Hayashi Masao, Matsuda Yuichi, Motogi Kazuhiro

ASTROPHYSICAL JOURNAL LETTERS 911 巻 ( 1 ) 頁： L1 - L1 2021年4月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal Letters

We report the time variability of the late-time radio emission in a Type I superluminous supernova (SLSN), PTF10hgi, at z = 0.0987. The Karl G. Jansky Very Large Array 3 GHz observations at 8.6 and 10 yr after the explosion both detected radio emission with a ∼40% decrease in flux density in the second epoch. This is the first report of a significant variability of the late-time radio light curve in an SLSN. Through combination with previous measurements in two other epochs, we constrained both the rise and decay phases of the radio light curve over three years, peaking at approximately 8-9 yr after the explosion with a peak luminosity of L3 GHz = 2 × 1021WHz-1. Possible scenarios for the origin of the variability are an active galactic nucleus (AGN) in the host galaxy, an afterglow caused by the interaction between an off-axis jet and circumstellar medium, and a wind nebula powered by a newly born magnetar. Comparisons with models show that the radio light curve can be reproduced by both the afterglow model and magnetar wind nebula model. Considering the flat radio spectrum at 1-15 GHz and an upper limit at 0.6 GHz obtained in previous studies, plausible scenarios are a low-luminosity flat-spectrum AGN or a magnetar wind nebula with a shallow injection spectral index. © 2021 The American Astronomical Society. All rights reserved.

DOI： 10.3847/2041-8213/abef03

その他リンク： https://iopscience.iop.org/article/10.3847/2041-8213/abef03/pdf

Revisited Cold Gas Content with Atomic Carbon [CI] in z=2.5 Protocluster Galaxies 査読有り

Lee Minju M., Tanaka Ichi, Iono Daisuke, Kawabe Ryohei, Kodama Tadayuki, Kohno Kotaro, Saito Toshiki, Tamura Yoichi

ASTROPHYSICAL JOURNAL 909 巻 ( 2 ) 頁： 181 - 181 2021年3月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We revisit the cold gas contents of galaxies in a protocluster at z = 2.49 using the lowest neutral atomic carbon transition [C i] 3 P 1 - 3 P 0 from Atacama Large Millimeter/submillimeter Array observations. We aim to test if the same gas-mass calibration adopted in field galaxies can be applied to protocluster galaxies. Five galaxies out of 16 targeted galaxies are detected in the [C i] line, and these are all previously detected in CO (3-2) and CO (4-3) and three in 1.1 mm dust continuum. We investigate the line luminosity relations between CO and [C i] in the protocluster and compare with other previous studies. We then compare the gas mass based on three gas tracers of [C i], CO(3-2), and dust if at least one of the last two tracers are available. Using the calibration adopted for field main-sequence galaxies, the [C i]-based gas measurements are lower than or comparable to the CO-based gas measurements by -0.35 dex at the lowest with the mean deviation of -0.14 dex. The differences between [C i]- and the dust- based measurements are relatively mild by up to 0.16 dex with the mean difference of 0.02 dex. Taking these all together with calibration uncertainties, with the [C i] line, we reconfirm our previous findings that the mean gas fraction is comparable to field galaxies for a stellar-mass range of . However, at least for these secure five detections, the depletion timescale decreases more rapidly with stellar mass than field galaxies that might be related to earlier quenching in dense environments.

DOI： 10.3847/1538-4357/abdbb5

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/abdbb5/pdf

A puzzling non-detection of [OIII] and [CII] from a z approximate to 7.7 galaxy observed with ALMA 査読有り

Binggeli C., Inoue A. K., Hashimoto T., Toribio M. C., Zackrisson E., Ramstedt S., Mawatari K., Harikane Y., Matsuo H., Okamoto T., Ota K., Shimizu I, Tamura Y., Taniguchi Y., Umehata H.

ASTRONOMY & ASTROPHYSICS 646 巻頁： A26 - A26 2021年2月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astronomy and Astrophysics

Context. Characterizing the galaxy population in the early Universe holds the key to understanding the evolution of these objects and the role they played in cosmic reionization. However, there have been very few observations at the very highest redshifts to date. Aims. In order to shed light on the properties of galaxies in the high-redshift Universe and their interstellar media, we observe the Lyman-α emitting galaxy z7_GSD_3811 at z = 7.664 with bands 6 and 8 at the Atacama Large Millimeter/submillimeter Array (ALMA). Methods. We target the far-infrared [O iii] 88 µm and [C ii] 158 µm emission lines and dust continuum in the star-forming galaxy z7_GSD_3811 with ALMA. We combine these measurements with earlier observations in the rest-frame ultraviolet (UV) in order to characterize the object and compare the results to those of earlier studies that observed [O iii] and [C ii] emission in high-redshift galaxies. Results. The [O iii] 88 µm and [C ii] 158 µm emission lines are undetected at the position of z7_GSD_3811, with 3σ upper limits of 1.6 × 108 L and 4.0 × 107 L, respectively. We do not detect any dust continuum in band 6 nor band 8. The measured rms in the band 8 and band 6 continua are 26 and 9.9 µJy beam−1, respectively. Similar to several other high-redshift galaxies, z7_GSD_3811 exhibits low [C ii] emission for its star formation rate compared to local galaxies. Furthermore, our upper limit on the [O iii] line luminosity is lower than the previously observed [O iii] lines in high-redshift galaxies with similar UV luminosities. Our ALMA band 6 and 8 dust continuum observations imply that z7_GSD_3811 likely has a low dust content, and our non-detections of the [O iii] and [C ii] lines could indicate that z7_GSD_3811 has a low metallicity (Z. 0.1 Z).

DOI： 10.1051/0004-6361/202038180

Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XII. Extended [C ii] Structure (Merger or Outflow) in a z=6.72 Red Quasar 査読有り

Izumi Takuma, Onoue Masafusa, Matsuoka Yoshiki, Strauss Michael A., Fujimoto Seiji, Umehata Hideki, Imanishi Masatoshi, Kawamuro Taiki, Nagao Tohru, Toba Yoshiki, Kohno Kotaro, Kashikawa Nobunari, Inayoshi Kohei, Kawaguchi Toshihiro, Iwasawa Kazushi, Inoue Akio K., Goto Tomotsugu, Baba Shunsuke, Schramm Malte, Suh Hyewon, Harikane Yuichi, Ueda Yoshihiro, Silverman John D., Hashimoto Takuya, Hashimoto Yasuhiro, Ikarashi Soh, Iono Daisuke, Lee Chien-Hsiu, Lee Kianhong, Minezaki Takeo, Nakanishi Kouichiro, Nakano Suzuka, Tamura Yoichi, Tang Ji-Jia

ASTROPHYSICAL JOURNAL 908 巻 ( 2 ) 頁： 235 - 235 2021年2月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present Atacama Large Millimeter/submillimeter Array [C ii] 158 μm line and far-infrared (FIR) continuum emission observations toward HSC J120505.09-000027.9 (J1205-0000) at z = 6.72 with a beam size of ∼0.″8 × 0.″5 (or 4.1 kpc × 2.6 kpc), the most distant red quasar known to date. Red quasars are modestly reddened by dust and are thought to be in rapid transition from an obscured starburst to an unobscured normal quasar, driven by powerful active galactic nucleus (AGN) feedback that blows out a cocoon of interstellar medium. The FIR continuum of J1205-0000 is bright, with an estimated luminosity of L FIR ∼ 3 × 1012 L o˙. The [C ii] line emission is extended on scales of r ∼ 5 kpc, greater than that of the FIR continuum. The line profiles at the extended regions are complex and broad (FWHM ∼ 630-780 km s-1). Although it is not practical to identify the nature of this extended structure, possible explanations include (i) companion/merging galaxies and (ii) massive AGN-driven outflows. For the case of (i), the companions are modestly star-forming (∼10 M o˙ yr-1) but are not detected by our Subaru optical observations (y AB,5σ = 24.4 mag). For the case of (ii), our lower limit to the cold neutral outflow rate is ∼100 M o˙ yr-1. The outflow kinetic energy and momentum are both much lower than predicted in energy-conserving wind models, suggesting that the AGN feedback in this quasar is not capable of completely suppressing its star formation.

DOI： 10.3847/1538-4357/abd7ef

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/abd7ef/pdf

The University of Tokyo atacama observatory 6.5m telescope: On-sky performance evaluations of the mid-infrared instrument MIMIZUKU on the Subaru telescope

Kamizuka T., Miyata T., Sako S., Ohsawa R., Asano K., Uchiyama M.S., Mori T., Yoshida Y., Tachibana K., Michifuji T., Uchiyama M., Sakon I., Onaka T., Kataza H., Aoki T., Doi M., Hatsukade B., Kato N., Kohno K., Konishi M., Minezaki T., Morokuma T., Numata M., Motohara K., Sameshima H., Soyano T., Takahashi H., Tanabé T., Tanaka M., Tarusawa K., Koshida S., Tamura Y., Terao Y., Kushibiki K., Nakamura H., Yoshii Y.

Proceedings of SPIE - The International Society for Optical Engineering 11447 巻頁： 114475X 2020年12月

記述言語：英語掲載種別：研究論文（国際会議プロシーディングス）出版者・発行元：Proceedings of SPIE - The International Society for Optical Engineering

The Mid-Infrared Multi-field Imager for gaZing at the UnKnown Universe (MIMIZUKU) is developed as the first-generation mid-infrared instrument for the University of Tokyo Atacama Observatory (TAO) 6.5-m telescope. MIMIZUKU performs medium-band imaging and low-resolution spectroscopy (R ∼100-600) in 2-38 µm and enables highest-spatial-resolution observations in the long-wavelength mid-infrared beyond 25 µm. In addition, MIMIZUKU has a unique optical device called 'Field Stacker', which enables us to observe a distant (<25 arcmin) pair of a target and a reference object simultaneously and improves accuracy of atmospheric calibration. This function is expected to improve photometric accuracy and quality of spectroscopic data even in the long-wavelength mid-infrared regions, where the atmospheric absorption is severe. In 2018, engineering observations of MIMIZUKU at the Subaru telescope were carried out, and its first-light was successfully achieved. In the engineering observations, we evaluated the imaging and spectroscopic functions in the mid-infrared wavelengths (7-26 µm) and found that MIMIZUKU has the performance of spatial resolution, spectral resolution, and system efficiency almost as designed. The Field Stacker was also tested, and it was confirmed that the Field Stacker device enables us to perform spectroscopic observations not only in the 10-µm band but also in the 20-µm band, where the spectroscopic observations are difficult even at the Maunakea site. We report the results of these on-sky performance evaluations.

DOI： 10.1117/12.2560789

The University of Tokyo Atacama Observatory 6.5m Telescope: Overview and construction status

Yoshii Y., Doi M., Miyata T., Kohno K., Tanaka M., Minezaki T., Sako S., Morokuma T., Tanabe T., Hatsukade B., Konishi M., Kamizuka T., Asano K., Sameshima H., Kato N., Numata M., Takahashi H., Aoki T., Soyano T., Tarusawa K., Yoshikawa K., Motohara K., Tamura Y., Koshida S., Handa T., Bronfman L., Ruiz M., Hamuy M., Mendez R., Escala A.

Proceedings of SPIE - The International Society for Optical Engineering 11445 巻頁： 1144514 2020年12月

記述言語：英語掲載種別：研究論文（国際会議プロシーディングス）出版者・発行元：Proceedings of SPIE - The International Society for Optical Engineering

Institute of Astronomy, Graduate School of Science, the University of Tokyo is promoting the University of Tokyo Atacama Observatory Project, which is to construct an infrared-optimized 6.5m telescope at the summit of Co. Chajnantor (5640m altitude) in northern Chile. The high altitude and dry climate (PWV-0.5mm) realize transparent atmosphere in the infrared wavelength. The project is now approaching the final phase of the construction. Production of major components are almost completed: Production and preassembly test of a telescope mount and dome enclosure have been completed in Japan, and they are being transported to Chile. Three mirrors, the 6.5m primary, 0.9m secondary, and 1.1m-0.75m tertiary mirrors and their support systems have been all completed and tested in the USA. An aluminizing chamber have been fabricated in China, and its tests have been carried out in Japan. Development of two facility instruments, SWIMS and MIMIZUKU, are also completed. They were transported to the Subaru telescope, successfully saw the first light in 2018, and are confirmed to have the performance as designed. On-site construction work at the summit is now underway. Expansion of a summit access road from the ALMA concession was completed in 2019. Installation of foundation will follow, and then erection of the dome enclosure and a control building. The construction works are delayed by COVID-19, and we expect to complete the dome enclosure by Q3 of 2021. The telescope will be installed inside the dome and see the engineering first light by early 2022.

DOI： 10.1117/12.2560238

Wind- and Operation-Induced Vibration Measurements of the Main Reflector of the Nobeyama 45 m Radio Telescope 査読有り

Hashimoto Ikumi, Chiba Masakatsu, Okada Nozomi, Ogawa Hideo, Kawabe Ryohei, Minamidani Tetsuhiro, Tamura Yoichi, Kimura Kimihiro

JOURNAL OF VIBRATION ENGINEERING & TECHNOLOGIES 8 巻 ( 6 ) 頁： 909 - 923 2020年12月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Journal of Vibration Engineering and Technologies

Purpose: As deformations of the main reflector of a radio telescope directly affect the observations, the evaluation of the deformation is extremely important. Dynamic characteristics of the main reflector of the Nobeyama 45 m Radio Telescope, Japan, are measured under two conditions: the first is when the pointing observation is in operation, and the second is when the reflector is stationary and is subjected to wind loads when the observation is out of operation. Methods: Dynamic characteristics of the main reflector are measured using piezoelectric accelerometers. Results and Conclusion: When the telescope is in operation, a vibration mode with one nodal line horizontally or vertically on the reflector is induced, depending on whether the reflector is moving in the azimuthal or elevational planes, whereas under windy conditions, vibration modes that have two to four nodal lines are simultaneously induced. The predominant mode is dependent on the direction of wind loads.

DOI： 10.1007/s42417-020-00202-9

ALMA Deep Field in SSA22: A near-infrared-dark submillimeter galaxy at z=4.0 査読有り

Umehata Hideki, Smail Ian, Swinbank A. M., Kohno Kotaro, Tamura Yoichi, Wang Tao, Ao Yiping, Hatsukade Bunyo, Kubo Mariko, Nakanishi Kouchiro, Hayatsu Natsuki N.

ASTRONOMY & ASTROPHYSICS 640 巻頁： L8 - L8 2020年8月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astronomy and Astrophysics

Deep surveys with the Atacama Large Millimeter Array (ALMA) have uncovered a population of dusty star-forming galaxies which are faint or even undetected at optical to near-infrared wavelengths. Their faintness at short wavelengths makes the detailed characterization of the population challenging. Here we present a spectroscopic redshift identification and a characterization of one of these near-infrared-dark galaxies discovered by an ALMA deep survey. The detection of [Ca I](1-0) and CO(4-3) emission lines determines the precise redshift of the galaxy, ADF22.A2, to be za =a 3.9913a ±a 0.0008. On the basis of a multi-wavelength analysis, ADF22.A2 is found to be a massive, star-forming galaxy with a stellar mass of Ma - = 1.1-0.6+1.3 × 1011 MaS and SFR = 430-150+230a MaS yr-1. The molecular gas mass was derived to be M(H2)[CI]a =a (5.9a ±a 1.5)×1010a MaS , indicating a gas fraction of ≈35%, and the ratios of L[CI](1-0)/LIR and L[CI](1-0)/LCO(4-3) suggest that the nature of the interstellar medium in ADF22.A2 is in accordance with those of other bright submillimeter galaxies. The properties of ADF22.A2, including the redshift, star-formation rate, stellar mass, and depletion time scale (τdepa ≈a 0.1-0.2 Gyr), also suggest that ADF22.A2 has the characteristics expected for the progenitors of quiescent galaxies at zaaa 3. Our results demonstrate the power of ALMA contiguous mapping and line scan, which help us to obtain an unbiased view of galaxy formation in the early Universe.

DOI： 10.1051/0004-6361/202038146

ALMA twenty-six arcmin(2) survey of GOODS-S at one millimeter (ASAGAO): Millimeter properties of stellar mass selected galaxies 査読有り

Yamaguchi Yuki, Kohno Kotaro, Hatsukade Bunyo, Wang Tao, Yoshimura Yuki, Ao Yiping, Dunlop James S., Egami Eiichi, Espada Daniel, Fujimoto Seiji, Hayatsu Natsuki H., Ivison Rob J., Kodama Tadayuki, Kusakabe Haruka, Nagao Tohru, Ouchi Masami, Rujopakarn Wiphu, Tadaki Ken-ichi, Tamura Yoichi, Ueda Yoshihiro, Umehata Hideki, Wang Wei-Hao

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 72 巻 ( 4 ) 頁： 69 2020年8月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

We make use of the ALMA twenty-Six Arcmin2 survey of GOODS-S At One-millimeter (ASAGAO), deep 1.2 mm continuum observations of a 26-arcmin2 region in the Great Observatories Origins Deep Survey-South (GOODS-S) obtained with Atacama Large Millimeter/sub-millimeter Array (ALMA), to probe dust-enshrouded star formation in K-band selected (i.e., stellar mass selected) galaxies, which are drawn from the FourStar Galaxy Evolution Survey (ZFOURGE) catalog. Based on the ASAGAO combined map, which was created by combining ASAGAO and ALMA archival data in the GOODS-South field, we find that 24 ZFOURGE sources have 1.2 mm counterparts with a signal-to-noise ratio >4.5 (1σ ≃ 30-70 μJy beam−1 at 1.2 mm). Their median redshift is estimated to be zmedian = 2.38 ± 0.14. They generally follow the tight relationship of the stellar mass versus star formation rate (i.e., the main sequence of star-forming galaxies). ALMA-detected ZFOURGE sources exhibit systematically larger infrared (IR) excess (IRX ≡ LIR/LUV) compared to ZFOURGE galaxies without ALMA detections even though they have similar redshifts, stellar masses, and star formation rates. This implies the consensus stellar-mass versus IRX relation, which is known to be tight among rest-frame-ultraviolet-selected galaxies, cannot fully predict the ALMA detectability of stellar-mass-selected galaxies. We find that ALMA-detected ZFOURGE sources are the main contributors to the cosmic IR star formation rate density at z = 2-3.

DOI： 10.1093/pasj/psaa057

その他リンク： http://academic.oup.com/pasj/article-pdf/72/4/69/33562710/psaa057.pdf

Spatially resolved molecular gas properties of host galaxy of Type I superluminous supernova SN 2017egm 査読有り

Hatsukade Bunyo, Morokuma-Matsui Kana, Hayashi Masao, Tominaga Nozomu, Tamura Yoichi, Niinuma Kotaro, Motogi Kazuhiro, Morokuma Tomoki, Matsuda Yuichi

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 72 巻 ( 4 ) 頁： L6 2020年8月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

We present the results of CO(1-0) observations of the host galaxy of a Type I superluminous supernova (SLSN-I), SN 2017egm, one of the closest SLSNe-I at z = 0.03063, by using the Atacama Large Millimeter/submillimeter Array. The molecular gas mass of the host galaxy is Mgas = (4.8 ± 0.3) × 109 M☉, placing it on the sequence of normal star-forming galaxies in an Mgas-star-formation rate (SFR) plane. The molecular hydrogen column density at the location of SN 2017egm is higher than that of the Type II SN PTF10bgl, which is also located in the same host galaxy, and those of other Type II and Ia SNe located in different galaxies, suggesting that SLSNe-I have a preference for a dense molecular gas environment. On the other hand, the column density at the location of SN 2017egm is comparable to those of Type Ibc SNe. The surface densities of molecular gas and the SFR at the location of SN 2017egm are consistent with those of spatially resolved local star-forming galaxies and follow the Schmidt-Kennicutt relation. These facts suggest that SLSNe-I can occur in environments with the same star-formation mechanism as in normal star-forming galaxies.

DOI： 10.1093/pasj/psaa052

Detections of far-infrared [OIII] and dust emission in a galaxy at z = 8.312: Early metal enrichment in the heart of the reionization era 国際共著国際誌

Tamura Y., Mawatari K., Hashimoto T., Inoue A.K., Zackrissonm E., Christensen L., Binggeli C., Matsuda Y., Matsuo H., Takeuchi T.T., Asano R.S., Sunaga K., Shimizu I., Okamoto T., Yoshida N., Lee M., Shibuya T., Taniguchi Y., Umehata H., Hatsukade B., Kohno K., Ota K.

Proceedings of the International Astronomical Union 15 巻 ( S341 ) 頁： 211 - 215 2020年6月

担当区分：筆頭著者,　責任著者記述言語：英語掲載種別：研究論文（国際会議プロシーディングス）出版者・発行元：Proceedings of the International Astronomical Union

We present ALMA detection of the [O iii] 88 μm line and 850 μm dust continuum emission in a Y-dropout Lyman break galaxy, MACS0416-Y1. The [O iii] detection confirms the object with a spectroscopic redshift to be z = 8.3118±0.0003. The 850 μm continuum intensity (0.14 mJy) implies a large dust mass on the order of 4×106M . The ultraviolet-to-far infrared spectral energy distribution modeling, where the [O iii] emissivity model is incorporated, suggests the presence of a young (τage 4 Myr), star-forming (SFR 60M yr-1), and moderately metal-polluted (Z 0.2Z ) stellar component with a stellar mass of 3 × 108M . An analytic dust mass evolution model with a single episode of star formation does not reproduce the metallicity and dust mass in 4 Myr, suggesting an underlying evolved stellar component as the origin of the dust mass.

DOI： 10.1017/s1743921319002436

その他リンク： http://stacks.iop.org/0004-637X/874/i=1/a=27?key=crossref.08977684a624e2093b8b0428fd4f056e

Large Population of ALMA Galaxies atz > 6 with Very High [Oiii] 88 mu m to [Cii] 158 mu m Flux Ratios: Evidence of Extremely High Ionization Parameter or PDR Deficit? 査読有り

Harikane Yuichi, Ouchi Masami, Inoue Akio K., Matsuoka Yoshiki, Tamura Yoichi, Bakx Tom, Fujimoto Seiji, Moriwaki Kana, Ono Yoshiaki, Nagao Tohru, Tadaki Ken-ichi, Kojima Takashi, Shibuya Takatoshi, Egami Eiichi, Ferrara Andrea, Gallerani Simona, Hashimoto Takuya, Kohno Kotaro, Matsuda Yuichi, Matsuo Hiroshi, Pallottini Andrea, Sugahara Yuma, Vallini Livia

ASTROPHYSICAL JOURNAL 896 巻 ( 2 ) 2020年6月

ALMA detection of the [OIII] 88 μm line in a highly-magnified Lyman break galaxy at z = 6.1 国際誌

Sunaga K., Tamura Y., Lee M., Mawatari K., Inoue A.K., Hashimoto T., Matsuo H., Taniguchi A.

Proceedings of the International Astronomical Union 15 巻 ( S341 ) 頁： 309 - 311 2020年6月

担当区分：責任著者記述言語：英語掲載種別：研究論文（国際会議プロシーディングス）出版者・発行元：Proceedings of the International Astronomical Union

We present a 4.7σ detection of the [OIII] 88 μm line in a gravitationally-lensed Lyman break galaxy, RXC J2248-ID3, using the Atacama Large Millimeter/submillimeter Array (ALMA). We did not detect [CII] 158 μm and rest-frame 90 μm dust continuum emission, suggesting that the bulk of the interstellar medium (ISM) is ionized. Our two-component SED model combining the previous Hubble Space Telescope (HST) data and new photometry obtained from Very Large Telescope (VLT), Spitzer and ALMA suggests the presence of young (∼2 Myr) and mature (∼600 Myr) stellar components with the metallicity of Z = 0.2Z . Our findings are in contrast with previous results claiming a very young, metal-poor stellar component.

DOI： 10.1017/s174392131900245x

Rapid evolution and transformation into quiescence?: ALMA view on z > 6 low-luminosity quasars 国際誌 Open Access

Izumi T., Onoue M., Matsuoka Y., Nagao T., Strauss M.A., Imanishi M., Kashikawa N., Fujimoto S., Kohno K., Toba Y., Umehata H., Goto T., Ueda Y., Shirakata H., Silverman J.D., Greene J.E., Harikane Y., Hashimoto Y., Ikarashi S., Iono D., Iwasawa K., Lee C.H., Minezaki T., Nakanishi K., Tamura Y., Tang J.J., Taniguchi A.

Proceedings of the International Astronomical Union 15 巻 ( S352 ) 頁： 139 - 143 2020年6月

記述言語：英語掲載種別：研究論文（国際会議プロシーディングス）出版者・発行元：Proceedings of the International Astronomical Union

We present ALMA [CII] line and far-infrared (FIR) continuum observations of seven z > 6 low-luminosity quasars (M1450 > -25 mag) discovered by our on-going Subaru Hyper Suprime-Cam survey. The [CII] line was detected in all targets with luminosities of ∼(2-10) × 108 Lo, about one order of magnitude smaller than optically luminous quasars. Also found was a wide scatter of FIR continuum luminosity, ranging from LFIR < 1011Lo to 1/42 × 1012Lo. With the [CII]-based dynamical mass, we suggest that a significant fraction of low-luminosity quasars are located on or even below the local Magorrian relation, particularly at the massive end of the galaxy mass distribution. This is a clear contrast to the previous finding that luminous quasars tend to have overmassive black holes relative to the relation. Our result is expected to show a less-biased nature of the early co-evolution of black holes and their host galaxies.

DOI： 10.1017/s1743921319009487

Panchromatic Analysis for Nature of HIgh-z galaxies Tool (PANHIT) 国際誌

Mawatari K., Inoue A.K., Yamanaka S., Hashimoto T., Tamura Y.

Proceedings of the International Astronomical Union 15 巻 ( S341 ) 頁： 285 - 286 2020年6月

記述言語：英語掲載種別：研究論文（国際会議プロシーディングス）出版者・発行元：Proceedings of the International Astronomical Union

We have developed a new SED fitting tool specialized for frontier redshift galaxies. It is a common case for high-z galaxies that the available data are restricted to rich optical to near-infrared photometry and few far-infrared (FIR) data deep enough to detect the faint object (e.g., HST/WFC3 + Spitzer/IRAC + ALMA). In such situation, one cannot perform a complicated modeling of dust emission in FIR regime. We then adopt simple treatment for the dust emission using empirical LIRG templates. Instead, we adopt a sophisticated and physically motivated modeling for stellar and nebular emission parts in rest-frame UV-to-optical regime. Our new code fits not only broad band photometry but also spectral emission line flux. There is an option to fit observed SED with two templates with different physical properties. Our new code, PANHIT, is now in public, and was already applied to some high-z frontier galaxies.

DOI： 10.1017/s1743921319002606

Dust evolution in galaxies at z > 7 国際誌

Takeuchi T.T., Asano R.S., Nagasaki S., Nozawa T., Tamura Y., Mawatari K., Inoue A.K.

Proceedings of the International Astronomical Union 15 巻 ( S341 ) 頁： 312 - 313 2020年6月

記述言語：英語掲載種別：研究論文（国際会議プロシーディングス）出版者・発行元：Proceedings of the International Astronomical Union

Recently huge amount of dust Mdust ≃ 106-7M in galaxies at z = 7-8 has been discovered by ALMA observations. The suggested timescale of the dust production was a few-several×108 yr, while the stellar mass was several × 109M . This amount of dust cannot be easily explained only by a supply from supernovae if we consider the dust destruction by reverse shocks. We propose that these values can be consistently explained if we take into account the grain growth in the interstellar medium (ISM). This scenario successfully reproduces the evolution of the dust mass, as well as the SFR, and stellar mass simultaneously. We conclude that even at such an early epoch of the Universe, the dust grain growth in the ISM plays a significant role in galaxies.

DOI： 10.1017/s1743921319003107

ALMA Observations of Molecular Gas in the Host Galaxies of Long-duration GRBs 国際誌

Hatsukade, Bunyo, Ohta, Kouji, Hashimoto, Tetsuya, Kohno, Kotaro, Nakanishi, Kouichiro, Niino, Yuu, Tamura, Yoichi

Yamada Conference LXXI: Gamma-ray Bursts in the Gravitational Wave Era 2019 頁： 157 - 159 2020年5月

DESHIMA on ASTE: On-Sky Responsivity Calibration of the Integrated Superconducting Spectrometer 査読有り

Takekoshi Tatsuya, Karatsu Kenichi, Suzuki Junya, Tamura Yoichi, Oshima Tai, Taniguchi Akio, Asayama Shin'ichiro, Bakx Tom J. L. C., Baselmans Jochem J. A., Bosma Sjoerd, Bueno Juan, Chin Kah Wuy, Fujii Yasunori, Fujita Kazuyuki, Huiting Robert, Ikarashi Soh, Ishida Tsuyoshi, Ishii Shun, Kawabe Ryohei, Klapwijk Teun M., Kohno Kotaro, Kouchi Akira, Llombart Nuria, Maekawa Jun, Murugesan Vignesh, Nakatsubo Shunichi, Naruse Masato, Ohtawara Kazushige, Pascual Laguna Alejandro, Suzuki Koyo, Thoen David J., Tsukagoshi Takashi, Ueda Tetsutaro, de Visser Pieter J., van der Werf Paul P., Yates Stephen J. C., Yoshimura Yuki, Yurduseven Ozan, Endo Akira

JOURNAL OF LOW TEMPERATURE PHYSICS 199 巻 ( 1-2 ) 頁： 231 - 239 2020年4月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Journal of Low Temperature Physics

We are developing an ultra-wideband spectroscopic instrument, DESHIMA (DEep Spectroscopic HIgh-redshift MApper), based on the technologies of an on-chip filter bank and microwave kinetic inductance detector (MKID) to investigate dusty starburst galaxies in the distant universe at millimeter and submillimeter wavelengths. An on-site experiment of DESHIMA was performed using the ASTE 10-m telescope. We established a responsivity model that converts frequency responses of the MKIDs to line-of-sight brightness temperature. We estimated two parameters of the responsivity model using a set of skydip data taken under various precipitable water vapor (PWV 0.4–3.0 mm) conditions for each MKID. The line-of-sight brightness temperature of sky is estimated using an atmospheric transmission model and the PWVs. As a result, we obtain an average temperature calibration uncertainty of 1 σ= 4 %, which is smaller than other photometric biases. In addition, the average forward efficiency of 0.88 in our responsivity model is consistent with the value expected from the geometrical support structure of the telescope. We also estimate line-of-sight PWVs of each skydip observation using the frequency response of MKIDs and confirm the consistency with PWVs reported by the Atacama Large Millimeter/submillimeter Array.

DOI： 10.1007/s10909-020-02338-0

その他リンク： http://link.springer.com/article/10.1007/s10909-020-02338-0/fulltext.html

ALMA uncovers the [C II] emission and warm dust continuum in a z=8.31 Lyman break galaxy 査読有り

Bakx Tom J. L. C., Tamura Yoichi, Hashimoto Takuya, Inoue Akio K., Lee Minju M., Mawatari Ken, Ota Kazuaki, Umehata Hideki, Zackrisson Erik, Hatsukade Bunyo, Kohno Kotaro, Matsuda Yuichi, Matsuo Hiroshi, Okamoto Takashi, Shibuya Takatoshi, Shimizu Ikkoh, Taniguchi Yoshiaki, Yoshida Naoki

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 493 巻 ( 3 ) 頁： 4294 - 4307 2020年4月

ALMA CO Observations of the Host Galaxies of Long-duration Gamma-Ray Bursts. I. Molecular Gas Scaling Relations 査読有り

Hatsukade Bunyo, Ohta Kouji, Hashimoto Tetsuya, Kohno Kotaro, Nakanishi Kouichiro, Niino Yuu, Tamura Yoichi

ASTROPHYSICAL JOURNAL 892 巻 ( 1 ) 頁： 42 - 42 2020年3月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present the results of CO observations toward 14 host galaxies of long-duration gamma-ray bursts (GRBs) at z = 0.1-2.5 by using the Atacama Large Millimeter/submillimeter Array. We successfully detected CO (3-2) or CO (4-3) emission in eight hosts (z = 0.3-2), which more than doubles the sample size of GRB hosts with CO detection. The derived molecular gas mass is M gas = (0.2-6) × 1010 M o assuming metallicity-dependent CO-to-H2 conversion factors. By using the largest sample of GRB hosts with molecular gas estimates (25 in total, of which 14 are CO detected), including results from the literature, we compared molecular gas properties with those of other star-forming galaxies (SFGs). The GRB hosts tend to have a higher molecular gas mass fraction (μ gas) and a shorter gas depletion timescale (t depl) as compared with other SFGs at similar redshifts, especially at z ≲ 1. This could be a common property of GRB hosts or an effect introduced by the selection of targets that are typically above the main-sequence line. To eliminate the effect of selection bias, we analyzed μ gas and t depl as a function of the distance from the main-sequence line (δMS). We find that the GRB hosts follow the same scaling relations as other SFGs, where μ gas increases and t depl decreases with increasing δMS. No molecular gas deficit is observed when compared to other SFGs of similar star formation rate and stellar mass. These findings suggest that the same star formation mechanism is expected to be happening in GRB hosts as in other SFGs.

DOI： 10.3847/1538-4357/ab7992

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/ab7992

A new off-point-less observing method for millimeter and submillimeter spectroscopy with a frequency-modulating local oscillator 査読有り

Taniguchi A., Tamura Y., Kohno K., Takahashi S., Horigome O., Maekawa J., Sakai T., Kuno N., Minamidani T.

Publications of the Astronomical Society of Japan 72 巻 ( 1 ) 頁： 2 2020年2月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

We propose a new observing method for single-dish millimeter and submillimeter spectroscopy using a heterodyne receiver equipped with a frequency-modulating local oscillator (FMLO). Unlike conventional switching methods, which extract astronomical signals by subtracting the reference spectra of off-sources from those of on-sources, the FMLO method does not need to obtain any off-source spectra; rather, it estimates them from the on-source spectra themselves. The principle uses high-dump-rate (10 Hz) spectroscopy with radio frequency modulation achieved by fast sweeping of a local oscillator of a heterodyne receiver. Because sky emission (i.e., off-source) fluctuates as 1/f and is spectrally correlated, it can be estimated and subtracted from time series spectra (a timestream) by principal component analysis. Meanwhile, astronomical signals remain in the timestream since they are modulated to a higher time-frequency domain. The FMLO method therefore achieves (1) a remarkably high observation efficiency, (2) reduced spectral baseline wiggles, and (3) software-based sideband separation. We developed an FMLO system for the Nobeyama 45\:m telescope and a data reduction procedure for it. Frequency modulation was realized by a tunable and programmable first local oscillator. With observations of Galactic sources, we demonstrate that the observation efficiency of the FMLO method is dramatically improved compared to conventional switching methods. Specifically, we find that the time to achieve the same noise level is reduced by a factor of 3.0 in single-pointed observations and by a factor of 1.2 in mapping observations. The FMLO method can be applied to observations of fainter (mK) spectral lines and larger (deg^{2}) mapping. It offers much more efficient and baseline-stable observations compared to conventional switching methods.

DOI： 10.1093/pasj/psz121

Large format imaging spectrograph for the Large Submillimeter Telescope (LST)

Kohno Kotaro, Kawabe Ryohei, Tamura Yoichi, Endo Akira, Baselmans Jochem J. A., Karatsu Kenichi, Inoue Akio, Moriwaki Kana, Hayatsu Natsuki H., Yoshida Naoki, Yoshimura Yuki, Hatsukade Bunyo, Umehata Hideki, Oshima Tai, Takekoshi Tatsuya, Taniguchi Akio, Klaassen Pamela, Mroczkowski Tony, Cicone Claudia, Bertoldi Frank, Dannerbauer Helmut, Tosaki Tomoka

MILLIMETER, SUBMILLIMETER, AND FAR-INFRARED DETECTORS AND INSTRUMENTATION FOR ASTRONOMY X 11453 巻頁： 114530N 2020年

記述言語：英語掲載種別：研究論文（国際会議プロシーディングス）出版者・発行元：Proceedings of SPIE - The International Society for Optical Engineering

We present a conceptual study of a large format imaging spectrograph for next-generation large (50-m class) single-dish telescopes, i.e., the Large Submillimeter Telescope (LST) and Atacama Large Aperture Submillimeter Telescope (AtLAST). Recent discoveries of high-redshift star-forming galaxies at z=8-9 and candidate quiescent galaxies at z∼6 indicate the onset of earliest star formation just a few 100 million years after the Big Bang (i.e., z = 12-15), and LST/AtLAST will provide a unique pathway to uncover spectroscopically-identified ''first forming galaxies'' in the pre-reionization era, once it will be equipped with a large format imaging spectrograph. We describe the preliminary of 3-band, medium resolution (R=2000) imaging spectrograph with ∼1.5 M detectors in total based on the KATANA concept (Karatsu et al.∼2019), which exploits technologies of the integrated superconducting spectrometer (ISS) and a large-format imaging array like A-MKID.

DOI： 10.1117/12.2561238

TiEMPO: Open-source time-dependent end-to-end model for simulating ground-based submillimeter astronomical observations

Huijten Esmee, Roelvink Yannick, Brackenhoff Stefanie A., Taniguchi Akio, Bakx Tom, Marthi Kaushal B., Zaalberg Stan, Baselmans Jochem J. A., Chin Kah Wuy, Huiting Robert, Karatsu Kenichi, Laguna Alejandro Pascual, Tamura Yoichi, Takekoshi Tatsuya, Yates Stephen J. C., van Hoven Maarten, Endo Akira

MILLIMETER, SUBMILLIMETER, AND FAR-INFRARED DETECTORS AND INSTRUMENTATION FOR ASTRONOMY X 11453 巻頁： 114533C 2020年

記述言語：英語掲載種別：研究論文（国際会議プロシーディングス）出版者・発行元：Proceedings of SPIE - The International Society for Optical Engineering

The next technological breakthrough in millimeter-submillimeter astronomy is 3D imaging spectrometry with wide instantaneous spectral bandwidths and wide fields of view. The total optimization of the focal-plane instrument, the telescope, the observing strategy, and the signal-processing software must enable efficient removal of foreground emission from the Earth's atmosphere, which is time-dependent and highly nonlinear in frequency. Here we present TiEMPO: Time-dependent End-To-end Model for Post-process Optimization of the DESHIMA spectrometer. TiEMPO utilizes a dynamical model of the atmosphere and parametrized models of the astronomical source, the telescope, the instrument, and the detector. The output of TiEMPO is a timestream of sky brightness temperature and detected power, which can be analyzed by standard signal-processing software. We first compare TiEMPO simulations with an on-sky measurement by the wideband DESHIMA spectrometer, and find good agreement in the noise power spectral density and sensitivity. We then use TiEMPO to simulate the detection of the line emission spectrum of a high-redshift galaxy using the DESHIMA 2.0 spectrometer in development. The TiEMPO model is open source. Its modular and parametrized design enables users to adapt it to design and optimize the end-To-end performance of spectroscopic and photometric instruments on existing and future telescopes.

DOI： 10.1117/12.2561014

Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs). VIII. A less biased view of the early co-evolution of black holes and host galaxies 査読有り

Izumi Takuma, Onoue Masafusa, Matsuoka Yoshiki, Nagao Tohru, Strauss Michael A., Imanishi Masatoshi, Kashikawa Nobunari, Fujimoto Seiji, Kohno Kotaro, Toba Yoshiki, Umehata Hideki, Goto Tomotsugu, Ueda Yoshihiro, Shirakata Hikari, Silverman John D., Greene Jenny E., Harikane Yuichi, Hashimoto Yasuhiro, Ikarashi Soh, Iono Daisuke, Iwasawa Kazushi, Lee Chien-Hsiu, Minezaki Takeo, Nakanishi Kouichiro, Tamura Yoichi, Tang Ji-Jia, Taniguchi Akio

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 71 巻 ( 6 ) 2019年12月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

We present ALMA [C II] line and far-infrared (FIR) continuum observations of three z > 6 low-luminosity quasars (M1450 > –25 mag) discovered by our Subaru Hyper Suprime-Cam (HSC) survey. The [C II] line was detected in all three targets with luminosities of (2.4–9.5) × 108 L⊙, about one order of magnitude smaller than optically luminous (M1450 ≲ –25 mag) quasars. The FIR continuum luminosities range from < 9 × 1010 L⊙ (3 σ limit) to ∼2 × 1012 L⊙, indicating a wide range in star formation rates in these galaxies. Most of the HSC quasars studied thus far show [C II]/FIR luminosity ratios similar to local star-forming galaxies. Using the [C II]-based dynamical mass (Mdyn) as a surrogate for bulge stellar mass (Mbulge), we find that a significant fraction of low-luminosity quasars are located on or even below the local MBH–Mbulge relation, particularly at the massive end of the galaxy mass distribution. In contrast, previous studies of optically luminous quasars have found that black holes are overmassive relative to the local relation. Given the low luminosities of our targets, we are exploring the nature of the early co-evolution of supermassive black holes and their hosts in a less biased way. Almost all of the quasars presented in this work are growing their black hole mass at a much higher pace at z ∼ 6 than the parallel growth model, in which supermassive black holes and their hosts grow simultaneously to match the local MBH–Mbulge relation at all redshifts. As the low-luminosity quasars appear to realize the local co-evolutionary relation even at z ∼ 6, they should have experienced vigorous starbursts prior to the currently observed quasar phase to catch up with the relation.

DOI： 10.1093/pasj/psz096

Detections of [O III] 88 mu m in two quasars in the reionization epoch 査読有り

Hashimoto Takuya, Inoue Akio K., Tamura Yoichi, Matsuo Hiroshi, Mawatari Ken, Yamaguchi Yuki

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 71 巻 ( 6 ) 2019年12月

First [N II]122 mu m Line Detection in a QSO-SMG Pair BRI 1202-0725 at z=4.69 査読有り

Lee Minju M., Nagao Tohru, De Breuck Carlos, Carniani Stefano, Cresci Giovanni, Hatsukade Bunyo, Kawabe Ryohei, Kohno Kotaro, Maiolino Roberto, Mannucci Filippo, Marconi Alessandro, Nakanishi Kouichiro, Saito Toshiki, Tamura Yoichi, Troncoso Paulina, Umehata Hideki, Yun Min

ASTROPHYSICAL JOURNAL LETTERS 883 巻 ( 2 ) 頁： L29 2019年10月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal Letters

We report the first detection obtained with the Atacama Large Millimeter/submillimeter Array of the [N ii] 122 μm line emission from a galaxy group BRI 1202-0725 at z = 4.69 consisting of a quasi-stellar object (QSO) and a submillimeter-bright galaxy (SMG). Combining this with a detection of [N ii] 205 μm line in both galaxies, we constrain the electron densities of the ionized gas based on the line ratio of [N ii] 122/205. The derived electron densities are and cm-3 for the SMG and the QSO, respectively. The electron density of the SMG is similar to that of the Galactic Plane and to the average of the local spirals. However, higher electron densities (by up to a factor of three) could be possible for systematic uncertainties of the line flux estimates. The electron density of the QSO is comparable to high-z star-forming galaxies at z = 1.5-2.3, obtained using rest-frame optical lines and with the lower limits suggested from stacking analysis on lensed starbursts at z = 1-3.6 using the same tracer of [N ii]. Our results suggest a large scatter of electron densities in global scale at fixed star formation rates for extreme starbursts. The success of the [N ii] 122 μm and 205 μm detections at z = 4.69 demonstrates the power of future systematic surveys of extreme starbursts at z > 4 for probing the interstellar medium conditions and the effects on surrounding environments.

DOI： 10.3847/2041-8213/ab412e

Large Population of ALMA Galaxies at z>6 with Very High [OIII]88um to [CII]158um Flux Ratios: Evidence of Extremely High Ionization Parameter or PDR Deficit? 査読有り

Harikane, Yuichi, Ouchi, Masami, Inoue, Akio K., Matsuoka, Yoshiki, Tamura, Yoichi, Bakx, Tom, Fujimoto, Seiji, Moriwaki, Kana, Ono, Yoshiaki, Nagao, Tohru, Tadaki, Ken-ichi, Kojima, Takashi, Shibuya, Takatoshi, Egami, Eiichi, Ferrara, Andrea, Gallerani, Simona, Hashimoto, Takuya, Kohno, Kotaro, Matsuda, Yuichi, Matsuo, Hiroshi, Pallottini, Andrea, Sugahara, Yuma, Vallini, Livia

2019年10月

掲載種別：研究論文（学術雑誌）出版者・発行元：arXiv e-prints

We present our new ALMA observations targeting [OIII]88um, [CII]158um, [NII]122um, and dust continuum emission for three Lyman break galaxies at z=6.0293-6.2037 identified in the Subaru/Hyper Suprime-Cam survey. We clearly detect [OIII] and [CII] lines from all of the galaxies at 4.3-11.8sigma levels, and identify multi-band dust continuum emission in two of the three galaxies, allowing us to estimate infrared luminosities and dust temperatures simultaneously. In conjunction with previous ALMA observations for six galaxies at z>6, we confirm that all the nine z=6-9 galaxies have high [OIII]/[CII] ratios of L[OIII]/L[CII]~3-20, ~10 times higher than z~0 galaxies. We also find a positive correlation between the [OIII]/[CII] ratio and the Lya equivalent width (EW) at the >91% confidence level. We carefully investigate physical origins of the high [OIII]/[CII] ratios at z=6-9 using Cloudy, and find that high density of the interstellar medium, low C/O abundance ratio, and the cosmic microwave background attenuation are responsible to only a part of the z=6-9 galaxies. Instead, the observed high [OIII]/[CII] ratios are explained by 10-100 times higher ionization parameters or low photodissociation region (PDR) covering fractions of 0-10%, both of which are consistent with our [NII] observations. The latter scenario can be reproduced with a density bounded nebula with PDR deficit, which would enhance the Lya, Lyman continuum, and C+ ionizing photons escape from galaxies, consistent with the [OIII]/[CII]-Lya EW correlation we find. <P />...

A Radio-to-millimeter Census of Star-forming Galaxies in Protocluster 4C 23.56 at z=2.5: Global and Local Gas Kinematics 査読有り

Lee Minju M., Tanaka Ichi, Kawabe Ryohei, Aretxaga Itziar, Hatsukade Bunyo, Izumi Takuma, Kajisawa Masaru, Kodama Tadayuki, Kohno Kotaro, Nakanishi Kouichiro, Saito Toshiki, Tadaki Ken-ichi, Tamura Yoichi, Umehata Hideki, Zeballos Milagros

ASTROPHYSICAL JOURNAL 883 巻 ( 1 ) 頁： 92 2019年9月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present a study of the gas kinematics of star-forming galaxies associated with protocluster 4C 23.56 at z = 2.49 using 0.″4 resolution CO (4-3) data taken with ALMA. Eleven Hα emitters (HAEs) are detected in CO (4-3), including six HAEs that were previously detected in CO (3-2) at a coarser angular resolution. The detections in both CO lines are broadly consistent in the line widths and the redshifts, confirming both detections. With an increase in the number of spectroscopic redshifts, we confirm that the protocluster is composed of two merging groups with a total halo mass of log (M cl/M o) = 13.4-13.6, suggesting that the protocluster would evolve into a Virgo-like cluster (>1014 M o). We compare the CO line widths and the CO luminosities with other (proto)clusters (n gal = 91) and general field (n gal = 80) galaxies from other studies. The 4C 23.56 protocluster galaxies have CO line widths and luminosities comparable to other protocluster galaxies on average. On the other hand, the CO line widths are on average broader by ≈50% compared to field galaxies, while the median CO luminosities are similar. The broader line widths can be attributed to both effects of unresolved gas-rich mergers and/or compact gas distribution, which is supported by our limited but decent angular resolution observations and the size estimate of three galaxies. Based on these results, we argue that gas-rich mergers may play a role in the retention of the specific angular momentum to a value similar to that of field populations during cluster assembly, though we need to verify this with a larger number of samples.

DOI： 10.3847/1538-4357/ab3b5b

ADF22: Blind Detections of [C II] Line Emitters Shown to be Spurious 査読有り国際誌

Natsuki H. Hayatsu, R. J. Ivison, Paola Andreani, Hideki Umehata, Yuichi Matsuda, Naoki Yoshida, Kotaro Kohno, Bunyo Hatsukade, Akio K. Inoue, Yoichi Tamura, Tutomu T. Takeuchi, Seiji Fujimoto, Minju M. Lee, Tohru Nagao, Yiping Ao

Research Notes of the AAS 3 巻 ( 7 ) 頁： 97 2019年7月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：American Astronomical Society

We report Atacama Large Millimetre/submillimeter Array (ALMA) Cycle-5 follow-up observations of two candidate [CII] emitters at z ~ 6 in the ALMA deep field in SSA22 (ADF22). The candidates were detected blindly in a Cycle-2 ALMA survey covering ~ 5 square arcmins, with a single tuning, along with two CO lines associated with galaxies at lower redshifts. Various tests suggested at least one of the two > 6-sigma [CII] candidates should be robust (Hayatsu et al. 2017). Nevertheless, our new, deeper observations recover neither candidate, demonstrating a higher contamination rate than expected. The cause of the spurious detections is under investigation but at present it remains unclarified.

DOI： 10.3847/2515-5172/ab3228

ALMA Observations of Molecular Gas in the Host Galaxy of AT2018cow 査読有り

Morokuma-Matsui Kana, Morokuma Tomoki, Tominaga Nozomu, Hatsukade Bunyo, Hayashi Masao, Tamura Yoichi, Matsuda Yuichi, Motogi Kazuhito, Niinuma Kotaro, Konishi Masahiro

ASTROPHYSICAL JOURNAL LETTERS 879 巻 ( 1 ) 頁： L13 2019年7月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal Letters

We investigate the molecular gas in and star formation properties of the host galaxy (CGCG 137-068) of a mysterious transient, AT2018cow, at kpc and larger scales, using archival band-3 data from the Atacama Large Millimeter/submillimeter Array (ALMA). AT2018cow is the nearest fast-evolving luminous transient (FELT); this is the first study unveiling molecular-gas properties of FELT hosts. The achieved rms and beam size are 0.21 mJy beam-1 at a velocity resolution of 40 km s-1 and 3.″66 × 2.″71 (1.1 kpc × 0.8 kpc), respectively. CO(J = 1-0) emission is successfully detected. The total molecular gas mass inferred from the CO data is (1.85 0.04) × 108 M o with the Milky Way CO-to-H2 conversion factor. The H2 column density at the AT2018cow site is estimated to be 8.6 × 1020 cm-2. The ALMA data reveal that (1) CGCG 137-068 is a normal star-forming (SF) dwarf galaxy in terms of its molecular gas and star formation properties, and (2) that AT2018cow is located between a CO peak and a blue star cluster. These properties suggest ongoing star formation and favor the explosion of a massive star as the progenitor of AT2018cow. We also find that CGCG 137-068 has a solar or super-solar metallicity. If the metallicity of the other FELT hosts is not higher than average, then some properties of SF dwarf galaxies other than metallicity may be related to FELTs.

DOI： 10.3847/2041-8213/ab2915

The absence of [C II] 158 mu m emission in spectroscopically confirmed galaxies at z > 8 査読有り

Laporte N., Katz H., Ellis R. S., Lagache G., Bauer F. E., Boone F., Inoue A. K., Hashimoto T., Matsuo H., Mawatari K., Tamura Y.

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 487 巻 ( 1 ) 頁： L81 - L85 2019年7月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society: Letters

The scatter in the relationship between the strength of [C ii] 158 $mu$m emission and the star formation rate at high redshift has been the source of much recent interest. Although the relationship is well established locally, several intensely star-forming galaxies have been found whose [C ii] 158 $mu$m emission is either weak, absent, or spatially offset from the young stars. Here we present new ALMA data for the two most distant gravitationally lensed and spectroscopically confirmed galaxies, A2744-YD4 at z = 8.38 and MACS1149-JD1 at z = 9.11, both of which reveal intense [O iii] 88 $mu$m emission. In both cases we provide stringent upper limits on the presence of [C ii] 158 $mu$m with respect to [O iii] 88 $mu$m. We review possible explanations for this apparent redshift-dependent [C ii] deficit in the context of our recent hydrodynamical simulations. Our results highlight the importance of using several emission line diagnostics with ALMA to investigate the nature of the interstellar medium in early galaxies.

DOI： 10.1093/mnrasl/slz094

その他リンク： http://academic.oup.com/mnrasl/article-pdf/487/1/L81/28864236/slz094.pdf

ALMA 26 arcmin(2) Survey of GOODS-S at 1mm (ASAGAO): Near-infrared-dark Faint ALMA Sources 査読有り

Yamaguchi Yuki, Kohno Kotaro, Hatsukade Bunyo, Wang Tao, Yoshimura Yuki, Ao Yiping, Caputi Karina I, Dunlop James S., Egami Eiichi, Espada Daniel, Fujimoto Seiji, Hayatsu Natsuki H., Ivison Rob J., Kodama Tadayuki, Kusakabe Haruka, Nagao Tohru, Ouchi Masami, Rujopakarn Wiphu, Tadaki Ken-ichi, Tamura Yoichi, Ueda Yoshihiro, Umehata Hideki, Wang Wei-Hao, Yun Min S.

ASTROPHYSICAL JOURNAL 878 巻 ( 1 ) 頁： 73 2019年6月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We report detections of two 1.2 mm continuum sources (S 1.2 mm ∼ 0.6 mJy) without any counterparts in the deep H- and/or K-band image (i.e., K-band magnitude ≳26 mag). These near-infrared-dark faint millimeter sources are uncovered by ASAGAO, a deep and wide-field (≃26 arcmin2) Atacama Large Millimeter/submillimeter Array (ALMA) 1.2 mm survey. One has a red IRAC (3.6 and 4.5 μm) counterpart, and the other has been independently detected at 850 and 870 μm using SCUBA2 and ALMA Band 7, respectively. Their optical-to-radio spectral energy distributions indicate that they can lie at z ≳ 3-5 and can be in the early phase of massive galaxy formation. Their contribution to the cosmic star formation rate density is estimated to be ∼1 ×10-3 M o yr-1 Mpc-3 if they lie somewhere in the redshift range of z ∼ 3-5. This value can be consistent with, or greater than, that of bright submillimeter galaxies (S 870 μm > 4.2 mJy) at z ∼ 3-5. We also uncover three more candidate near-infrared-dark faint ALMA sources without any counterparts (S 1.2 mm ∼ 0.45-0.86 mJy). These results show that an unbiased ALMA survey can reveal the dust-obscured star formation activities, which were missed in previous deep optical/near-infrared surveys.

DOI： 10.3847/1538-4357/ab0d22

Molecular Gas Properties in the Host Galaxy of GRB 080207 査読有り

Hatsukade Bunyo, Hashimoto Tetsuya, Kohno Kotaro, Nakanishi Kouichiro, Ohta Kouji, Niino Yuu, Tamura Yoichi, Toth L. Viktor

ASTROPHYSICAL JOURNAL 876 巻 ( 2 ) 頁： 91 - 91 2019年5月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present the results of CO(1-0) and CO(4-3) observations of the host galaxy of a long-duration gamma-ray burst GRB 080207 at z = 2.0858 by using the Karl G. Jansky Very Large Array and the Atacama Large Millimeter/submillimeter Array. The host is detected in CO(1-0) and CO(4-3), becoming the first case for a gamma-ray burst (GRB) host with more than two CO transitions detected combined with CO(2-1) and CO(3-2) in the literature. Adopting a metallicity-dependent CO-to-H2 conversion factor, we derive a molecular gas mass of M gas = 8.7 × 1010 M o, which places the host in a sequence of normal star-forming galaxies in an M gas-star formation rate (SFR) plane. A modified blackbody fit to the far-infrared-millimeter photometry results in a dust temperature of 37 K and a dust mass of M dust = 1.5 × 108 M o. The spatially resolved CO(4-3) observations allow us to examine the kinematics of the host. The CO velocity field shows a clear rotation and is reproduced by a rotation-dominated disk model with a rotation velocity of 350 km s-1 and a half-light radius of 2.4 kpc. The CO spectral line energy distribution derived from the four CO transitions is similar to that of starburst galaxies, suggesting a high excitation condition. Comparison of molecular gas properties between the host and normal (main-sequence) galaxies at similar redshifts shows that they share common properties such as gas mass fraction, gas depletion timescale, gas-to-dust ratio, location in the M gas-SFR (or surface density) relation, and kinematics, suggesting that long-duration GRBs can occur in normal star-forming environments at z ∼ 2.

DOI： 10.3847/1538-4357/ab1649

CNO Emission of an Unlensed Submillimeter Galaxy at z=4.3 査読有り

Tadaki Ken-ichi, Iono Daisuke, Hatsukade Bunyo, Kohno Kotaro, Lee Minju M., Matsuda Yuichi, Michiyama Tomonari, Nakanishi Kouichiro, Nagao Tohru, Saito Toshiki, Tamura Yoichi, Ueda Junko, Umehata Hideki

ASTROPHYSICAL JOURNAL 876 巻 ( 1 ) 頁： 1 2019年5月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present the results from Atacama Large Millimeter/submillimeter Array observations of [N ii] 205 μm, [C ii] 158 μm, and [O iii] 88 μm lines in an unlensed submillimeter galaxy at z = 4.3, COSMOS-AzTEC-1, hosting a compact starburst core with an effective radius of ∼1 kpc. The [C ii] and [N ii] emission are spatially resolved in 0.″3-resolution (1 kpc in radius). The kinematic properties of the [N ii] emission are consistent with those of the CO(4-3) and [C ii] emission, suggesting that the ionized gas feels the same gravitational potential as the associated molecular gas and photodissociation regions (PDRs). On the other hand, the spatial extent is different among the lines and dust continuum: the [C ii] emitting gas is the most extended and the dust is the most compact, leading to a difference of the physical conditions in the interstellar medium. We derive the incident far-ultraviolet flux and the hydrogen gas density through PDR modeling by properly subtracting the contribution of ionized gas to the total [C ii] emission. The observed [C ii] emission is likely produced by dense PDRs with cm-3 and G 0 = 103.5-3.75 in the central 1 kpc region and cm-3 and G 0 = 103.25-3.5 in the central 3 kpc region. We have also successfully measured the line ratio of [O iii]/[N ii] in the central 3 kpc region of COSMOS-AzTEC-1 at z = 4.3, which is the highest redshift where both nitrogen and oxygen lines are detected. Under the most likely physical conditions, the measured luminosity ratio of L [O iii]/L [N ii] = 6.4 ±; 2.2 indicates a near solar metallicity with Z gas = 0.7-1.0 Z o, suggesting a chemically evolved system at z = 4.3.

DOI： 10.3847/1538-4357/ab1415

Exploration and characterization of the earliest epoch of galaxy formation: beyond the re-ionization era 査読有り国際誌

Kohno, Kotaro, Tamura, Yoichi, Inoue, Akio, Kawabe, Ryohei, Oshima, Tai, Hatsukade, Bunyo, Takekoshi, Tatsuya, Yoshimura, Yuki, Umehata, Hideki, Dannerbauer, Helmut, Cicone, Claudia, Bertoldi, Frank

Astro2020: Decadal Survey on Astronomy and Astrophysics 2019年5月

記述言語：英語掲載種別：研究論文（学術雑誌）

Recent ALMA detection of the bright [OIII] 88 um line at z = 9.11, indicates the onset of star formation at z 15. In order to uncover a large number of z=10-15 galaxies, we argue two possible pathways: (1) a blind spectroscopic survey of [OIII] 88 um line emitters, and (2) a high-cadence survey of transient sources to catch the pop-III GRBs. <P />...

The case for a 'sub-millimeter SDSS': a 3D map of galaxy evolution to z 10 査読有り国際誌

Geach, James, Banerji, Manda, Bertoldi, Frank, Bethermin, Matthieu, Casey, Caitlin M., Chen, Chian-Chou, Clements, David L., Cicone, Claudia, Combes, Francoise, Conselice, Christopher, Cooray, Asantha, Coppin, Kristen, Daddi, Emanuele, Dannerbauer, Helmut, Dave, Romeel, Doherty, Matthew, Dunlop, James S., Edge, Alastair, Farrah, Duncan, Franco, Maximilien, Fuller, Gary, Garratt, Tracy, Gear, Walter, Greve, Thomas R., Hatziminaoglou, Evanthia, Hayward, Christopher C., Ivison, Rob J., Kawabe, Ryohei, Klaassen, Pamela, Knudsen, Kirsten K., Kohno, Kotaro, Koprowski, Maciej, Lagos, Claudia D. P., Magdis, Georgios E., Magnelli, Benjamin, McGee, Sean L., Michalowski, Michal, Mroczkowski, Tony, Noroozian, Omid, Narayanan, Desika, Oliver, Seb, Riechers, Dominik, Rujopakarn, Wiphu, Scott, Douglas, Serjeant, Stephen, Smith, Matthew W. L., Swinbank, Mark, Tamura, Yoichi, van der Werf, Paul, van Kampen, Eelco, Verma, Aprajita, Vieira, Joaquin, Wagg, Jeff, Walter, Fabian, Wang, Lingyu, Wootten, Al, Yun, Min S.

Bulletin of the American Astronomical Society 2019年5月

Mapping Galaxy Clusters in the Distant Universe 査読有り国際誌

Dannerbauer, Helmut, van Kampen, Eelco, Afonso, Jose, Andreani, Paola, Battaia, Fabrizio Arrigoni, Bertoldi, Frank, Casey, Caitlin, Chen, Chian-Chou, Clements, David L., De Breuck, Carlos, Frye, Brenda, Geach, James, Harrington, Kevin, Hayashi, Masao, Jin, Shuowen, Klaassen, Pamela, Kohno, Kotaro, Lehnert, Matthew D., Matute, Israel, Mroczkowski, Tony, Noble, Allison, Pappalardo, Ciro, Tamura, Yoichi, Zavala, Jorge

Bulletin of the American Astronomical Society 2019年5月

Environmental impacts on molecular gas in protocluster galaxies at z similar to 2 査読有り

Tadaki Ken-ichi, Kodama Tadayuki, Hayashi Masao, Shimakawa Rhythm, Koyama Yusei, Lee Minju, Tanaka Ichi, Hatsukade Bunyo, Iono Daisuke, Kohno Kotaro, Matsuda Yuichi, Suzuki Tomoko L., Tamura Yoichi, Toshikawa Jun, Umehata Hideki

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 71 巻 ( 2 ) 頁： 40 2019年4月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

We present the results from ALMA CO(3-2) observations of 66 Hα-selected galaxies in three protoclusters around radio galaxies: PKS 1138-262 (z = 2.16), USS 1558-003 (z = 2.53), and 4C 23.56 (z = 2.49). The pointing areas have an overdensity of ∼100 compared to the mean surface number density of galaxies in field environments. We detect the CO emission line in 16 star-forming galaxies, including six previously published galaxies, to measure the molecular gas mass. In the stellar mass range of 10.5 < log (Mstar/M⊙) < 11.0, the protocluster galaxies have larger gas mass fractions and longer gas depletion timescales compared to the scaling relations established for field galaxies. On the other hand, the amounts of molecular gas in more massive galaxies with log (Mstar/M⊙) > 11.0 are comparable in mass to the scaling relation, or smaller. Our results suggest that the environmental effects on gas properties are mass dependent: in high-density environments, gas accretion through cosmic filaments is accelerated in less massive galaxies, while this is suppressed in the most massive system.

DOI： 10.1093/pasj/psz005

The Excitation State of Galactic Diffuse Molecular Gas, Investigated with ALMA Observations of Multi-transition Absorption Lines 査読有り

Ando Ryo, Kohno Kotaro, Umehata Hideki, Izumi Takuma, Ishii Shun, Nishimura Yuri, Sorai Kazuo, Tosaki Tomoka, Taniguchi Akio, Tamura Yoichi

ASTROPHYSICAL JOURNAL 871 巻 ( 2 ) 2019年2月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We report Atacama Large Millimeter/submillimeter Array (ALMA) observations of 243-263 GHz absorption lines from Galactic diffuse molecular gas seen against three extragalactic radio-loud objects, J1717-337, J1625-254, and NRAO530. No significant absorption features were detected in our new sensitive ALMA Band 6 (λ ≃ 1.2 mm) spectra (1σ ≃ 2-4 mJy beam -1 with a velocity resolution of 1 km s -1 ), despite the fact that the obtained spectra cover the line frequencies of c-C 3 H 2 , CS, H 13 CN, HCO, H 13 CO + , SiO, and C 2 H, and that the lower transition absorption lines of these molecular species have been detected in ALMA Band 3 (λ ≃ 3 mm) observations toward these three Galactic molecular absorption systems. By combining the upper limits of the higher transitions that we obtain in this study and the archival detections of the lower transitions, we constrain the excitation temperatures of these species in the Galactic diffuse medium to be below 10 K, in spite of their PDR-like chemical states, where elevated column density ratios of HCO to H 13 CO + are previously reported. These constraints are in line with the widely accepted view of the diffuse molecular clouds, where the molecular excitation is almost in equilibrium with the cosmic microwave background, although its kinetic temperature can be a few tens of Kelvin. Molecular abundance patterns seem to be similar in the Galactic diffuse gas and nearby active galaxies observed with a kpc-scale beam, suggesting the importance of observations with a parsec-scale resolution, which can resolve individual molecular clouds.

DOI： 10.3847/1538-4357/aafa6f

ALMA twenty-six arcmin<SUP>2</SUP> survey of GOODS-S at one millimeter (ASAGAO): Source catalog and number counts 査読有り

Hatsukade Bunyo, Kohno Kotaro, Yamaguchi Yuki, Umehata Hideki, Ao Yiping, Aretxaga Itziar, Caputi Karina I., Dunlop James S., Egami Eiichi, Espada Daniel, Fujimoto Seiji, Hayatsu Natsuki H., Hughes David H., Ikarashi Soh, Iono Daisuke, Ivison Rob J., Kawabe Ryohei, Kodama Tadayuki, Lee Minju, Matsuda Yuichi, Nakanishi Kouichiro, Ohta Kouji, Ouchi Masami, Rujopakarn Wiphu, Suzuki Tomoko, Tamura Yoichi, Ueda Yoshihiro, Wang Tao, Wang Wei-Hao, Wilson Grant W., Yoshimura Yuki, Yun Min S.

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 70 巻 ( 6 ) 頁： 239 - 240 2018年12月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

We present the survey design, data reduction, construction of images, and source catalog of the Atacama Large Millimeter/submillimeter Array (ALMA) twenty-six arcmin2 survey of GOODS-S at one millimeter (ASAGAO). ASAGAO is a deep (1 σ depth ∼ 61 μJy beam−1 for a 250 kλ-tapered map with a synthesized beam size of 0.51 × 0.45) and wide area (26 arcmin2) survey on a contiguous field at 1.2 mm. By combining with ALMA archival data in the GOODS-South field, we obtained a deeper map in the same region (1 σ depth ∼ 30 μJy beam−1 for a deep region with a 250 kλ-taper, and a synthesized beam size of 0.59 × 0.53), providing the largest sample of sources (25 sources at ≥5.0 σ, 45 sources at ≥4.5 σ) among ALMA blank-field surveys to date. The number counts show that 52+−118 % of the extragalactic background light at 1.2 mm is resolved into discrete sources at S1.2 mm > 135 μJy. We create infrared (IR) luminosity functions (LFs) in the redshift range of z = 1–3 from the ASAGAO sources with Ks-band counterparts, and constrain the faintest luminosity of the LF at 2.0 < z < 3.0. The LFs are consistent with previous results based on other ALMA and SCUBA-2 observations, which suggest a positive luminosity evolution and negative density evolution with increasing redshift. We find that obscured star-formation of sources with IR luminosities of log (LIR/L) 11.8 account for ≈60%–90% of the z ∼ 2 cosmic star-formation rate density.

DOI： 10.1093/pasj/psy104

Development of Multi-temperature Calibrator for the TES Bolometer Camera: System Design 査読有り

Takekoshi Tatsuya, Ohtawara Kazushige, Oshima Tai, Ishii Shun, Izumi Natsuko, Izumi Takuma, Yamaguchi Masayuki, Suzuki Shunta, Muraoka Kazuyuki, Hirota Akihiko, Saito Fumiaki, Nakatsubo Shunichi, Kouchi Akira, Ito Tetsuya, Uemizu Kazunori, Fujii Yasunori, Tamura Yoichi, Kohno Kotaro, Kawabe Ryohei

JOURNAL OF LOW TEMPERATURE PHYSICS 193 巻 ( 5-6 ) 頁： 1003 - 1009 2018年12月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Journal of Low Temperature Physics

We developed a simple add-on, cryogen-free, and low-power consumption calibrator for a new transition-edge sensor (TES) bolometer camera mounted on the ASTE 10-m telescope. To measure the responsivity of the TES bolometers and accurately correct for the nonlinearity and atmospheric extinction, we designed a motor-driven rotating filter wheel system installed in front of the cryostat window. This calibrator is required to cover the loading power under various atmospheric conditions, which corresponds to precipitable water vapor (PWV) of 0.5–4 mm. For this range of PWV, 25–100 K blackbodies are necessary for the observing bands of 1.1 and 0.85 mm. To simulate the temperature range, bolometers in the cryostat are also optically coupled to the low-temperature stage (< 4 K) inside the cryostat by spherical mirrors. In addition, we used moderately absorptive polystyrene plates that are placed between a spherical mirror and the cryostat window. Various combinations of filters result in eight different temperatures by the filter wheel system and simulate the atmospheric emission under various weather conditions at the ASTE site.

DOI： 10.1007/s10909-018-1916-1

Development of Multi-temperature Calibrator for the TES Bolometer Camera: Deployment at ASTE 査読有り

Oshima Tai, Ohtawara Kazushige, Takekoshi Tatsuya, Ishii Shun, Izumi Natsuko, Izumi Takuma, Yamaguchi Masayuki, Suzuki Shunta, Muraoka Kazuyuki, Hirota Akihiko, Saito Fumiaki, Nakatsubo Shunichi, Kouchi Akira, Ito Tetsuya, Uemizu Kazunori, Fujii Yasunori, Tamura Yoichi, Kohno Kotaro, Kawabe Ryohei

JOURNAL OF LOW TEMPERATURE PHYSICS 193 巻 ( 5-6 ) 頁： 996 - 1002 2018年12月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Journal of Low Temperature Physics

We developed and deployed a simple add-on multi-temperature calibrator for our multicolor transition edge sensor (TES) bolometer camera aimed at simultaneous observation with observing wavelengths of 1.1 and 0.85 mm. To cover the power loading level from the atmospheric emission corresponding to precipitable water vapor (PWV) of 0.5–4 mm, the calibrator consists of spherical mirrors to show the low-temperature stages of the cryostat and filters with moderate opacity to mimic the eight-temperature cold blackbodies. The loading powers introduced by each filter were self-calibrated by measuring the load curves of the TES bolometers when a filter was placed in front of the cryostat window. Each science observation was preceded by the calibration process, which measures the response of the TES bolometers to the atmosphere and filters of various opacities. Then, the responsivities of TES bolometers were derived to convert their output signal to the loading power and correct for the nonlinearity inherent in its response. Furthermore, the loading power falling on the TES bolometers from atmospheric emission measured at various PWV was in good correlation with the PWV measured with the radiometer, which enables the atmospheric extinction correction by fast and sensitive bolometers compared to the available radiometers with the modest sampling speeds.

DOI： 10.1007/s10909-018-2009-x

The distribution and physical properties of high-redshift [O III] emitters in a cosmological hydrodynamics simulation 査読有り

Moriwaki Kana, Yoshida Naoki, Shimizu Ikkoh, Harikane Yuichi, Matsuda Yuichi, Matsuo Hiroshi, Hashimoto Takuya, Inoue Akio K., Tamura Yoichi, Nagao Tohru

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 481 巻 ( 1 ) 頁： L84 - L88 2018年11月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Monthly Notices of the Royal Astronomical Society: Letters

Recent observations with the Atacama Large Millimeter/submillimeter Array (ALMA) detected far-infrared emission lines such as the [OIII] 88μm line from galaxies at z ~ 7-9. We use a cosmological simulation of galaxy formation to study the physical properties of [O III] 88μm emitters. In a comoving volume of 50 h-1 Mpc on a side, we locate 34 galaxies with stellar masses greater than 108 M⊙ at z = 9, and more than 270 such galaxies at z = 7. We calculate the [O III] 88μm luminosities (LOIII,88) by combining a physical model of HII regions with emission line calculations using the photoionization code CLOUDY.We show that the resulting LOIII,88, for a given star formation rate, is slightly higher than predicted from the empirical relation for local galaxies, and is consistent with recent observations of galaxies at redshifts 7-9. Bright [O III] emitters with LOIII,88 > 108 L⊙ have star formation rates higher than 3M⊙ yr-1, and the typical metallicity is ~0.1Z⊙. The galaxies are hosted by dark matter haloes with masses greater than 1011M⊙. We propose to use the [OIII] 5007Å line, to be detected by James Webb Space Telescope, to study the properties of galaxies whose [OIII] 88 μm line emission has been already detected with ALMA.

DOI： 10.1093/mnrasl/sly167

Extremely Dense Cores Associated with Chandra Sources in Ophiuchus A: Forming Brown Dwarfs Unveiled? 査読有り

Kawabe Ryohei, Hara Chihomi, Nakamura Fumitaka, Saigo Kazuya, Kamazaki Takeshi, Shimajiri Yoshito, Tomida Kengo, Takakuwa Shigehisa, Tsuboi Yohko, Machida Masahiro N., Di Francesco James, Friesen Rachel, Hirano Naomi, Oasa Yumiko, Tamura Motohide, Tamura Yoichi, Tsukagoshi Takashi, Wilner David

ASTROPHYSICAL JOURNAL 866 巻 ( 2 ) 2018年10月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

On the basis of various data such as ALMA, JVLA, Chandra, Herschel, and Spitzer, we confirmed that two protostellar candidates in Oph A are bona fide protostars or proto-brown dwarfs (proto-BDs) in extremely early evolutionary stages. Both objects are barely visible across infrared (IR; i.e., near-IR to far-IR) bands. The physical nature of the cores is very similar to that expected in first hydrostatic cores (FHSCs), objects theoretically predicted in the evolutionary phase prior to stellar core formation with gas densities of ∼1011-12 cm-3. This suggests that the evolutionary stage is close to the FHSC formation phase. The two objects are associated with faint X-ray sources, suggesting that they are in very early phase of stellar core formation with magnetic activity. In addition, we found the CO outflow components around both sources, which may originate from the young outflows driven by these sources. The masses of these objects are calculated to be ∼0.01-0.03 M o from the dust continuum emission. These physical properties are consistent with that expected from the numerical model of forming brown dwarfs. These facts (the X-ray detection, CO outflow association, and FHSC-like spectral energy distributions) strongly indicate that the two objects are proto-BDs or will be in the very early phase of protostars, which will evolve to more massive protostars if they gain enough mass from their surroundings. The ages of these two objects are likely to be within ∼103 years after the protostellar core (or second core) formation, taking into account the outflow dynamical times (≲500 years).

DOI： 10.3847/1538-4357/aae153

Detections of [OIII] 88 $\mu$m in Two Quasars in the Reionization Epoch 査読有り

Hashimoto, Takuya, Inoue, Akio K., Tamura, Yoichi, Matsuo, Hiroshi, Mawatari, Ken, Yamaguchi, Yuki

2018年10月

掲載種別：研究論文（学術雑誌）出版者・発行元：arXiv e-prints

With the Atacama Large Millimeter/sub-millimeter Array (ALMA), we report detections of the far-infrared (FIR) [OIII] 88 $\mu$m line and the underlying dust continuum in the two quasars in the reionization epoch, J205406.48-000514.8 (hereafter J2054-0005) at $z=6.0391\pm0.0002$ and J231038.88+185519.7 (hereafter J2310+1855) at $z=6.0035\pm0.0007$. The [OIII] luminosity of J2054-0005 and J2310+1855 are $L_{\rm [OIII]} = (6.8\pm0.6) \times 10^{9}$ and $(2.4\pm0.6) \times 10^{9}$ $L_{\rm \odot}$, corresponding to $\approx$ 0.05\%\ and 0.01\%\ of the total infrared luminosity, $L_{\rm TIR}$, respectively. Combining these [OIII] luminosities with [CII] 158 $\mu$m luminosities in the literature, we find that J2054-0005 and J2310+1855 have the [OIII]-to-[CII] luminosity ratio of $2.1\pm0.4$ and $0.3\pm0.1$, respectively, the latter of which is the lowest among objects so far reported at $z>6$. Combining [OIII] observations at $z\approx6-9$ from our study and the literature, we identify the [OIII] line deficit: objects with larger $L_{\rm TIR}$ have lower $L_{\rm [OIII]}$-to-$L_{\rm TIR}$ ratios. Furthermore, we also find that the anti-correlation is shifted toward higher $L_{\rm TIR}$ value when compared to the local [OIII] line deficit. <P />...

AzTEC 1.1 mm observations of high-z protocluster environments: SMG overdensities and misalignment between AGN jets and SMG distribution 査読有り国際誌

Zeballos, M., Aretxaga, I., Hughes, D. H., Humphrey, A., Wilson, G. W., Austermann, J., Dunlop, J. S., Ezawa, H., Ferrusca, D., Hatsukade, B., Ivison, R. J., Kawabe, R., Kim, S., Kodama, T., Kohno, K., Montaña, A., Nakanishi, K., Plionis, M., Sánchez-Argüelles, D., Stevens, J. A., Tamura, Y., Velazquez, M., Yun, M. S.

Monthly Notices of the Royal Astronomical Society 2018年10月

記述言語：英語掲載種別：研究論文（学術雑誌）

We present observations at 1.1 mm towards 16 powerful radio galaxies and a radio-quiet quasar at 0.5 < z < 6.3 acquired with the AzTEC camera mounted at the James Clerk Maxwell Telescope and Atacama Submillimeter Telescope Experiment to study the spatial distribution of submillimetre galaxies (SMGs) towards possible protocluster regions. The survey covers a total area of 1.01 sq deg with rms depths of 0.52-1.44 mJy and detects 728 sources above 3σ. We find overdensities of a factor of ̃2 in the source counts of three individual fields (4C+23.56, PKS1138-262, and MRC0355-037) over areas of ̃200 sq deg. When combining all fields, the source-count analysis finds an overdensity that reaches a factor ≳3 at S<SUB>1.1mm</SUB> ≥ 4 mJy covering a 1.5-arcmin-radius area centred on the active galactic nucleus. The large size of our maps allows us to establish that beyond a radius of 1.5 arcmin, the radial surface density of SMGs falls to that of a blank field. In addition, we find a trend for SMGs to align closely to a perpendicular direction with respect to the radio jets of the powerful central radio galaxies (73_{+13}^{-14} deg). This misalignment is found over projected comoving scales of 4-20 Mpc, departs from perfect alignment (0 deg) by ̃5σ, and apparently has no dependence on SMG luminosity. Under the assumption that the AzTEC sources are at the redshift of the central radio galaxy, the misalignment reported here can be interpreted as SMGs preferentially inhabiting mass-dominant filaments funnelling material towards the protoclusters, which are also the parent structures of the radio galaxies. <P />...

DOI： 10.1093/mnras/sty1714

The gravitationally unstable gas disk of a starburst galaxy 12 billion years ago 査読有り

Tadaki K., Iono D., Yun M. S., Aretxaga I., Hatsukade B., Hughes D. H., Ikarashi S., Izumi T., Kawabe R., Kohno K., Lee M., Matsuda Y., Nakanishi K., Saito T., Tamura Y., Ueda J., Umehata H., Wilson G. W., Michiyama T., Ando M., Kamieneski P.

NATURE 560 巻 ( 7720 ) 頁： 613 - + 2018年8月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Nature

Galaxies in the early Universe that are bright at submillimetre wavelengths (submillimetre-bright galaxies) are forming stars at a rate roughly 1,000 times higher than the Milky Way. A large fraction of the new stars form in the central kiloparsec of the galaxy1–3, a region that is comparable in size to the massive, quiescent galaxies found at the peak of cosmic star-formation history4 and the cores of present-day giant elliptical galaxies. The physical and kinematic properties inside these compact starburst cores are poorly understood because probing them at relevant spatial scales requires extremely high angular resolution. Here we report observations with a linear resolution of 550 parsecs of gas and dust in an unlensed, submillimetre-bright galaxy at a redshift of z = 4.3, when the Universe was less than two billion years old. We resolve the spatial and kinematic structure of the molecular gas inside the heavily dust-obscured core and show that the underlying gas disk is clumpy and rotationally supported (that is, its rotation velocity is larger than the velocity dispersion). Our analysis of the molecular gas mass per unit area suggests that the starburst disk is gravitationally unstable, which implies that the self-gravity of the gas is stronger than the differential rotation of the disk and the internal pressure due to stellar-radiation feedback. As a result of the gravitational instability in the disk, the molecular gas would be consumed by star formation on a timescale of 100 million years, which is comparable to gas depletion times in merging starburst galaxies5.

DOI： 10.1038/s41586-018-0443-1

ALMA deep field in SSA22: Survey design and source catalog of a 20 arcmin<SUP>2</SUP> survey at 1.1 mm 査読有り

Umehata Hideki, Hatsukade Bunyo, Smail Ian, Alexander David M., Ivison Rob J., Matsuda Yuichi, Tamura Yoichi, Kohno Kotaro, Kato Yuta, Hayatsu Natsuki H., Kubo Mariko, Ikarashi Soh

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 70 巻 ( 4 ) 2018年8月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

To search for dust-obscured star-formation activity in the early Universe, it is essential to obtain a deep and wide submillimeter/millimeter map. The advent of the Atacama Large Millimeter/submillimeter Array (ALMA) has enabled us to obtain such maps with sufficiently high spatial resolution to be free from source confusion. We present a new 1.1 mm-wave map obtained by ALMA in the SSA22 field. The field contains a remarkable proto-cluster at z = 3.09; therefore, it is an ideal region to investigate the role of a large-scale cosmic web on dust-obscured star formation. The typical 1σ depth of our map is 73 μJy beam−1 with a 0.5 resolution. Combining the present survey with earlier, archived observations, we map an area of 20 arcmin2 (71 comoving Mpc2 at z = 3.09). Within the combined survey area we have detected 35 sources at a signal-to-noise ratio (S/N) >5, with flux densities of S1.1mm = 0.43-5.6 mJy, equivalent to star-formation rates of 100-1000 M yr−1 at z = 3.09, for a Chabrier initial mass function: 17 sources out of 35 are new detections. The cumulative number counts show an excess by a factor of three to five compared to blank fields. The excess suggests enhanced, dust-enshrouded star-formation activity in the proto-cluster on a 10 comoving Mpc scale, indicating accelerated galaxy evolution in this overdense region.

DOI： 10.1093/pasj/psy065

ALMA 26 Arcmin<SUP>2</SUP> Survey of GOODS-S at One Millimeter (ASAGAO): Average Morphology of High-<i>z</i> Dusty Star-forming Galaxies in an Exponential Disk (<i>n</i> ≃ 1) 査読有り

Fujimoto Seiji, Ouchi Masami, Kohno Kotaro, Yamaguchi Yuki, Hatsukade Bunyo, Ueda Yoshihiro, Shibuya Takatoshi, Inoue Shigeki, Oogi Taira, Toft Sune, Gomez-Guijarro Carlos, Wang Tao, Espada Daniel, Nagao Tohru, Tanaka Ichi, Ao Yiping, Umehata Hideki, Taniguchi Yoshiaki, Nakanishi Kouichiro, Rujopakarn Wiphu, Ivison R. J., Wang Wei-hao, Lee Minju M., Tadaki Ken-ichi, Tamura Yoichi, Dunlop J. S.

ASTROPHYSICAL JOURNAL 861 巻 ( 1 ) 2018年7月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present morphological properties of dusty star-forming galaxies at z = 1-3 determined with the high-resolution (FWHM ∼ 0.″19) Atacama Large Milllimeter/submillimeter Array (ALMA) 1 mm map of our ASAGAO survey covering a 26 arcmin2 area in GOODS-S. In conjunction with the ALMA archival data, our sample consists of 45 ALMA sources with infrared luminosity (L IR) range of ∼1011-1013 L o. To obtain an average rest-frame far-infrared (FIR) profile, we perform individual measurements and careful stacking of the ALMA sources using the uv-visibility method that includes positional-uncertainty and smoothing-effect evaluations through Monte Carlo simulations. We find that our sample has an average FIR-wavelength Sérsic index and effective radius of n FIR = 1.2 ± 0.2 and R e,FIR = 1.0-1.3 kpc, respectively, additionally with a point-source component at the center, indicative of the existence of active galactic nuclei. The average FIR profile agrees with a morphology of an exponential disk clearly distinguished from a de Vaucouleurs spheroidal profile (Sérsic index of 4). We also examine the rest-frame optical Sérsic index n opt and effective radius R e,opt with deep Hubble Space Telescope (HST) images. Interestingly, we obtain n opt = 0.9 ± 0.3 (≃n FIR) and R e,opt = 3.2 ± 0.6 kpc (>R e,FIR), suggesting that the dusty disk-like structure is embedded within a larger stellar disk. The rest-frame UV and FIR data of HST and ALMA provide us with a radial profile of the total star formation rate (SFR), where the infrared SFR dominates over the UV SFR at the center. Under the assumption of a constant SFR, a compact stellar distribution in z ∼ 1-2 compact quiescent galaxies (cQGs) is well reproduced, while a spheroidal stellar morphology of cQGs (n opt = 4) is not, suggestive of other important mechanism(s) such as dynamical dissipation.

DOI： 10.3847/1538-4357/aac6c4

Laboratory performance evaluation of the mid-infrared camera and spectrograph MIMIZUKU for the TAO 6.5-m telescope

Kamizuka, Takafumi, Uchiyama, Masahito S, Yamaguchi, Jumpei, Mori, Tomohiro, Ohsawa, Ryou, Yoshida, Yutaka, Sako, Shigeyuki, Miyata, Takashi, Asano, Kentaro, Uchiyama, Mizuho, Sakon, Itsuki, Onaka, Takashi, Kataza, Hirokazu, Aoki, Tsutomu, Doi, Mamoru, Hatsukade, Bunyo, Kato, Natsuko, Kohno, Kotaro, Konishi, Masahiro, Minezaki, Takeo, Morokuma, Tomoki, Motohara, Kentaro, Soyano, Takao, Takahashi, Hidenori, Tanabe, Toshihiko, Tanaka, Masuo, Tarusawa, Ken'ichi, Tamura, Yoichi, Yoichi, Koshida, Shintaro, Terao, Yasunori, Ohashi, Hirofumi, Kono, Yukihiro, Kushibiki, Kosuke, Yoshii, Yuzuru

Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series 10702 巻頁： 107022H 2018年7月

記述言語：英語掲載種別：研究論文（国際会議プロシーディングス）出版者・発行元：Proceedings of SPIE - The International Society for Optical Engineering

The Mid-Infrared Multi-field Imager for gaZing at the UnKnown Universe (MIMIZUKU) is a mid-infrared camera and spectrograph developed as a first-generation instrument on the University of Tokyo Atacama Observatory (TAO) 6.5-m telescope. MIMIZUKU covers a wide wavelength range from 2 to 38 μm and has a unique optical device called Field Stacker which realizes accurate calibration of variable atmospheric transmittance with a few percent accuracy. By utilizing these capabilities, MIMIZUKU realizes mid-infrared long-term monitoring, which has not been challenged well. MIMIZUKU has three optical channels, called NIR, MIR-S, and MIR-L, to realize the wide wavelength coverage. The MIR-S channel, which covers 6.8-26 μm, has been completed by now. We are planning to perform engineering observations with this channel at the Subaru telescope before the completion of the TAO 6.5-m telescope. In this paper, we report the results of the laboratory tests to evaluate the optical and detector performances of the MIR-S channel. As a result, we confirmed a pixel scale of 0.12 arcsec/pix and a vignetting- free field of view of 2./0 1./8. The instrument throughputs for imaging modes are measured to be 20-30%. Those for N - and Q -band spectroscopy modes are 17 and 5%, respectively. As for the detector performance, we derived the quantum efficiency to be 40-50% in the mid-infrared wavelength region and measured the readout noise to be 3000-6000 electrons, which are larger than the spec value. It was found that this large readout noise degrades the sensitivity of MIMIZUKU by a factor of two.

DOI： 10.1117/12.2312443

Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs). III. Star formation properties of the host galaxies at z greater than or similar to 6 studied with ALMA 査読有り

Izumi Takuma, Onoue Masafusa, Shirakata Hikari, Nagao Tohru, Kohno Kotaro, Matsuoka Yoshiki, Imanishi Masatoshi, Strauss Michael A., Kashikawa Nobunari, Schulze Andreas, Silverman John D., Fujimoto Seiji, Harikane Yuichi, Toba Yoshiki, Umehata Hideki, Nakanishi Kouichiro, Greene Jenny E., Tamura Yoichi, Taniguchi Akio, Yamaguchi Yuki, Goto Tomotsugu, Hashimoto Yasuhiro, Ikarashi Soh, Iono Daisuke, Iwasawa Kazushi, Lee Chien-Hsiu, Makiya Ryu, Minezaki Takeo, Tang Ji-Jia

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 70 巻 ( 3 ) 2018年6月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

We present our ALMA Cycle 4 measurements of the [C II] emission line and the underlying far-infrared (FIR) continuum emission from four optically low-luminosity (M1450 > -25) quasars at z ≳ 6 discovered by the Subaru Hyper Suprime Cam (HSC) survey. The [C II] line and FIR continuum luminosities lie in the ranges L[C II] = (3.8-10.2) × 108 L· and LFIR = (1.2-2.0) × 1011 L·, which are at least one order of magnitude smaller than those of optically-luminous quasars at z ≳ 6. We estimate the star formation rates (SFRs) of our targets as ≲ 23-40 M· yr-1. Their line and continuum-emitting regions are marginally resolved, and found to be comparable in size to those of optically-luminous quasars, indicating that their SFR or likely gas mass surface densities (key controlling parameter of mass accretion) are accordingly different. The L[C II]/LFIR ratios of the hosts, ≲ (2.2- 8.7) × 10-3, are fully consistent with local star-forming galaxies. Using the [C II] dynamics, we derived their dynamical masses within a radius of 1.5-2.5 kpc as ≲ (1.4-8.2) × 1010 M·. By interpreting these masses as stellar ones, we suggest that these faint quasar hosts are on or even below the star-forming main sequence at z ∼ 6, i.e., they appear to be transforming into quiescent galaxies. This is in contrast to the optically-luminous quasars at those redshifts, which show starburst-like properties. Finally, we find that the ratios of black hole mass to host galaxy dynamical mass of most of the low-luminosity quasars, including the HSC ones, are consistent with the local value. The mass ratios of the HSC quasars can be reproduced by a semi-analytical model that assumes merger-induced black hole host galaxy evolution.

DOI： 10.1093/pasj/psy026

Obscured Star Formation in the Host Galaxies of Superluminous Supernovae 査読有り

Hatsukade B., Tominaga N., Hayashi M., Konishi M., Matsuda Y., Morokuma T., Morokuma-Matsui K., Motogi K., Niinuma K., Tamura Y.

ASTROPHYSICAL JOURNAL 857 巻 ( 1 ) 頁： 72 - 72 2018年4月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present the results of 3 GHz radio continuum observations of the eight host galaxies of superluminous supernovae (SLSNe) at 0.1 < z < 0.3 by using the Karl G. Jansky Very Large Array. Four host galaxies are detected significantly, and two of them are found to have high star formation rates (SFRs > 20 M o yr-1) derived from radio emission, making them the most intensely star-forming host galaxies among SLSN host galaxies. We compare radio SFRs and optical SFRs, and find that three host galaxies have an excess in radio SFRs by a factor of >2, suggesting the existence of dust-obscured star formation, which cannot be traced by optical studies. Two of the three host galaxies, which are located in the galaxy main sequence based on optical SFRs, are found to be above the main sequence based on their radio SFRs. This suggests a higher fraction of starburst galaxies in SLSN hosts than estimated in previous studies. We calculate extinction from the ratio between radio SFRs and dust-uncorrected optical SFRs and find that the hosts are on the trend of increasing extinction with metallicity, which is consistent with the relation in local star-forming galaxies. We also place a constraint on a pulsar-driven SN model, which predicts quasi-steady synchrotron radio emission.

DOI： 10.3847/1538-4357/aab616

Molecular Gas Reservoirs in Cluster Galaxies at z=1.46 査読有り

Hayashi Masao, Tadaki Ken-ichi, Kodama Tadayuki, Kohno Kotaro, Yamaguchi Yuki, Hatsukade Bunyo, Koyama Yusei, Shimakawa Rhythm, Tamura Yoichi, Suzuki Tomoko L.

ASTROPHYSICAL JOURNAL 856 巻 ( 2 ) 頁： 118 - 118 2018年4月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present molecular gas reservoirs of 18 galaxies associated with the XMMXCS J2215.9-1738 cluster at z = 1.46. From Band 7 and Band 3 data of the Atacama Large Millimeter/submillimeter Array, we detect dust continuum emission at 870 μm and the CO J = 2-1 emission line from 8 and 17 member galaxies, respectively, within a clustercentric radius of R 200. The molecular gas masses derived from the CO and/or dust continuum luminosities show that the fraction of molecular gas mass and the depletion timescale for the cluster galaxies are larger than expected from the scaling relations of molecular gas on stellar mass and offset from the main sequence of star-forming galaxies in general fields. The galaxies closer to the cluster center in terms of both projected position and accretion phase seem to show a larger deviation from the scaling relations. We speculate that the environment of the galaxy cluster helps feed the gas through inflow to the member galaxies and reduce the efficiency of star formation. The stacked Band 3 spectrum of 12 quiescent galaxies with M stellar ∼ 1011 M o within 0.5R 200 shows no detection of a CO emission line, giving the upper limit of molecular gas mass and molecular gas fraction to be ≲1010 M o and ≲10%, respectively. Therefore, the massive galaxies in the cluster core quench the star formation activity while consuming most of the gas reservoirs.

DOI： 10.3847/1538-4357/aab3e7

ALMA 26 arcmin<SUP>2</SUP> Survey of GOODS-S at One-millimeter (ASAGAO): X-Ray AGN Properties of Millimeter-selected Galaxies 査読有り

Ueda Y., Hatsukade B., Kohno K., Yamaguchi Y., Tamura Y., Umehata H., Akiyama M., Ao Y., Aretxaga I., Caputi K., Dunlop J. S., Espada D., Fujimoto S., Hayatsu N. H., Imanishi M., Inoue A. K., Ivison R. J., Kodama T., Lee M. M., Matsuoka K., Miyaji T., Morokuma-Matsui K., Nagao T., Nakanishi K., Nyland K., Ohta K., Ouchi M., Rujopakarn W., Saito T., Tadaki K., Tanaka I., Taniguchi Y., Wang T., Wang W-H., Yoshimura Y., Yun M. S.

ASTROPHYSICAL JOURNAL 853 巻 ( 1 ) 2018年1月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We investigate the X-ray active galactic nucleus (AGN) properties of millimeter galaxies in the Great Observatories Origins Deep Survey South (GOODS-S) field detected with the Atacama Large Millimeter/submillimeter Array (ALMA), by utilizing the Chandra 7-Ms data, the deepest X-ray survey to date. Our millimeter galaxy sample comes from the ASAGAO survey covering 26 arcmin2 (12 sources at a 1.2 mm flux-density limit of mJy), supplemented by the deeper but narrower 1.3 mm survey of a part of the ASAGAO field by Dunlop et al. Ofthe 25 total millimeter galaxies, 14 have Chandra counterparts. The observed AGN fractions at are found to be 90+8-19% and 57+23-25% for the ultra-luminous and luminous infrared galaxies with log LIR/L⊙ = 12-12.8 and log IR/L⊙ = 11.5-12, respectively. The majority (∼2/3) of the ALMA and/or Herschel detected X-ray AGNs at z = 1.5-3 appear to be star-formation-dominant populations, having / ratios smaller than the "simultaneous evolution" value expected from the local black-hole-mass-to-stellar-mass (-M ∗) relation. On the basis of the and stellar mass relation, we infer that a large fraction of star-forming galaxies at have black hole masses that are smaller than those expected from the local -M ∗ relation. This contrasts previous reports on luminous AGNs at the same redshifts detected in wider and shallower surveys, which are subject to selection biases against lower luminosity AGNs. Our results are consistent with an evolutionary scenario in which star formation occurs first, and an AGN-dominant phase follows later, in objects that finally evolve into galaxies with classical bulges.

DOI： 10.3847/1538-4357/aa9f10

Development status of the simultaneous two-color near-infrared multi-object spectrograph SWIMS for the TAO 6.5m telescope

Konishi Masahiro, Motohara Kentaro, Takahashi Hidenori, Kato Natsuko, Terao Yasunori, Ohashi Hirofumi, Kono Yukihiro, Kushibiki Kosuke, Kodama Tadayuki, Hayashi Masao, Tanaka Ichi, Tadaki Ken-ichi, Toshikawa Jun, Koyama Yusei, Shimakawa Rhythm, Suzuki Tomoko, Tateuchi Ken, Kitagawa Yutaro, Kobayakawa Yutaka, Todo Soya, Aoki Tsutomu, Doi Mamoru, Hatsukade Bunyo, Kamizuka Takafumi, Kohno Kotaro, Minezaki Takeo, Miyata Takashi, Morokuma Tomoki, Sako Shigeyuki, Soyano Takao, Tanabc Toshihiko, Tanaka Masuo, Tarusawa Ken'ichi, Tamura Yoichi, Koshida Shintaro, Ohsawa Ryou, Uchiyama Masahito, Mori Tomohiro, Yamaguchi Jumpei, Yoshida Yutaka, Yoshii Yuzuru

GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY VII 10702 巻頁： 1070226 2018年

記述言語：日本語掲載種別：研究論文（国際会議プロシーディングス）出版者・発行元：Proceedings of SPIE - The International Society for Optical Engineering

The Simultaneous-color Wide-field Infrared Multi-object Spectrograph, SWIMS, is a first-generation near-infrared instrument for the University of Tokyo Atacama Observatory (TAO) 6.5m Telescope now being constructed in northern Chile. To utilize the advantage of the site that almost continuous atmospheric window appears from 0.9 to 2.5 μm, the instrument is capable of simultaneous two-color imaging with a field-of-view of 9.′6 in diameter or λ/Δλ 1000 multi-object spectroscopy at 0.9-2.5 μm in a single exposure. The instrument has been trans- ported in 2017 to the Subaru Telescope as a PI-type instrument for carrying out commissioning observations before starting science operation on the 6.5m telescope. In this paper, we report the latest updates on the instrument and present preliminary results from the on-sky performance verification observations.

DOI： 10.1117/12.2310060

VizieR Online Data Catalog: mm-wave size study of ALMA submm galaxies (Ikarashi+, 2017) 査読有り

Ikarashi} S, Caputi} K.~I, Ohta} K, Ivison} R.~J, Lagos} C.~D.~P, Bisigello} L, Hatsukade} B, Aretxaga} I, Dunlop} J.~S, Hughes} D.~H, Iono} D, Izumi} T, Kashikawa} N, Koyama} Y, Kawabe} R, Kohno} K, Motohara} K, Nakanishi} K, Tamura} Y, Umehata} H, Wilson} G.~W, Yabe} K, Yun} M

VizieR Online Data Catalog 頁： J/ApJ/849/L36 2018年

Deep Submillimeter and Radio Observations in the SSA22 Field. I. Powering Sources and the Lyα Escape Fraction of Lyα Blobs 査読有り

Ao Y., Matsuda Y., Henkel C., Iono D., Alexander D. M., Chapman S. C., Geach J., Hatsukade B., Hayes M., Hine N. K., Kato Y., Kawabe R., Kohno K., Kubo M., Lehnert M., Malkan M., Menten K. M., Nagao T., Norris R. P., Ouchi M., Saito T., Tamura Y., Taniguchi Y., Umehata H., Weiss A.

ASTROPHYSICAL JOURNAL 850 巻 ( 2 ) 2017年12月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We study the heating mechanisms and Lyα escape fractions of 35 Lyα blobs (LABs) at z ≈ 3.1 in the SSA22 field. Dust continuum sources have been identified in 11 of the 35 LABs, all with star formation rates (SFRs) above 100 M o yr-1. Likely radio counterparts are detected in 9 out of 29 investigated LABs. The detection of submillimeter dust emission is more linked to the physical size of the Lyα emission than to the Lyα luminosities of the LABs. A radio excess in the submillimeter/radio-detected LABs is common, hinting at the presence of active galactic nuclei. Most radio sources without X-ray counterparts are located at the centers of the LABs. However, all X-ray counterparts avoid the central regions. This may be explained by absorption due to exceptionally large column densities along the line-of-sight or by LAB morphologies, which are highly orientation dependent. The median Lyα escape fraction is about 3% among the submillimeter-detected LABs, which is lower than a lower limit of 11% for the submillimeter-undetected LABs. We suspect that the large difference is due to the high dust attenuation supported by the large SFRs, the dense large-scale environment as well as large uncertainties in the extinction corrections required to apply when interpreting optical data.

DOI： 10.3847/1538-4357/aa960f

J-GEM observations of an electromagnetic counterpart to the neutron star merger GW170817 査読有り

Utsumi Yousuke, Tanaka Masaomi, Tominaga Nozomu, Yoshida Michitoshi, Barway Sudhanshu, Nagayama Takahiro, Zenko Tetsuya, Aoki Kentaro, Fujiyoshi Takuya, Furusawa Hisanori, Kawabata Koji S., Koshida Shintaro, Lee Chien-Hsiu, Morokuma Tomoki, Motohara Kentaro, Nakata Fumiaki, Ohsawa Ryou, Ohta Kouji, Okita Hirofumi, Tajitsu Akito, Tanaka Ichi, Terai Tsuyoshi, Yasuda Naoki, Abe Fumio, Asakura Yuichiro, Bond Ian A., Miyazaki Shota, Sumi Takahiro, Tristram Paul J., Honda Satoshi, Itoh Ryosuke, Itoh Yoichi, Kawabata Miho, Morihana Kumiko, Nagashima Hiroki, Nakaoka Tatsuya, Ohshima Tomohito, Takahashi Jun, Takayama Masaki, Aoki Wako, Baar Stefan, Doi Mamoru, Finet Francois, Kanda Nobuyuki, Kawai Nobuyuki, Kim Ji Hoon, Kuroda Daisuke, Liu Wei, Matsubayashi Kazuya, Murata Katsuhiro L., Nagai Hiroshi, Saito Tomoki, Saito Yoshihiko, Sako Shigeyuki, Sekiguchi Yuichiro, Tamura Yoichi, Tanaka Masayuki, Uemura Makoto, Yamaguchi Masaki S.

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 69 巻 ( 6 ) 頁： 101 2017年12月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

GW170817 is the first detected gravitational wave source from a neutron star merger. We present the Japanese collaboration for gravitational-wave electro-magnetic (J-GEM) follow-up observations of SSS17a, an electromagnetic counterpart of GW170817. SSS17a shows a 2.5mag decline in the z band during the period between 1.7 and 7.7 d after the merger. Such a rapid decline is not comparable with supernovae light curves at any epoch. The color of SSS17a also evolves rapidly and becomes redder during later epochs: the z - H color has changed by approximately 2.5mag during the period between 0.7 and 7.7 d. The rapid evolutions of both the color and the optical brightness are consistent with the expected properties of a kilonova that is powered by the radioactive decay of newly synthesized r-process nuclei. Kilonova models with Lanthanide elements can reproduce the aforementioned observed properties well, which suggests that r-process nucleosynthesis beyond the second peak takes place in SSS17a. However, the absolute magnitude of SSS17a is brighter than the expected brightness of the kilonova models with an ejectamass of 0.01M⊙, which suggests a more intensemass ejection (~0.03M⊙) or possibly an additional energy source.

DOI： 10.1093/pasj/psx118

Kilonova from post-merger ejecta as an optical and near-Infrared counterpart of GW170817 査読有り

Tanaka Masaomi, Utsumi Yousuke, Mazzali Paolo A., Tominaga Nozomu, Yoshida Michitoshi, Sekiguchi Yuichiro, Morokuma Tomoki, Motohara Kentaro, Ohta Kouji, Kawabata Koji S., Abe Fumio, Aoki Kentaro, Asakura Yuichiro, Baar Stefan, Barway Sudhanshu, Bond Ian A., Doi Mamoru, Fujiyoshi Takuya, Furusawa Hisanori, Honda Satoshi, Itoh Yoichi, Kawabata Miho, Kawai Nobuyuki, Kim Ji Hoon, Lee Chien-Hsiu, Miyazaki Shota, Morihana Kumiko, Nagashima Hiroki, Nagayama Takahiro, Nakaoka Tatsuya, Nakata Fumiaki, Ohsawa Ryou, Ohshima Tomohito, Okita Hirofumi, Saito Tomoki, Sumi Takahiro, Tajitsu Akito, Takahashi Jun, Takayama Masaki, Tamura Yoichi, Tanaka Ichi, Terai Tsuyoshi, Tristram Paul J., Yasuda Naoki, Zenko Tetsuya

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 69 巻 ( 6 ) 頁： 102 2017年12月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

Recent detection of gravitationalwaves from a neutron star (NS)merger event GW170817 and identification of an electromagnetic counterpart provide a unique opportunity to study the physical processes in NS mergers. To derive properties of ejected material from the NS merger, we perform radiative transfer simulations of kilonova, optical and near-infrared emissions powered by radioactive decays of r-process nuclei synthesized in the merger. We find that the observed near-infrared emission lasting for >10 d is explained by 0.03M⊙ of ejecta containing lanthanide elements. However, the blue optical component observed at the initial phases requires an ejecta component with a relatively high electron fraction (Ye). We show that both optical and near-infrared emissions are simultaneously reproduced by the ejecta with a medium Ye of ~0.25. We suggest that a dominant component powering the emission is post-merger ejecta, which exhibits that the mass ejection after the first dynamical ejection is quite efficient. Our results indicate that NS mergers synthesize a wide range of r-process elements and strengthen the hypothesis that NS mergers are the origin of r-process elements in the Universe.

DOI： 10.1093/pasj/psx121

Diverse Nuclear Star-forming Activities in the Heart of NGC 253 Resolved with 10-pc-scale ALMA Images 査読有り

Ando Ryo, Nakanishi Kouichiro, Kohno Kotaro, Izumi Takuma, Martin Sergio, Harada Nanase, Takano Shuro, Kuno Nario, Nakai Naomasa, Sugai Hajime, Sorai Kazuo, Tosaki Tomoka, Matsubayashi Kazuya, Nakajima Taku, Nishimura Yuri, Tamura Yoichi

ASTROPHYSICAL JOURNAL 849 巻 ( 2 ) 頁： 81 - 81 2017年11月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present an 8 pc × 5 pc resolution view of the central ∼200 pc region of the nearby starburst galaxy NGC 253, based on ALMA Band 7 (λ ≈ 0.85 mm or v ∼ 350 GHz) observations covering 11 GHz. We resolve the nuclear starburst of NGC 253 into eight dusty star-forming clumps, 10 pc in scale, for the first time. These clumps, each of which contains (4-10) × 104 M∗odot; of dust (assuming that the dust temperature is 25 K) and up to 6 × 102 massive (O5V) stars, appear to be aligned in two parallel ridges, while they have been blended in previous studies. Despite the similarities in sizes and dust masses of these clumps, their line spectra vary drastically from clump to clump, although they are separated by only ∼10 pc. Specifically, one of the clumps, Clump 1, exhibits line-confusionlimited spectra with at least 36 emission lines from 19 molecules (including CH3OH, HNCO, H2CO, CH3CCH, H2CS, and H3MO+) and a hydrogen recombination line (H26α), while far fewer kinds of molecular lines are detected in some other clumps where fragile species, such as complex organic molecules and HNCO, completely disappear from their spectra. We demonstrate the existence of hot molecular gas (Trot (SO2) = 90 ± 11K) in the former clump, which suggests that the hot and chemically rich environments are localized within a 10-pc-scale starforming clump.

DOI： 10.3847/1538-4357/aa8fd4

Very Compact Millimeter Sizes for Composite Star-forming/AGN Submillimeter Galaxies 査読有り

Ikarashi Soh, Caputi Karina I., Ohta Kouji, Ivison R. J., Lagos Claudia D. P., Bisigello Laura, Hatsukade Bunyo, Aretxaga Itziar, Dunlop James S., Hughes David H., Iono Daisuke, Izumi Takuma, Kashikawa Nobunari, Koyama Yusei, Kawabe Ryohei, Kohno Kotaro, Motohara Kentaro, Nakanishi Kouichiro, Tamura Yoichi, Umehata Hideki, Wilson Grant W., Yabe Kiyoto, Yun Min S.

ASTROPHYSICAL JOURNAL LETTERS 849 巻 ( 2 ) 頁： L36 - L36 2017年11月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal Letters

We report the study of the far-infrared (IR) sizes of submillimeter galaxies (SMGs) in relation to their dustobscured star formation rate (SFR) and active galactic nuclei (AGN) presence, determined using mid-IR photometry. We determined the millimeter-wave (λobs = 1100 μm) sizes of 69 Atacama Large Millimeter/ submillimeter Array (ALMA)-identified SMGs, selected with ≥10 δ confidence on ALMA images (F1100 μm = 1.7-7.4 mJy). We found that all of the SMGs are located above an avoidance region in the sizeflux plane, as expected by the Eddington limit for star formation. In order to understand what drives the different millimeter-wave sizes in SMGs, we investigated the relation between millimeter-wave size and AGN fraction for 25 of our SMGs at z=1-3. We found that the SMGs for which the mid-IR emission is dominated by star formation or AGN have extended millimeter-sizes, with respective median Rc,e = 1.6-0.21+0.34 and 1.5 -0.24+0.93 kpc. Instead, the SMGs for which the mid-IR emission corresponds to star-forming/AGN composites have more compact millimeter-wave sizes, with median Rc,e1.0 -0.20+0.20kpc. The relation between millimeter-wave size and AGN fraction suggests that this size may be related to the evolutionary stage of the SMG. The very compact sizes for composite star-forming/AGN systems could be explained by supermassive black holes growing rapidly during the SMG coalescing, star-formation phase.

DOI： 10.3847/2041-8213/aa9572

その他リンク： https://iopscience.iop.org/article/10.3847/2041-8213/aa9572

Multi-messenger Observations of a Binary Neutron Star Merger 査読有り

Abbott B. P., Abbott R., Abbott T. D., Acernese F., Ackley K., Adams C., Adams T., Addesso P., Adhikari R. X., Adya V. B., Affeldt C., Afrough M., Agarwal B., Agathos M., Agatsuma K., Aggarwal N., Aguiar O. D., Aiello L., Ain A., Ajith P., Allen B., Allen G., Allocca A., Altin P. A., Amato A., Ananyeva A., Anderson S. B., Anderson W. G., Angelova S. V., Antier S., Appert S., Arai K., Araya M. C., Areeda J. S., Arnaud N., Arun K. G., Ascenzi S., Ashton G., Ast M., Aston S. M., Astone P., Atallah D. V., Aufmuth P., Aulbert C., AultONeal K., Austin C., Avila-Alvarez A., Babak S., Bacon P., Bader M. K. M., Bae S., Baker P. T., Baldaccini F., Ballardin G., Ballmer S. W., Banagiri S., Barayoga J. C., Barclay S. E., Barish B. C., Barker D., Barkett K., Barone F., Barr B., Barsotti L., Barsuglia M., Barta D., Barthelmy S. D., Bartlett J., Bartos I., Bassiri R., Basti A., Batch J. C., Bawaj M., Bayley J. C., Bazzan M., Becsy B., Beer C., Bejger M., Belahcene I., Bell A. S., Berger B. K., Bergmann G., Bero J. J., Berry C. P. L., Bersanetti D., Bertolini A., Betzwieser J., Bhagwat S., Bhandare R., Bilenko I. A., Billingsley G., Billman C. R., Birch J., Birney R., Birnholtz O., Biscans S., Biscoveanu S., Bisht A., Bitossi M., Biwer C., Bizouard M. A., Blackburn J. K., Blackman J., Blair C. D., Blair D. G., Blair R. M., Bloemen S., Bock O., Bode N., Boer M., Bogaert G., Bohe A., Bondu F., Bonilla E., Bonnand R., Boom B. A., Bork R., Boschi V., Bose S., Bossie K., Bouffanais Y., Bozzi A., Bradaschia C., Brady P. R., Branchesi M., Brau J. E., Briant T., Brillet A., Brinkmann M., Brisson V., Brockill P., Broida J. E., Brooks A. F., Brown D. A., Brown D. D., Brunett S., Buchanan C. C., Buikema A., Bulik T., Bulten H. J., Buonanno A., Buskulic D., Buy C., Byer R. L., Cabero M., Cadonati L., Cagnoli G., Cahillane C., Bustillo J. Caldern, Callister T. A., Calloni E., Camp J. B., Canepa M., Canizares P., Cannon K. C., Cao H., Cao J., Capano C. D., Capocasa E., Carbognani F., Caride S., Carney M. F., Diaz J. Casanueva, Casentini C., Caudill S., Cavagli M., Cavalier F., Cavalieri R., Cella G., Cepeda C. B., Cerd-Durn P., Cerretani G., Cesarini E., Chamberlin S. J., Chan M., Chao S., Charlton P., Chase E., Chassande-Mottin E., Chatterjee D., Chatziioannou K., Cheeseboro B. D., Chen H. Y., Chen X., Chen Y., Cheng H. -P., Chia H., Chincarini A., Chiummo A., Chmiel T., Cho H. S., Cho M., Chow J. H., Christensen N., Chu Q., Chua A. J. K., Chua S., Chung A. K. W., Chung S., Ciani G., Ciolfi R., Cirelli C. E., Cirone A., Clara F., Clark J. A., Clearwater P., Cleva F., Cocchieri C., Coccia E., Cohadon P. -F., Cohen D., Colla A., Collette C. G., Cominsky L. R., Constancio M., Conti L., Cooper S. J., Corban P., Corbitt T. R., Cordero-Carrion I., Corley K. R., Cornish N., Corsi A., Cortese S., Costa C. A., Coughlin M. W., Coughlin S. B., Coulon J. -P., Countryman S. T., Couvares P., Covas P. B., Cowan E. E., Coward D. M., Cowart M. J., Coyne D. C., Coyne R., Creighton J. D. E., Creighton T. D., Cripe J., Crowder S. G., Cullen T. J., Cumming A., Cunningham L., Cuoco E., Dal Canton T., Dlya G., Danilishin S. L., D'Antonio S., Danzmann K., Dasgupta A., Costa C. F. Da Silva, Dattilo V., Dave I., Davier M., Davis D., Daw E. J., Day B., De S., Debra D., Degallaix J., De laurentis M., Deleglise S., Del Pozzo W., Demos N., Denker T., Dent T., De Pietri R., Dergachev V., De Rosa R., DeRosa R. T., De Rossi C., DeSalvo R., De Varona O., Devenson J., Dhurandhar S., Diaz M. C., Di Fiore L., Di Giovanni M., Di Girolamo T., Di Lieto A., Di Pace S., Di Palma I., Di Renzo F., Doctor Z., Dolique V., Donovan F., Dooley K. L., Doravari S., Dorrington I., Douglas R., Alvarez M. Dovale, Downes T. P., Drago M., Dreissigacker C., Driggers J. C., Du Z., Ducrot M., Dupej P., Dwyer S. E., Edo T. B., Edwards M. C., Effler A., Eggenstein H. -B., Ehrens P., Eichholz J., Eikenberry S. S., Eisenstein R. A., Essick R. C., Estevez D., Etienne Z. B., Etzel T., Evans M., Evans T. M., Factourovich M., Fafone V., Fair H., Fairhurst S., Fan X., Farinon S., Farr B., Farr W. M., Fauchon-Jones E. J., Favata M., Fays M., Fee C., Fehrmann H., Feicht J., Fejer M. M., Fernandez-Galiana A., Ferrante I., Ferreira E. C., Ferrini F., Fidecaro F., Finstad D., Fiori I., Fiorucci D., Fishbach M., Fisher R. P., Fitz-Axen M., Flaminio R., Fletcher M., Fong H., Font J. A., Forsyth P. W. F., Forsyth S. S., Fournier J. -D., Frasca S., Frasconi F., Frei Z., Freise A., Frey R., Frey V., Fries E. M., Fritschel P., Frolov V. V., Fulda P., Fyffe M., Gabbard H., Gadre B. U., Gaebel S. M., Gair J. R., Gammaitoni L., Ganija M. R., Gaonkar S. G., Garcia-Quiros C., Garufi F., Gateley B., Gaudio S., Gaur G., Gayathri V., Gehrels N., Gemme G., Genin E., Gennai A., George D., George J., Gergely L., Germain V., Ghonge S., Ghosh Abhirup, Ghosh Archisman, Ghosh S., Giaime J. A., Giardina K. D., Giazotto A., Gill K., Glover L., Goetz E., Goetz R., Gomes S., Goncharov B., Gonzlez G., Castro J. M. Gonzalez, Gopakumar A., Gorodetsky M. L., Gossan S. E., Gosselin M., Gouaty R., Grado A., Graef C., Granata M., Grant A., Gras S., Gray C., Greco G., Green A. C., Gretarsson E. M., Griswold B., Groot P., Grote H., Grunewald S., Gruning P., Guidi G. M., Guo X., Gupta A., Gupta M. K., Gushwa K. E., Gustafson E. K., Gustafson R., Halim O., Hall B. R., Hall E. D., Hamilton E. Z., Hammond G., Haney M., Hanke M. M., Hanks J., Hanna C., Hannam M. D., Hannuksela O. A., Hanson J., Hardwick T., Harms J., Harry G. M., Harry I. W., Hart M. J., Haster C. -J., Haughian K., Healy J., Heidmann A., Heintze M. C., Heitmann H., Hello P., Hemming G., Hendry M., Heng I. S., Hennig J., Heptonstall A. W., Heurs M., Hild S., Hinderer T., Hoak D., Hofman D., Holt K., Holz D. E., Hopkins P., Horst C., Hough J., Houston E. A., Howell E. J., Hreibi A., Hu Y. M., Huerta E. A., Huet D., Hughey B., Husa S., Huttner S. H., Huynh-Dinh T., Indik N., Inta R., Intini G., Isa H. N., Isac J. -M., Isi M., Iyer B. R., Izumi K., Jacqmin T., Jani K., Jaranowski P., Jawahar S., Jimenez-Forteza F., Johnson W. W., Jones D. I., Jones R., Jonker R. J. G., Ju L., Junker J., Kalaghatgi C. V., Kalogera V., Kamai B., Kandhasamy S., Kang G., Kanner J. B., Kapadia S. J., Karki S., Karvinen K. S., Kasprzack M., Katolik M., Katsavounidis E., Katzman W., Kaufer S., Kawabe K., Kefelian F., Keitel D., Kemball A. J., Kennedy R., Kent C., Key J. S., Khalili F. Y., Khan I., Khan S., Khan Z., Khazanov E. A., Kijbunchoo N., Kim Chunglee, Kim J. C., Kim K., Kim W., Kim W. S., Kim Y. -M., Kimbrell S. J., King E. J., King P. J., Kinley-Hanlon M., Kirchhoff R., Kissel J. S., Kleybolte L., Klimenko S., Knowles T. D., Koch P., Koehlenbeck S. M., Koley S., Kondrashov V., Kontos A., Korobko M., Korth W. Z., Kowalska I., Kozak D. B., Krmer C., Kringel V., Krishnan B., Krlak A., Kuehn G., Kumar P., Kumar R., Kumar S., Kuo L., Kutynia A., Kwang S., Lackey B. D., Lai K. H., Landry M., Lang R. N., Lange J., Lantz B., Lanza R. K., Larson S. L., Lartaux-Vollard A., Lasky P. D., Laxen M., Lazzarini A., Lazzaro C., Leaci P., Leavey S., Lee C. H., Lee H. K., Lee H. M., Lee H. W., Lee K., Lehmann J., Lenon A., Leonardi M., Leroy N., Letendre N., Levin Y., Li T. G. F., Linker S. D., Littenberg T. B., Liu J., Lo R. K. L., Lockerbie N. A., London L. T., Lord J. E., Lorenzini M., Loriette V., Lormand M., Losurdo G., Lough J. D., Lousto C. O., Lovelace G., Lck H., Lumaca D., Lundgren A. P., Lynch R., Ma Y., Macas R., Macfoy S., Machenschalk B., MacInnis M., Macleod D. M., Hernandez I. Magaa, Magaa-Sandoval F., Zertuche L. Magaa, Magee R. M., Majorana E., Maksimovic I., Man N., Mandic V., Mangano V., Mansell G. L., Manske M., Mantovani M., Marchesoni F., Marion F., Mrka S., Mrka Z., Markakis C., Markosyan A. S., Markowitz A., Maros E., Marquina A., Marsh P., Martelli F., Martellini L., Martin I. W., Martin R. M., Martynov D. V., Mason K., Massera E., Masserot A., Massinger T. J., Masso-Reid M., Mastrogiovanni S., Matas A., Matichard F., Matone L., Mavalvala N., Mazumder N., McCarthy R., McClelland D. E., McCormick S., McCuller L., McGuire S. C., McIntyre G., McIver J., McManus D. J., McNeill L., Mcrae T., McWilliams S. T., Meacher D., Meadors G. D., Mehmet M., Meidam J., Mejuto-Villa E., Melatos A., Mendell G., Mercer R. A., Merilh E. L., Merzougui M., Meshkov S., Messenger C., Messick C., Metzdorff R., Meyers P. M., Miao H., Michel C., Middleton H., Mikhailov E. E., Milano L., Mueller A. L., Mueller B. B., Miller J., Millhouse M., Milovich-Goff M. C., Minazzoli O., Minenkov Y., Ming J., Mishra C., Mitra S., Mitrofanov V. P., Mitselmakher G., Mittleman R., Moffa D., Moggi A., Mogushi K., Mohan M., Mohapatra S. R. P., Montani M., Moore C. J., Moraru D., Moreno G., Morriss S. R., Mours B., Mow-Lowry C. M., Mueller G., Muir A. W., Mukherjee Arunava, Mukherjee D., Mukherjee S., Mukund N., Mullavey A., Munch J., Muniz E. A., Muratore M., Murray P. G., Napier K., Nardecchia I., Naticchioni L., Nayak R. K., Neilson J., Nelemans G., Nelson T. J. N., Nery M., Neunzert A., Nevin L., Newport J. M., Newton G., Ng K. K. Y., Nguyen P., Nguyen T. T., Nichols D., Nielsen A. B., Nissanke S., Nitz A., Noack A., Nocera F., Nolting D., North C., Nuttall L. K., Oberling J., O'Dea G. D., Ogin G. H., Oh J. J., Oh S. H., Ohme F., Okada M. A., Oliver M., Oppermann P., Oram Richard J., O'Reilly B., Ormiston R., Ortega L. F., O'Shaughnessy R., Ossokine S., Ottaway D. J., Overmier H., Owen B. J., Pace A. E., Page J., Page M. A., Pai A., Pai S. A., Palamos J. R., Palashov O., Palomba C., Pal-Singh A., Pan Howard, Pan Huang-Wei, Pang B., Pang P. T. H., Pankow C., Pannarale F., Pant B. C., Paoletti F., Paoli A., Papa M. A., Parida A., Parker W., Pascucci D., Pasqualetti A., Passaquieti R., Passuello D., Patil M., Patricelli B., Pearlstone B. L., Pedraza M., Pedurand R., Pekowsky L., Pele A., Penn S., Perez C. J., Perreca A., Perri L. M., Pfeiffer H. P., Phelps M., Piccinni O. J., Pichot M., Piergiovanni F., Pierro V., Pillant G., Pinard L., Pinto I. M., Pirello M., Pitkin M., Poe M., Poggiani R., Popolizio P., Porter E. K., Post A., Powell J., Prasad J., Pratt J. W. W., Pratten G., Predoi V., Prestegard T., Price L. R., Prijatelj M., Principe M., Privitera S., Prodi G. A., Prokhorov L. G., Puncken O., Punturo M., Puppo P., Prrer M., Qi H., Quetschke V., Quintero E. A., Quitzow-James R., Raab F. J., Rabeling D. S., Radkins H., Raffai P., Raja S., Rajan C., Rajbhandari B., Rakhmanov M., Ramirez K. E., Ramos-Buades A., Rapagnani P., Raymond V., Razzano M., Read J., Regimbau T., Rei L., Reid S., Reitze D. H., Ren W., Reyes S. D., Ricci F., Ricker P. M., Rieger S., Riles K., Rizzo M., Robertson N. A., Robie R., Robinet F., Rocchi A., Rolland L., Rollins J. G., Roma V. J., Romano R., Romel C. L., Romie J. H., Rosinska D., Ross M. P., Rowan S., Rdiger A., Ruggi P., Rutins G., Ryan K., Sachdev S., Sadecki T., Sadeghian L., Sakellariadou M., Salconi L., Saleem M., Salemi F., Samajdar A., Sammut L., Sampson L. M., Sanchez E. J., Sanchez L. E., Sanchis-Gual N., Sandberg V., Sanders J. R., Sassolas B., Sathyaprakash B. S., Saulson P. R., Sauter O., Savage R. L., Sawadsky A., Schale P., Scheel M., Scheuer J., Schmidt J., Schmidt P., Schnabel R., Schofield R. M. S., Schonbeck A., Schreiber E., Schuette D., Schulte B. W., Schutz B. F., Schwalbe S. G., Scott J., Scott S. M., Seidel E., Sellers D., Sengupta A. S., Sentenac D., Sequino V., Sergeev A., Shaddock D. A., Shaffer T. J., Shah A. A., Shahriar M. S., Shaner M. B., Shao L., Shapiro B., Shawhan P., Sheperd A., Shoemaker D. H., Shoemaker D. M., Siellez K., Siemens X., Sieniawska M., Sigg D., Silva A. D., Singer L. P., Singh A., Singhal A., Sintes A. M., Slagmolen B. J. J., Smith B., Smith J. R., Smith R. J. E., Somala S., Son E. J., Sonnenberg J. A., Sorazu B., Sorrentino F., Souradeep T., Spencer A. P., Srivastava A. K., Staats K., Staley A., Steinke M., Steinlechner J., Steinlechner S., Steinmeyer D., Stevenson S. P., Stone R., Stops D. J., Strain K. A., Stratta G., Strigin S. E., Strunk A., Sturani R., Stuver A. L., Summerscales T. Z., Sun L., Sunil S., Suresh J., Sutton P. J., Swinkels B. L., Szczepanczyk M. J., Tacca M., Tait S. C., Talbot C., Talukder D., Tanner D. B., Tpai M., Taracchini A., Tasson J. D., Taylor J. A., Taylor R., Tewari S. V., Theeg T., Thies F., Thomas E. G., Thomas M., Thomas P., Thorne K. A., Thorne K. S., Thrane E., Tiwari S., Tiwari V., Tokmakov K. V., Toland K., Tonelli M., Tornasi Z., Torres-Forn A., Torrie C. I., Toyr D., Travasso F., Traylor G., Trinastic J., Tringali M. C., Trozzo L., Tsang K. W., Tse M., Tso R., Tsukada L., Tsuna D., Tuyenbayev D., Ueno K., Ugolini D., Unnikrishnan C. S., Urban A. L., Usman S. A., Vahlbruch H., Vajente G., Valdes G., Van Bakel N., Van Beuzekom M., van den Brand J. F. J., van den Broeck C., Vander-Hyde D. C., van der Schaaf L., van Heijningen J. V., van Veggel A. A., Vardaro M., Varma V., Vass S., Vasuth M., Vecchio A., Vedovato G., Veitch J., Veitch P. J., Venkateswara K., Venugopalan G., Verkindt D., Vetro F., Vicere A., Viets A. D., Vinciguerra S., Vine D. J., Vinet J. Y., Vitale S., Vo T., Vocca H., Vorvick C., Vyatchanin S. P., Wade A. R., Wade L. E., Wade M., Walet R., Walker M., Wallace L., Walsh S., Wang G., Wang H., Wang J. Z., Wang W. H., Wang Y. F., Ward R. L., Warner J., Was M., Watchi J., Weaver B., Wei L. -W., Weinert M., Weinstein A. J., Weiss R., Wen L., Wessel E. K., Wessels P., Westerweck J., Westphal T., Wette K., Whelan J. T., Whitcomb S. E., Whiting B. F., Whittle C., Wilken D., Williams D., Williams R. D., Williamson A. R., Willis J. L., Willke B., Wimmer M. H., Winkler W., Wipf C. C., Wittel H., Woan G., Woehler J., Wofford J., Wong K. W. K., Worden J., Wright J. L., Wu D. S., Wysocki D. M., Xiao S., Yamamoto H., Yancey C. C., Yang L., Yap M. J., Yazback M., Yu Hang, Yu Haocun, Yvert M., Zadrozny A., Zanolin M., Zelenova T., Zendri J. -P., Zevin M., Zhang L., Zhang M., Zhang T., Zhang Y. -H., Zhao C., Zhou M., Zhou Z., Zhu S. J., Zhu X. J., Zimmerman A. B., Zucker M. E., Zweizig J., Wilson-Hodge C. A., Bissaldi E., Blackburn L., Briggs M. S., Burns E., Cleveland W. H., Connaughton V., Gibby M. H., Giles M. M., Goldstein A., Hamburg R., Jenke P., Hui C. M., Kippen R. M., Kocevski D., McBreen S., Meegan C. A., Paciesas W. S., Poolakkil S., Preece R. D., Racusin J., Roberts O. J., Stanbro M., Veres P., von Kienlin A., Savchenko V., Ferrigno C., Kuulkers E., Bazzano A., Bozzo E., Brandt S., Chenevez J., Courvoisier T. J. -L., Diehl R., Domingo A., Hanlon L., Jourdain E., Laurent P., Lebrun F., Lutovinov A., Martin-Carrillo A., Mereghetti S., Natalucci L., Rodi J., Roques J. -P., Sunyaev R., Ubertini P., Aartsen M. G., Ackermann M., Adams J., Aguilar J. A., Ahlers M., Ahrens M., Al Samarai I., Altmann D., Andeen K., Anderson T., Ansseau I., Anton G., Argelles C., Auffenberg J., Axani S., Bagherpour H., Bai X., Barron J. P., Barwick S. W., Baum V., Bay R., Beatty J. J., Tjus J. Becker, Bernardini E., Besson D. Z., Binder G., Bindig D., Blaufuss E., Blot S., Bohm C., Borner M., Bos F., Bose D., Boser S., Botner O., Bourbeau E., Bourbeau J., Bradascio F., Braun J., Brayeur L., Brenzke M., Bretz H. -P., Bron S., Brostean-Kaiser J., Burgman A., Carver T., Casey J., Casier M., Cheung E., Chirkin D., Christov A., Clark K., Classen L., Coenders S., Collin G. H., Conrad J. M., Cowen D. F., Cross R., Day M., De Andre J. P. A. M., De Clercq C., DeLaunay J. J., Dembinski H., De Ridder S., Desiati P., De Vries K. D., De Wasseige G., De With M., DeYoung T., Diaz-Velez J. C., Di Lorenzo V., Dujmovic H., Dumm J. P., Dunkman M., Dvorak E., Eberhardt B., Ehrhardt T., Eichmann B., Eller P., Evenson P. A., Fahey S., Fazely A. R., Felde J., Filimonov K., Finley C., Flis S., Franckowiak A., Friedman E., Fuchs T., Gaisser T. K., Gallagher J., Gerhardt L., Ghorbani K., Giang W., Glauch T., Glsenkamp T., Goldschmidt A., Gonzalez J. G., Grant D., Griffith Z., Haack C., Hallgren A., Halzen F., Hanson K., Hebecker D., Heereman D., Helbing K., Hellauer R., Hickford S., Hignight J., Hill G. C., Hoffman K. D., Hoffmann R., Hokanson-Fasig B., Hoshina K., Huang F., Huber M., Hultqvist K., Hnnefeld M., In S., Ishihara A., Jacobi E., Japaridze G. S., Jeong M., Jero K., Jones B. J. P., Kalaczynski P., Kang W., Kappes A., Karg T., Karle A., Keivani A., Kelley J. L., Kheirandish A., Kim J., Kim M., Kintscher T., Kiryluk J., Kittler T., Klein S. R., Kohnen G., Koirala R., Kolanoski H., Kopke L., Kopper C., Kopper S., Koschinsky J. P., Koskinen D. J., Kowalski M., Krings K., Kroll M., Krckl G., Kunnen J., Kunwar S., Kurahashi N., Kuwabara T., Kyriacou A., Labare M., Lanfranchi J. L., Larson M. J., Lauber F., Lesiak-Bzdak M., Leuermann M., Liu Q. R., Lu L., Lnemann J., Luszczak W., Madsen J., Maggi G., Mahn K. B. M., Mancina S., Maruyama R., Mase K., Maunu R., McNally F., Meagher K., Medici M., Meier M., Menne T., Merino G., Meures T., Miarecki S., Micallef J., Moment G., Montaruli T., Moore R. W., Moulai M., Nahnhauer R., Nakarmi P., Naumann U., Neer G., Niederhausen H., Nowicki S. C., Nygren D. R., Pollmann A. Obertacke, Olivas A., O'Murchadha A., Palczewski T., Pandya H., Pankova D. V., Peiffer P., Pepper J. A., Heros C. Perez De Los, Pieloth D., Pinat E., Price P. B., Przybylski G. T., Raab C., Rdel L., Rameez M., Rawlins K., Rea I. C., Reimann R., Relethford B., Relich M., Resconi E., Rhode W., Richman M., Robertson S., Rongen M., Rott C., Ruhe T., Ryckbosch D., Rysewyk D., Slzer T., Herrera S. E. Sanchez, Sandrock A., Sandroos J., Santander M., Sarkar S., Sarkar S., Satalecka K., Schlunder P., Schmidt T., Schneider A., Schoenen S., Schoneberg S., Schumacher L., Seckel D., Seunarine S., Soedingrekso J., Soldin D., Song M., Spiczak G. M., Spiering C., Stachurska J., Stamatikos M., Stanev T., Stasik A., Stettner J., Steuer A., Stezelberger T., Stokstad R. G., Stosl A., Strotjohann N. L., Stuttard T., Sullivan G. W., Sutherland M., Taboada I., Tatar J., Tenholt F., Ter-Antonyan S., Terliuk A., Tesic G., Tilav S., Toale P. A., Tobin M. N., Toscano S., Tosi D., Tselengidou M., Tung C. F., Turcati A., Turley C. F., Ty B., Unger E., Usner M., Vandenbroucke J., Van Driessche W., Van Eijndhoven N., Vanheule S., Van Santen J., Vehring M., Vogel E., Vraeghe M., Walck C., Wallace A., Wallraff M., Wandler F. D., Wandkowsky N., Waza A., Weaver C., Weiss M. J., Wendt C., Werthebach J., Whelan B. J., Wiebe K., Wiebusch C. H., Wille L., Williams D. R., Wills L., Wolf M., Wood T. R., Woolsey E., Woschnagg K., Xu D. L., Xu X. W., Xu Y., Yanez J. P., Yodh G., Yoshida S., Yuan T., Zoll M., Balasubramanian A., Mate S., Bhalerao V., Bhattacharya D., Vibhute A., Dewangan G. C., Rao A. R., Vadawale S. V., Svinkin D. S., Hurley K., Aptekar R. L., Frederiks D. D., Golenetskii S. V., Kozlova A. V., Lysenko A. L., Oleynik Ph. P., Tsvetkova A. E., Ulanov M. V., Cline T., Li T. P., Xiong S. L., Zhang S. N., Lu F. J., Song L. M., Cao X. L., Chang Z., Chen G., Chen L., Chen T. X., Chen Y., Chen Y. B., Chen Y. P., Cui W., Cui W. W., Deng J. K., Dong Y. W., Du Y. Y., Fu M. X., Gao G. H., Gao H., Gao M., Ge M. Y., Gu Y. D., Guan J., Guo C. C., Han D. W., Hu W., Huang Y., Huo J., Jia S. M., Jiang L. H., Jiang W. C., Jin J., Jin Y. J., Li B., Li C. K., Li G., Li M. S., Li W., Li X., Li X. B., Li X. F., Li Y. G., Li Z. J., Li Z. W., Liang X. H., Liao J. Y., Liu C. Z., Liu G. Q., Liu H. W., Liu S. Z., Liu X. J., Liu Y., Liu Y. N., Lu B., Lu X. F., Luo T., Ma X., Meng B., Nang Y., Nie J. Y., Ou G., Qu J. L., Sai N., Sun L., Tan Y., Tao L., Tao W. H., Tuo Y. L., Wang G. F., Wang H. Y., Wang J., Wang W. S., Wang Y. S., Wen X. Y., Wu B. B., Wu M., Xiao G. C., Xu H., Xu Y. P., Yan L. L., Yang J. W., Yang S., Yang Y. J., Zhang A. M., Zhang C. L., Zhang C. M., Zhang F., Zhang H. M., Zhang J., Zhang Q., Zhang S., Zhang T., Zhang W., Zhang W. C., Zhang W. Z., Zhang Y., Zhang Y., Zhang Y. F., Zhang Y. J., Zhang Z., Zhang Z. L., Zhao H. S., Zhao J. L., Zhao X. F., Zheng S. J., Zhu Y., Zhu Y. X., Zou C. L., Albert A., Andre M., Anghinolfi M., Ardid M., Aubert J. -J., Aublin J., Avgitas T., Baret B., Barrios-Marti J., Basa S., Belhorma B., Bertin V., Biagi S., Bormuth R., Bourret S., Bouwhuis M. C., Brnzas H., Bruijn R., Brunner J., Busto J., Capone A., Caramete L., Carr J., Celli S., El Moursli R. Cherkaoui, Chiarusi T., Circella M., Coelho J. A. B., Coleiro A., Coniglione R., Costantini H., Coyle P., Creusot A., Diaz A. F., Deschamps A., De Bonis G., Distefano C., Di Palma I., Domi A., Donzaud C., Dornic D., Drouhin D., Eberl T., El Bojaddaini I., El Khayati N., Elsasser D., Enzenhofer A., Ettahiri A., Fassi F., Felis I., Fusco L. A., Gay P., Giordano V., Glotin H., Gregoire T., Ruiz R. Gracia, Graf K., Hallmann S., Van Haren H., Heijboer A. J., Hello Y., Hernndez-Rey J. J., Hossl J., Hofestdt J., Hugon C., Illuminati G., James C. W., De Jong M., Jongen M., Kadler M., Kalekin O., Katz U., Kiessling D., Kouchner A., Kreter M., Kreykenbohm I., Kulikovskiy V., Lachaud C., Lahmann R., LefSvre D., Leonora E., Lotze M., Loucatos S., Marcelin M., Margiotta A., Marinelli A., Martinez-Mora J. A., Mele R., Melis K., Michael T., Migliozzi P., Moussa A., Navas S., Nezri E., Organokov M., Pavalas G. E., Pellegrino C., Perrina C., Piattelli P., Popa V., Pradier T., Quinn L., Racca C., Riccobene G., Sanchez-Losa A., Saldaa M., Salvadori I., Samtleben D. F. E., Sanguineti M., Sapienza P., Sieger C., Spurio M., Stolarczyk Th., Taiuti M., Tayalati Y., Trovato A., Turpin D., Tonnis C., Vallage B., Van Elewyck V., Versari F., Vivolo D., Vizzoca A., Wilms J., Zornoza J. D., Zuniga J., Beardmore A. P., Breeveld A. A., Burrows D. N., Cenko S. B., Cusumano G., D'Al A., De Pasquale M., Emery S. W. K., Evans P. A., Giommi P., Gronwall C., Kennea J. A., Krimm H. A., Kuin N. P. M., Lien A., Marshall F. E., Melandri A., Nousek J. A., Oates S. R., Osborne J. P., Pagani C., Page K. L., Palmer D. M., Perri M., Siegel M. H., Sbarufatti B., Tagliaferri G., Tohuvavohu A., Tavani M., Verrecchia F., Bulgarelli A., Evangelista Y., Pacciani L., Feroci M., Pittori C., Giuliani A., Del Monte E., Donnarumma I., Argan A., Trois A., Ursi A., Cardillo M., Piano G., Longo F., Lucarelli F., Munar-Adrover P., Fuschino F., Labanti C., Marisaldi M., Minervini G., Fioretti V., Parmiggiani N., Gianotti F., Trifoglio M., Di Persio G., Antonelli L. A., Barbiellini G., Caraveo P., Cattaneo P. W., Costa E., Colafrancesco S., D'Amico F., Ferrari A., Morselli A., Paoletti F., Picozza P., Pilia M., Rappoldi A., Soffitta P., Vercellone S., Foley R. J., Coulter D. A., Kilpatrick C. D., Drout M. R., Piro A. L., Shappee B. J., Siebert M. R., Simon J. D., Ulloa N., Kasen D., Madore B. F., Murguia-Berthier A., Pan Y. -C., Prochaska J. X., Ramirez-Ruiz E., Rest A., Rojas-Bravo C., Berger E., Soares-Santos M., Annis J., Alexander K. D., Allam S., Balbinot E., Blanchard P., Brout D., Butler R. E., Chornock R., Cook E. R., Cowperthwaite P., Diehl H. T., Drlica-Wagner A., Drout M. R., Durret F., Eftekhari T., Finley D. A., Fong W., Frieman J. A., Fryer C. L., Garcia-Bellido J., Gruendl R. A., Hartley W., Herner K., Kessler R., Lin H., Lopes P. A. A., Lourenco A. C. C., Margutti R., Marshall J. L., Matheson T., Medina G. E., Metzger B. D., Muoz R. R., Muir J., Nicholl M., Nugent P., Palmese A., Paz-Chinchn F., Quataert E., Sako M., Sauseda M., Schlegel D. J., Scolnic D., Secco L. F., Smith N., Sobreira F., Villar V. A., Vivas A. K., Wester W., Williams P. K. G., Yanny B., Zenteno A., Zhang Y., Abbott T. M. C., Banerji M., Bechtol K., Benoit-Levy A., Bertin E., Brooks D., Buckley-Geer E., Burke D. L., Capozzi D., Rosell A. Carnero, Kind M. Carrasco, Castander F. J., Crocce M., Cunha C. E., D'Andrea C. B., Da Costa L. N., Davis C., Depoy D. L., Desai S., Dietrich J. P., Eifler T. F., Fernandez E., Flaugher B., Fosalba P., Gaztanaga E., Gerdes D. W., Giannantonio T., Goldstein D. A., Gruen D., Gschwend J., Gutierrez G., Honscheid K., James D. J., Jeltema T., Johnson M. W. G., Johnson M. D., Kent S., Krause E., Kron R., Kuehn K., Lahav O., Lima M., Maia M. A. G., March M., Martini P., McMahon R. G., Menanteau F., Miller C. J., Miquel R., Mohr J. J., Nichol R. C., Ogando R. L. C., Plazas A. A., Romer A. K., Roodman A., Rykoff E. S., Sanchez E., Scarpine V., Schindler R., Schubnell M., Sevilla-Noarbe I., Sheldon E., Smith M., Smith R. C., Stebbins A., Suchyta E., Swanson M. E. C., Tarle G., Thomas R. C., Troxel M. A., Tucker D. L., Vikram V., Walker A. R., Wechsler R. H., Weller J., Carlin J. L., Gill M. S. S., Li T. S., Marriner J., Neilsen E., Haislip J. B., Kouprianov V. V., Reichart D. E., Sand D. J., Tartaglia L., Valenti S., Yang S., Benetti S., Brocato E., Campana S., Cappellaro E., Covino S., D'Avanzo P., D'Elia V., Getman F., Ghirlanda G., Ghisellini G., Limatola L., Nicastro L., Palazzi E., Pian E., Piranomonte S., Possenti A., Rossi A., Salafia O. S., Tomasella L., Amati L., Antonelli L. A., Bernardini M. G., Bufano F., Capaccioli M., Casella P., Dadina M., De Cesare G., Di Paola A., Giuffrida G., Giunta A., Israel G. L., Lisi M., Maiorano E., Mapelli M., Masetti N., Pescalli A., Pulone L., Salvaterra R., Schipani P., Spera M., Stamerra A., Stella L., Testa V., Turatto M., Vergani D., Aresu G., Bachetti M., Buffa F., Burgay M., Buttu M., Caria T., Carretti E., Casasola V., Castangia P., Carboni G., Casu S., Concu R., Corongiu A., Deiana G. L., Egron E., Fara A., Gaudiomonte F., Gusai V., Ladu A., Loru S., Leurini S., Marongiu L., Melis A., Melis G., Migoni Carlo, Milia Sabrina, Navarrini Alessandro, Orlati A., Ortu P., Palmas S., Pellizzoni A., Perrodin D., Pisanu T., Poppi S., Righini S., Saba A., Serra G., Serrau M., Stagni M., Surcis G., Vacca V., Vargiu G. P., Hunt L. K., Jin Z. P., Klose S., Kouveliotou C., Mazzali P. A., Moller P., Nava L., Piran T., Selsing J., Vergani S. D., Wiersema K., Toma K., Higgins A. B., Mundell C. G., Alighieri S. Di Serego, Gtz D., Gao W., Gomboc A., Kaper L., Kobayashi S., Kopac D., Mao J., Starling R. L. C., Steele I., Van der Horst A. J., Acero F., Atwood W. B., Baldini L., Barbiellini G., Bastieri D., Berenji B., Bellazzini R., Bissaldi E., Blandford R. D., Bloom E. D., Bonino R., Bottacini E., Bregeon J., Buehler R., Buson S., Cameron R. A., Caputo R., Caraveo P. A., Cavazzuti E., Chekhtman A., Cheung C. C., Chiang J., Ciprini S., Cohen-Tanugi J., Cominsky L. R., Costantin D., Cuoco A., D'Ammando F., De Palma F., Digel S. W., Di Lalla N., Di Mauro M., Di Venere L., Dubois R., Fegan S. J., Focke W. B., Franckowiak A., Fukazawa Y., Funk S., Fusco P., Gargano F., Gasparrini D., Giglietto N., Giordano F., Giroletti M., Glanzman T., Green D., Grondin M. -H., Guillemot L., Guiriec S., Harding A. K., Horan D., Jhannesson G., Kamae T., Kensei S., Kuss M., La Mura G., Latronico L., Lemoine-Goumard M., Longo F., Loparco F., Lovellette M. N., Lubrano P., Magill J. D., Maldera S., Manfreda A., Mazziotta M. N., McEnery J. E., Meyer M., Michelson P. F., Mirabal N., Monzani M. E., Morselli A., Moskalenko I. V., Negro M., Nuss E., Ojha R., Omodei N., Orienti M., Orlando E., Palatiello M., Paliya V. S., Paneque D., Pesce-Rollins M., Piron F., Porter T. A., Principe G., Rain S., Rando R., Razzano M., Razzaque S., Reimer A., Reimer O., Reposeur T., Rochester L. S., Parkinson P. M. Saz, Sgro C., Siskind E. J., Spada F., Spandre G., Suson D. J., Takahashi M., Tanaka Y., Thayer J. G., Thayer J. B., Thompson D. J., Tibaldo L., Torres D. F., Torresi E., Troja E., Venters T. M., Vianello G., Zaharijas G., Allison J., Bannister K. W., Dobie D., Kaplan D. L., Lenc E., Lynch C., Murphy T., Sadler E. M., Hotan A., James C. W., Oslowski S., Raja W., Shannon R. M., Whiting M., Arcavi I., Howell D. A., McCully C., Hosseinzadeh G., Hiramatsu D., Poznanski D., Barnes J., Zaltzman M., Vasylyev S., Maoz D., Cooke J., Bailes M., Wolf C., Deller A. T., Lidman C., Wang L., Gendre B., Andreoni I., Ackley K., Pritchard T. A., Bessell M. S., Chang S. -W., Moller A., Onken C. A., Scalzo R. A., Ridden-Harper R., Sharp R. G., Tucker B. E., Farrell T. J., Elmer E., Johnston S., Krishnan V. Venkatraman, Keane E. F., Green J. A., Jameson A., Hu L., Ma B., Sun T., Wu X., Wang X., Shang Z., Hu Y., Ashley M. C. B., Yuan X., Li X., Tao C., Zhu Z., Zhang H., Suntzeff N. B., Zhou J., Yang J., Orange B., Morris D., Cucchiara A., Giblin T., Klotz A., Staff J., Thierry P., Schmidt B. P., Tanvir N. R., Levan A. J., Cano Z., De Ugarte-Postigo A., Evans P., Gonzalez-Fernandez C., Greiner J., Hjorth J., Irwin M., Kruhler T., Mandel I., Milvang-Jensen B., O'Brien P., Rol E., Rosetti S., Rosswog S., Rowlinson A., Steeghs D. T. H., Thene C. C., Ulaczyk K., Watson D., Bruun S. H., Cutter R., Jaimes R. Figuera, Fujii Y. I., Fruchter A. S., Gompertz B., Jakobsson P., Hodosan G., Jergensen U. G., Kangas T., Kann D. A., Rabus M., Schroder S. L., Stanway E. R., Wijers R. A. M. J., Lipunov V. M., Gorbovskoy E. S., Kornilov V. G., Tyurina N. V., Balanutsa P. V., Kuznetsov A. S., Vlasenko D. M., Podesta R. C., Lopez C., Podesta F., Levato H. O., Saffe C., Mallamaci C. C., Budnev N. M., Gress O. A., Kuvshinov D. A., Gorbunov I. A., Vladimirov V. V., Zimnukhov D. S., Gabovich A. V., Yurkov V. V., Sergienko Yu. P., Rebolo R., Serra-Ricart M., Tlatov A. G., Ishmuhametova Yu. V., Abe F., Aoki K., Aoki W., Asakura Y., Baar S., Barway S., Bond I. A., Doi M., Finet F., Fujiyoshi T., Furusawa H., Honda S., Itoh R., Kanda N., Kawabata K. S., Kawabata M., Kim J. H., Koshida S., Kuroda D., Lee C. -H., Liu W., Matsubayashi K., Miyazaki S., Morihana K., Morokuma T., Motohara K., Murata K. L., Nagai H., Nagashima H., Nagayama T., Nakaoka T., Nakata F., Ohsawa R., Ohshima T., Ohta K., Okita H., Saito T., Saito Y., Sako S., Sekiguchi Y., Sumi T., Tajitsu A., Takahashi J., Takayama M., Tamura Y., Tanaka I., Tanaka M., Terai T., Tominaga N., Tristram P. J., Uemura M., Utsumi Y., Yamaguchi M. S., Yasuda N., Yoshida M., Zenko T., Adams S. M., Allison J. R., Anupama G. C., Bally J., Barway S., Bellm E., Blagorodnova N., Cannella C., Chandra P., Chatterjee D., Clarke T. E., Cobb B. E., Cook D. O., Copperwheat C., De K., Emery S. W. K., Evans P. A., Feindt U., Foster K., Fox O. D., Frail D. A., Fremling C., Frohmaier C., Garcia J. A., Ghosh S., Giacintucci S., Goobar A., Gottlieb O., Grefenstette B. W., Hallinan G., Harrison F., Heida M., Helou G., Ho A. Y. Q., Horesh A., Hotokezaka K., Ip W. -H., Itoh R., Jacobs Bob, Jencson J. E., Kasen D., Kasliwal M. M., Kassim N. E., Kim H., Kiran B. S., Kuin N. P. M., Kulkarni S. R., Kupfer T., Lau R. M., Madsen K., Mazzali P. A., Miller A. A., Miyasaka H., Mooley K., Myers S. T., Nakar E., Ngeow C. -C., Nugent P., Ofek E. O., Palliyaguru N., Pavana M., Perley D. A., Peters W. M., Pike S., Piran T., Qi H., Quimby R. M., Rana J., Rosswog S., Rusu F., Sadler E. M., Van Sistine A., Sollerman J., Xu Y., Yan L., Yatsu Y., Yu P. -C., Zhang C., Zhao W., Chambers K. C., Huber M. E., Schultz A. S. B., Bulger J., Flewelling H., Magnier E. A., Lowe T. B., Wainscoat R. J., Waters C., Willman M., Ebisawa K., Hanyu C., Harita S., Hashimoto T., Hidaka K., Hori T., Ishikawa M., Isobe N., Iwakiri W., Kawai H., Kawai N., Kawamuro T., Kawase T., Kitaoka Y., Makishima K., Matsuoka M., Mihara T., Morita T., Morita K., Nakahira S., Nakajima M., Nakamura Y., Negoro H., Oda S., Sakamaki A., Sasaki R., Serino M., Shidatsu M., Shimomukai R., Sugawara Y., Sugita S., Sugizaki M., Tachibana Y., Takao Y., Tanimoto A., Tomida H., Tsuboi Y., Tsunemi H., Ueda Y., Ueno S., Yamada S., Yamaoka K., Yamauchi M., Yatabe F., Yoneyama T., Yoshii T., Coward D. M., Crisp H., Macpherson D., Andreoni I., Laugier R., Noysena K., Klotz A., Gendre B., Thierry P., Turpin D., Im M., Choi C., Kim J., Yoon Y., Lim G., Lee S. -K., Lee C. -U., Kim S. -L., Ko S. -W., Joe J., Kwon M. -K., Kim P. -J., Lim S. -K., Choi J. -S., Fynbo J. P. U., Malesani D., Xu D., Smartt S. J., Jerkstrand A., Kankare E., Sim S. A., Fraser M., Inserra C., Maguire K., Leloudas G., Magee M., Shingles L. J., Smith K. W., Young D. R., Kotak R., Gal-Yam A., Lyman J. D., Homan D. S., Agliozzo C., Anderson J. P., Angus C. R., Ashall C., Barbarino C., Bauer F. E., Berton M., Botticella M. T., Bulla M., Cannizzaro G., Cartier R., Cikota A., Clark P., De Cia A., Della Valle M., Dennefeld M., Dessart L., Dimitriadis G., Elias-Rosa N., Firth R. E., Flors A., Frohmaier C., Galbany L., Gonzlez-Gaitn S., Gromadzki M., Gutierrez C. P., Hamanowicz A., Harmanen J., Heintz K. E., Hernandez M. -S., Hodgkin S. T., Hook I. M., Izzo L., James P. A., Jonker P. G., Kerzendorf W. E., Kostrzewa-Rutkowska Z., Kromer M., Kuncarayakti H., Lawrence A., Manulis I., Mattila S., McBrien O., Mller A., Nordin J., O'Neill D., Onori F., Palmerio J. T., Pastorello A., Patat F., Pignata G., Podsiadlowski P., Razza A., Reynolds T., Roy R., Ruiter A. J., Rybicki K. A., Salmon L., Pumo M. L., Prentice S. J., Seitenzahl I. R., Smith M., Sollerman J., Sullivan M., Szegedi H., Taddia F., Taubenberger S., Terreran G., Van Soelen B., Vos J., Walton N. A., Wright D. E., Wyrzykowski L., Yaron O., Chen T. -W., Krhler T., Schady P., Wiseman P., Greiner J., Rau A., Schweyer T., Klose S., Guelbenzu A. Nicuesa, Palliyaguru N. T., Shara M. M., Williams T., Vaisanen P., Potter S. B., Colmenero E. Romero, Crawford S., Buckley D. A. H., Mao J., Diaz M. C., Macri L. M., Lambas D. Garcia, de Oliveira C. Mendes, Castellon J. L. Nilo, Ribeiro T., Sanchez B., Schoenell W., Abramo L. R., Akras S., Alcaniz J. S., Artola R., Beroiz M., Bonoli S., Cabral J., Camuccio R., Chavushyan V., Coelho P., Colazo C., Costa-Duarte M. V., Larenas H. Cuevas, Romero M. Dominguez, Dultzin D., Fernandez D., Garcia J., Girardini C., Goncalves D. R., Goncalves T. S., Gurovich S., Jimenez-Teja Y., Kanaan A., Lares M., de Oliveira R. Lopes, Lopez-Cruz O., Melia R., Molino A., Padilla N., Penuela T., Placco V. M., Quinones C., Rivera A. Ramirez, Renzi V., Riguccini L., Rios-Lopez E., Rodriguez H., Sampedro L., Schneiter M., Sodre L., Starck M., Torres-Flores S., Tornatore M., Zadrozny A., Castro-Tirado A. J., Tello J. C., Hu Y. -D., Zhang B. -B., Cunniffe R., Castellon A., Hiriart D., Caballero-Garcia M. D., Jelinek M., Kubanek P., Del Pulgar C. Perez, Park I. H., Jeong S., Ceron J. M. Castro, Pandey S. B., Yock P. C., Querel R., Fan Y., Wang C., Beardsley A., Brown I. S., Crosse B., Emrich D., Franzen T., Gaensler B. M., Horsley L., Johnston-Hollitt M., Kenney D., Morales M. F., Pallot D., Sokolowski M., Steele K., Tingay S. J., Trott C. M., Walker M., Wayth R., Williams A., Wu C., Yoshida A., Sakamoto T., Kawakubo Y., Yamaoka K., Takahashi I., Asaoka Y., Ozawa S., Torii S., Shimizu Y., Tamura T., Ishizaki W., Cherry M. L., Ricciarini S., Penacchioni A. V., Marrocchesi P. S., Pozanenko A. S., Volnova A. A., Mazaeva E. D., Minaev P. Yu., Krugov M. A., Kusakin A. V., Reva I. V., Moskvitin A. S., Rumyantsev V. V., Inasaridze R., Klunko E. V., Tungalag N., Schmalz S. E., Burhonov O., Abdalla H., Abramowski A., Aharonian F., Benkhali F. Ait, Angner E. O., Arakawa M., Arrieta M., Aubert P., Backes M., Balzer A., Barnard M., Becherini Y., Tjus J. Becker, Berge D., Bernhard S., Bernrhr K., Blackwell R., Bottcher M., Boisson C., Bolmont J., Bonnefoy S., Bordas P., Bregeon J., Brun F., Brun P., Bryan M., Bchele M., Bulik T., Capasso M., Caroff S., Carosi A., Casanova S., Cerruti M., Chakraborty N., Chaves R. C. G., Chen A., Chevalier J., Colafrancesco S., Condon B., Conrad J., Davids I. D., Decock J., Deil C., Devin J., Dewilt P., Dirson L., Djannati-Atao A., Donath A., Drury L. O'C., Dutson K., Dyks J., Edwards T., Egberts K., Emery G., Ernenwein J. -P., Eschbach S., Farnier C., Fegan S., Fernandes M. V., Fiasson A., Fontaine G., Funk S., Fssling M., Gabici S., Gallant Y. A., Garrigoux T., Gate F., Giavitto G., Giebels B., Glawion D., Glicenstein J. F., Gottschall D., Grondin M. -H., Hahn J., Haupt M., Hawkes J., Heinzelmann G., Henri G., Hermann G., Hinton J. A., Hofmann W., Hoischen C., Holch T. L., Holler M., Horns D., Ivascenko A., Iwasaki H., Jacholkowska A., Jamrozy M., Jankowsky D., Jankowsky F., Jingo M., Jouvin L., Jung-Richardt I., Kastendieck M. A., Katarzynski K., Katsuragawa M., Khangulyan D., Khelifi B., King J., Klepser S., Klochkov D., Kluzniak W., Komin Nu., Kosack K., Krakau S., Kraus M., Krger P. P., Laffon H., Lamanna G., Lau J., Lees J. -P., Lefaucheur J., Lemiere A., Lemoine-Goumard M., Lenain J. -P., Leser E., Lohse T., Lorentz M., Liu R., Lypova I., Malyshev D., Marandon V., Marcowith A., Mariaud C., Marx R., Maurin G., Maxted N., Mayer M., Meintjes P. J., Meyer M., Mitchell A. M. W., Moderski R., Mohamed M., Mohrmann L., Mor K., Moulin E., Murach T., Nakashima S., De Naurois M., Ndiyavala H., Niederwanger F., Niemiec J., Oakes L., O'Brien P., Odaka H., Ohm S., Ostrowski M., Oya I., Padovani M., Panter M., Parsons R. D., Pekeur N. W., Pelletier G., Perennes C., Petrucci P. -O., Peyaud B., Piel Q., Pita S., Poireau V., Poon H., Prokhorov D., Prokoph H., Phlhofer G., Punch M., Quirrenbach A., Raab S., Rauth R., Reimer A., Reimer O., Renaud M., Reyes R. De Los, Rieger F., Rinchiuso L., Romoli C., Rowell G., Rudak B., Rulten C. B., Sahakian V., Saito S., Sanchez D. A., Santangelo A., Sasaki M., Schlickeiser R., Schssler F., Schulz A., Schwanke U., Schwemmer S., Seglar-Arroyo M., Settimo M., Seyffert A. S., Shafi N., Shilon I., Shiningayamwe K., Simoni R., Sol H., Spanier F., Spir-Jacob M., Stawarz L., Steenkamp R., Stegmann C., Steppa C., Sushch I., Takahashi T., Tavernet J. -P., Tavernier T., Taylor A. M., Terrier R., Tibaldo L., Tiziani D., Tluczykont M., Trichard C., Tsirou M., Tsuji N., Tuffs R., Uchiyama Y., Van der Walt D. J., Van Eldik C., Van Rensburg C., Van Soelen B., Vasileiadis G., Veh J., Venter C., Viana A., Vincent P., Vink J., Voisin F., Volk H. J., Vuillaume T., Wadiasingh Z., Wagner S. J., Wagner P., Wagner R. M., White R., Wierzcholska A., Willmann P., WRnlein A., Wouters D., Yang R., Zaborov D., Zacharias M., Zanin R., Zdziarski A. A., Zech A., Zefi F., Ziegler A., Zorn J., Zywucka N., Fender R. P., Broderick J. W., Rowlinson A., Wijers R. A. M. J., Stewart A. J., Ter Veen S., Shulevski A., Kavic M., Simonetti J. H., League C., Tsai J., Obenberger K. S., Nathaniel K., Taylor G. B., Dowell J. D., Liebling S. L., Estes J. A., Lippert M., Sharma I., Vincent P., Farella B., Abeysekara A. U., Albert A., Alfaro R., Alvarez C., Arceo R., Arteaga-Velzquez J. C., Rojas D. Avila, Solares H. A. Ayala, Barber A. S., Gonzalez J. Becerra, Becerril A., Belmont-Moreno E., BenZvi S. Y., Berley D., Bernal A., Braun J., Brisbois C., Caballero-Mora K. S., Capistrn T., Carramiana A., Casanova S., Castillo M., Cotti U., Cotzomi J., De Leon S. Coutio, De Leon C., De la Fuente E., Hernandez R. Diaz, Dichiara S., Dingus B. L., DuVernois M. A., Diaz-Velez J. C., Ellsworth R. W., Engel K., Enriquez-Rivera O., Fiorino D. W., Fleischhack H., Fraija N., Garcia-Gonzlez J. A., Garfias F., Gerhardt M., Muoz A. Gonzolez, Gonzlez M. M., Goodman J. A., Hampel-Arias Z., Harding J. P., Hernandez S., Hernandez-Almada A., Hona B., Hntemeyer P., Iriarte A., Jardin-Blicq A., Joshi V., Kaufmann S., Kieda D., Lara A., Lauer R. J., Lennarz D., Vargas H. Leon, Linnemann J. T., Longinotti A. L., Raya G. Luis, Luna-Garcia R., Lopez-Coto R., Malone K., Marinelli S. S., Martinez O., Martinez-Castellanos I., Martinez-Castro J., Martinez-Huerta H., Matthews J. A., Miranda-Romagnoli P., Moreno E., Mostaf M., Nellen L., Newbold M., Nisa M. U., Noriega-Papaqui R., Pelayo R., Pretz J., Perez-Perez E. G., Ren Z., Rho C. D., Riviere C., Rosa-Gonzlez D., Rosenberg M., Ruiz-Velasco E., Salazar H., Greus F. Salesa, Sandoval A., Schneider M., Schoorlemmer H., Sinnis G., Smith A. J., Springer R. W., Surajbali P., Tibolla O., Tollefson K., Torres I., Ukwatta T. N., Weisgarber T., Westerhoff S., Wisher I. G., Wood J., Yapici T., Yodh G. B., Younk P. W., Zhou H., Alvarez J. D., Aab A., Abreu P., Aglietta M., Albuquerque I. F. M., Albury J. M., Allekotte I., Almela A., Castillo J. Alvarez, Alvarez-Muiz J., Anastasi G. A., Anchordoqui L., Andrada B., Andringa S., Aramo C., Arsene N., Asorey H., Assis P., Avila G., Badescu A. M., Balaceanu A., Barbato F., Luz R. J. Barreira, Becker K. H., Bellido J. A., Berat C., Bertaina M. E., Bertou X., Biermann P. L., Biteau J., Blaess S. G., Blanco A., Blazek J., Bleve C., Bohacova M., Bonifazi C., Borodai N., Botti A. M., Brack J., Brancus I., Bretz T., Bridgeman A., Briechle F. L., Buchholz P., Bueno A., Buitink S., Buscemi M., Caballero-Mora K. S., Caccianiga L., Cancio A., Canfora F., Caruso R., Castellina A., Catalani F., Cataldi G., Cazon L., Chavez A. G., Chinellato J. A., Chudoba J., Clay R. W., Cerutti A. C. Cobos, Colalillo R., Coleman A., Collica L., Coluccia M. R., Conceicao R., Consolati G., Contreras F., Cooper M. J., Coutu S., Covault C. E., Cronin J., D'Amico S., Daniel B., Dasso S., Daumiller K., Dawson B. R., Day J. A., De Almeida R. M., De Jong S. J., De Mauro G., Neto J. R. T. De Mello, De Mitri I., De Oliveira J., De Souza V., Debatin J., Deligny O., Castro M. L. Diaz, Diogo F., Dobrigkeit C., D'Olivo J. C., Dorosti Q., Dos Anjos R. C., Dova M. T., Dundovic A., Ebr J., Engel R., Erdmann M., Erfani M., Escobar C. O., Espadanal J., Etchegoyen A., Falcke H., Farmer J., Farrar G., Fauth A. C., Fazzini N., Feldbusch F., Fenu F., Fick B., Figueira J. M., Filipcic A., Freire M. M., Fujii T., Fuster A., Gaior R., Garcia B., Gate F., Gemmeke H., Gherghel-Lascu A., Ghia P. L., Giaccari U., Giammarchi M., Giller M., Glas D., Glaser C., Golup G., Berisso M. Gomez, Vitale P. F. Gomez, Gonzlez N., Gorgi A., Gottowik M., Grillo A. F., Grubb T. D., Guarino F., Guedes G. P., Halliday R., Hampel M. R., Hansen P., Harari D., Harrison T. A., Harvey V. M., Haungs A., Hebbeker T., Heck D., Heimann P., Herve A. E., Hill G. C., Hojvat C., Holt E. W., Homola P., Horandel J. R., Horvath P., Hrabovsky M., Huege T., Hulsman J., Insolia A., Isar P. G., Jandt I., Johnsen J. A., Josebachuili M., Jurysek J., Kaapa A., Kampert K. H., Keilhauer B., Kemmerich N., Kemp J., Kieckhafer R. M., Klages H. O., Kleifges M., Kleinfeller J., Krause R., Krohm N., Kuempel D., Mezek G. Kukec, Kunka N., Awad A. Kuotb, Lago B. L., LaHurd D., Lang R. G., Lauscher M., Legumina R., De Oliveira M. A. Leigui, Letessier-Selvon A., Lhenry-Yvon I., Link K., Lo Presti D., Lopes L., Lopez R., Casado A. Lopez, Lorek R., Luce Q., Lucero A., Malacari M., Mallamaci M., Mandat D., Mantsch P., Mariazzi A. G., Maris I. C., Marsella G., Martello D., Martinez H., Bravo O. Martinez, Meza J. J. Masias, Mathes H. J., Mathys S., Matthews J., Matthiae G., Mayotte E., Mazur P. O., Medina C., Medina-Tanco G., Melo D., Menshikov A., Merenda K. -D., Michal S., Micheletti M. I., Middendorf L., Miramonti L., Mitrica B., Mockler D., Mollerach S., Montanet F., Morello C., Morlino G., Mueller A. L., Mueller G., Mueller M. A., Mueller S., Mussa R., Naranjo I., Nguyen P. H., Niculescu-Oglinzanu M., Niechciol M., Niemietz L., Niggemann T., Nitz D., Nosek D., Novotny V., Nozka L., Nunez L. A., Oikonomou F., Olinto A., Palatka M., Pallotta J., Papenbreer P., Parente G., Parra A., Paul T., Pech M., Pedreira F., Kala J. P., Pea-Rodriguez J., Pereira L. A. S., Perlin M., Perrone L., Peters C., Petrera S., Phuntsok J., Pierog T., Pimenta M., Pirronello V., Platino M., Plum M., Poh J., Porowski C., Prado R. R., Privitera P., Prouza M., Quel E. J., Querchfeld S., Quinn S., Ramos-Pollan R., Rautenberg J., Ravignani D., Ridky J., Riehn F., Risse M., Ristori P., Rizi V., De Carvalho W. Rodrigues, Fernandez G. Rodriguez, Rojo J. Rodriguez, Roncoroni M. J., Roth M., Roulet E., Rovero A. C., Ruehl P., Saffi S. J., Saftoiu A., Salamida F., Salazar H., Saleh A., Salina G., Sanchez F., Sanchez-Lucas P., Santos E. M., Santos E., Sarazin F., Sarmento R., Sarmiento-Cano C., Sato R., Schauer M., Scherini V., Schieler H., Schimp M., Schmidt D., Scholten O., Schovnek P., Schroder F. G., Schroder S., Schulz A., Schumacher J., Sciutto S. J., Segreto A., Shadkam A., Shellard R. C., Sigl G., Silli G., Smida R., Snow G. R., Sommers P., Sonntag S., Soriano J. F., Squartini R., Stanca D., Stanic S., Stasielak J., Stassi P., Stolpovskiy M., Strafella F., Streich A., Suarez F., Suarez-Duran M., Sudholz T., Suomijarvi T., Supanitsky A. D., Supik J., Swain J., Szadkowski Z., Taboada A., Taborda O. A., Timmermans C., Peixoto C. J. Todero, Tomankova L., Tome B., Elipe G. Torralba, Travnicek P., Trini M., Tueros M., Ulrich R., Unger M., Urban M., Galicia J. F. Valdes, Valio I., Valore L., Van Aar G., Van Bodegom P., Van den Berg A. M., Van Vliet A., Varela E., Cardenas B. Vargas, Vazquez R. A., Veberic D., Ventura C., Quispe I. D. Vergara, Verzi V., Vicha J., Villaseor L., Vorobiov S., Wahlberg H., Wainberg O., Walz D., Watson A. A., Weber M., Weindl A., Wiedenski M., Wiencke L., Wilczynski H., Wirtz M., Wittkowski D., Wundheiler B., Yang L., Yushkov A., Zas E., Zavrtanik D., Zavrtanik M., Zepeda A., Zimmermann B., Ziolkowski M., Zong Z., Zuccarello F., Kim S., Schulze S., Bauer F. E., Corral-Santana J. M., De Gregorio-Monsalvo I., Gonzlez-Lopez J., Hartmann D. H., Ishwara-Chandra C. H., Martin S., Mehner A., Misra K., Michalowski M. J., Resmi L., Paragi Z., Agudo I., An T., Beswick R., Casadio C., Frey S., Jonker P., Kettenis M., Marcote B., Moldon J., Szomoru A., Langevelde H. J., Yang J., Cwiek A., Cwiok M., Czyrkowski H., Dabrowski R., Kasprowicz G., Mankiewicz L., Nawrocki K., Opiela R., Piotrowski L. W., Wrochna G., Zaremba M., Zarnecki A. F., Haggard D., Nynka M., Ruan J. J., Bland P. A., Booler T., Devillepoix H. A. R., De Gois J. S., Hancock P. J., Howie R. M., Paxman J., Sansom E. K., Towner M. C., Tonry J., Coughlin M., Stubbs C. W., Denneau L., Heinze A., Stalder B., Weiland H., Eatough R. P., Kramer M., Kraus A., Troja E., Piro L., Gonzlez J. Becerra, Butler N. R., Fox O. D., Khandrika H. G., Kutyrev A., Lee W. H., Ricci R., Ryan R. E. Jr., Sanchez-Ramirez R., Veilleux S., Watson A. M., Wieringa M. H., Burgess J. M., Van Eerten H., Fontes C. J., Fryer C. L., Korobkin O., Wollaeger R. T., Camilo F., Foley A. R., Goedhart S., Makhathini S., Oozeer N., Smirnov O. M., Fender R. P., Woudt P. A.

ASTROPHYSICAL JOURNAL LETTERS 848 巻 ( 2 ) 頁： L12 - L12 2017年10月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal Letters

On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40-+88 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 M☉. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ∼10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta.

DOI： 10.3847/2041-8213/aa91c9

その他リンク： https://iopscience.iop.org/article/10.3847/2041-8213/aa91c9/pdf

Blind Millimeter Line Emitter Search using ALMA Data Toward Gravitational Lensing Clusters 査読有り

Yamaguchi Yuki, Kohno Kotaro, Tamura Yoichi, Oguri Masamune, Ezawa Hajime, Hayatsu Natsuki H., Kitayama Tetsu, Matsuda Yuichi, Matsuo Hiroshi, Oshima Tai, Ota Naomi, Izumi Takuma, Umehata Hideki

ASTROPHYSICAL JOURNAL 845 巻 ( 2 ) 頁： 108 - 108 2017年8月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We present the results of a blind millimeter line emitter search using ALMA Band 6 data with a single-frequency tuning toward four gravitational lensing clusters (RXJ1347.5-1145, Abell S0592, MACS J0416.1-2403, and Abell 2744). We construct 3D signal-to-noise ratio (S/N) cubes with 60 and 100 MHz binning, and search for millimeter line emitters. We do not detect any line emitters with a peak S/N > 5, although we do find a line emitter candidate with a peak S/N ≃ 4.5. These results provide upper limits to the CO(3-2), CO(4-3), CO(5-4), and [C ii] luminosity functions at z ≃ 0.3, 0.7, 1.2, and 6, respectively. Because of the magnification effect of gravitational lensing clusters, the new data provide the first constraints on the CO and [C ii] luminosity functions at unprecedentedly low luminosity levels, i.e., down to ≲10-3 - 10-1 Mpc-3 dex-1 at L'CO ∼ 108-1010 K km s-1 pc2 and ≲10-3-10-2 Mpc-3 dex-1 at L[CII] ∼ 108-1010 L⊙, respectively. Although the constraints to date are not yet stringent, we find that the evolution of the CO and [C ii] luminosity functions are broadly consistent with the predictions of semi-analytical models. This study demonstrates that the wide observations with a single-frequency tuning toward gravitational lensing clusters are promising for constraining the CO and [C ii] luminosity functions.

DOI： 10.3847/1538-4357/aa80e0

Properties of molecular gas in galaxies in the early and mid stages of interaction. II. Molecular gas fraction 査読有り

Kaneko Hiroyuki, Kuno Nario, Iono Daisuke, Tamura Yoichi, Tosaki Tomoka, Nakanishi Kouichiro, Sawada Tsuyoshi

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 69 巻 ( 4 ) 2017年8月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

We have investigated properties of the interstellar medium in interacting galaxies in early and mid stages using mapping data of 12CO(J = 1–0) and H I. Assuming the standard CO–H2 conversion factor, we found no difference in molecular gas mass, atomic gas mass, and total gas mass (the sum of atomic and molecular gas mass) between interacting galaxies and isolated galaxies. However, interacting galaxies have a higher global molecular gas fraction fmolglobal (the ratio of molecular gas mass to total gas mass averaged over a whole galaxy) at 0.71 ± 0.15 than isolated galaxies (0.52 ± 0.18). The distribution of the local molecular gas fraction fmol, the ratio of the surface density of molecular gas to that of the total gas, is different from the distribution in typical isolated galaxies. By a pixel-to-pixel comparison, isolated spiral galaxies show a gradual increase in fmol along the surface density of total gas until it is saturated at 1.0, while interacting galaxies show no clear relation. We performed pixel-to-pixel theoretical model fits by varying metallicity and external pressure. According to the model fitting, external pressure can explain the trend of fmol in the interacting galaxies. Assuming half of the standard CO–H2 conversion factor for interacting galaxies, the results of pixel-to-pixel theoretical model fitting get worse than adopting the standard conversion factor, although fmolglobal of interacting galaxies (0.62 ± 0.17) becomes the same as in isolated galaxies. We conclude that external pressure occurs due to the shock prevailing over a whole galaxy or due to collisions between giant molecular clouds even in the early stage of the interaction. The external pressure accelerates an efficient transition from atomic gas to molecular gas. Regarding the chemical timescale, high fmol can be achieved at the very early stage of interaction even if the shock induced by the collision of galaxies ionizes interstellar gas.

DOI： 10.1093/pasj/psx041

ALMA Observations of the Gravitational Lens SDP.9 査読有り

Wong Kenneth C., Ishida Tsuyoshi, Tamura Yoichi, Suyu Sherry H., Oguri Masamune, Matsushita Satoki

ASTROPHYSICAL JOURNAL LETTERS 843 巻 ( 2 ) 2017年7月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal Letters

We present long-baseline ALMA observations of the strong gravitational lens H-ATLAS J090740.0-004200 (SDP.9), which consists of an elliptical galaxy at zL = 0.6129 lensing a background submillimeter galaxy into two extended arcs. The data include Band 6 continuum observations, as well as CO J = 6-5 molecular line observations, from which we measure an updated source redshift of zS = 1.5747. The image morphology in the ALMA data is different from that of the Hubble Space Telescope (HST) data, indicating a spatial offset between the stellar, gas, and dust component of the source galaxy. We model the lens as an elliptical power law density profile with external shear using a combination of archival HST data and conjugate points identified in the ALMA data. Our best model has an Einstein radius of θE = 0.66 ± 0.01 and a slightly steeper than isothermal mass profile slope. We search for the central image of the lens, which can be used constrain the inner mass distribution of the lens galaxy including the central supermassive black hole, but do not detect it in the integrated CO image at a 3σ rms level of 0.0471 Jy km s-1.

DOI： 10.3847/2041-8213/aa7d4a

A Radio-to-mm Census of Star-forming Galaxies in Protocluster 4C23.56 at Z=2.5: Gas Mass and Its Fraction Revealed with ALMA 査読有り

Lee Minju M., Tanaka Ichi, Kawabe Ryohei, Kohno Kotaro, Kodama Tadayuki, Kajisawa Masaru, Yun Min S., Nakanishi Kouichiro, Iono Daisuke, Tamura Yoichi, Hatsukade Bunyo, Umehata Hideki, Saito Toshiki, Izumi Takuma, Aretxaga Itziar, Tadaki Ken-ichi, Zeballos Milagros, Ikarashi Soh, Wilson Grant W., Hughes David H., Ivison R. J.

ASTROPHYSICAL JOURNAL 842 巻 ( 1 ) 頁： 55 - 55 2017年6月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal

We investigate gas contents of star-forming galaxies associated with protocluster 4C23.56 at z = 2.49 by using the redshifted CO (3-2) and 1.1 mm dust continuum with the Atacama Large Millimeter/submillimeter Array. The observations unveil seven CO detections out of 22 targeted Hα emitters (HAEs) and four out of 19 in 1.1 mm dust continuum. They have high stellar mass (M∗ > 4 × 1010 Mo) and exhibit a specific star-formation rate typical of main-sequence star-forming galaxies at z ∼ 2.5. Different gas-mass estimators from CO (3-2) and 1.1 mm yield consistent values for simultaneous detections. The gas mass (Mgas) and gas fraction (fgas) are comparable to those of field galaxies, with Mgas = [0.3, 1.8] × 1011 × (αco/4.36 × A(Z))) M⊙, where αco is the CO-to-H2 conversion factor and A(Z) is the additional correction factor for the metallicity dependence of αco, and fgas = 0.53 ± 0.07 from CO (3-2). Our measurements place a constraint on the cosmic gas density of high-z protoclusters, indicating that the protocluster is characterized by a gas density higher than that of the general fields by an order of magnitude. We found p(H2) ∼ 5 × 109 M⊙ Mpc-3 with the CO(3-2) detections. The five ALMA CO detections occur in the region of highest galaxy surface density, where the density positively correlates with global star-forming efficiency (SFE) and stellar mass. Such correlations possibly indicate a critical role of the environment on early galaxy evolution at high-z protoclusters, though future observations are necessary for confirmation.

DOI： 10.3847/1538-4357/aa74c2

Evolutionary Phases of Gas-rich Galaxies in a Galaxy Cluster at z=1.46 査読有り

Hayashi Masao, Kodama Tadayuki, Kohno Kotaro, Yamaguchi Yuki, Tadaki Ken-ichi, Hatsukade Bunyo, Koyama Yusei, Shimakawa Rhythm, Tamura Yoichi, Suzuki Tomoko L.

ASTROPHYSICAL JOURNAL LETTERS 841 巻 ( 2 ) 2017年6月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Astrophysical Journal Letters

We report a survey of molecular gas in galaxies in the XMMXCS J2215.9-1738 cluster at z = 1.46. We have detected emission lines from 17 galaxies within a radius of R 200 from the cluster center, in Band 3 data of the Atacama Large Millimeter/submillimeter Array, with a coverage of 93-95 GHz in frequency and 2.33 arcmin2 in spatial direction. The lines are all identified as CO J = 2-1 emission lines from cluster members at by their redshifts and the colors of their optical and near-infrared (NIR) counterparts. The line luminosities reach down to Lco(2-1) = 4.5 × 109K K km s-1 pc2. The spatial distribution of galaxies with a detection of CO(2-1) suggests that they disappear from the very center of the cluster. The phase-space diagram showing relative velocity versus cluster-centric distance indicates that the gas-rich galaxies have entered the cluster more recently than the gas-poor star-forming galaxies and passive galaxies located in the virialized region of this cluster. The results imply that the galaxies experienced ram-pressure stripping and/or strangulation during the course of infall toward the cluster center and then the molecular gas in the galaxies at the cluster center was depleted by star formation.

DOI： 10.3847/2041-8213/aa71ad

ALMA deep field in SSA22: Blindly detected CO emitters and [C II] emitter candidates 査読有り

Hayatsu Natsuki H., Matsuda Yuichi, Umehata Hideki, Yoshida Naoki, Smail Ian, Swinbank A. Mark, Ivison Rob, Kohno Kotaro, Tamura Yoichi, Kubo Mariko, Iono Daisuke, Hatsukade Bunyo, Nakanishi Kouichiro, Kawabe Ryohei, Nagao Tohru, Inoue Akio K., Takeuchi Tsutomu T., Lee Minju, Ao Yiping, Fujimoto Seiji, Izumi Takuma, Yamaguchi Yuki, Ikarashi Soh, Yamada Toru

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 69 巻 ( 3 ) 2017年6月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

We report the identification of four millimeter line-emitting galaxies with the Atacama Large Milli/submillimeter Array (ALMA) in SSA22 Field (ADF22). We analyze the ALMA 1.1-mm survey data, with an effective survey area of 5 arcmin 2, frequency ranges of 253.1-256.8 and 269.1-272.8 GHz, angular resolution of 0.″7 and rms noise of 0.8 mJy beam -1 at 36 km s -1 velocity resolution. We detect four line-emitter candidates with significance levels above 6σ. We identify one of the four sources as a CO(9-8) emitter at z = 3.1 in a member of the proto-cluster known in this field. Another line emitter with an optical counterpart is likely a CO(4-3) emitter at z = 0.7. The other two sources without any millimeter continuum or optical/near-infrared counterpart are likely to be [C ii] emitter candidates at z = 6.0 and 6.5. The equivalent widths of the [C ii] candidates are consistent with those of confirmed high-redshift [C ii] emitters and candidates, and are a factor of 10 times larger than that of the CO(9-8) emitter detected in this search. The [C ii] luminosity of the candidates are 4-7 × 10 8 L ⊙. The star formation rates (SFRs) of these sources are estimated to be 10-20 M ⊙ yr -1 if we adopt an empirical [C ii] luminosity-SFR relation. One of them has a relatively low S/N ratio, but shows features characteristic of emission lines. Assuming that at least one of the two candidates is a [C ii] emitter, we derive a lower limit of [C ii]-based star formation rate density (SFRD) at z ∼ 6. The resulting value of >10 -2 M ⊙ yr -1 Mpc -3 is consistent with the dust-uncorrected UV-based SFRD. Future millimeter/submillimeter surveys can be used to detect a number of high-redshift line emitters, with which to study the star formation history in the early universe.

DOI： 10.1093/pasj/psx018

Rotating Starburst Cores in Massive Galaxies at z = 2.5 査読有り国際誌 Open Access

Ken-ichi Tadaki, Tadayuki Kodama, Erica J. Nelson, Sirio Belli, Natascha M. Förster Schreiber, Reinhard Genzel, Masao Hayashi, Rodrigo Herrera-Camus, Yusei Koyama, Philipp Lang, Dieter Lutz, Rhythm Shimakawa, Linda J. Tacconi, Hannah Übler, Emily Wisnioski, Stijn Wuyts, Bunyo Hatsukade, Magdalena Lippa, Kouichiro Nakanishi, Soh Ikarashi, Kotaro Kohno, Tomoko L. Suzuki, Yoichi Tamura, Ichi Tanaka

The Astrophysical Journal Letters 841 巻 ( 2 ) 頁： L25 2017年6月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：American Astronomical Society

<jats:title>Abstract</jats:title>
<jats:p>We present spatially resolved ALMA observations of the CO <jats:inline-formula>
<jats:tex-math>
<?CDATA $J=3-2$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa7338ieqn1.gif" xlink:type="simple" />
</jats:inline-formula> emission line in two massive galaxies at <jats:italic>z</jats:italic> = 2.5 on the star-forming main sequence. Both galaxies have compact dusty star-forming cores with effective radii of <jats:inline-formula>
<jats:tex-math>
<?CDATA ${R}_{{\rm{e}}}=1.3\pm 0.1\,\mathrm{kpc}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa7338ieqn2.gif" xlink:type="simple" />
</jats:inline-formula> and <jats:inline-formula>
<jats:tex-math>
<?CDATA ${R}_{{\rm{e}}}=1.2\pm 0.1\,\mathrm{kpc}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa7338ieqn3.gif" xlink:type="simple" />
</jats:inline-formula> in the 870 <jats:italic>μ</jats:italic>m continuum emission. The spatial extent of star-forming molecular gas is also compact with <jats:inline-formula>
<jats:tex-math>
<?CDATA ${R}_{{\rm{e}}}=1.9\pm 0.4\,\mathrm{kpc}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa7338ieqn4.gif" xlink:type="simple" />
</jats:inline-formula> and <jats:inline-formula>
<jats:tex-math>
<?CDATA ${R}_{{\rm{e}}}=2.3\pm 0.4\,\mathrm{kpc}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa7338ieqn5.gif" xlink:type="simple" />
</jats:inline-formula>, but more extended than the dust emission. Interpreting the observed position–velocity diagrams with dynamical models, we find the starburst cores to be rotation dominated with the ratio of the maximum rotation velocity to the local velocity dispersion of <jats:inline-formula>
<jats:tex-math>
<?CDATA ${v}_{\max }/{\sigma }_{0}={7.0}_{-2.8}^{+2.5}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa7338ieqn6.gif" xlink:type="simple" />
</jats:inline-formula> (<jats:inline-formula>
<jats:tex-math>
<?CDATA ${v}_{\max }={386}_{-32}^{+36}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa7338ieqn7.gif" xlink:type="simple" />
</jats:inline-formula> km s<jats:sup>−1</jats:sup>) and <jats:inline-formula>
<jats:tex-math>
<?CDATA ${v}_{\max }/{\sigma }_{0}={4.1}_{-1.5}^{+1.7}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa7338ieqn8.gif" xlink:type="simple" />
</jats:inline-formula> (<jats:inline-formula>
<jats:tex-math>
<?CDATA ${v}_{\max }={391}_{-41}^{+54}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa7338ieqn9.gif" xlink:type="simple" />
</jats:inline-formula> km s<jats:sup>−1</jats:sup>). Given that the descendants of these massive galaxies in the local universe are likely ellipticals with <jats:inline-formula>
<jats:tex-math>
<?CDATA $v/\sigma $?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa7338ieqn10.gif" xlink:type="simple" />
</jats:inline-formula> nearly an order of magnitude lower, the rapidly rotating galaxies would lose significant net angular momentum in the intervening time. The comparisons among dynamical, stellar, gas, and dust mass suggest that the starburst CO-to-H<jats:sub>2</jats:sub> conversion factor of <jats:inline-formula>
<jats:tex-math>
<?CDATA ${\alpha }_{\mathrm{CO}}=0.8\,{M}_{\odot }$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjlaa7338ieqn11.gif" xlink:type="simple" />
</jats:inline-formula> (K km s<jats:sup>−1</jats:sup> pc<jats:sup>−2</jats:sup>)<jats:sup>−1</jats:sup> is appropriate in the spatially resolved cores. The dense cores are likely to be formed in extreme environments similar to the central regions of local ultraluminous infrared galaxies. Our work also demonstrates that a combination of medium-resolution CO and high-resolution dust continuum observations is a powerful tool for characterizing the dynamical state of molecular gas in distant galaxies.</jats:p>

DOI： 10.3847/2041-8213/aa7338

A statistical study of giant molecular clouds traced by <SUP>13</SUP>CO, C<SUP>18</SUP>O, CS, and CH<sub>3</sub>OH in the disk of NGC 1068 based on ALMA observations 査読有り

Tosaki Tomoka, Kohno Kotaro, Harada Nanase, Tanaka Kunihiko, Egusa Fumi, Izumi Takuma, Takano Shuro, Nakajima Taku, Taniguchi Akio, Tamura Yoichi

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 69 巻 ( 2 ) 2017年4月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

We present 1″.4 (98 pc) resolution ALMA observations of 13CO(J = 1-0), C18O(J = 1-0), CS(J = 2-1), and CH3OH(JK = 2K-1K) molecular rotational lines in the central 1′ (4.2 kpc) diameter region of NGC 1068 to study the physical and chemical properties of giant molecular clouds (GMCs) and to test whether these GMC-scale properties are linked to the larger-scale galactic environment. Using the derived 13CO cube, we have identified 187 high-significance (>8σ) GMCs by employing the CLUMPFIND algorithm. The molecular gas masses of GMCs (M13CO), derived from the 13CO data, range from 1.8 × 104 M⊙ to 4.2 × 107 M⊙. A mass function of GMCs in NGC 1068 has been obtained for the first time at ∼100 pc resolution. We find the slope of the mass function γ = -1.25 ± 0.07 for a mass range of M13CO ≥ 105 M⊙. This is shallower than the GMCs in the disk regions of the Milky Way, M 51, and NGC 300. Further, we find that the high mass cut-off of the GMC mass function occurs at M13CO ∼ 6 × 107 M⊙, which is an order of magnitude larger than that in the nuclear bar region of M 51, indicating that the more massive clouds dominate the mass budget in NGC 1068. The observed C18O(J = 1-0)/13CO(J = 1-0) intensity ratios are found to be fairly uniform (0.27 ± 0.05) among the identified GMCs. In contrast, the CH3OH(JK = 2K-1K)/13CO(J = 1-0) ratios exhibit striking spatial variation across the disk, with the smallest values around the bar-end (<0.03), and larger ratios along the spiral arms (∼0.1-0.2). We find that GMCs with detectable methanol emission tend to have systematically larger velocity widths than those without methanol emission, suggesting that (relatively weak) shocks are responsible for the enhancement of the CH3OH/13CO ratios of GMCs in the disk of NGC 1068.

DOI： 10.1093/pasj/psw122

J-GEM follow-up observations of the gravitational wave source GW151226 査読有り

Yoshida Michitoshi, Utsumi Yousuke, Tominaga Nozomu, Morokuma Tomoki, Tanaka Masaomi, Asakura Yuichiro, Matsubayashi Kazuya, Ohta Kouji, Abe Fumio, Chimasu Sho, Furusawa Hisanori, Itoh Ryosuke, Itoh Yoichi, Kanda Yuka, Kawabata Koji S., Kawabata Miho, Koshida Shintaro, Koshimoto Naoki, Kuroda Daisuke, Moritani Yuki, Motohara Kentaro, Murata Katsuhiro L., Nagayama Takahiro, Nakaoka Tatsuya, Nakata Fumiaki, Nishioka Tsubasa, Saito Yoshihiko, Terai Tsuyoshi, Tristram Paul J., Yanagisawa Kenshi, Yasuda Naoki, Doi Mamoru, Fujisawa Kenta, Kawachi Akiko, Kawai Nobuyuki, Tamura Yoichi, Uemura Makoto, Yatsu Yoichi

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 69 巻 ( 1 ) 頁： 9 2017年2月

記述言語：日本語掲載種別：研究論文（学術雑誌）出版者・発行元：Publications of the Astronomical Society of Japan

We report the results of optical-infrared follow-up observations of the gravitational wave (GW) event GW151226 detected by the Advanced LIGO in the framework of J-GEM (Japanese collaboration for Gravitational wave ElectroMagnetic follow-up). We performed wide-field optical imaging surveys with the Kiso Wide Field Camera (KWFC), Hyper Suprime-Cam (HSC), and MOA-cam3. The KWFC survey started at 2.26 d after the GW event and covered 778 deg2 centered at the high Galactic region of the skymap of GW151226. We started the HSC follow-up observations from ∼12 d after the event and covered an area of 63.5 deg2 of the highest probability region of the northern sky with limiting magnitudes of 24.6 and 23.8 for the i and z bands, respectively. MOA-cam3 covered 145 deg2 of the skymap with the MOA-red filter ∼2.5mon after the GW alert. The total area covered by the wide-field surveys was 986.5 deg2. The integrated detection probability for the observed area was ∼29%. We also performed galaxy-targeted observations with six optical and near-infrared telescopes from 1.61 d after the event. A total of 238 nearby (≥100Mpc) galaxies were observed with a typical I band limiting magnitude of ∼19.5. We detected 13 supernova candidates with the KWFC survey, and 60 extragalactic transients with the HSC survey. Two thirds of the HSC transients were likely supernovae and the remaining one third were possible active galactic nuclei. With our observational campaign, we found no transients that are likely to be associated with GW151226.

DOI： 10.1093/pasj/psw113

Extremely Red Submillimeter Galaxies: New z ≳ 4–6 Candidates Discovered Using ALMA and Jansky VLA 査読有り国際誌 Open Access

Soh Ikarashi, R. J. Ivison, Karina I. Caputi, Kouichiro Nakanishi, Claudia D. P. Lagos, M. L. N. Ashby, Itziar Aretxaga, James S. Dunlop, Bunyo Hatsukade, David H. Hughes, Daisuke Iono, Takuma Izumi, Ryohei Kawabe, Kotaro Kohno, Kentaro Motohara, Kouji Ohta, Yoichi Tamura, Hideki Umehata, Grant W. Wilson, Kiyoto Yabe, Min S. Yun

The Astrophysical Journal 835 巻 ( 2 ) 頁： 286 2017年2月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：American Astronomical Society

<jats:title>Abstract</jats:title>
<jats:p>We present the detailed characterization of two extremely red submillimeter galaxies (SMGs), ASXDF1100.053.1 and 231.1, with the Atacama Large Millimeter/submillimeter Array (ALMA) and the Jansky Very Large Array. These SMGs were originally selected using AzTEC at 1100 <jats:italic>μ</jats:italic>m, and are observed by <jats:italic>Herschel</jats:italic> to be faint at 100–500 <jats:italic>μ</jats:italic>m. Their (sub)millimeter colors are as red as—or redder—than known <jats:italic>z</jats:italic> ≳ 5 SMGs; indeed, ASXDF1100.053.1 is redder than HFLS 3, which lies at <jats:italic>z</jats:italic> = 6.3. They are also faint and red in the near-/mid-infrared: ∼1 <jats:italic>μ</jats:italic>Jy at IRAC 4.5 <jats:italic>μ</jats:italic>m and <0.2 <jats:italic>μ</jats:italic>Jy in the <jats:italic>K</jats:italic>
<jats:sub>s</jats:sub> filter. These SMGs are also faint in the radio waveband, where <jats:italic>F</jats:italic>
<jats:sub>6GHz</jats:sub> = 4.5 <jats:italic>μ</jats:italic>Jy for ASXDF1100.053.1 and <jats:italic>F</jats:italic>
<jats:sub>1.4GHz</jats:sub> = 28 <jats:italic>μ</jats:italic>Jy for ASXDF1100.231.1, suggestive of <jats:inline-formula>
<jats:tex-math>
<?CDATA $z={6.5}_{-1.1}^{+1.4}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa566eieqn1.gif" xlink:type="simple" />
</jats:inline-formula> and <jats:inline-formula>
<jats:tex-math>
<?CDATA $z={4.1}_{-0.7}^{+0.6}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa566eieqn2.gif" xlink:type="simple" />
</jats:inline-formula> for ASXDF1100.053.1 and 231.1, respectively. ASXDF1100.231.1 has a flux excess in the 3.6 <jats:italic>μ</jats:italic>m filter, probably due to H<jats:italic>α</jats:italic> emission at <jats:italic>z</jats:italic> = 4–5. Derived properties of ASXDF1100.053.1 for <jats:italic>z</jats:italic> = 5.5–7.5 and 231.1 for <jats:italic>z</jats:italic> = 3.5–5.5 are as follows: their infrared luminosities are [6.5 − 7.4] × 10<jats:sup>12</jats:sup> and [4.2–4.5] × 10<jats:sup>12</jats:sup>
<jats:italic>L</jats:italic>
<jats:sub>⊙</jats:sub>; their stellar masses are [0.9–2] × 10<jats:sup>11</jats:sup> and [0.4–3] × 10<jats:sup>10</jats:sup>
<jats:italic>M</jats:italic>
<jats:sub>⊙</jats:sub>; their circularized half-light radii in the ALMA maps are ∼1 and ≲0.2 kpc (∼2–3 kpc for 90% of the total flux). Last, their surface infrared luminosity densities, Σ<jats:sub>IR</jats:sub>, are ∼1 × 10<jats:sup>12</jats:sup> and ≳1.5 × 10<jats:sup>13</jats:sup>
<jats:italic>L</jats:italic>
<jats:sub>⊙</jats:sub> kpc<jats:sup>−2</jats:sup>, similar to values seen for local (U)LIRGs. These data suggest that ASXDF1100.053.1 and 231.1 are compact SMGs at <jats:italic>z</jats:italic> ≳ 4 and can plausibly evolve into <jats:italic>z</jats:italic> ≳ 3 compact quiescent galaxies.</jats:p>

DOI： 10.3847/1538-4357/835/2/286

ALMA Deep Field in SSA22: Source Catalog and Number Counts 査読有り国際誌 Open Access

Hideki Umehata, Yoichi Tamura, Kotaro Kohno, R. J. Ivison, Ian Smail, Bunyo Hatsukade, Kouichiro Nakanishi, Yuta Kato, Soh Ikarashi, Yuichi Matsuda, Seiji Fujimoto, Daisuke Iono, Minju Lee, Charles C. Steidel, Tomoki Saito, D. M. Alexander, Min S. Yun, Mariko Kubo

The Astrophysical Journal 835 巻 ( 1 ) 頁： 98 - 98 2017年1月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：American Astronomical Society

<jats:title>Abstract</jats:title>
<jats:p>We present results from a deep 2′ × 3′ (comoving scale of 3.7 Mpc × 5.5 Mpc at <jats:italic>z</jats:italic> = 3) survey at 1.1 mm, taken with the Atacama Large Millimeter/submillimeter Array (ALMA) in the SSA22 field. We observe the core region of a <jats:italic>z</jats:italic> = 3.09 protocluster, achieving a typical rms sensitivity of 60 <jats:italic>μ</jats:italic>Jy beam<jats:sup>−1</jats:sup> at a spatial resolution of 0.″7. We detect 18 robust ALMA sources at a signal-to-noise ratio (S/N) > 5. Comparison between the ALMA map and a 1.1 mm map, taken with the AzTEC camera on the Atacama Submillimeter Telescope Experiment (ASTE), indicates that three submillimeter sources discovered by the AzTEC/ASTE survey are resolved into eight individual submillimeter galaxies (SMGs) by ALMA. At least 10 of our 18 ALMA SMGs have spectroscopic redshifts of <jats:italic>z</jats:italic> ≃ 3.09, placing them in the protocluster. This shows that a number of dusty starburst galaxies are forming simultaneously in the core of the protocluster. The nine brightest ALMA SMGs with S/N > 10 have a median intrinsic angular size of <jats:inline-formula>
<jats:tex-math>
<?CDATA $0\buildrel{\prime\prime}\over{.} {32}_{-0.06}^{+0.13}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa5107ieqn1.gif" xlink:type="simple" />
</jats:inline-formula> (<jats:inline-formula>
<jats:tex-math>
<?CDATA ${2.4}_{-0.4}^{+1.0}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa5107ieqn2.gif" xlink:type="simple" />
</jats:inline-formula> physical kpc at <jats:italic>z</jats:italic> = 3.09), which is consistent with previous size measurements of SMGs in other fields. As expected, the source counts show a possible excess compared to the counts in the general fields at <jats:italic>S</jats:italic>
<jats:sub>1.1mm</jats:sub> ≥ 1.0 mJy, due to the protocluster. Our contiguous mm mapping highlights the importance of large-scale structures on the formation of dusty starburst galaxies.</jats:p>

DOI： 10.3847/1538-4357/835/1/98

ALMA Reveals Strong [C II] Emission in a Galaxy Embedded in a Giant Ly α Blob at z = 3.1 査読有り国際誌

Hideki Umehata, Yuichi Matsuda, Yoichi Tamura, Kotaro Kohno, Ian Smail, R. J. Ivison, Charles C. Steidel, Scott C. Chapman, James E. Geach, Matthew Hayes, Tohru Nagao, Yiping Ao, Ryohei Kawabe, Min S. Yun, Bunyo Hatsukade, Mariko Kubo, Yuta Kato, Tomoki Saito, Soh Ikarashi, Kouichiro Nakanishi, Minju Lee, Takuma Izumi, Masao Mori, Masami Ouchi

The Astrophysical Journal 834 巻 ( 2 ) 2017年1月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：American Astronomical Society

We report the result from observations conducted with the Atacama Large
Millimeter/submillimeter Array (ALMA) to detect [CII] 158 um fine structure
line emission from galaxies embedded in one of the most spectacular Lyman-alpha
blobs (LABs) at z=3.1, SSA22-LAB1. Of three dusty star-forming galaxies
previously discovered by ALMA 860 um dust continuum survey toward SSA22-LAB1,
we detected the [CII] line from one, LAB1-ALMA3 at z=3.0993+/-0.0004. No line
emission was detected, associated with the other ALMA continuum sources or from
three rest-frame UV/optical selected z_spec~3.1 galaxies within the field of
view. For LAB1-ALMA3, we find relatively bright [CII] emission compared to the
infrared luminosity (L_[CII]/L_[CII]) and an extremely high [CII] 158 um and
[NII] 205 um emission line ratio (L_[CII]/L_[NII]>55). The relatively strong
[CII] emission may be caused by abundant photodissociation regions and
sub-solar metallicity, or by shock heating. The origin of the unusually strong
[CII] emission could be causally related to the location within the giant LAB,
although the relationship between extended Lyman-alpha emission and ISM
conditions of associated galaxies is yet to be understand.

DOI： 10.3847/2041-8213/834/2/L16

BULGE-FORMING GALAXIES WITH AN EXTENDED ROTATING DISK AT z ∼ 2 査読有り国際誌 Open Access

Ken-ichi Tadaki, Reinhard Genzel, Tadayuki Kodama, Stijn Wuyts, Emily Wisnioski, Natascha M. Förster Schreiber, Andreas Burkert, Philipp Lang, Linda J. Tacconi, Dieter Lutz, Sirio Belli, Richard I. Davies, Bunyo Hatsukade, Masao Hayashi, Rodrigo Herrera-Camus, Soh Ikarashi, Shigeki Inoue, Kotaro Kohno, Yusei Koyama, J. Trevor Mendel, Kouichiro Nakanishi, Rhythm Shimakawa, Tomoko L. Suzuki, Yoichi Tamura, Ichi Tanaka, Hannah Übler, Dave J. Wilman

The Astrophysical Journal 834 巻 ( 2 ) 頁： 135 2017年1月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：American Astronomical Society

<jats:title>ABSTRACT</jats:title>
<jats:p>We present 0.″2-resolution Atacama Large Millimeter/submillimeter Array observations at 870 <jats:italic>μ</jats:italic>m for 25 H<jats:italic>α</jats:italic>-seleced star-forming galaxies around the main sequence at <jats:italic>z</jats:italic> = 2.2–2.5. We detect significant 870 <jats:italic>μ</jats:italic>m continuum emission in 16 (64%) of these galaxies. The high-resolution maps reveal that the dust emission is mostly radiated from a single region close to the galaxy center. Exploiting the visibility data taken over a wide <jats:italic>uv</jats:italic> distance range, we measure the half-light radii of the rest-frame far-infrared emission for the best sample of 12 massive galaxies with log(<jats:italic>M</jats:italic>
<jats:sub>*</jats:sub>/<jats:italic>M</jats:italic>
<jats:sub>⊙</jats:sub>) > 11. We find nine galaxies to be associated with extremely compact dust emission with <jats:italic>R</jats:italic>
<jats:sub>1/2,870 <jats:italic>μ</jats:italic>m</jats:sub> < 1.5 kpc, which is more than a factor of 2 smaller than their rest-optical sizes, <jats:inline-formula>
<jats:tex-math>
<?CDATA $\langle {R}_{1/2,1.6\mu {\rm{m}}}\rangle =3.2\,\mathrm{kpc}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa499bieqn1.gif" xlink:type="simple" />
</jats:inline-formula>, and is comparable with optical sizes of massive quiescent galaxies at similar redshifts. As they have an exponential disk with Sérsic index of <jats:inline-formula>
<jats:tex-math>
<?CDATA $\langle {n}_{1.6\mu {\rm{m}}}\rangle =1.2$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa499bieqn2.gif" xlink:type="simple" />
</jats:inline-formula> in the rest-optical, they are likely to be in the transition phase from extended disks to compact spheroids. Given their high star formation rate surface densities within the central 1 kpc of <jats:inline-formula>
<jats:tex-math>
<?CDATA $\langle {\rm{\Sigma }}{\mathrm{SFR}}_{1\mathrm{kpc}}\rangle =40$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa499bieqn3.gif" xlink:type="simple" />
</jats:inline-formula>
<jats:italic>M</jats:italic>
<jats:sub>⊙</jats:sub> yr<jats:sup>−1</jats:sup> kpc<jats:sup>−2</jats:sup>, the intense circumnuclear starbursts can rapidly build up a central bulge with Σ<jats:italic>M</jats:italic>
<jats:sub>*,1 kpc</jats:sub> > 10<jats:sup>10</jats:sup>
<jats:italic>M</jats:italic>
<jats:sub>⊙</jats:sub> kpc<jats:sup>−2</jats:sup> in several hundred megayears, i.e., by <jats:italic>z</jats:italic> ∼ 2. Moreover, ionized gas kinematics reveal that they are rotation supported with an angular momentum as large as that of typical star-forming galaxies at <jats:italic>z</jats:italic> = 1–3. Our results suggest that bulges are commonly formed in extended rotating disks by internal processes, not involving major mergers.</jats:p>

DOI： 10.3847/1538-4357/834/2/135

　前のページ - 次のページ　

1