Updated on 2021/08/06

写真a

 
MORIHANA Kumiko
 
Organization
Institute of Liberal Arts and Sciences Lecturer
Title
Lecturer

Degree 1

  1. 博士 (理学) ( 2012.3   東京大学 ) 

Research Areas 1

  1. Natural Science / Astronomy

Education 2

  1. The University of Tokyo   Graduate School, Division of Natural Science

    2009.4 - 2012.3

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    Country: Japan

  2. Kobe University   Graduate School, Division of Human and Environmental Studies

    2007.4 - 2009.3

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    Country: Japan

Professional Memberships 1

  1. 日本天文学会

 

Papers 23

  1. 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   Vol. 2021 ( 5 )   2021.5

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    Language:Japanese   Publishing type:Research paper (scientific journal)   Publisher: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

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  2. Follow-up observations for IceCube-170922A: Detection of rapid near-infrared variability and intensive monitoring of TXS 0506+056

    Morokuma Tomoki, Utsumi Yousuke, Ohta Kouji, Yamanaka Masayuki, Kawabata Koji S., Inoue Yoshiyuki, Tanaka Masaomi, Yoshida Michitoshi, Itoh Ryosuke, Sasada Mahito, Tominaga Nozomu, Mori Hiroki, Kawabata Miho, Nakaoka Tatsuya, Chogi Maiko, Abe Taisei, Huang Ruochen, Kawahara Naoki, Kimura Hiroki, Nagashima Hiroki, Takagi Kengo, Yamazaki Yuina, Liu Wei, Ohsawa Ryou, Sako Shigeyuki, Murata Katsuhiro L., Morihana Kumiko, Gilligan Christina K., Isogai Keisuke, Kimura Mariko, Wakamatsu Yasuyuki, Ohnishi Ryuhei, Takayama Masaki, Honda Satoshi, Matsuoka Yoshiki, Yamashita Takuji, Nagataki Shigehiro, Tanaka Yasuyuki T.

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   Vol. 73 ( 1 ) page: 25 - 43   2021.2

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    Language:Japanese   Publishing type:Research paper (scientific journal)  

    DOI: 10.1093/pasj/psaa110

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  3. SPICA Mid-infrared Instrument (SMI): The latest design and specifications

    Wada Takehiko, Kaneda Hidehiro, Kokusho Takuma, Suzuki Toyoaki, Morihana Kumiko, Tsuchikawa Takurou, Kuroda Yuki, Ishikawa Daichi, Oyabu Shinki, Isobe Naoki, Ishihara Daisuke, Matsuhara Hideo, Nagase Koichi, Nakagawa Takao, Ootsubo Takafumi, Yamagishi Mitsuyoshi, Maeshima Hiroshi, Onishi Shunsuke, Matsumoto Kosei, Itoh Satoshi, Uchiyama Mizuho, Lau Ryan, Ebihara Hiromichi, Inami Hanae, Kawabata Koji, Kasaba Yasumasa, Sakanoi Takeshi, Ita Yoshifusa, Akiyama Masayuki, Sakon Itsuki, Kamizuka Takafumi, Miyata Takashi, Tsumura Kohji, Naruse Masato, Ohyama Youichi, Wang Shiang-Yu, Shibai Hiroshi

    SPACE TELESCOPES AND INSTRUMENTATION 2020: OPTICAL, INFRARED, AND MILLIMETER WAVE   Vol. 11443   2021

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    Language:Japanese   Publishing type:Research paper (scientific journal)   Publisher:Proceedings of SPIE - The International Society for Optical Engineering  

    SMI (SPICA Mid-infrared Instrument) is one of the three focal-plane science instruments for SPICA. SMI is the Japanese-led instrument proposed and managed by a university consortium. SMI covers the wavelength range from 10 to 36 μm with four separate channels: the low-resolution (R = 60 - 160) spectroscopy function for 17 - 36 μm, the broad-band (R = 5) imaging function at 34 μm, the mid-resolution (R = 1400 - 2600) spectroscopy function for 18 - 36 μm, and the high-resolution (R = 29000) spectroscopy function for 10 - 18 μm. In this presentation, we will show the latest design and specifications of SMI as a result of feasibility studies.

    DOI: 10.1117/12.2561157

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  4. Hydrogen recombination near-infrared line mapping of Centaurus A with IRSF/SIRIUS

    Katayama Risako, Kaneda Hidehiro, Kokusho Takuma, Morihana Kumiko, Suzuki Toyoaki, Oyabu Shinki, Yamagishi Mitsuyoshi, Tsuchikawa Takuro

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   Vol. 72 ( 5 )   2020.10

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    Language:Japanese   Publishing type:Research paper (scientific journal)   Publisher:Publications of the Astronomical Society of Japan  

    Centaurus A (Cen A) is one of the most famous galaxies hosting an active galactic nucleus (AGN), where the interaction between AGNactivities and surrounding interstellar and intergalactic media has been investigated. Recent studies reported detections of Hα emission from clouds in the galactic halo toward the northeast and southwest of the nucleus of Cen A, suggesting that AGN jets may have triggered star formation there. We performed near-infrared line mapping of Cen A with the IRSF 1.4m telescope, using the narrow-band filter tuned for Paβ, from which we find that Paβ emission is not detected significantly from either of the northeast or southwest regions. The upper limit of the Paβ/Hα ratio in the northeast region is compatible with that expected for a typical HII region, in line with the scenario that AGNs have triggered star formation there. On the other hand, the upper limit of Paβ/Hα in the southwest region is significantly lower than that expected for a typical HII region. A possible explanation of the low Paβ/Hα ratio in the southwest region is the scattering of Hα and Paβ photons from the center of Cen A by dust grains in the halo clouds. From the upper limit of Paβ/Hα in the southwest region, we obtain constraints on the dust size distribution, which is found to be compatible with those seen in the interstellar medium of our Galaxy.

    DOI: 10.1093/pasj/psaa081

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  5. Hydrogen recombination near-infrared line mapping of Centaurus A with IRSF/SIRIUS (vol 72, pg 88, 2020)

    Katayama Risako, Kaneda Hidehiro, Kokusho Takuma, Morihana Kumiko, Suzuki Toyoaki, Oyabu Shinki, Yamagishi Mitsuyoshi, Tsuchikawa Takuro

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   Vol. 72 ( 5 )   2020.10

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    Language:Japanese   Publishing type:Research paper (scientific journal)   Publisher:Publications of the Astronomical Society of Japan  

    In the Advance Access version of article [PASJ 72, 88 (2020); doi: 10.1093/pasj/psaa081], the contour levels listed in the caption of figure 1 were incorrect. This error has been corrected in both online and print versions of the article.

    DOI: 10.1093/pasj/psaa094

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  6. SN 2019ein: New Insights into the Similarities and Diversity among High-velocity Type Ia Supernovae

    Kawabata Miho, Maeda Keiichi, Yamanaka Masayuki, Nakaoka Tatsuya, Kawabata Koji S., Adachi Ryo, Akitaya Hiroshi, Burgaz Umut, Hanayama Hidekazu, Horiuchi Takashi, Hosokawa Ryohei, Iida Kota, Imazato Fumiya, Isogai Keisuke, Jiang Ji-an, Katoh Noriyuki, Kimura Hiroki, Kino Masaru, Kuroda Daisuke, Maehara Hiroyuki, Matsubayashi Kazuya, Morihana Kumiko, Murata Katsuhiro L., Nagao Takashi, Niwano Masafumi, Nogami Daisaku, Oeda Motoki, Ono Tatsuharu, Onozato Hiroki, Otsuka Masaaki, Saito Tomoki, Sasada Mahito, Shiraishi Kazuki, Sugiyama Haruki, Taguchi Kenta, Takahashi Jun, Takagi Kengo, Takagi Seiko, Takayama Masaki, Tozuka Miyako, Sekiguchi Kazuhiro

    ASTROPHYSICAL JOURNAL   Vol. 893 ( 2 )   2020.4

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    Language:Japanese   Publishing type:Research paper (scientific journal)   Publisher:Astrophysical Journal  

    We present optical observations of the Type Ia supernova (SN) 2019ein, starting two days after the estimated explosion date. The spectra and light curves show that SN 2019ein belongs to a high-velocity (HV) and broad-line group with a relatively rapid decline in the light curves (Δm 15(B) = 1.36 ± 0.02 mag) and a short rise time (15.37 ± 0.55 days). The Si ii λ6355 velocity, associated with a photospheric component but not with a detached high-velocity feature, reached ∼20,000 km s-1 12 days before the B-band maximum. The line velocity, however, decreased very rapidly and smoothly toward maximum light, to ∼13,000 km s-1, which is relatively low among HV SNe. This indicates that the speed of the spectral evolution of HV SNe Ia is correlated with not only the velocity at maximum light, but also the light-curve decline rate, as is the case for normal-velocity (NV) SNe Ia. Spectral synthesis modeling shows that the outermost layer at >17,000 km s-1 is well described by an O-Ne-C burning layer extending to at least 25,000 km s-1, and there is no unburnt carbon below 30,000 km s-1; these properties are largely consistent with the delayed detonation scenario and are shared with the prototypical HV SN 2002bo despite the large difference in Δm 15(B). This structure is strikingly different from that derived for the well-studied NV SN 2011fe. We suggest that the relation between the mass of 56Ni (or Δm 15) and the extent of the O-Ne-C burning layer provides an important constraint on the explosion mechanism(s) of HV and NV SNe.

    DOI: 10.3847/1538-4357/ab8236

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  7. New narrow-band filter system for the IRSF 1.4m telescope

    Morihana K., Nagayama T., Tsujimoto M., Yamagishi M., Ebisawa K.

    Proceedings of SPIE - The International Society for Optical Engineering   Vol. 11447   2020

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    Language:Japanese   Publishing type:Research paper (scientific journal)   Publisher:Proceedings of SPIE - The International Society for Optical Engineering  

    Narrow-band filters can detect emission and absorption line features from multiple sources in a field of view simultaneously without spectroscopy. However, it is difficult to estimate and subtract the continuum component from sources of different spectral slope, especially when the equivalent width of the target lines is small. For example, Cataclysmic Variables have equivalent widths of hydrogen recombination emission lines of about -10 to -100 angstroms, but many of the ones that have been detected by conventional NB filters so far have a large equivalent width. We have therefore constructed novel narrow-band filters with transmission bands on both sides of the central wavelengths of the Paβ (1.282 µm) and Brγ (2.167 µm) emission lines so that we can evaluate the continuum level more accurately than the conventional filters having transmission in only one side of the target line. We installed the narrow-band filters to the Simultaneous three-color InfraRed Imager for Unbiased Survey (SIRIUS) in the InfraRed Survey Facility (IRSF) telescope at South African Astronomical Observatory (SAAO), and evaluated their performance. We found that the narrow-band filters can detect emission line features with an equivalent width of several tens of angstroms. Thus, this filter set is useful for detecting emission line features from targets with small equivalent widths that have been difficult to detect with the conventional NB filter set.

    DOI: 10.1117/12.2576307

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  8. Near- to mid-infrared spectroscopy of the heavily obscured AGN LEDA 1712304 with AKARI/IRC

    Tsuchikawa T., Kaneda H., Oyabu S., Kokusho T., Morihana K., Kobayashi H., Yamagishi M., Toba Y.

    ASTRONOMY & ASTROPHYSICS   Vol. 626   2019.6

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    Language:Japanese   Publishing type:Research paper (scientific journal)   Publisher:Astronomy and Astrophysics  

    Context. Although heavily obscured active galactic nuclei (AGNs) have been found by many observational studies, the properties of the surrounding dust are poorly understood. Using AKARI/IRC spectroscopy, we discovered a new heavily obscured AGN in LEDA 1712304 which shows a deep spectral absorption feature due to silicate dust. Aims. We study the infrared (IR) spectral properties of circumnuclear silicate dust in LEDA 1712304. Methods. We performed IR spectral fitting, considering silicate dust properties such as composition, porosity, size, and crystallinity. Spectral energy distribution fitting was also performed on the flux densities in the UV to submillimeter range to investigate the global spectral properties. Results. The best-fit model indicates 0.1? μm-sized porous amorphous olivine (Mg2xFe2-2xSiO4; x? =? 0.4) with 4% crystalline pyroxene. The optical depth is τsil? ∼? 2.3, while the total IR luminosity and stellar mass are estimated to be LIR? =? (5 ± 1)×1010? L? and Mstar? =? (2.7 ± 0.8)×109? M?, respectively. In such low LIR and Mstar ranges, there are few galaxies that show such a large τsil. Conclusion. The silicate dust in the AGN torus of LEDA 1712304 has properties that are notably similar to those in other AGNs overall, but slightly different in the wing shape of the absorption profile. The porosity of the silicate dust suggests dust coagulation or processing in the circumnuclear environments, while the crystallinity suggests that the silicate dust is relatively fresh.

    DOI: 10.1051/0004-6361/201935483

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  9. High polarization degree of the continuum of comet 2P/Encke based on spectropolarimetric signals during its 2017 apparition

    Kwon Y. G., Ishiguro M., Shinnaka Y., Nakaoka T., Kuroda D., Hanayama H., Takahashi J., Baar S., Saito T., Kawabata M., Uemura M., Morokuma T., Murata K. L., Takagi S., Morihana K., Nagayama T., Sekiguchi K., Kawabata K. S., Akitaya H.

    ASTRONOMY & ASTROPHYSICS   Vol. 620   2018.12

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    Language:Japanese   Publishing type:Research paper (scientific journal)   Publisher:Astronomy and Astrophysics  

    Context. Spectropolarimetry is a powerful technique for investigating the physical properties of gas and solid materials in cometary comae without mutual contamination, but only a few spectropolarimetric studies have been conducted to extract each component. Aims. We attempt to derive the continuum (i.e., scattered light from dust coma) polarization degree of comet 2P/Encke, free of the influence of molecular emissions. The target is unique in that its orbit is dynamically decoupled from Jupiter, like the main-belt asteroids, but it ejects gas and dust like ordinary comets. Methods. We observed the comet using the Hiroshima Optical and Near-Infrared Camera attached to the Cassegrain focus of the 150 cm Kanata telescope on UT 2017 February 21 when the comet was at the solar phase angle of α = 75°.7. Results. We find that the continuum polarization degree with respect to the scattering plane is P cont, r = 33.8 ± 2.7% at the effective wavelength of 0.82 μm, which is significantly higher than those of cometary dust in a high-P max group at similar phase angles. Assuming that an ensemble polarimetric response of the dust of 2P/Encke as a function of phase angle is morphologically similar with those of other comets, its maximum polarization degree is estimated to P max â40% at α max â 100°. In addition, we obtain the polarization degrees of the C 2 swan bands (0.51-0.56 μm), the NH 2 α bands (0.62-0.69 μm), and the CN-red system (0.78-0.94 μm) in a range of 3-19%, which depend on the molecular species and rotational quantum numbers of each branch. The polarization vector is aligned nearly perpendicularly to the scattering plane with an average of 0°.4 over a wavelength range of 0.50-0.97 μm. Conclusions. From the observational evidence, we conjecture that the high polarization degree of 2P/Encke might be attributable to a dominance of large dust particles around the nucleus, which have remained after frequent perihelion passages near the Sun.

    DOI: 10.1051/0004-6361/201833968

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  10. Suzaku and NuSTAR X-ray spectroscopy of gamma Cassiopeiae and HD 110432

    Tsujimoto Masahiro, Morihana Kumiko, Hayashi Takayuki, Kitaguchi Takao

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   Vol. 70 ( 6 )   2018.12

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    Language:Japanese   Publishing type:Research paper (scientific journal)   Publisher:Publications of the Astronomical Society of Japan  

    γ Cas and its dozen analogs comprise a small but distinct class of X-ray sources. They are early Be-type stars with an exceptionally hard thermal X-ray emission. The X-ray production mechanism has been under intense debate. Two competing ideas are (i) the magnetic activities in the Be star and its disk, and (ii) themass accretion onto the unidentified white dwarf (WD). We adopt the latter as a working hypothesis and apply physical models developed to describe the X-ray spectra of classicalWDbinaries containing a latetype companion. Models of non-magnetic and magnetic accreting WDs were applied to γ Cas and its brightest analog HD110432 using the Suzaku and NuSTAR data. The spectra were fitted by the two models, including the Fe fluorescence and the Compton reflection in a consistent geometry. The derived physical parameters are in a reasonable range in comparison to their classical WD binary counterparts. Additional pieces of evidence in the X-ray spectra-partial covering, Fe L lines, Fe I fluorescence-were not conclusive enough to classify these two sources into a subclass of accreting WD binaries. We discuss further observations, especially long-term temporal behaviors, which are important to elucidate the nature of these sources, if indeed they host accreting WDs.

    DOI: 10.1093/pasj/psy111

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  11. X-Ray, Optical, and Near-infrared Monitoring of the New X-Ray Transient MAXI J1820+070 in the Low/Hard State

    Shidatsu Megumi, Nakahira Satoshi, Yamada Satoshi, Kawamuro Taiki, Ueda Yoshihiro, Negoro Hitoshi, Murata Katsuhiro L., Itoh Ryosuke, Tachibana Yutaro, Adachi Ryo, Yatsu Yoichi, Kawai Nobuyuki, Hanayama Hidekazu, Horiuchi Takashi, Akitaya Hiroshi, Saito Tomoki, Takayama Masaki, Ohshima Tomohito, Katoh Noriyuki, Takahashi Jun, Nagayama Takahiro, Yamanaka Masayuki, Kawabata Miho, Nakaoka Tatsuya, Takagi Seiko, Morokuma Tomoki, Morihana Kumiko, Maehara Hiroyuki, Sekiguchi Kazuhiro

    ASTROPHYSICAL JOURNAL   Vol. 868 ( 1 )   2018.11

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    Language:Japanese   Publishing type:Research paper (scientific journal)   Publisher:Astrophysical Journal  

    We report X-ray, optical, and near-infrared monitoring of the new X-ray transient MAXI J1820+070 discovered with MAXI on 2018 March 11. Its X-ray intensity reached ∼2 crab at 2-20 keV at the end of March, and then gradually decreased until the middle of June. In this period, the X-ray spectrum was described by Comptonization of the disk emission, with a photon index of ∼1.5 and an electron temperature of ∼50 keV, which is consistent with a black hole X-ray binary in the low/hard state. The electron temperature was slightly decreased, and the photon index increased, with increasing flux. The source showed significant X-ray flux variation on a timescale of seconds. This short-term variation was found to be associated with changes in the spectral shape, and the photon index became slightly harder at higher fluxes. This suggests that the variation was produced by a change in the properties of the hot electron cloud responsible for the strong Comptonization. Modeling a multi-wavelength spectral energy distribution around the X-ray flux peak at the end of March, covering the near-infrared to X-ray bands, we found that the optical and near-infrared fluxes were likely contributed substantially by the jet emission. Before this outburst, the source was never detected in the X-ray band with MAXI (with a 3σ upper limit of ∼0.2 mcrab at 4-10 keV, obtained from seven years of data from 2009 to 2016), whereas weak optical and infrared activity was found at flux levels ∼3 orders of magnitude lower than the peak fluxes in the outburst.

    DOI: 10.3847/1538-4357/aae929

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  12. The Spectroscopic Variations of the FU Orionis Object V960 Mon

    Takagi Yuhei, Honda Satoshi, Arai Akira, Morihana Kumiko, Takahashi Jun, Oasa Yumiko, Itoh Yoichi

    ASTRONOMICAL JOURNAL   Vol. 155 ( 2 )   2018.2

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    Language:Japanese   Publishing type:Research paper (scientific journal)   Publisher:Astronomical Journal  

    We present the results of the spectroscopic monitoring of the FU Orionis type star V960 Mon. Spectroscopic variations of an FU Orionis type star will provide valuable information of its physical nature and the mechanism of the outburst. We conducted medium-resolution (R ∼ 10000) spectroscopic observations of V960 Mon with the 2 m Nayuta telescope at the Nishi-Harima Astronomical Observatory, from 2015 January to 2017 January, for 53 nights in total. We focused on Hα line and nearby atomic lines, and we detected the strength variations in both absorption and emission lines. The observed variation in the equivalent width of the absorption lines corresponds to a decrease in effective temperature and increase in surface gravity. These variations were likely to originate from the luminosity fading of the accretion disk due to the decrease in mass accretion rate.

    DOI: 10.3847/1538-3881/aaa545

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  13. On the satisfaction of the practical training for high school and undergraduate students in Nishi-Harima Astronomical Observatory

    Takayama Masaki, Itoh Yoichi, Morihana Kumiko, Takagi Yuhei

    Stars and Galaxies   Vol. 1 ( 0 ) page: 28 - 38   2018

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    Language:Japanese   Publishing type:Research paper (scientific journal)   Publisher:Center for Astronomy, University of Hyogo  

    As one of the educational dissemination activities of Nishi-Harima Astronomical Observatory, we have conducted astronomy practical training for high school and undergraduate students. We have conducted a questionnaire aiming at survey of satisfaction from the users and improvement of the quality since July 2015. In this paper, we surveyed the questionnaires from July 2015 to October 2018 and investigated to the satisfaction from the users for our training menu. The questionnaire was conducted for a total of 140 schools and organizations, and 89 responses wereobtained. The recovery rate was 64%. As a result, it was revealed that the majority of the users answered that they were satisfied with the content of the practical training. In addition, we found that the satisfaction level of "daytime observation of stars and sun", "astronomy lecture", "night observation practice" and the overall practice increased in recent years. On the other hand, we found that "tour of the observation with Nayuta" showed a downward trend in satisfaction and there is room for improvement. We also conducted a survey on the difficulty level of each practice menu. As a result, it was found that the answer choosing "proper" reached 86 % of the total number of responses. Considering the trend of the satisfaction from the users and the answer for the difficulty level, we concluded that our astronomy practice training at Nishi-Harima Astronomical Observatory is almost as expected by the user.

    DOI: 10.32231/starsandgalaxies.1.0_28

  14. J-GEM observations of an electromagnetic counterpart to the neutron star merger GW170817

    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   Vol. 69 ( 6 )   2017.12

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    Language:Japanese   Publishing type:Research paper (scientific journal)   Publisher: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

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  15. Kilonova from post-merger ejecta as an optical and near-Infrared counterpart of GW170817

    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   Vol. 69 ( 6 )   2017.12

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    Language:Japanese   Publishing type:Research paper (scientific journal)   Publisher: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

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  16. Multi-messenger Observations of a Binary Neutron Star Merger

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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   Vol. 848 ( 2 )   2017.10

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    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

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  17. OISTER optical and near-infrared monitoring observations of peculiar radio-loud active galactic nucleus SDSSJ110006.07+442144.3

    Morokuma Tomoki, Tanaka Masaomi, Tanaka Yasuyuki T., Itoh Ryosuke, Tominaga Nozomu, Gandhi Poshak, Pian Elena, Mazzali Paolo, Ohta Kouji, Matsumoto Emiko, Shibata Takumi, Akimoto Hinako, Akitaya Hiroshi, Ali Gamal B., Aoki Tsutomu, Doi Mamoru, Ebisuda Nana, Essam Ahmed, Fujisawa Kenta, Fukushima Hideo, Goda Shuhei, Gouda Yuya, Hanayama Hidekazu, Hashiba Yasuhito, Hashimoto Osamu, Hayashida Kenzo, Hiratsuka Yuichiro, Honda Satoshi, Imai Masataka, Inoue Kanichiro, Ishibashi Michiko, Iwata Ikuru, Izumiura Hideyuki, Kanda Yuka, Kawabata Miho, Kawaguchi Kenji, Kawai Nobuyuki, Kokubo Mitsuru, Kuroda Daisuke, Maehara Hiroyuki, Mito Hiroyuki, Mitsuda Kazuma, Miyagawa Ryota, Miyaji Takeshi, Miyamoto Yusuke, Morihana Kumiko, Moritani Yuki, Morokuma-Matsui Kana, Murakami Kotone, Murata Katsuhiro L., Nagayama Takahiro, Nakamura Kazuki, Nakaoka Tatsuya, Niinuma Kotaro, Nishimori Takafumi, Nogami Daisaku, Oasa Yumiko, Oda Tatsunori, Ohshima Tomohito, Saito Yoshihiko, Sakata Shuichiro, Sako Shigeyuki, Sarugaku Yuki, Sawada-Satoh Satoko, Seino Genta, Sorai Kazuo, Soyano Takao, Taddia Francesco, Takahashi Jun, Takagi Yuhei, Takaki Katsutoshi, Takata Koji, Tarusawa Ken'ichi, Uemura Makoto, Ui Takahiro, Urago Riku, Ushioda Kazutoshi, Watanabe Jun-ichi, Watanabe Makoto, Yamashita Satoshi, Yanagisawa Kenshi, Yonekura Yoshinori, Yoshida Michitoshi

    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN   Vol. 69 ( 5 )   2017.10

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    We present monitoring campaign observations at optical and near-infrared (NIR) wavelengths for a radio-loud active galactic nucleus (AGN) at z = 0.840, SDSS J110006.07+442144.3 (hereafter, J1100+4421), which was identified during a flare phase in late 2014 February. The campaigns consist of three intensive observing runs from the discovery to 2015 March, mostly within the scheme of the OISTER collaboration. Optical-NIR light curves and simultaneous spectral energy distributions (SEDs) are obtained. Our measurements show the strongest brightening in 2015 March. We found that the optical-NIR SEDs of J1100+4421 show an almost steady shape despite the large and rapid intranight variability. This constant SED shape is confirmed to extend to ∼5 μm in the observed frame using the archival WISE data. Given the lack of absorption lines and the steep power-law spectrum of α ν ∼ -1.4, where fνναν, synchrotron radiation by a relativistic jet with no or small contributions from the host galaxy and the accretion disk seems most plausible as an optical-NIR emission mechanism. The steep optical-NIR spectral shape and the large amplitude of variability are consistent with this object being a low ν peak jet-dominated AGN. In addition, sub-arcsecond resolution optical imaging data taken with Subaru Hyper Suprime-Cam does not show a clear extended component and the spatial scales are significantly smaller than the large extensions detected at radio wavelengths. The optical spectrum of a possible faint companion galaxy does not show any emission lines at the same redshift, and hence a merging hypothesis for this AGN-related activity is not supported by our observations.

    DOI: 10.1093/pasj/psx075

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  18. Broad-lined Supernova 2016coi with a Helium Envelope

    Yamanaka Masayuki, Nakaoka Tatsuya, Tanaka Masaomi, Maeda Keiichi, Honda Satoshi, Hanayama Hidekazu, Morokuma Tomoki, Imai Masataka, Kinugasa Kenzo, Murata Katsuhiro L., Nishimori Takefumi, Hashimoto Osamu, Gima Hirotaka, Hosoya Kensuke, Ito Ayano, Karita Mayu, Kawabata Miho, Morihana Kumiko, Morikawa Yuto, Murakami Kotone, Nagayama Takahiro, Ono Tatsuharu, Onozato Hiroki, Sarugaku Yuki, Sato Mitsuteru, Suzuki Daisuke, Takahashi Jun, Takayama Masaki, Yaguchi Hijiri, Akitaya Hiroshi, Asakura Yuichiro, Kawabata Koji S., Kuroda Daisuke, Nogami Daisaku, Oasa Yumiko, Omodaka Toshihiro, Saito Yoshihiko, Sekiguchi Kazuhiro, Tominaga Nozomu, Uemura Makoto, Watanabe Makoto

    ASTROPHYSICAL JOURNAL   Vol. 837 ( 1 )   2017.3

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    We present the early-phase spectra and the light curves of the broad-lined (BL) supernova (SN) 2016coi from t = 7 to 67 days after the estimated explosion date. This SN was initially reported as a BL Type SN Ic (SN Ic-BL). However, we found that spectra up to t = 12 days exhibited the He i λ5876, λ6678, and λ7065 absorption lines. We show that the smoothed and blueshifted spectra of normal SNe Ib are remarkably similar to the observed spectrum of SN 2016coi. The line velocities of SN 2016coi were similar to those of SNe Ic-BL and significantly faster than those of SNe Ib. Analyses of the line velocity and light curve suggest that the kinetic energy and the total ejecta mass of SN 2016coi are similar to those of SNe Ic-BL. Together with BL SNe 2009bb and 2012ap, for which the detection of He i was also reported, these SNe could be transitional objects between SNe Ic-BL and SNe Ib, and be classified as BL Type "Ib" SNe (SNe "Ib"-BL). Our work demonstrates the diversity of the outermost layer in BL SNe, which should be related to the variety of the evolutionary paths.

    DOI: 10.3847/1538-4357/aa5f57

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  19. NO EVIDENCE OF INTRINSIC OPTICAL/NEAR-INFRARED LINEAR POLARIZATION FOR V404 CYGNI DURING ITS BRIGHT OUTBURST IN 2015: BROADBAND MODELING AND CONSTRAINT ON JET PARAMETERS

    Tanaka Y. T., Itoh R., Uemura M., Inoue Y., Cheung C. C., Watanabe M., Kawabata K. S., Fukazawa Y., Yatsu Y., Yoshii T., Tachibana Y., Fujiwara T., Saito Y., Kawai N., Kimura M., Isogai K., Kato T., Akitaya H., Kawabata M., Nakaoka T., Shiki K., Takaki K., Yoshida M., Imai M., Gouda S., Gouda Y., Akimoto H., Honda S., Hosoya K., Ikebe A., Morihana K., Ohshima T., Takagi Y., Takahashi J., Watanabe K., Kuroda D., Morokuma T., Murata K., Nagayama T., Nogami D., Oasa Y., Sekiguchi K.

    ASTROPHYSICAL JOURNAL   Vol. 823 ( 1 )   2016.5

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    We present simultaneous optical and near-infrared (NIR) polarimetric results for the black hole binary V404 Cyg spanning the duration of its seven-day-long optically brightest phase of its 2015 June outburst. The simultaneous R- and K s-band light curves showed almost the same temporal variation except for the isolated (∼30-minute duration) orphan K s-band flare observed at MJD 57193.54. We did not find any significant temporal variation of polarization degree (PD) and position angle (PA) in both R and K s bands throughout our observations, including the duration of the orphan NIR flare. We show that the observed PD and PA are predominantly interstellar in origin by comparing the V404 Cyg polarimetric results with those of the surrounding sources within the 7′ × 7′ field of view. The low intrinsic PD (less than a few percent) implies that the optical and NIR emissions are dominated by either disk or optically thick synchrotron emission, or both. We also present the broadband spectra of V404 Cyg during the orphan NIR flare and a relatively faint and steady state by including quasi-simultaneous Swift/XRT and INTEGRAL fluxes. By adopting a single-zone synchrotron plus inverse-Compton model as widely used in modeling of blazars, we constrained the parameters of a putative jet. Because the jet synchrotron component cannot exceed the Swift/XRT disk/corona flux, the cutoff Lorentz factor in the electron energy distribution is constrained to be <102, suggesting that particle acceleration is less efficient in this microquasar jet outburst compared to active galactic nucleus jets. We also suggest that the loading of the baryon component inside the jet is inevitable based on energetic arguments.

    DOI: 10.3847/0004-637X/823/1/35

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  20. OPTICAL AND NEAR-INFRARED POLARIMETRY FOR A HIGHLY DORMANT COMET 209P/LINEAR

    Kuroda Daisuke, Ishiguro Masateru, Watanabe Makoto, Akitaya Hiroshi, Takahashi Jun, Hasegawa Sunao, Ui Takahiro, Kanda Yuka, Takaki Katsutoshi, Itoh Ryosuke, Moritani Yuki, Imai Masataka, Goda Shuhei, Takagi Yuhei, Morihana Kumiko, Honda Satoshi, Arai Akira, Hanayama Hidekazu, Nagayama Takahiro, Nogami Daisaku, Sarugaku Yuki, Murata Katsuhiro, Morokuma Tomoki, Saito Yoshihiko, Oasa Yumiko, Sekiguchi Kazuhiro, Watanabe Jun-ichi

    ASTROPHYSICAL JOURNAL   Vol. 814 ( 2 )   2015.12

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    We conducted an optical and near-infrared polarimetric observation of the highly dormant Jupiter-Family Comet, 209P/LINEAR. Because of its low activity, we were able to determine the linear polarization degrees of the coma dust particles and nucleus independently, that is Pn = % at α = 92.°2 and Pn = % at α = 99.°5 for the nucleus, and Pc = % at α = 92.°2 and % at α = 99.°5 for the coma. We detected no significant variation in P at the phase angle coverage of 92.°2-99.°5, which may imply that the obtained polarization degrees are nearly at maximum in the phase-polarization curves. By fitting with an empirical function, we obtained the maximum values of linear polarization degrees Pmax = 30.8% for the nucleus and Pmax = 29.6% for the dust coma. The Pmax of the dust coma is consistent with those of dust-rich comets. The low geometric albedo of Pv = 0.05 was derived from the slope-albedo relationship and was associated with high We examined Pmax-albedo relations between asteroids and 209P, and found that the so-called Umov law seems to be applicable on this cometary surface.

    DOI: 10.1088/0004-637X/814/2/156

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  21. DUST FROM COMET 209P/LINEAR DURING ITS 2014 RETURN: PARENT BODY OF A NEW METEOR SHOWER, THE MAY CAMELOPARDALIDS

    Ishiguro Masateru, Kuroda Daisuke, Hanayama Hidekazu, Takahashi Jun, Hasegawa Sunao, Sarugaku Yuki, Watanabe Makoto, Imai Masataka, Goda Shuhei, Akitaya Hiroshi, Takagi Yuhei, Morihana Kumiko, Honda Satoshi, Arai Akira, Sekiguchi Kazuhiro, Oasa Yumiko, Saito Yoshihiko, Morokuma Tomoki, Murata Katsuhiro, Nogami Daisaku, Nagayama Takahiro, Yanagisawa Kenshi, Yoshida Michitoshi, Ohta Kouji, Kawai Nobuyuki, Miyaji Takeshi, Fukushima Hideo, Watanabe Jun-ichi, Opitom Cyrielle, Jehin Emmanuel, Gillon Michael, Vaubaillon Jeremie J.

    ASTROPHYSICAL JOURNAL LETTERS   Vol. 798 ( 2 )   2015.1

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    We report a new observation of the Jupiter family comet 209P/LINEAR during its 2014 return. The comet is recognized as a dust source of a new meteor shower, the May Camelopardalids. 209P/LINEAR was apparently inactive at a heliocentric distance rh = 1.6 AU and showed weak activity at rh ≤ 1.4 AU. We found an active region of <0.001% of the entire nuclear surface during the comet's dormant phase. An edge-on image suggests that particles up to 1 cm in size (with an uncertainty of factor 3-5) were ejected following a differential power-law size distribution with index q = -3.25 ± 0.10. We derived a mass-loss rate of 2-10 kg s-1 during the active phase and a total mass of ≈5 × 107 kg during the 2014 return. The ejection terminal velocity of millimeter- to centimeter-sized particles was 1-4 m s-1, which is comparable to the escape velocity from the nucleus (1.4 m s-1). These results imply that such large meteoric particles marginally escaped from the highly dormant comet nucleus via the gas drag force only within a few months of the perihelion passage.

    DOI: 10.1088/2041-8205/798/2/L34

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  22. THE ACCRETION DISK AND IONIZED ABSORBER OF THE 9.7 hr DIPPING BLACK HOLE BINARY MAXI J1305-704

    Shidatsu M., Ueda Y., Nakahira S., Done C., Morihana K., Sugizaki M., Mihara T., Hori T., Negoro H., Kawai N., Yamaoka K., Ebisawa K., Matsuoka M., Serino M., Yoshikawa T., Nagayama T., Matsunaga N.

    ASTROPHYSICAL JOURNAL   Vol. 779 ( 1 )   2013.12

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    Language:Japanese   Publishing type:Research paper (scientific journal)   Publisher:Astrophysical Journal  

    We report the results from X-ray studies of the newly discovered black hole candidate MAXI J1305-704 based on Suzaku and Swift observations in the low/hard and high/soft states, respectively. The long Suzaku observation shows two types of clear absorption dips, both of which recur on a dip interval of 9.74 ± 0.04 hr, which we identify with the orbital period. There is also partially ionized absorption in the nondip (persistent) emission in both the high/soft state and, very unusually, the low/hard state. However, this absorption (in both states) has substantially lower ionization than that seen in other high inclination systems, where the material forms a homogeneous disk wind. Here instead the absorption is most likely associated with clumpy, compact structures associated with the dipping material, which we see uniquely in this source likely because we view it at a very large inclination angle. A large inclination angle is also favored, together with a low black hole mass, to explain the high disk temperature seen in the fairly low luminosity high/soft state, as Doppler boosting enhances the disk temperature at high inclination. The disk radius inferred from these data is significantly smaller than that of the soft component seen in the low/hard state, supporting models where the disk is truncated at low luminosities. We find, however, that the lack of variability power on timescales of ∼50 s in the Suzaku low/hard state data is difficult to explain, even with a low-mass black hole. © 2013. The American Astronomical Society. All rights reserved..

    DOI: 10.1088/0004-637X/779/1/26

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  23. THE 37 MONTH MAXI/GSC SOURCE CATALOG OF THE HIGH GALACTIC-LATITUDE SKY

    Hiroi Kazuo, Ueda Yoshihiro, Hayashida Masaaki, Shidatsu Megumi, Sato Ryosuke, Kawamuro Taiki, Sugizaki Mutsumi, Nakahira Satoshi, Serino Motoko, Kawai Nobuyuki, Matsuoka Masaru, Mihara Tatehiro, Morii Mikio, Nakajima Motoki, Negoro Hitoshi, Sakamoto Takanori, Tomida Hiroshi, Tsuboi Yohko, Tsunemi Hiroshi, Ueno Shiro, Yamaoka Kazutaka, Yoshida Atsumasa, Asada Masato, Eguchi Satoshi, Hanayama Takanori, Higa Masaya, Ishikawa Kazuto, Ishikawa Masaki, Isobe Naoki, Kohama Mitsuhiro, Kimura Masashi, Morihana Kumiko, Nakagawa Yujin E., Nakano Yuki, Nishimura Yasunori, Ogawa Yuji, Sasaki Masayuki, Sugimoto Juri, Takagi Toshihiro, Usui Ryuichi, Yamamoto Takayuki, Yamauchi Makoto, Yoshidome Koshiro

    ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES   Vol. 207 ( 2 )   2013.8

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    Language:Japanese   Publishing type:Research paper (scientific journal)   Publisher:Astrophysical Journal, Supplement Series  

    We present a catalog of high Galactic-latitude (|b| > 10°) X-ray sources detected in the first 37 months of data of the Monitor of All-sky X-ray Image/Gas Slit Camera (MAXI/GSC). To achieve the best sensitivity, we develop a background model of the GSC that well reproduces the data based on the detailed on-board calibration. Source detection is performed through image fits with a Poisson likelihood algorithm. The catalog contains 500 objects detected with significances of s D, 4-10 keV ≥ 7 in the 4-10 keV band. The limiting sensitivity is ≈7.5 × 10-12 erg cm-2 s-1 (≈0.6 mCrab) in the 4-10 keV band for 50% of the survey area, which is the highest ever achieved in an all-sky survey mission covering this energy band. We summarize the statistical properties of the catalog and results from cross matching with the Swift/BAT 70 month catalog, the meta-catalog of X-ray detected clusters of galaxies, and the MAXI/GSC 7 month catalog. Our catalog lists the source name (2MAXI), position and its error, detection significances and fluxes in the 4-10 keV and 3-4 keV bands, the hardness ratio, and the basic information of the likely counterpart available for 296 sources. © 2013. The American Astronomical Society. All rights reserved.

    DOI: 10.1088/0067-0049/207/2/36

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Presentations 1

  1. SPICA Mid-infrared Instrument (SMI): The latest design and specifications

    Wada T.

    Proceedings of SPIE - The International Society for Optical Engineering  2020  Proceedings of SPIE - The International Society for Optical Engineering

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KAKENHI (Grants-in-Aid for Scientific Research) 6

  1. 重力波の電磁波対応天体を観測するための可視光・近赤外線多色同時撮像カメラの製作

    Grant number:20H04734  2020.4 - 2022.3

    新学術領域研究(研究領域提案型)

    森鼻 久美子

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    Authorship:Principal investigator 

    Grant amount:\2470000 ( Direct Cost: \1900000 、 Indirect Cost:\570000 )

    2017年8月に検出された重力波GW170817は、中性子合体による重力波の初めての電磁波対応天体であった。南アフリカ天文台IRSF望遠鏡で、この電磁波対応天体の近赤外線での光度変化、色変化を観測し、理論モデルとの比較からrプロセスで生成される重元素が生成された可能性が示唆された。 しかし、可視光と近赤外線データに時間的な同時性がないため、短時間での色変化は分からなかった。
    そこで本研究では、重力波源の電磁波対応天体の可視近赤外線同時観測をIRSF望遠鏡で可能にするシステムを構築する。IRSF望遠鏡の近赤外線3波長同時観測カメラに可視カメラを搭載し、可視近赤外線5バンド同時撮像観測を可能にする。

  2. 新しいHα輝線天体検出方法による銀河面リッジX線放射を構成する点源天体の研究

    Grant number:19H01939  2019.4 - 2023.3

    永山 貴宏

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    Authorship:Coinvestigator(s) 

    私達が考案した、水素の再結合線Hα(656.3 nm)を放射する輝線星を効率よく探すための、「輝線波長とその両側の近傍波長を同時に観測する」カメラを開発する。このカメラを用いて、銀河面をサーベイ観測し、星全体に対し、Hα輝線星が含まれる割合をHα輝線の等価幅ごとに調べ、輝線星の個数密度を調べる。そして、発見以来30年以上にわたって、起源が分かっていない銀河面リッジX線放射が輝線星(激変星)などの暗いX線天体の重ね合わせで説明可能であるかを検証する。
    本研究は水素原子のHα輝線を放射する星(輝線星)を効率よく発見するための新しいカメラを製作し、そのカメラを用いて輝線星のサーベイ観測を行うことを目的としており、2019年度はこのカメラの基本部品の検討・設計・製作を行った。
    このカメラで最も重要な部品が45度の斜入射でHα輝線(656.3nm)を透過し、その近傍の連続線を反射して切り分ける狭帯域フィルタである。研究開始前から斜入射であることにより、切り分けが難しいことが予想されており、このフィルタの製作が本研究の最大の課題であった。光学薄膜メーカーのシミュレーションによれば、本カメラに適した入射角度(45度)、入射ビーム(F8)では、λ<610nm、および、λ>695nmで入射角度によらず良い反射特性が得られることが分かった。一方、観測天文学の観点から既知の輝線天体のスペクトルを文献で調べ、λ~600nm、および、λ~700nm付近には目立った輝線・吸収線がないことが分かった。そのため、Hα輝線と対とする両脇の波長の中心波長を、λ=605nm、λ=705nmと定め、45度入射でHα輝線付近のみ透過し、λ<610nmおよび、λ>695nmを反射する狭帯域フィルタを製作した。メーカーの出荷時の検査では仕様を満たしており、我々自身による測定はまだ行われていないものの、本カメラの実現に目途が立った。
    並行して、この狭帯域フィルタ、および、F値の変換と光学収差の補正を行うレンズ、CCDカメラを設置する部品の設計と試作を行った。また、使用するCCD検出素子を駆動するためのデジタル回路の設計・製作を行った。
    2019年度の目標は、Hα輝線とそれ以外の波長を切り分ける45度入射の狭帯域フィルタを製作することであった。製作自体は完了できたが、測定は完了していない。
    カメラ光学系を配置・収納する部品も設計と試作までできている。
    以上により、「やや遅れている」と判断した。
    2020年度は、昨年度作成した45度入射Hα狭帯域フィルタの透過・反射特性を測定・評価する。また、F変換・視野補正レンズなどを段階的に組み合わせていき、光学調整と結像性能の評価を行い、設計通りの結像性能が得られるようにする。
    また、検出素子として用いるCCD(KAF-1001)を駆動する小型回路、および、ペルチェを用いた小型真空冷却容器を製作し、KAF-1001の動作試験を行う。あわせて、露出時間を制御する機械式シャッターの製作も行う
    光学系、および、CCDカメラを組み合わせて、総合的な試験を行い、年度の後半に鹿児島大学1m望遠鏡に取り付け、試験観測を行う。試験観測では、望遠鏡に取り付けた状態でのCCDの冷却温度(暗電流)、読み出しノイズ、Hα波長、および連続線波長での結像性能、限界等級を評価する。
    既知の輝線星が含まれる視野の観測を行い、Hα輝線波長、および連続線波長での明るさの比較から、その輝線星が正しく輝線星として選出されるか、また選出できるようにするためにはどのような観測・解析手法が必要かを研究し、最終的には輝線線として検出可能なHα輝線の等価幅を決定し、何がその値を制限しているかを調べる。
    これらの情報をもとに次年度以降の輝線星サーベイの計画を練る。

  3. 近赤外線を用いた銀河面リッジX線放射を構成する天体種族の解明

    Grant number:17K18019  2017.4 - 2021.3

    森鼻 久美子

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    Authorship:Principal investigator 

    Grant amount:\4420000 ( Direct Cost: \3400000 、 Indirect Cost:\1020000 )

    天の川銀河の銀河面に沿って分布する見かけ上拡がったX線放射に銀河面リッジX線放射 (リッジ放射) がある。リッジ放射は数千万度にも及ぶ熱的放射で、X線スペクトル中に電離度の異なる3本の鉄輝線を持つ。リッジ放射は銀河バルジ領域では、暗いX線点源の重ね合わせであることが分かっている。その点源は定性的には磁場を持つ激変星やフレア星が考えられているものの、個々のX線点源の乏しい光子統計のため、個々のX線点源の正体をX線観測のみで調べることが難しい。また、銀河面上の他の領域でも暗いX線点源の重ね合わせで説明可能なのか、真に拡がった高温プラズマが放射起源なのか明らかになっていない。
    そこで本研究は、星間吸収の影響が小さい近赤外線を用いて、銀河面上の激変星探査を行い、リッジ放射の起源を探っている。構成する種族としてこれまで考えられてきた激変星の近赤外線スペクトル中の水素の再結合線 (Paβ 1.28 μm)に着目し、Paβ波長帯にのみ透過幅をもつ狭帯域フィルターと本研究の1年目に製作したPaβ連続光取得用フィルターを用いて銀河面上の深いX線観測がある領域のマッピング観測を行なった。昨年度は悪天候のため、全領域の約2割の観測を終え、今年度は残りの領域のマッピング観測を継続して行ない、全視野の約9割の観測を終えた。観測した領域の視野の測光を行い、激変星候補天体を抽出した。
    さらに、すばる望遠鏡による銀河バルジ領域の近赤外線深観測データの解析により、バルジ領域のX線点源の約50%に近赤外線で対応天体を見つけた。加えて、Gaia衛星DR2により初めてバルジ領域のX線放射の構成点源を視線方向に分解し、近赤外線、X線の性質を合わせて、バルジ領域の放射に寄与する天体種族は、磁場の強い激変星よりも磁場の弱い激変星や非接触型連星系の白色矮性連星系が寄与していることが分かった。
    本研究での観測対象領域であり、チャンドラX線衛星により深いX線観測が行われているNorma arm 領域 (336.5度<銀経<338.5度, -0.4度<銀緯<0.4度、全61視野) を昨年度に引き続きPaβ波長域に透過幅を持つ狭帯域フィルター及びPaβ用連続光取得用フィルターで観測を行なった。その結果、全観測領域の約9割の領域の撮像データを取得することができた。輝線用フィルターと連続光用フィルターでの測光を行い、激変星候補天体を視野ごとに抽出した。
    また、暗いX線点源の重ね合わせでX線放射が説明できる銀河バルジ領域のすばる望遠鏡でのJHKsバンドでの深撮像観測およびGaia衛星DR2のデータを用いて、バルジ領域の暗いX線点源を3次元方向に分解した。また、X線光度と赤外線光度の比から、バルジ領域のX線放射を主に構成しているのは、これまで考えられていた磁場の強い激変星に加えて、磁場の弱い激変星と質量降着率が小さい非接触型連星系をなす白色矮星連星系であることを示唆した。
    今年度の夏に、観測領域の残り1割の視野のデータを取得し、Norma arm領域の全領域の観測を終え、全領域での激変星候補天体を抽出する。抽出した激変星候補天体のX線での性質を合わせて、個々の候補天体が激変星かどうかの判別を行う。
    また、すばる望遠鏡、Gaia衛星での結果をまとめ、銀河バルジ領域の構成種族について投稿論文としてまとめて発表する。

  4. 重力波の電磁波対応天体を観測するための可視光・近赤外線多色同時撮像カメラの製作

    2020.4

    科学研究費補助金 

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    Authorship:Principal investigator 

  5. 新しいHα輝線天体検出方法による銀河面リッジX線放射を構成する点源天体の研究

    2019.4

    科学研究費補助金  基盤研究(B)

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    Authorship:Coinvestigator(s) 

  6. 近赤外線を用いた銀河面リッジX線放射を構成する天体種族の解明

    2017.4

    科学研究費補助金  若手研究(B)

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