研究者詳細 - 田村　陽一

論文 - 田村　陽一

分割表示 143 件中 21 - 40 件目／全件表示 >>

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>
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</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>
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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

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