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OASA Yumiko
| Natural science course | Associate Professor |
| Graduate School of Education |
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■ Paper- A Novel Survey for Young Substellar Objects with the W-band Filter. VII. Water-bearing Objects in the Core of the ρ Ophiuchi Cloud Complex
Tanvi Sharma; Wen Ping Chen; Beth Biller; Loic Albert; Belinda Damian; Jessy Jose; Bhavana Lalchand; Michael C. Liu; Yumiko Oasa
ASTROPHYSICAL JOURNAL, Volume：980, Number：2, Feb. 2025, [Reviewed], [Last]
We present a study of very low mass stars and brown dwarfs in the rich star-forming core of the rho Ophiuchi cloud complex. The selection of the sample relies on detecting the inherent water absorption characteristic in young substellar objects. Of the 22 water-bearing candidates selected, 15 have a spectral type of M6 or later. Brown dwarf candidates too faint for membership determination by Gaia have their proper motions derived by deep-infrared images spanning 6 yr. Astrometric analysis confirms 21/22 sources as members, with one identified as a contaminant. Infrared colors and the spectral energy distribution of each water-bearing candidate are used to diagnose the mass, age, and possible existence of circumstellar dust. A total of 15 sources exhibit evidence of disks in their spectral energy distributions, as late as in M8-type objects. Spectroscopy for bright candidates has confirmed one as an M8 member and verified two sources (with disks) exhibiting signatures of magnetospheric accretion.
IOP Publishing Ltd, English, Scientific journal
DOI：https://doi.org/10.3847/1538-4357/ada3c3
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DOI ID：10.3847/1538-4357/ada3c3, ISSN：0004-637X, eISSN：1538-4357, SCOPUS ID：85217924727, Web of Science ID：WOS:001421900200001 - The possible long-term periodic variability of the extremely luminous quasar WISE J090924.01+000211.1
Takashi Horiuchi; Yoshiki Toba; Toru Misawa; Katsuhiro L. Murata; Keisuke Isogai; Yoichi Yatsu; Ichiro Takahashi; Mahito Sasada; Masafumi Niwano; Narikazu Higuchi; Shunsuke Hayatsu; Hibiki Seki; Yumiko Oasa; Rikuto Sato
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：77, Number：1, First page：193, Last page：207, Dec. 2024, [Reviewed]
The extremely luminous infrared galaxy (ELIRG), WISE J090924.01+000211.1 (hereafter WISE J0909+0002, z= 1.87) is an extraordinary object with a quasar aspect. This study performed monitoring observations of WISE J0909+0002 with the 105 cm Murikabushi telescope, Okayama and Akeno 50 cm telescopes/MITSUME (g'. R., and L bands), and the SaCRA 55 cm telescope/MuSaSHI (r, i, and z bands) for three years. We obtain the following results by combining the UV/optical light curves of the CRTS, Pan-STARRS, and ZTF archive data, and our observational data: (1) the light curves of WISE J0909+0002 present quasi-periodic (sinusoidal) oscillations with the rest-frame period of similar to 660-689 d; (2) the structure functions of WISE J0909+0002 do not show a damped random walk (DRW) trend; (3) the mock DRW light curves present periodic-like trend on rare occasions in 10000 simulations; (4) the relativistic boost scenario is favored, since the relation between variability amplitude and power-law slope ratio is consistent with the theoretical prediction of this scenario, and a substantial parameter space exists between the inclination angles and the black hole mass; (5) the circumbinary disk model is insufficient to explain the spectral energy distribution of our target; (6) the significant radio flux density of WISE J0909+0002 is not detected from the VLA FIRST Survey, thus the radio jet precession scenario is ruled out. The Doppler boost scenario is, from our results, likely as a cause of the periodic variability; consequently the quasi-periodic oscillations in WISE J0909+0002 is possibly interpreted by a supermassive black hole binary. Additional observations to investigate the continuity of the periodic trend would bring new insights into mechanisms of the quasi-periodic oscillations and/or ELIRGS.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/psae109
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DOI ID：10.1093/pasj/psae109, ISSN：0004-6264, eISSN：2053-051X, SCOPUS ID：85217204398, Web of Science ID：WOS:001385107500001 - MASTER OT J030227.28+191754.5: An unprecedentedly energetic dwarf nova outburst
Yusuke Tampo; Taichi Kato; Keisuke Isogai; Mariko Kimura; Naoto Kojiguchi; Daisaku Nogami; Junpei Ito; Masaaki Shibata; Masayuki Yamanaka; Kenta Taguchi; Hiroyuki Maehara; Hiroshi Itoh; Katsura Matsumoto; Momoka Nakagawa; Yukitaka Nishida; Shawn Dvorak; Katsuhiro L. Murata; Ryohei Hosokawa; Yuri Imai; Naohiro Ito; Masafumi Niwano; Shota Sato; Ryotaro Noto; Ryodai Yamaguchi; Malte Schramm; Yumiko Oasa; Takahiro Kanai; Yu Sasaki; Tamas Tordai; Tonny Vanmunster; Seiichiro Kiyota; Nataly Katysheva; Sergey Yu Shugarov; Alexandra M. Zubareva; Sergei Antipin; Natalia Ikonnikova; Alexandr Belinski; Pavol A. Dubovsky; Tomas Medulka; Jun Takahashi; Masaki Takayama; Tomohito Ohshima; Tomoki Saito; Miyako Tozuka; Shigeyuki Sako; Masaomi Tanaka; Nozomu Tominaga; Takashi Horiuchi; Hidekazu Hanayama; Daniel E. Reichart; Vladimir V. Kouprianov; James W. Davidson; Daniel B. Caton; Filipp D. Romanov; David J. Lane; Franz-Josef Hambsch; Norio Narita; Akihiko Fukui; Masahiro Ikoma; Motohide Tamura; Koji S. Kawabata; Tatsuya Nakaoka; Ryo Imazawa
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：76, Number：6, First page：1228, Last page：1245, Oct. 2024, [Reviewed]
We present a detailed study of the MASTER OT J030227.28+191754.5 outburst in 2021-2022, which reached an amplitude of 10.2mag and a duration of 60d. The detections of (1) the double-peaked optical emission lines, and (2) the early and ordinary superhumps, established that MASTER OT J030227.28+191754.5 is an extremely energetic WZ Sge-type dwarf nova (DN). Based on the superhump observations, we obtained its orbital period and mass ratio as 0.05986(1)d and 0.063(1), respectively. These values are within a typical range for low-mass-ratio DNe. According to the binary parameters derived based on the thermal-tidal instability model, our analyses showed that (1) the standard disk model requires an accretion rate similar or equal to 1020gs(-1) to explain its peak optical luminosity, and (2) large mass was stored in the disk at the outburst onset. These factors cannot be explained solely by the impact of its massive (greater than or similar to 1.15M(circle dot)) primary white dwarf implied by Kimura et al. (2023, ApJ, 951, 124). Instead, we propose that the probable origin of this enormously energetic DN outburst is the even lower quiescence viscosity than other WZ Sge-type DNe. This discussion is qualitatively valid for most possible binary parameter spaces unless the inclination is low enough (less than or similar to 40 degrees) for the disk to be bright, explaining the outburst amplitude. Such low inclinations, however, would not allow detectable amplitude of early superhumps in the current thermal-tidal instability model. The optical spectra at outburst maximum showed strong emission lines of the Balmer, He i, and He ii series, the core of which is narrower than similar to 800kms(-1). Considering its binary parameters, a Keplerian disk cannot explain this narrow component, but the presumable origin is disk winds.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/psae082
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DOI ID：10.1093/pasj/psae082, ISSN：0004-6264, eISSN：2053-051X, SCOPUS ID：85212857821, Web of Science ID：WOS:001331590900001 - Internal 1000 au Scale Structures of the R CrA Cluster-forming Cloud. I. Filamentary Structures
Kengo Tachihara; Naofumi Fukaya; Kazuki Tokuda; Yasumasa Yamasaki; Takeru Nishioka; Daisei Abe; Tsuyoshi Inoue; Naoto Harada; Ayumu Shoshi; Shingo Nozaki; Asako Sato; Mitsuki Omura; Kakeru Fujishiro; Misato Fukagawa; Masahiro N. Machida; Takahiro Kanai; Yumiko Oasa; Toshikazu Onishi; Kazuya Saigo; Yasuo Fukui
ASTROPHYSICAL JOURNAL, Volume：968, Number：2, Jun. 2024, [Reviewed]
We report Atacama Large Millimeter/submillimeter Array/Atacama Compact Array observations of a high-density region of the Corona Australis cloud forming a young star cluster, and the results of resolving internal structures. In addition to embedded Class 0/I protostars in the continuum, a number of complex dense filamentary structures are detected in the (CO)-O-18 and SO lines by the 7 m array. These are substructures of the molecular clump that are detected by the total power array as extended emission. We identify 101 and 37 filamentary structures with widths of a few thousand astronomical units in (CO)-O-18 and SO, respectively, which are called feathers. The typical column density of the feathers in (CO)-O-18 is about 10(22) cm(-2), and the volume density and line mass are similar to 10(5) cm(-3) and a few M-circle dot pc(-1), respectively. This line mass is significantly smaller than the critical line mass expected for cold and dense gas. These structures have complex velocity fields, indicating a turbulent interior. The number of feathers associated with Class 0/I protostars is only similar to 10, indicating that most of them do not form stars but rather are transient structures. The formation of feathers can be interpreted as a result of colliding gas flow because the morphology is well reproduced by MHD simulations, and this is supported by the presence of H I shells in the vicinity. The colliding gas flows may accumulate gas and form filaments and feathers, and trigger the active star formation of the R CrA cluster.
IOP Publishing Ltd, English, Scientific journal
DOI：https://doi.org/10.3847/1538-4357/ad40a6
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DOI ID：10.3847/1538-4357/ad40a6, ISSN：0004-637X, eISSN：1538-4357, SCOPUS ID：85196793698, Web of Science ID：WOS:001250763800001 - Evolution of accretion disk structure of the black hole X-ray binary MAXI J1820+070 during the rebrightening phase
Tomohiro Yoshitake; Megumi Shidatsu; Yoshihiro Ueda; Daisaku Nogami; Katsuhiro L. Murata; Narikazu Higuchi; Keisuke Isogai; Hiroyuki Maehara; Shin Mineshige; Hitoshi Negoro; Nobuyuki Kawai; Yoichi Yatsu; Mahito Sasada; Ichiro Takahashi; Masafumi Niwano; Tomoki Saito; Masaki Takayama; Yumiko Oasa; Takuya Takarada; Takumi Shigeyoshi
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：76, Number：2, First page：251, Last page：264, Apr. 2024, [Reviewed]
To understand the evolution of global accretion disk structure in the "rebrightening" phase of MAXI J1820+070, we perform a comprehensive analysis of its near infrared/optical/UV to X-ray spectral energy distribution (SED) utilizing data obtained by OISTER, Las Cumbres Observatory (LCO), Swift, NICER, and NuSTAR in 2019. Optical spectra observed with Seimei telescope in 2019 and 2020 are also analyzed. On the basis of the optical and X-ray light curves and their flux ratios, we divide the whole phase into three periods, Periods I (flux rise), II (decay), and III (dim). In the first two periods, the source stayed in the low/hard state (LHS), where the X-ray (0.3-30 keV) and optical/UV SED can both be fitted with power-law models. We interpret that the X-ray emission arises from hot corona via Comptonization, whereas the optical/UV flux is dominated by synchrotron radiation from the jets, with a partial contribution from the irradiated disk. The optical/UV power-law component smoothly connects to a simultaneous radio flux, supporting its jet origin. Balmer line profiles in the optical spectra indicate that the inner radius of an irradiated disk slightly decreased from similar to 2 x 10(5)r(g) (Period I) to similar to 1 x 10(5)r(g) (Period II), where r(g) is the gravitational radius, implying a change of the hot corona geometry. In Period III, the SED can be reproduced by an advection-dominated accretion flow and jet emission. However, the double-peaked H alpha emission line indicates that a cool disk remained at large radii.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/psae005
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DOI ID：10.1093/pasj/psae005, ISSN：0004-6264, eISSN：2053-051X, SCOPUS ID：85189938201, Web of Science ID：WOS:001158737100001 - Research and education experience using the SaCRA telescope for the teacher training undergraduate students
大朝 由美子
Volume：未定, 2024
International conference proceedings - Continuous research on understanding and interests in astronomy for prospective teacher students: Changes over the decade
大朝由美子
Stars and Galaxies (Web), Volume：6, First page：8, Dec. 2023, [Reviewed]
This paper aims to investigate the the fundamental knowledge, comprehension, awareness, and interest in the realm of astronomy among university students aspiring to become teachers. We have conducted questionnaire surveys from 2013 to 2023 among 3432 students in the Faculty of Education, a teacher-training department, in order to assess their interest in science and astronomy and their understanding of astronomical concepts studied during elementary/junior-high school. As a result, there has been a consistent interest around 80-90% in science among education and science major students over the past decade. There appears to be no clear trend of “decline in students’ positive attitude toward science” during this period. While there was a relatively high retention of knowledge regarding diurnal/annual motions and the classification of the Sun and Moon, there was a lower comprehension of astrophysical characteristics. From comparisons of the percentage of correct responses, interest in science/astronomy, direct experiences in astronomical observations using telescopes and/or gazing our Milky Way, and learning “earth science” in high school, it was found that there existed a discernible gap in understanding astrophysical characteristics, while there were no significant differences in understanding diurnal/annual motions and the classification of the Sun/Moon. The logistic regression analyses on the students’ interests, experiences, and understanding of astronomy indicated that direct experiences, interests, and/or curiosity in astronomy, as well as studying “earth science” in high school, could have a impact on knowledge and understanding of astronomy. Furthermore, a comparison between first-year and subsequent years’ surveys for science major students aspiring to become science teachers at elementary, junior high, and high schools revealed a progressive improvement in understanding. The results suggest that studying astronomy during university, often considered the final opportunity to learn astronomy, could significantly contribute to nurturing essential knowledge and scientific literacy for teachers. In summary, in order to enhance and retain the fundamental understanding of astronomy among university students in teacher training programs, it is recommended to implement the following strategies: （1） observational experiences and hands-on learning utilizing telescopes, （2） studying “earth science （basic）” in high school, and （3） educational practices involving astronomical observations at the university level.
Center for Astronomy, University of Hyogo, Japanese
DOI：https://doi.org/10.32231/starsandgalaxies.6.0_8
DOI ID：10.32231/starsandgalaxies.6.0_8, ISSN：2434-270X, eISSN：2434-270X, J-Global ID：202402244940085525 - Chromospheric activities of pre-main-sequence stars
Mai Yamashita; Yoichi Itoh; Yuhei Takagi; Yumiko Oasa
Proceedings of the International Astronomical Union, Volume：19, Number：S365, First page：368, Last page：374, Dec. 2023
We investigated chromospheric activities of pre-main-sequence (PMS) stars. First, we studied the Ca II infrared triplet emission lines with Subaru/HDS and other spectroscopic instruments. Most PMS stars have narrow Ca II lines whose intensities are as large as the maximum of the zero-age main-sequence (ZAMS) stars. The chromosphere of PMS stars is suggested to be filled by the Ca II emitting region. Second, we found many faint chromospheric emission lines such as Mg I and Fe I for more than half of the ZAMS stars. Third, we searched the periodic light variation caused by a starspot for the 26 PMS stars. Their TESS light variations and Ca II emission line strengths show the positive correlation, and are located on the extensions of the superflare stars. In summary, PMS stars have very active chromosphere driven by strong dynamo process due to the fast rotation and the long convection timescale.
International conference proceedings
DOI：https://doi.org/10.1017/S1743921323005392
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DOI ID：10.1017/S1743921323005392, ISSN：1743-9213, eISSN：1743-9221, SCOPUS ID：85217101385 - A Novel Survey for Young Substellar Objects with the W-band Filter. VI. Spectroscopic Census of Substellar Members and the IMF of the σ Orionis Cluster
Belinda Damian; Jessy Jose; Beth Biller; Gregory J. Herczeg; Loic Albert; Katelyn Allers; Zhoujian Zhang; Michael C. C. Liu; Sophie Dubber; K. T. Paul; Wen-Ping Chen; Bhavana Lalchand; Tanvi Sharma; Yumiko Oasa
ASTROPHYSICAL JOURNAL, Volume：951, Number：2, Jul. 2023, [Reviewed]
Low-mass stars and substellar objects are essential in tracing the initial mass function (IMF). We study the nearby young & sigma; Orionis cluster (d & SIM; 408 pc, age & SIM; 1.8 Myr) using deep near-infrared (NIR) photometric data in the J, W, and H bands from WIRCam on the Canada-France-Hawaii Telescope. We use the water absorption feature to select brown dwarfs photometrically and confirm their nature spectroscopically with IRTF-SpeX. Additionally we select candidate low-mass stars for spectroscopy and analyze their membership and those of literature sources using astrometry from Gaia DR3. We obtain NIR spectra for 28 very-low-mass stars and brown dwarfs and estimate their spectral type between M3 and M8.5 (masses ranging between 0.3 and 0.01 M (& ODOT;)). Apart from these, we also identify five new planetary-mass candidates which require further spectroscopic confirmation of youth. We compile a comprehensive catalog of 170 spectroscopically confirmed members in the central region of the cluster, for a wide mass range of & SIM;19-0.004 M (☉). We estimate the star-to-brown-dwarf ratio to be & SIM;4, within the range reported for other nearby star-forming regions. With the updated catalog of members we trace the IMF down to 4 M (Jup) and we find that a two-segment power law fits the substellar IMF better than a log-normal distribution.
IOP Publishing Ltd, English, Scientific journal
DOI：https://doi.org/10.3847/1538-4357/acd115
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DOI ID：10.3847/1538-4357/acd115, ISSN：0004-637X, eISSN：1538-4357, SCOPUS ID：85165409811, Web of Science ID：WOS:001026196200001 - Multicolor and multi-spot observations of Starlink's Visorsat
Takashi Horiuchi; Hidekazu Hanayama; Masatoshi Ohishi; Tatsuya Nakaoka; Ryo Imazawa; Koji S. Kawabata; Jun Takahashi; Hiroki Onozato; Tomoki Saito; Masayuki Yamanaka; Daisaku Nogami; Yusuke Tampo; Naoto Kojiguchi; Jumpei Ito; Masaaki Shibata; Malte Schramm; Yumiko Oasa; Takahiro Kanai; Kohei Oide; Katsuhiro L. Murata; Ryohei Hosokawa; Yutaka Takamatsu; Yuri Imai; Naohiro Ito; Masafumi Niwano; Seiko Takagi; Tatsuharu Ono; Vladimir V. Kouprianov
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：75, Number：3, First page：584, Last page：606, Jun. 2023
This study provides the results of simultaneous multicolor observations for the first Visorsat (STARLINK-1436) and the ordinary Starlink satellite (STARLINK-1113) in the U, B, V, g, r, i, RC, IC, z, J, H, and K-s bands to quantitatively investigate the extent to which Visorsat reduces its reflected light. Our results are as follows: (1) in most cases, Visorsat is fainter than STARLINK-1113, and the sunshade on Visorsat therefore contributes to the reduction of the reflected sunlight; (2) the magnitude at 550 km altitude (normalized magnitude) of both satellites often reaches the naked-eye limiting magnitude (<6.0); (3) from a blackbody radiation model of the reflected flux, the peak of the reflected components of both satellites is around the z band; and (4) the albedo of the near-infrared range is larger than that of the optical range. Under the assumption that Visorsat and STARLINK-1113 have the same reflectivity, we estimate the covering factor, Cf, of the sunshade on Visorsat, using the blackbody radiation model: the covering factor ranges from 0.18 <= C-f <= 0.92. From the multivariable analysis of the solar phase angle (Suntarget-observer), the normalized magnitude, and the covering factor, the phase angle versus covering factor distribution presents a moderate anti-correlation between them, suggesting that the magnitudes of Visorsat depend not only on the phase angle but also on the orientation of the sunshade along our line of sight. However, the impact on astronomical observations from Visorsat-designed satellites remains serious. Thus, new countermeasures are necessary for the Starlink satellites to further reduce reflected sunlight.y
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/psad021
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DOI ID：10.1093/pasj/psad021, ISSN：0004-6264, eISSN：2053-051X, SCOPUS ID：85171739652, Web of Science ID：WOS:000965502500001 - A Novel Survey for Young Substellar Objects with the W-band Filter. V. IC 348 and Barnard 5 in the Perseus Cloud
Bhavana Lalchand; Wen-Ping Chen; Beth A. Biller; Loic Albert; Katelyn Allers; Sophie Dubber; Zhoujian Zhang; Michael C. Liu; Jessy Jose; Belinda Damian; Tanvi Sharma; Mickael Bonnefoy; Yumiko Oasa
ASTRONOMICAL JOURNAL, Volume：164, Number：4, Oct. 2022, [Reviewed]
We report the discovery of substellar objects in the young star cluster IC 348 and the neighboring Barnard 5 dark cloud, both at the eastern end of the Perseus star-forming complex. The substellar candidates are selected using narrowband imaging, i.e., on and off photometric technique with a filter centered around the water absorption feature at 1.45 mu m, a technique proven to be efficient in detecting water-bearing substellar objects. Our spectroscopic observations confirm three brown dwarfs in IC 348. In addition, the source WBIS 03492858+3258064, reported in this work, is the first confirmed brown dwarf discovered toward Barnard 5. Together with the young stellar population selected via near- and mid-infrared colors using the Two Micron All Sky Survey and the Wide-field Infrared Survey Explorer, we diagnose the relation between stellar versus substellar objects with the associated molecular clouds. Analyzed by Gaia EDR3 parallaxes and kinematics of the cloud members across the Perseus region, we propose the star formation scenario of the complex under influence of the nearby OB association.
IOP Publishing Ltd, English, Scientific journal
DOI：https://doi.org/10.3847/1538-3881/ac8547
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DOI ID：10.3847/1538-3881/ac8547, ISSN：0004-6256, eISSN：1538-3881, arXiv ID：arXiv:2208.08637, SCOPUS ID：85137776787, Web of Science ID：WOS:000850355400001 - Multiwavelength observations of the black hole X-ray binary MAXI J1820+070 in the rebrightening phase
Tomohiro Yoshitake; Megumi Shidatsu; Yoshihiro Ueda; Shin Mineshige; Katsuhiro L. Murata; Ryo Adachi; Hiroyuki Maehara; Daisaku Nogami; Hitoshi Negoro; Nobuyuki Kawai; Masafumi Niwano; Ryohei Hosokawa; Tomoki Saito; Yumiko Oasa; Takuya Takarada; Takumi Shigeyoshi
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：74, Number：4, First page：805, Last page：814, Aug. 2022
We report the results of quasi-simultaneous multiwavelength (near-infrared, optical, UV, and X-ray) observations of the Galactic X-ray black hole binary MAXI J1820+070 performed in 2019 May 10-13, similar to 60d after the onset of the first rebrightening phase. It showed a much larger optical-to-X-ray luminosity ratio (similar to 8) than in the initial outburst epoch. The primary components of the spectral energy distribution (SED) can be best interpreted by a radiatively inefficient accretion flow (RIAF) spectrum showing a luminosity peak in the optical band. By comparison with theoretical calculations, we estimate the mass accretion rate to be (M)over dot/(8L(Edd)/c(2)) similar to 10(-3), where c is the light speed and L-Edd is the Eddington luminosity. In addition to the RIAF emission, a blue power-law component is detected in the optical-UV SED, which is most likely synchrotron radiation from the jet. The optical spectrum taken at the Seimei telescope shows a weak and narrow H alpha emission line, the emitting region of which is constrained to be greater than or similar to 2 x 10(4) times the gravitational radius. We suggest that the entire disk structure cannot be described by a single RIAF solution but cooler material responsible for the H alpha emission must exist at the outermost region.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/psac038
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DOI ID：10.1093/pasj/psac038, ISSN：0004-6264, eISSN：2053-051X, arXiv ID：arXiv:2412.11442, SCOPUS ID：85136302451, Web of Science ID：WOS:000805625400001 - Characterizing atmospheric composition of the extrasolar planets estimated by the multiwavelength transit observations
大朝 由美子
Volume：1, First page：29, Last page：30, 2022
Scientific journal - Optical and near-infrared multiple wavelength observational studies of pre-main sequence stars
大朝 由美子
Volume：1, First page：27, Last page：28, 2022
Scientific journal - ASASSN-18aan: An eclipsing SU UMa-type cataclysmic variable with a 3.6-hr orbital period and a late G-type secondary star
Yasuyuki Wakamatsu; John R. Thorstensen; Naoto Kojiguchi; Keisuke Isogai; Mariko Kimura; Ryuhei Ohnishi; Taichi Kato; Hiroshi Itoh; Yuki Sugiura; Sho Sumiya; Hanami Matsumoto; Daiki Ito; Kengo Nikai; Hiroshi Akitaya; Chihiro Ishioka; Kohei Oide; Takahiro Kanai; Yoshinori Uzawa; Yumiko Oasa; Tamas Tordai; Tonny Vanmunster; Sergey Yu Shugarov; Masayuki Yamanaka; Mahito Sasada; Kengo Takagi; Yuki Nishinaka; Yuina Yamazaki; Ikki Otsubo; Tatsuya Nakaoka; Katsuhiro L. Murata; Ryou Ohsawa; Masahiro Morita; Makoto Ichiki; Sjoerd Dufoer; Masanori Mizutani; Takashi Horiuchi; Miyako Tozuka; Masaki Takayama; Tomohito Ohshima; Tomoki Saito; Pavol A. Dubovsky; Geoff Stone; Ian Miller; Daisaku Nogami
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：73, Number：5, First page：1209, Last page：1224, Oct. 2021
We report photometric and spectroscopic observations of the eclipsing SU UMa-type dwarf nova ASASSN-18aan. We observed the 2018 superoutburst with 2.3 mag brightening and found the orbital period (P-orb) to be 0.149454(3) d, or 3.59 hr. This is longward of the period gap, establishing ASASSN-18aan as one of a small number of long-Porb SU UMa-type dwarf novae. The estimated mass ratio, [q = M-2/M-1 = 0.278(1)], is almost identical to the upper limit of tidal instability by the 3: 1 resonance. From eclipses, we found that the accretion disk at the onset of the superoutburst may reach the 3: 1 resonance radius, suggesting that the superoutburst of ASASSN-18aan results from the tidal instability. Considering the case of long-P-orb WZ Sge-type dwarf novae, we suggest that the tidal dissipation at the tidal truncation radius is enough to induce SU UMa-like behavior in relatively high-q systems such as SU UMa-type dwarf novae, but that this is no longer effective in low-q systems such as WZ Sge-type dwarf novae. The unusual nature of the system extends to the secondary star, for which we find a spectral type of G9, much earlier than typical for the orbital period, and a secondary mass M-2 of around 0.18 M-circle dot, smaller than expected for the orbital period and the secondary's spectral type. We also see indications of enhanced sodium abundance in the secondary's spectrum. Anomalously hot secondaries are seen in a modest number of other CVs and related objects. These systems evidently underwent significant nuclear evolution before the onset of mass transfer. In the case of ASASSN-18aan, this apparently resulted in a mass ratio lower than typically found at the system's P-orb, which may account for the occurrence of a superoutburst at this relatively long period.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/psab003
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DOI ID：10.1093/pasj/psab003, ISSN：0004-6264, eISSN：2053-051X, SCOPUS ID：85117316138, Web of Science ID：WOS:000708521000003 - J-GEM optical and near-infrared follow-up of gravitational wave events during LIGO's and Virgo's third observing run
Mahito Sasada; Yousuke Utsumi; Ryosuke Itoh; Nozomu Tominaga; Masaomi Tanaka; Tomoki Morokuma; Kenshi Yanagisawa; Koji S. Kawabata; Takayuki Ohgami; Michitoshi Yoshida; Fumio Abe; Ryo Adachi; Hiroshi Akitaya; Yang Chong; Kazuki Daikuhara; Ryo Hamasaki; Satoshi Honda; Ryohei Hosokawa; Kota Iida; Fumiya Imazato; Chihiro Ishioka; Takumi Iwasaki; Mingjie Jian; Yuhei Kamei; Takahiro Kanai; Hidehiro Kaneda; Ayane Kaneko; Noriyuki Katoh; Nobuyuki Kawai; Keiichiro Kubota; Yuma Kubota; Hideo Mamiya; Kazuya Matsubayashi; Kumiko Morihana; Katsuhiro L. Murata; Takahiro Nagayama; Noriatsu Nakamura; Tatsuya Nakaoka; Yuu Niino; Yuki Nishinaka; Masafumi Niwano; Daisaku Nogami; Yumiko Oasa; Miki Oeda; Futa Ogawa; Ryou Ohsawa; Kouji Ohta; Kohei Oide; Hiroki Onozato; Shigeyuki Sako; Tomoki Saito; Yuichiro Sekiguchi; Toshikazu Shigeyama; Takumi Shigeyoshi; Minori Shikauchi; Kazuki Shiraishi; Daisuke Suzuki; Kengo Takagi; Jun Takahashi; Takuya Takarada; Masaki Takayama; Himeka Takeuchi; Yasuki Tamura; Ryoya Tanaka; Sayaka Toma; Miyako Tozuka; Nagomi Uchida; Yoshinori Uzawa; Masayuki Yamanaka; Moeno Yasuda; Yoichi Yatsu
PROGRESS OF THEORETICAL AND EXPERIMENTAL PHYSICS, Volume：2021, Number：5, May 2021
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 similar to 100 Mpc with a probability area of <= 500 deg(2).
OXFORD UNIV PRESS INC, English, Scientific journal
DOI：https://doi.org/10.1093/ptep/ptab007
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DOI ID：10.1093/ptep/ptab007, ISSN：2050-3911, eISSN：2050-3911, SCOPUS ID：85109454577, Web of Science ID：WOS:000671556400010 - Multi-wavelength photometry during the 2018 superoutburst of the WZ Sge-type dwarf nova EG Cancri
Mariko Kimura; Keisuke Isogai; Taichi Kato; Naoto Kojiguchi; Yasuyuki Wakamatsu; Ryuhei Ohnishi; Yuki Sugiura; Hanami Matsumoto; Sho Sumiya; Daiki Ito; Kengo Nikai; Katsura Matsumoto; Sergey Yu Shugarov; Natalia Katysheva; Hiroshi Itoh; Pavol A. Dubovsky; Igor Kudzej; Hiroshi Akitaya; Kohei Oide; Takahiro Kanai; Chihiro Ishioka; Yoshinori Uzawa; Yumiko Oasa; Tonny Vanmunster; Arto Oksanen; Tamas Tordai; Katsuhiro L. Murata; Kazuki Shiraishi; Ryo Adachi; Motoki Oeda; Yutaro Tachibana; Seiichiro Kiyota; Elena P. Pavlenko; Kirill Antonyuk; Oksana Antonyuk; Nikolai Pit; Aleksei Sosnovskij; Julia Babina; Alex Baklanov; Koji S. Kawabata; Miho Kawabata; Tatsuya Nakaoka; Masayuki Yamanaka; Kiyoshi Kasai; Ian Miller; Stephen M. Brincat; Wei Liu; Mahito Sasada; Daisaku Nogami
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：73, Number：1, First page：1, Last page：13, Feb. 2021
We report on the multi-wavelength photometry of the 2018 superoutburst in EG Cnc. We have detected stage A superhumps and long-lasting late-stage superhumps via the optical photometry and have constrained the binary mass ratio and its possible range. The median value of the mass ratio is 0.048 and the upper limit is 0.057, which still implies that EG Cnc is one of the possible candidates for period bouncers. This object also showed multiple rebrightenings in this superoutburst which are the same as those in its previous superoutburst in 1996-1997, despite the difference in the main superoutburst. This would represent that the rebrightening type is inherent to each object and is independent of the initial disk mass at the beginning of superoutbursts. We also found that B - I and J - K-s colors were unusually red just before the rebrightening phase and became bluer during the quiescence between rebrightenings, which would mean that the low-temperature mass reservoir at the outermost disk accreted with time after the main superoutburst. Also, the ultraviolet flux was sensitive to rebrightenings as well as the optical flux, and the U - B color became redder during the rebrightening phase, which would indicate that the inner disk became cooler when this object repeated rebrightenings. Our results thus basically support the idea that the cool mass reservoir in the outermost disk is responsible for rebrightenings.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/psaa089
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DOI ID：10.1093/pasj/psaa089, ISSN：0004-6264, eISSN：2053-051X, SCOPUS ID：85121825894, Web of Science ID：WOS:000640917300001 - FOREST unbiased Galactic plane imaging survey with the Nobeyama 45 m telescope (FUGIN). VII. Molecular fraction of H i clouds
Hiroyuki Nakanishi; Shinji Fujita; Kengo Tachihara; Natsuko Izumi; Mitsuhiro Matsuo; Tomofumi Umemoto; Yumiko Oasa; Tsuyoshi Inoue
Publications of the Astronomical Society of Japan, Volume：72, Number：3, Jun. 2020
We analyze molecular-gas formation in neutral atomic hydrogen (H i) clouds using the latest CO data, obtained from the FOREST (four-beam receiver system on the 45 m telescope) unbiased Galactic plane imaging survey with the Nobeyama 45 m telescope, and using H i data taken from the Very Large Array Galactic plane survey. We applied a dendrogram algorithm to the H i data cube to identify H i clouds, and we calculated the H i mass and molecular-gas mass by summing the CO line intensity within each H i cloud. On the basis of the results, we created a catalog of 5737 identified H i clouds with local standard of rest (LSR) velocity of VLSR ≤-20 km s-1 in galactic longitude and latitude ranges of 20° ≤ l ≤ 50° and-1° ≤ b ≤ 1°, respectively. We found that most of the H i clouds are distributed within a Galactocentric distance of 16 kpc, and most of them are in the cold neutral medium phase. In addition, we determined that the high-mass end of the H i mass function is fitted well with a power-law function with an index of 2.3. Although two sequences of self-gravitating and diffuse clouds are expected to appear in the M tot-$M-{\,{\rm H}-2}$ diagram according to previous works based on a plane-parallel model, the observational data show only a single sequence with large scattering within these two sequences. This implies that most of the clouds are mixtures of these two types of clouds. Moreover, we suggest the following scenario of molecular-gas formation: An H i-dominant cloud evolved with increasing H2 mass along a path of $M-{\,{\rm H}-2} \propto M-{\,\rm tot}^2$ by collecting diffuse gas before reaching and moving along the curves of the two sequences.
Scientific journal
DOI：https://doi.org/10.1093/pasj/psaa027
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DOI ID：10.1093/pasj/psaa027, ISSN：0004-6264, eISSN：2053-051X, SCOPUS ID：85089679353 - Spectroscopic Survey of Hα Emission Line Stars Associated with Bright Rimmed Clouds
Kensuke Hosoya; Yoichi Itoh; Yumiko Oasa; Ranjan Gupta; Asoke Kumar Sen
Volume：09, Number：02, First page：154, Last page：471, May 2020
The results of a spectroscopic survey of H alpha emission line stars
associated with fourteen bright rimmed clouds are presented. Slit-less optical
spectroscopy was carried out with the Inter University Centre for Astronomy and
Astrophysics (IUCAA) 2m telescope and IUCAA Faint Object Spectrograph and
Camera (IFOSC). H alpha emission line was detected from 173 objects. Among them
85 objects have a strong H alpha emission line with its equivalent width larger
than 10 A. Those are classical T Tauri stars. 52 objects have a weak H alpha
emission line with its equivalent width less than 10 A and do not show
intrinsic near-infrared excess. Those are weak-line T Tauri stars. On the other
hand, 36 objects have a weak H alpha emission line (<10 A), although they show
intrinsic near-infrared excess. Such objects are not common in low-mass star
forming regions. Those are misfits of the general concept on formation process
of a low-mass star, in which it evolves from a classical T Tauri star to a
weak-line T Tauri star. Those might be weak-line T Tauri stars with a flared
disk in which gas is heated by ultraviolet radiation from a nearby early-type
star. Alternatively, we propose pre-transitional disk objects as their
evolutional stage.
DOI：https://doi.org/10.4236/ijaa.2019.92012
DOI ID：10.4236/ijaa.2019.92012, ISSN：2161-4717, eISSN：2161-4725, arXiv ID：arXiv:2006.00219 - A Novel Survey for Young Substellar Objects with the W-band Filter. II. The Coolest and Lowest Mass Members of the Serpens-South Star-forming Region
Jessy Jose; Beth A. Biller; Loic Albert; Sophie Dubber; Katelyn Allers; Gregory J. Herczeg; Michael C. Liu; Samuel Pearson; Bhavana Lalchand; Wen-Ping Chen; Mickael Bonnefoy; Etienne Artigau; Philippe Delorme; Po-shih Chiang; Zhoujian Zhang; Yumiko Oasa
ASTROPHYSICAL JOURNAL, Volume：892, Number：2, Apr. 2020
Given its relative proximity (similar to 430 pc), compact size (<20 '), young age (similar to 0.5 Myr), and rich number of young stellar objects, the Serpens-South star-forming region is a promising site for studying young substellar objects, yet the low-mass members of this region remain largely undiscovered. In this article we report on a deep photometric survey using a custom 1.45 mu m filter (W band), as well as standard J and H near-IR filters, in order to identify candidate low-mass young brown dwarfs in the Serpens-South region. We constructed a reddening-insensitive index (Q) by combining J, H and W-band photometry for survey objects, in order to identify candidate low-mass members of Serpens based on the strength of the water-absorption feature at 1.45 mu m in the atmospheres of mid-M and later objects. We then conducted spectroscopic follow-up to confirm youth and spectral type for our candidates. This is the first survey to identify the very low-mass and coolest members of Serpens-South. We identify four low-mass candidate Serpens members, which all display IR excess emission, indicating the likely presence of circumstellar disks around them. One of the four candidate low-mass members in our list, SERP182918-020245, exhibits Pa beta and Br gamma emission features, confirming its youth and ongoing magnetospheric accretion. Our new candidate members have spectral types >M4 and are the coolest and lowest mass candidate members yet identified in Serpens-South.
IOP PUBLISHING LTD, English, Scientific journal
DOI：https://doi.org/10.3847/1538-4357/ab74dd
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85085116787&origin=inward
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DOI ID：10.3847/1538-4357/ab74dd, ISSN：0004-637X, eISSN：1538-4357, SCOPUS ID：85085116787, Web of Science ID：WOS:000523729300001 - Multi-wavelength SimultaneouS High throughput Imager and polarimeter (MuSaSHI) : development and its performance
Yumiko Oasa; Kazutoshi Ushioda; Yoshiki Shibata; Genta Seino; Masaru Kino; Hiroshi Akitaya
GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY VIII, Volume：11447, 2020
We describe a development and performance evaluations for Multi-wavelength SimultaneouS High throughput Imager and polarimeter called as "MuSaSHI" . The science drivers are high-precision muticolor photometric studies of time-variable astronomical phenomena such as variable stars, transiting planets and asteroids. MuSaSHI is designed to be mounted on the SaCRA telescope at Saitama University, dedicated for relatively wide field imaging and polarimetry in the three optical bands (r: 550 to 680 nm, i: 700 to 810 nm, z: 820 to 1000 nm) . The instrument is equipped with three Back-Illuminated thinned e2v CCDs which provide simultaneous r, i , z images having a field of view of 12.8 x 12.4 arcmin with a pixel scale of 0.73 arcsec. The optical system of MuSaSHI is composed of only two dichroic mirrors and three bandpass filters without lens, so that the total throughput is high especially at z band (similar to 50%). In addition, the optics of MuSaSHI is designed for fast telescopes (F similar to 6.5) and with portability in mind so that it is able to be mounted on a larger aperture telescope with slower beam. The limiting magnitudes with 60 sec integration (10 sigma) are r(lim) = 16.8, in(lim) = 17.1, and z(lim) = 17.2 mag. We demonstrate relative photometric precisions of < 0.1 % in the all bands for a KO V star WASP-84 which hosts a transiting planet with 30s exposure observations.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.2560903
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DOI ID：10.1117/12.2560903, ISSN：0277-786X, eISSN：1996-756X, SCOPUS ID：85107502029, Web of Science ID：WOS:000850778200111 - Extremely Dense Cores Associated with Chandra Sources in Ophiuchus A: Forming Brown Dwarfs Unveiled?
Ryohei Kawabe; Chihomi Hara; Fumitaka Nakamura; Kazuya Saigo; Takeshi Kamazaki; Yoshito Shimajiri; Kengo Tomida; Shigehisa Takakuwa; Yohko Tsuboi; Masahiro N. Machida; James Di Francesco; Rachel Friesen; Naomi Hirano; Yumiko Oasa; Motohide Tamura; Yoichi Tamura; Takashi Tsukagoshi; David Wilner
ASTROPHYSICAL JOURNAL, Volume：866, Number：2, Oct. 2018
On the basis of various data such as ALMA, JVLA, Chandra, Herschel, and Spitzer, we confirmed that two protostellar candidates in Oph A are bona fide protostars or proto-brown dwarfs (proto-BDs) in extremely early evolutionary stages. Both objects are barely visible across infrared (IR; i.e., near-IR to far-IR) bands. The physical nature of the cores is very similar to that expected in first hydrostatic cores (FHSCs), objects theoretically predicted in the evolutionary phase prior to stellar core formation with gas densities of similar to 10(11-12 )cm(-3). This suggests that the evolutionary stage is close to the FHSC formation phase. The two objects are associated with faint X-ray sources, suggesting that they are in very early phase of stellar core formation with magnetic activity. In addition, we found the CO outflow components around both sources, which may originate from the young outflows driven by these sources. The masses of these objects are calculated to be similar to 0.01-0.03 M-circle dot from the dust continuum emission. These physical properties are consistent with that expected from the numerical model of forming brown dwarfs. These facts (the X-ray detection, CO outflow association, and FHSC-like spectral energy distributions) strongly indicate that the two objects are proto-BDs or will be in the very early phase of protostars, which will evolve to more massive protostars if they gain enough mass from their surroundings. The ages of these two objects are likely to be within similar to 10(3) years after the protostellar core (or second core) formation, taking into account the outflow dynamical times (less than or similar to 500 years).
IOP PUBLISHING LTD, English, Scientific journal
DOI：https://doi.org/10.3847/1538-4357/aae153
DOI ID：10.3847/1538-4357/aae153, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000448201700006 - FOREST unbiased Galactic plane imaging survey with the Nobeyama 45 m telescope (FUGIN). I. Project overview and initial results
Tomofumi Umemoto; Tetsuhiro Minamidani; Nario Kuno; Shinji Fujita; Mitsuhiro Matsuo; Atsushi Nishimura; Kazufumi Torii; Tomoka Tosaki; Mikito Kohno; Mika Kuriki; Yuya Tsuda; Akihiko Hirota; Satoshi Ohashi; Mitsuyoshi Yamagishi; Toshihiro Handa; Hiroyuki Nakanishi; Toshihiro Omodaka; Nagito Koide; Naoko Matsumoto; Toshikazu Onishi; Kazuki Tokuda; Masumichi Seta; Yukinori Kobayashi; Kengo Tachihara; Hidetoshi Sano; Yusuke Hattori; Sachiko Onodera; Yumiko Oasa; Kazuhisa Kamegai; Masato Tsuboi; Yoshiaki Sofue; Aya E. Higuchi; James O. Chibueze; Norikazu Mizuno; Mareki Honma; Erik Muller; Tsuyoshi Inoue; Kana Morokuma-Matsui; Hiroko Shinnaga; Takeaki Ozawa; Ryo Takahashi; Satoshi Yoshiike; Jean Costes; Sho Kuwahara
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：69, Number：5, Oct. 2017
The FUGIN project is one of legacy projects using a new multi-beam FOREST (four-beam receiver system on the 45m telescope). This project aims to simultaneously investigate the distribution, kinematics, and physical properties of both diffuse and dense molecular gases in the Galaxy by observing (CO)-C-12, (CO)-C-13, and (CO)-O-18 J = 1-0 lines simultaneously. Mapping regions are parts of the first quadrant (10 degrees <= l <= 50 degrees, | b| <= 1 degrees) and the third quadrant (198 degrees <= l = 236 degrees, | b| <= 1.) of the Galaxy, where spiral arms, bar structure, and the molecular gas ring are included. This survey achieves the highest angular resolution to date (similar to 20") for theGalactic plane survey in the COJ= 1-0 lines, whichmakes it possible to find dense clumps located farther away than the previous surveys. FUGIN will provide us an invaluable dataset for investigating the physics of the Galactic interstellar medium (ISM), particularly the evolution of interstellar gas covering galactic-scale structures to the internal structures of giant molecular clouds, such as small filaments/clumps/cores. We present an overview of the FUGIN project, the observation plan and initial results. These results reveal wide-field and detailed structures of molecular clouds, such as entangled filaments that have not been obvious in previous surveys, and large-scale kinematics of molecular gas, such as spiral arms.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/psx061
DOI ID：10.1093/pasj/psx061, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000412643200006 - EXTREMELY BRIGHT SUBMILLIMETER GALAXIES BEYOND THE LUPUS-I STAR-FORMING REGION
Y. Tamura; R. Kawabe; Y. Shimajiri; T. Tsukagoshi; Y. Nakajima; Y. Oasa; D. J. Wilner; C. J. Chandler; K. Saigo; K. Tomida; M. S. Yun; A. Taniguchi; K. Kohno; B. Hatsukade; I. Aretxaga; J. E. Austermann; R. Dickman; H. Ezawa; W. M. Goss; M. Hayashi; D. H. Hughes; M. Hiramatsu; S. Inutsuka; R. Ogasawara; N. Ohashi; T. Oshima; K. S. Scott; G. W. Wilson
The Astrophysical Journal, Jul. 2015
Scientific journal
DOI：https://doi.org/10.1088/0004-637X/808/2/121
DOI ID：10.1088/0004-637X/808/2/121, ORCID：183400104 - 「 ヒカリ ・ セキガイセン テンモンガク ダイガク カン レンケイ 」 トクシュウ(1)
大朝 由美子
Volume：109, Number：2, First page：107, Last page：112, 2015
Japanese, Scientific journal
ISSN：0374-2466, CiNii Articles ID：40020718818, CiNii Books ID：AN00154555 - Time-series photometry of Earth flyby asteroid 2012 DA14
Tsuyoshi Terai; Seitaro Urakawa; Jun Takahashi; Fumi Yoshida; Goichi Oshima; Kenta Aratani; Hisaki Hoshi; Taiki Sato; Kazutoshi Ushioda; Yumiko Oasa
Oct. 2013
Context. The object 2012 DA14 is a near-Earth asteroid with a size of several
tens of meters. It had approached closely the Earth on 15 February, 2013 UT,
providing an opportunity for precise measurements of this tiny asteroid. Aims.
The solar phase angle of 2012 DA14 had varied widely around its closest
approach but was almost constant during the following night. We performed
time-series photometric observations on those two nights to determine the
rotational properties and phase effect. Methods. The observations were carried
out using the 0.55-m telescope at Saitama University, Japan. The R-band images
were obtained continuously over a 2 hr period at the closest approach and for
about 5 hr on the next night. Results. The lightcurve data from the second
night indicates a rotational period of 11.0 +1.8/-0.6 hr and a peak-to-peak
amplitude of 1.59 +/- 0.02 mag. The brightness variation before and after the
closest approach was separated into two components that are derived from the
rotation and phase effect. We found that the phase curve slope of this asteroid
is significantly shallower than those of other L-type asteroids. Conclusions.
We suggest that 2012 DA14 is coated with a coarse surface that lacks fine
regolith particles and/or a high albedo surface.
DOI：https://doi.org/10.1051/0004-6361/201322158
DOI ID：10.1051/0004-6361/201322158, arXiv ID：arXiv:1310.0577 - High-resolution near-infrared images of the T tauri binary system XZ Tauri
Tomonori Hioki; Yoichi Itoh; Yumiko Oasa; Misato Fukagawa; Tomoyuki Kudo; Satoshi Mayama; Tae-Soo Pyo; Masahiko Hayashi; Saeko S. Hayashi; Miki Ishii; Motohide Tamura
Publications of the Astronomical Society of Japan, Volume：61, Number：6, First page：1271, Last page：1279, 2009, [Reviewed]
We present a high-resolution (∼0."1 = 14 AU) H-band image of XZ Tau, a 0."3-separated classical T Tauri binary system, taken with the Coronagraphic Imager with Adaptive Optics (CIAO) on the Subaru Telescope. We found a scattered light nebula extending to ∼2."4 from the secondary, XZ Tau S, in the northeast region of the binary. Its surface brightness is ∼ 16.2 mag arcsec-2 in the H-band, and decreases as r -1.6±0.1. Combined with the HST/ACS Polarimetric images and the [Fe II] λ1.644μm spectra taken with the Infrared Camera and Spectrograph (IRCS) on the Subaru Telescope, the elongated structure is identified as a wall of a cavity blown by the previously known blueshifted outflow. By a comparison with previous measurements, we estimated that the orbital period is 1010±260yr and the total mass of the binary is 0.62 ±0.36 M⊙. The observed H-band magnitudes of both the primary and the secondary varied by as much as 1 mag over this decade. These H-band inconstancies may arise from a variable accretion rate and changing extinction toward each component. © 2009. Astronomical Society of Japan.
Astronomical Society of Japan, English, Scientific journal
DOI ID：10.1093/pasj/61.6.1271, ISSN：0004-6264, CiNii Articles ID：10026421665, CiNii Books ID：AA1082896X, ORCID：74077297, SCOPUS ID：76649130988 - Metallicity measurements of Pleiades young dwarfs
Hitoshi Funayama; Yoichi Itoh; Yumiko Oasa; Eri Toyota; Osamu Hashimoto; Tadashi Mukai
Publications of the Astronomical Society of Japan, Volume：61, Number：5, First page：931, Last page：939, 2009, [Reviewed]
We present metallicity analyses of A, F, and G stars in the Pleiades cluster. High-resolution spectroscopic observations of 25 stars were made with the HIDES spectrograph on the Okayama 1.88-m telescope and the GAOES spectrograph on the Gunma 1.5-m telescope. The resultant optical spectra had an S/N of 70-220. We measured the equivalent widths of ∼60 neutral iron and ∼ 15 single-ionized iron absorption lines to determine stellar parameters and metallicities. We derived me metallicities of 22 stars by adapting the method of equivalent-width measurements. The average metallicity was +0.03 ± 0.05 dex. The dispersion was comparable to the statistical uncertainties of the metallicity measurements
in addition, the metallicities of all 22 stars fell within the dispersion range, indicating their uniform metallicities. A comparison of our results with previous studies confirmed a high probability of metallicity homogeneity in Pleiades. © 2009. Astronomical Society of Japan.
Oxford University Press, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/61.5.931
DOI ID：10.1093/pasj/61.5.931, ISSN：0004-6264, eISSN：2053-051X, CiNii Articles ID：10025601164, CiNii Books ID：AA1082896X, ORCID：74077319, SCOPUS ID：72149124230 - H-band image of a planetary companion around hr 8799 in 2002
Misato Fukagawa; Yoichi Itoh; Motohide Tamura; Yumiko Oasa; Saeko S. Hayashi; Yutaka Fujita; Hiroshi Shibai; Masahiko Hayashi
Astrophysical Journal, Volume：696, Number：1, First page：L1, Last page：L5, 2009, [Reviewed]
The discovery of three planetary companions around HR 8799 marked a significant epoch in direct imaging of extrasolar planets. Given the importance of this system, we re-analyzed H-band images of HR 8799 obtained with the Subaru 36-elements adaptive optics (AO) in 2002 July. The low-order AO imaging combined with the classical point-spread function (PSF) subtractions even revealed the extrasolar planet, HR 8799b. Our observations in 2002 confirmed that it has been orbiting HR 8799 in a counterclockwise direction. The flux of HR 8799b was consistent with those in the later epochs within the uncertainty of 0.25 mag, further supporting the planetary mass estimate by Marois et al. © 2009. The American Astronomical Society. All rights reserved.
Institute of Physics Publishing, English, Scientific journal
DOI：https://doi.org/10.1088/0004-637X/696/1/L1
DOI ID：10.1088/0004-637X/696/1/L1, ISSN：1538-4357, ORCID：74077325, arXiv ID：arXiv:0903.1919, SCOPUS ID：64849098302 - Radial velocity search for extrasolar planets in visual binary systems
Eri Toyota; Yoichi Itoh; Shinichiro Ishiguma; Seitaro Urakawa; Daisuke Murata; Yumiko Oasa; Hiroko Matsuyama; Hitoshi Funayama; BuN'Ei Sato; Tadashi Mukai
Publications of the Astronomical Society of Japan, Volume：61, Number：1, First page：19, Last page：28, 2009, [Reviewed]
We searched for extrasolar planets in visual binary systems using precise Doppler-shift measurements taken over a period of 4 yr. Using the High Dispersion Echelle Spectrograph (HIDES) equipped on the Okayama Astrophysical Observatory (OAO) 188 cm reflector, we achieved a radial-velocity precision of about 10 m s-1. We monitored both primary and secondary stars of six visual binary systems, and primary stars of three visual binaries. Among them, three objects show large radial-velocity variations. ADS 7311 A exhibits a decreasing trend in radial velocity with a best-fit slope of-30 m s-1 yr-1, while 31 Dra A shows an increasing trend with a best-fit slope of +220 m s-1 yr-1. These long-term trends in radial velocity may be attributable to unseen companions. BDS 10966 A shows a periodic variation in radial velocity with a period of 840 d and a semiamplitude of about 120 m s-1, implying an association of a planetary-mass companion, rotational modulation, or nonradial oscillation of the photosphere. In any case, we should mention the nonassociation between BDS 10966 A and B, suggested by the different proper motions, radial velocities, and Hipparcos parallaxes. © 2009. Astronomical Society of Japan.
Oxford University Press, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/61.1.19
DOI ID：10.1093/pasj/61.1.19, ISSN：0004-6264, eISSN：2053-051X, ORCID：74077397, SCOPUS ID：65249139505, Web of Science ID：WOS:000264417900003 - LUMINOSITY AND MASS FUNCTIONS AT THE VERY LOW MASS SIDE IN NGC 1333
Yumiko Oasa; Motohide Tamura; K. Sunada; Koji Sugitani
Volume：136, First page：1372, Last page：1387, Aug. 2008
We present the results of a deep near-infrared (NIR) imaging survey searching for very low mass young stellar objects (YSOs) in the embedded cluster associated with the Perseus molecular cloud. Our observations cover an area of ~5'× 5' in the NGC 1333-S region at J-, H-, and Ks-bands. The 10σ limiting magnitudes exceed 18 mag in all three bands. Based on NIR color-color diagrams, embedded YSO candidates were identified using NIR excesses. The derived frequency of these YSO candidates with NIR excess emission among all the detected sources is 58+10 –13%. The higher frequency of YSOs with NIR excesses implies that NGC 1333 is an active and young star-forming region. Approximately half of the YSO candidates exhibit extremely low luminosity, indicating very low mass. Combining the reddening-corrected luminosity with theoretical evolutionary models, the low-luminosity YSO candidates are considered to be young substellar-mass objects. Furthermore, some sources could have planetary masses. In addition, we carried out CO molecular-line observations of the same cloud region. The results suggested that the YSO candidates are likely formed on the side of the parent molecular cloud and star-formation activity could be high. The K-band luminosity function of all the detected sources revealed a significant population of extremely low-luminosity sources in NGC 1333. The reddening-corrected J-band luminosity function of the YSO candidates does not clearly decline to the completeness limit and seems to be bimodal. We also argue that the fraction of substellar objects is larger than those in other young clusters and the mass function of the YSO candidates appears to be increasing toward the substellar-mass regime, similar to that of dust clumps. It implies that substellar-mass distributions may depend on the initial conditions of the molecular cloud.
DOI：https://doi.org/10.1088/0004-6256/136/3/1372
DOI ID：10.1088/0004-6256/136/3/1372, ISSN：0004-6256, eISSN：1538-3881 - Radial velocity search for extrasolar planets in binary systems
E. Toyota; Y. Itoh; S. Ishiguma; D. Murata; Y. Oasa; B. Sato; T. Mukai
ESO Astrophysics Symposia, Volume：2008, First page：321, Last page：322, 2008, [Reviewed]
We have started a search for extrasolar planets in visual binary systems from 2003. We monitor them by precise radial velocity measurements, using HIgh Dispersion Echelle Spectrograph(HIDES) equipped on the Okayama Astrophysical Observatory's(OAO) 188 cm telescope. Radial velocity precision of better than 10 m/s has achieved with an iodine absorption cell during our observational span. We here report the current status of the survey. © 2008 Springer-Verlag Berlin Heidelberg.
ESO Astrophysics Symposia, English, International conference proceedings
DOI：https://doi.org/10.1007/978-3-540-75485-5_84
DOI ID：10.1007/978-3-540-75485-5_84, ISSN：1431-2433, ORCID：74077364, SCOPUS ID：36448987201 - Discovery of a scattering disk around the low-mass T Tauri star FN Tauri
T. Kudo; M. Tamura; Y. Kitamura; M. Hayashi; E. Kokubo; M. Fukagawa; S. S. Hayashi; M. Ishii; Y. Itoh; S. Mayama; M. Momose; J. Morino; Y. Oasa; T. S. Pyo; H. Suto
Astrophysical Journal, Volume：673, Number：1, First page：L67, Last page：L70, 2008, [Reviewed]
We have discovered an optically thick, nearly face-on circumstellar disk around a single M5 classical T Tauri star, FN Tau, using the coronagraphic imager CIAO on the Subaru telescope. This is the least massive T Tauri star whose circumstellar structure has been directly imaged as a scattering disk. The surface brightness in the H band declines as a power law of r -25±0.1 (110.1 ≤ r ≤ 260 AU), suggesting that the disk is flared. The disk morphology appears to be relatively featureless except for an azimuthal asymmetry in the surface brightness, indicating that the disk is not perfectly face-on but is slightly tilted. The disk mass, derived from a simple disk emission model with previous photometry at optical to millimeter wavelengths, is ∼0.007 M⊙, 6% of the mass of the central star. The disk around FN Tau is one of the best targets for disk and planet formation studies around M stars. © 2008. The American Astronomical Society. All rights reserved.
Institute of Physics Publishing, English, Scientific journal
DOI：https://doi.org/10.1086/527474
DOI ID：10.1086/527474, ISSN：1538-4357, ORCID：74077381, SCOPUS ID：67949101792 - Metallicity of pleiades dwarf
H. Funayama; Y. Itoh; Y. Oasa; E. Toyota; T. Mukai
ESO Astrophysics Symposia, Volume：2008, First page：285, Last page：286, 2008, [Reviewed]
The goal of our study is to discuss how planet-hosting stars (PHSs) are born by analyzing the chemical homogeneity in open clusters. We obtained the spectra of 18 A,F,G stars in the Pleiades by the high-resolution spectroscopic observations in last January. Out of the 18 stars, the metallcities of 10 stars were derived, and their mean metallicity was obtained to be [Fe/H]mean = +0.02±0.14dex. This high dispersion may imply the chemical diversity in Pleiades. We report the results of our analysis. © 2008 Springer-Verlag Berlin Heidelberg.
ESO Astrophysics Symposia, English, International conference proceedings
DOI：https://doi.org/10.1007/978-3-540-75485-5_67
DOI ID：10.1007/978-3-540-75485-5_67, ISSN：1431-2433, ORCID：74077324, SCOPUS ID：36448962027 - Near-infrared spectroscopy of faint companions around young stellar objects associated with the Taurus molecular cloud
Yoichi Itoh; Motohide Tamura; Masahiko Hayashi; Yumiko Oasa; Saeko S. Hayashi; Misato Fukagawa; Tomoyuki Kudo; Satoshi Mayama; Miki Ishii; Tae-Soo Pyo; Takuya Yamashita; Junichi Morino
Publications of the Astronomical Society of Japan, Volume：60, Number：2, First page：209, Last page：218, 2008, [Reviewed]
We have conducted near-infrared spectroscopy of 26 faint objects around young stellar objects in the Taurus molecular cloud. These objects were detected during a course of near-infrared coronagraphic searches for companions around 72 young stellar objects with the Subaru Telescope and the near-infrared coronagraph CIAO (coronagraphic imager with adaptive optics). A comparison of the Subaru and HST archive images revealed that three central stars and faint companions share common proper motions, suggesting that they are physically associated with each other. None of the 26 sources show deep water absorption bands at near-infrared, except for DH Tau B. This result indicates that all of them, but DH Tau B, have a high photospheric temperature or a large amount of excess from circumstellar materials © 2008. Astronomical Society of Japan.
Oxford University Press, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/60.2.209
DOI ID：10.1093/pasj/60.2.209, ISSN：0004-6264, ORCID：74077326, SCOPUS ID：44949250101 - Near-infrared coronagraphic observations of a classical T Tauri star, DO Taurus
Yoichi Itoh; Masahiko Hayashi; Motohide Tamura; Yumiko Oasa; Tomonori Hioki; Misato Fukagawa; Tomoyuki Kudo
Publications of the Astronomical Society of Japan, Volume：60, Number：2, First page：223, Last page：226, 2008, [Reviewed]
A high angular resolution near-infrared image of a classical T Tauri star, DO Tau, was obtained with Coronagraphic Imager with Adaptive Optics (CIAO) mounted on the Subaru Telescope. Circumstellar emission was detected at ∼ 1.".7 from the central star in the direction of the redshifted jet. No emission was found toward the opposite direction. We also found one faint point source 3."46 away from the central star. The following observation will reveal whether it is an associated planetary mass object or a background object. © 2008. Astronomical Society of Japan.
Oxford University Press, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/60.2.223
DOI ID：10.1093/pasj/60.2.223, ISSN：0004-6264, ORCID：74077282, SCOPUS ID：44949127336 - Near-infrared coronagraphic observations of the T tauri binary system UY Aur
Tomonori Hioki; Yoichi Itoh; Yumiko Oasa; Misato Fukagawa; Tomoyuki Kudo; Satoshi Mayama; Hitoshi Funayama; Masahiko Hayashi; Saeko S. Hayashi; Tae-Soo Pyo; Miki Ishii; Takayuki Nishikawa; Motohide Tamura
Astronomical Journal, Volume：134, Number：2, First page：880, Last page：885, 2007, [Reviewed]
We present a near-infrared image of UY Aur, a 0.9″ separated binary system, using the Coronagraphic Imager with Adaptive Optics on the Subaru Telescope. Thanks to adaptive optics, the spatial resolution of our image was ∼0.1″ in the full width at half-maximum of the point-spread function, the highest achieved. By comparison with previous measurements, we estimated that the orbital period is ∼1640 ± 90 yr and the total mass of the binary is ∼ 1.73 ± 0.29 M⊙. The observed H-band magnitude of the secondary varies by as much as 1.3 mag within a decade, while that of the primary is rather stable. This inconstancy may arise from photospheric variability caused by an uneven accretion rate or from the rotation of the secondary. We detected a half-ring-shaped circumbinary disk around the binary with a bright southwestern part but a barely detectable northeastern portion. The brightness ratio is ≳57 ± 5. Its inner radius and inclination are about 520 AU and 42° ± 3°, respectively. The disk is not uniform but has remarkable features, including a clumpy structure along the disk, circumstellar material inside the inner cavity, and an extended armlike structure. The circumstellar material inside the cavity probably corresponds to a clump or material accreting from the disk onto the binary. The armlike structure is part of the disk, created by accretion from the outer region of the disk or encounters with other stellar systems. © 2007. The American Astronomical Society. All rights reserved.
University of Chicago Press, English, Scientific journal
DOI：https://doi.org/10.1086/519737
DOI ID：10.1086/519737, ISSN：0004-6256, ORCID：74077317, SCOPUS ID：34547995042 - Subaru near-infrared multicolor images of class II young stellar object, RNO 91
Satoshi Mayama; Motohide Tamura; Masahiko Hayashi; Yoichi Itoh; Miki Ishii; Misato Fukagawa; Saeko S. Hayashi; Yumiko Oasa; Tomoyuki Kudo
Publications of the Astronomical Society of Japan, Volume：59, Number：6, First page：1153, Last page：1160, 2007, [Reviewed]
We conducted subarcsecond near-infrared imaging observations of RNO 91 with CIAO (Coronagraphic Imager with Adaptive Optics) mounted on the 8.2m Subaru telescope. We present our JHK band data along with optical images, which when considered together reveal a complex circumstellar structure. We examined the colors of associated nebulae and compared the geometry of the outflow/disk system suggested by our data with that already proposed on the basis of previous studies. Our K-band image shows bright circumstellar nebulosity detected within ∼ 2″ around the central source, while it is less conspicuous at shorter wavelengths. PA and the size of this red color nebulosity agree with those of the previously detected polarization disk. Agreements among these data indicate that this bright nebulosity region, which follows the reddening law, might be attributed to a disklike structure. At J and optical wavelengths, several blue knotlike structures are detected around and beyond the bright circumstellar nebulosity. We suggest that these knotty reflection nebulae may represent disintegrating fragments of an infalling envelope. The three-color composite image has the appearance of arc-shaped nebulosity. We interpret these structures as being roots of a bipolar cavity opening toward the northeast and the southwest. The complex distribution of reflection nebulosity seen around RNO 91 appears to confirm the interpretation that this source is an object dispersing its molecular envelope while transitioning from protostar to T Tauri star. © 2007. Astronomical Society of Japan.
Astronomical Society of Japan, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/59.6.1153
DOI ID：10.1093/pasj/59.6.1153, ISSN：0004-6264, ORCID：74077335, SCOPUS ID：39149110962 - Near-Infrared Extinction in The Coalsack Globule 2
Takahiro Naoi; Motohide Tamura; Tetsuya Nagata; Yasushi Nakajima; Hiroshi Suto; Koji Murakawa; Ryo Kandori; Sho Sasaki; Shogo Nishiyama; Yumiko Oasa; Koji Sugitani
Dec. 2006
We have conducted J, H, and Ks imaging observations for the Coalsack Globule
2 with the SIRIUS infrared camera on the IRSF 1.4 m telescope at SAAO, and
determined the color excess ratio, E(J-H)/E(H-Ks). The ratio is determined in
the same photometric system as our previous study for the rho Oph and Cha
clouds without any color transformation; this enables us to directly compare
the near-infrared extinction laws among these regions. The current ratio
E(J-H)/E(H-Ks) = 1.91 +- 0.01 for the extinction range 0.5 < E(J-H) <1.8 is
significantly larger than the ratios for the rho Oph and Cha clouds
(E(J-H)/E(H-Ks) = 1.60-1.69). This ratio corresponds to a large negative index
alpha = 2.34 +- 0.01 when the wavelength dependence of extinction is
approximated by a power law which might indicate little growth of dust grains,
or larger abundance of dielectric non-absorbing components such as silicates,
or both in this cloud. We also confirm that the color excess ratio for the
Coalsack Globule 2 has a trend of increasing with decreasing optical depth,
which is the same trend as the rho Oph and Cha clouds have.
DOI：https://doi.org/10.1086/512030
DOI ID：10.1086/512030, arXiv ID：astro-ph/0612620 - 特集 ISOLAB'05 プロシーディング 太陽系外に存在する生命を持つ地球型惑星の探査:大気の進化段階に応じた惑星放射スペクトルの特徴
Oasa Yumiko; Kikuchi Nobuhiro
Viva Origino, Volume：34, Number：4, First page：130, Last page：132, Dec. 2006
We report the calculation of spectra for various extrasolar Earth-like planets, which characterize their temperatures and atmospheres for evidence of habitability and life. Future space missions such as Darwin and Terrestrial Planet Finder (TPF) will ultimately offer the opportunity to obtain spectra of extrasolar planets situated within the habitable zones of stars and search for signs of life. The atmospheric biosignatures such as ozone, carbon dioxide, and methane, which are abundant in the Earth, could be attributable to primitive life in extrasolar terrestrial planets. In order to explore the possibility of diagnosing the existence of life from spectra, we have calculated synthesized global spectra for hypothetical terrestrial planets. We performed calculations of radiative-convective equilibrium and radiative transfer, taking into account the global cloud distribution, viewing angles, seasonal variation in solar insolation and surface temperatures, and consequently, the infrared radiation emitted to space. The Earth is our only example of a planet whose atmospheric composition is the consequence of the supply of gas from the presence of life. We examine characteristics for the anoxic / low-oxygen atmosphere of the Archean / Proterozoic Earth with the evolution of oxygenic photosynthesis using the photochemical models coupled to radiative-convective equilibrium code. We compare the derived atmospheric spectral feature of extrasolar Earth-like planets with different age and discuss the detectability of atmospheric constituents of extrasolar terrestrial planets.
The Society for the Study of the Origin and Evolution of Life Japan, Japanese
DOI：https://doi.org/10.50968/vivaorigino.34.4_130
DOI ID：10.50968/vivaorigino.34.4_130, ISSN：0910-4003, eISSN：1346-6933, CiNii Articles ID：110006162904, CiNii Books ID：AA11148698 - Coronagraphic search for extrasolar planets around ε Eri and Vega
Yoichi Itoh; Yumiko Oasa; Misato Fukaoawa
Astrophysical Journal, Volume：652, Number：2 I, First page：1729, Last page：1733, Dec. 2006, [Reviewed]
We present the results of a coronagraphic imaging search for extrasolar planets around the young main-sequence stars ε Eri and Vega. Concentrating the stellar light into the core of the point-spread function by the adaptive optic system and blocking the core by the occulting mask in the coronagraph, we have achieved the highest sensitivity for point sources in close vicinity of the both central stars. Nonetheless, we had no secure detection of a point source around the stars. The observations give the upper limits on the masses of the planets to (4-6)MJ and (5-10)MJ at a few arcseconds from ε Eri and Vega, respectively. Difruse structures are also not detected around both stars. © 2006. The American Astronomical Society. All rights reserved.
Institute of Physics Publishing, English, Scientific journal
DOI：https://doi.org/10.1086/508420
DOI ID：10.1086/508420, ISSN：1538-4357, eISSN：1538-4357, CiNii Articles ID：120003219966, ORCID：74077366, arXiv ID：astro-ph/0608362, SCOPUS ID：33845889536 - Photometric and spectroscopic studies of very low mass YSOs and young Brown Dwarfs in S106
Yumiko Oasa
Volume：2, First page：457, Last page：457, Aug. 2006
DOI：https://doi.org/10.1017/s1743921307002451
DOI ID：10.1017/s1743921307002451, ISSN：1743-9213, eISSN：1743-9221 - Radio observation of molecular clouds around the W5-East triggered star-forming region
Takahiro Niwa; Yoichi Itoh; Kengo Tachihara; Yumiko Oasa; Kazuyoshi Sunada; Koji Sugitani
Proceedings of the International Astronomical Union, Volume：2, Number：237, First page：454, Last page：454, Aug. 2006, [Reviewed]
Proceedings of the International Astronomical Union, English, International conference proceedings
DOI：https://doi.org/10.1017/S1743921307002426
DOI ID：10.1017/S1743921307002426, ISSN：1743-9213, eISSN：1743-9221, ORCID：74077436, SCOPUS ID：37049020257 - Very low luminosity young cluster and the luminosity and mass functions in S106
Yumiko Oasa; Motohide Tamura; Yasushi Nakajima; Yoichi Itoh; Toshinori Maihara; Fumihiko Iwamuro; Kentaro Motohara; Saeko S. Hayashi; Masahiko Hayashi; Norio Kaifu
Astronomical Journal, Volume：131, Number：3, First page：1608, Last page：1628, Mar. 2006, [Reviewed]
We present the results of deep near-infrared observations searching for very low mass young stellar objects (YSOs) in the massive star-forming region of S106 taken with the Subaru Telescope. The survey, whose limiting magnitude exceeds 20 mag in the JHK′ bands, is sensitive enough to provide unprecedented details in the two nebular lobes. In addition, it reveals a census of the stellar population down to objects below the deuterium-burning limit, a fiducial boundary between brown dwarfs and planetary-mass objects. Based on color-color diagrams, nearly 600 embedded YSO candidates with near-infrared excesses have been identified in an area of ∼5′ × 5′ that are not uniformly distributed but centrally concentrated. Combining the reddening-corrected luminosity of the YSO candidates with the theoretical evolutionary models, we suggest that there exists a substantial substellar population. If we divide the cluster into three subgroups based on stellar and cloud properties, both their luminosity functions and mass functions across the stellar-substellar boundary demonstrate local variation on a subparsec scale. Nevertheless, all the mass functions have distinct characteristics in common: they do not have any turnover and do not decline down to the completeness limits. Furthermore, the mass function for S106 appears to be more abundant in young substellar objects compared to those obtained for other young clusters, such as Trapezium and IC 348. This implies that the substellar mass function for young clusters may have a variation. © 2006. The American Astronomical Society. All rights reserved.
English, Scientific journal
DOI：https://doi.org/10.1086/500086
DOI ID：10.1086/500086, ISSN：0004-6256, ORCID：74077390, SCOPUS ID：33645220429 - Luminosity and Spectral Variation of Extrasolar Earth-like Planets
Oasa Yumiko; Kikuchi Nobuhiro
Abstracts for fall meeting of the Japanese Society for Planetary Science, Volume：2006f, First page：135, Last page：135, 2006
We report the calculation of spectra for various extrasolar Earth-like planets to search for them, which characterize their temperatures and atmospheres for evidence of habitability and life.
THE JAPANESE SOCIETY FOR PLANETARY SCIENCES
DOI：https://doi.org/10.14909/jsps.2006f.0.135.0
DOI ID：10.14909/jsps.2006f.0.135.0, CiNii Articles ID：130004636059 - Subaru near infrared coronagraphic images of T Tauri
Satoshi Mayama; Motohide Tamura; Masahiko Hayashi; Yoichi Itoh; Misato Fukagawa; Hiroshi Suto; Miki Ishii; Koji Murakawa; Yumiko Oasa; Saeko S. Hayashi; Takuya Yamashita; Junichi Morino; Shin Oya; Takahiro Naoi; Tae-Soo Pyo; Takayuki Nishikawa; Tomoyuki Kudo; Tomonori Usuda; Hiroyasu Ando; Shoken M. Miyama; Norio Kaifu
Publications of the Astronomical Society of Japan, Volume：58, Number：2, First page：375, Last page：382, 2006, [Reviewed]
High angular resolution near-infrared (JHK) adaptive optics images of T Tau were obtained with the infrared camera Coronagraphic Imager with Adaptive Optics (CIAO) mounted on the 8.2 m Subaru Telescope in 2002 and 2004. The images resolve a complex circumstellar structure around a multiple system. We resolved T Tau Sa and Sb as well as T Tau N and S. The estimated orbit of T Tau Sb indicates that it is probably bound to T Tau Sa. The K band flux of T Tau S decreased by ∼ 1.7 Jy in 2002 November compared with that in 2001 mainly because T Tau Sa became fainter. The arc-like ridge detected in our near-infrared images is consistent with what is seen at visible wavelengths, supporting the interpretation in previous studies that the arc is part of the cavity wall seen relatively pole-on. Halo emission is detected out to ∼ 2″ from T Tau N. This may be light scattered off the common envelope surrounding the T Tauri multiple system. © 2006. Astronomical Society of Japan.
Oxford University Press, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/58.2.375
DOI ID：10.1093/pasj/58.2.375, ISSN：0004-6264, ORCID：74077338, SCOPUS ID：33646811196 - Sequential formation of low-mass stars in the BRC 14 region
Matsuyanagi, I.; Itoh, Y.; Sugitani, K.; Oasa, Y.; Mukai, T.; Tamura, M.
Publications of the Astronomical Society of Japan, Volume：58, Number：4, First page：L29, Last page：L34, 2006, [Reviewed]
We have carried out a deep near-infrared survey of a bright-rimmed molecular
cloud, BRC 14 (IC 1848A). The 10 sigma limiting magnitude of the survey is 17.7
mag at the K-band. Seventy-four sources are classified as young stellar object
(YSO) candidates based on the near-infrared color-color diagram. The faintest
YSO candidates may have masses of an order of tenths of the solar mass,
assuming the age of 1 Myr. We examined three values as indicators of star
formation; fraction of the YSO candidates, extinctions of all sources, and
near-infrared excesses of the YSO candidates. All indicators increase from
outside of the rim to the center of the molecular cloud, which suggests that
the formation of the low-mass stars in the BRC 14 region proceeds from outside
to the center of the cloud.
Oxford University Press ({OUP}), English, Scientific journal
DOI：https://doi.org/10.1093/pasj/58.4.l29
DOI ID：10.1093/pasj/58.4.l29, ISSN：0004-6264, eISSN：2053-051X, CiNii Articles ID：120003219985, CiNii Books ID：AA1082896X, ORCID：74077278, arXiv ID：astro-ph/0605579, SCOPUS ID：33749358847 - P118 地球大気の化学進化と赤外放射 : 太陽光度の変動と居住可能性について
大朝,由美子; 菊地,信宏
Volume：88, First page：315, Oct. 2005
Japanese
CiNii Articles ID：110007600960, CiNii Books ID：AA11552241 - Atmospheric compositions and radiation spectra of extrasolar Earth-like planets
Oasa Yumiko; Kikuchi Nobuhiro
Abstracts for fall meeting of the Japanese Society for Planetary Science, Volume：2005f, First page：90, Last page：90, 2005
We report the calculation of spectra for various extrasolar Earth-like planets to search for them, which characterize their temperatures and atmospheres for evidence of habitability and life.
THE JAPANESE SOCIETY FOR PLANETARY SCIENCES
DOI：https://doi.org/10.14909/jsps.2005f.0.90.0
DOI ID：10.14909/jsps.2005f.0.90.0, CiNii Articles ID：130004636011 - Near-infrared images of protoplanetary disk surrounding HD 142527
M Fukagawa; M Tamura; Y Itoh; T Kudo; Y Imaeda; Y Oasa; SS Hayashi; M Hayashi
ASTROPHYSICAL JOURNAL, Volume：636, Number：2, First page：L153, Last page：L156, Jan. 2005, [Reviewed]
We discovered a unique morphology in a disk around the Herbig Ae star HD 142527 by near-infrared ( H and K bands) adaptive optics imaging observations. The almost face-on disk consists of two bright arcs facing one another along the east-west direction (banana-split structure) and one spiral arm extending to the north from the western arc. The eastern arc is located at similar to 100 - 400 AU in radius from the star, and the western one is detected at similar to 150 - 490 AU. The stellar position is displaced from the center of the disk by about 20 AU to the north, and also from the center of the inner hole. The two arcs show an asymmetry in their size and brightness; the larger western arc is brighter than the east one by about 2 mag. The morphology of the disk, consisting of a banana-split structure and a spiral arm, most likely suggests the presence of an unseen eccentric binary and a recent stellar encounter.
UNIV CHICAGO PRESS, English, Scientific journal
DOI：https://doi.org/10.1086/500128
DOI ID：10.1086/500128, ISSN：0004-637X, ORCID：74077374, SCOPUS ID：32044440262, Web of Science ID：WOS:000234469700024 - A Young Brown Dwarf Companion to DH Tauri
Itoh Yoichi; Hayashi Masahiko; Tamura Motohide; Tsuji Takashi; Oasa Yumiko; Fukagawa Misato; Hayashi Saeko S.; Naoi Takahiro; Ishii Miki; Mayama Satoshi; Morino Jun-ichi; Yamashita Takuya; Tae-Soo Pyo; Nishikawa Takayuki; Usuda Tomonori; Murakawa Koji / Suto Hiroshi / Oya Shin / Takato Naruhisa / Ando Hiroyasu / Miyama Shoken M. / Kobayashi Naoto / Kaifu Norio
The Astrophysical Journal, Volume：620, Number：2, First page：984, Last page：993, 2005
We present the detection of a young brown dwarf companion DH Tau B associated
with the classical T Tauri star DH Tau. Near-infrared coronagraphic
observations with CIAO on the Subaru Telescope have revealed DH Tau B with H =
\~15 mag located at 2.3" (330 AU) away from the primary DH Tau A. Comparing its
position with a Hubble Space Telescope archive image, we confirmed that DH Tau
A and B share the common proper motion, suggesting that they are physically
associated with each other. The near-infrared color of DH Tau B is consistent
with those of young stellar objects. The near-infrared spectra of DH Tau B show
deep water absorption bands, a strong K I absorption line, and a moderate Na I
absorption line. We derived its effective temperature and surface gravity of
Teff = 2700 -- 2800 K and log g = 4.0--4.5, respectively, by comparing the
observed spectra with synthesized spectra of low-mass objects. The location of
DH Tau B on the HR diagram gives its mass of 30 -- 50 M_Jupiter.
Institute of Physics, English, Scientific journal
DOI：https://doi.org/10.1086/427086
DOI ID：10.1086/427086, ISSN：0004-637X, CiNii Articles ID：120003219965, ORCID：74077354, arXiv ID：astro-ph/0411177, SCOPUS ID：20244374123 - A coronagraphic search for brown dwarfs and planets around nearby stars
T. Nakajima; J. I. Morino; T. Tsuji; H. Suto; M. Ishii; M. Tamura; M. Fukagawa; K. Murakawa; S. Miyama; H. Takami; N. Takato; S. Oya; S. Hayashi; T. Kudo; Y. Itoh; Y. Oasa; B. R. Oppenheimer
Astronomische Nachrichten, Volume：326, Number：10, First page：952, Last page：957, 2005, [Reviewed]
We have started a corongraphic search for brown dwarfs and planets around young nearby stars within 20 pc of the Sun, using the adaptive optics coronagraph, CIAO, on Subaru. The dynamic range we have achieved is ΔK = 13 at 2.5″ from the central star. For a typical target with K = 7 at 10 pc, the limiting absolute magnitude is MK = 20. We apply two kinematical age criteria to select M and K dwarfs statistically younger than 350Myr. The first criterion is a small velocity deviation from the velocity of LSR. The second is a (U, V, W) velocity vector similar to a particular young moving group. The combination of the age and magnitude limits implies that the mass limit for giant planet detection is about 2MJ. We show a sample image of a target field at 3 pc of the Sun with faint companion candidates, to be followed up for the common proper motion test. We give a brief description of our procedures for data acquisition, reduction, and analysis. ©2005 WILEY-VCH Verlag GmbH &
Co. KGaA, Weinheim.
English, International conference proceedings
DOI：https://doi.org/10.1002/asna.200510445
DOI ID：10.1002/asna.200510445, ISSN：0004-6337, ORCID：74077306, SCOPUS ID：29844434055 - Infrared Spectra of Extrasolar Terrestrial Planets with Cloud
Oasa Yumiko; Kikuchi Nobuhiro
Abstracts for fall meeting of the Japanese Society for Planetary Science, Volume：2004f, First page：86, Last page：86, 2004
One strategy in the search for life is the study of atmospheric spectral features for signs of severe disequilibrium chemistry that could be indicative of biological activity.In order to investigate the feasibility of observation, we have calculated the synthesized infrared spectra for several terrestrial-type atmospheres with clouds, which represent inhabited planets, our Earth, and other terrestrial planets including early Earth-type planets.
THE JAPANESE SOCIETY FOR PLANETARY SCIENCES
DOI：https://doi.org/10.14909/jsps.2004f.0.86.0
DOI ID：10.14909/jsps.2004f.0.86.0, CiNii Articles ID：130005011589 - High-resolution imaging polarimetry of HL Tau and magnetic field structure
P.W. Lucas; Fukagawa Misato; Tamura Motohide; A.F. Beckford; Itoh Yoichi; Murakawa Koji; Suto Hiroshi; Hayashi Saeko S.; Oasa Yumiko; Naoi Takahiro; Doi yoshiyuki; Ebizaka Noboru; Kaifu Norio
Monthly Notices of the Royal Astronomical Society, Volume：352, Number：4, First page：1347–1364, 2004
Blackwell, English, Scientific journal
DOI：https://doi.org/10.1111/j.1365-2966.2004.08026.x
DOI ID：10.1111/j.1365-2966.2004.08026.x, ISSN：0035-8711, CiNii Articles ID：120003219970, ORCID：74077385, SCOPUS ID：4344689027 - SPIRAL structure in the circumstellar disk around AB aurigae
Fukagawa, M.; Hayashi, M.; Tamura, M.; Itoh, Y.; Hayashi, S.S.; Oasa, Y.; Takeuchi, T.; Morino, J.-I.; Murakawa, K.; Oya, S.; Yamashita, T.; Suto, H.; Mayama, S.; Naoi, T.; Ishii, M.; Pyo, T.-S.; Nishikawa, T.; Takato, N.; Usuda, T.; Ando, H.; Iye, M.; Miyama, S.M.; Kaifu, N.
Astrophysical Journal, Volume：605, Number：1 II, 2004
Scientific journal
DOI：https://doi.org/10.1086/420699
DOI ID：10.1086/420699, ORCID：74077291, SCOPUS ID：2542552036 - Interferometric Observations of the T Tauri Stars in the MBM 12 Cloud
Itoh Yoichi; Sugitani Koji; Fukada Naoya; Nakanishi Kouichiro; Ogura Katsuo; Tamura Motohide; Marui Kazuko; Fujita Kenta; Oasa Yumiko; Fukagawa Misato
The Astrophysical Journal Letters, Volume：586, Number：2, First page：L141, Last page：L144, 2003
We have carried out a millimeter interferometric continuum survey toward 7
YSOs in the MBM 12 cloud. Thermal emissions associated with 2 YSOs were
detected above the 3-$\sigma$ level at 2.1 mm, and one also showed a 1.3 mm
thermal emission. Another object was marginally detected at 2.1 mm. Spectral
energy distributions of the YSOs are well fitted by a simple power-law disk
model. Masses of the circumstellar disks are estimated to be an order of $0.05
M_{\sun}$. The circumstellar disks in the MBM 12 cloud have properties in
common with the disks in nearby star-forming regions, in terms of disk
parameters such as a disk mass, as well as an infrared excess.
Institute of Physics, English, Scientific journal
DOI：https://doi.org/10.1086/374881
DOI ID：10.1086/374881, ISSN：0004-637X, CiNii Articles ID：120003219963, ORCID：74077391, arXiv ID：astro-ph/0302472, SCOPUS ID：0042591417 - Near-infrared imaging of the circumstellar disk around Herbig Ae star HD 150193A
Fukagawa, M.; Tamura, M.; Itoh, Y.; Hayashi, S.S.; Oasa, Y.
Astrophysical Journal, Volume：590, Number：1 II, First page：L49, Last page：L52, 2003
We present 01 resolution near-infrared imaging of Herbig Ae star HD 150193 (~6 Myr) and its T Tauri companion with the stellar coronagraphic camera (Coronagraphic Imager with Adaptive Optics) on the Subaru 8.2 m telescope. The images obtained reveal a circumstellar disk around the primary star extending from the edge of the coronagraphic mask at 50 AU to about 190 AU (13). No circumstellar structure was detected around the companion, which was separated by 165 AU (110) from the primary. For the circumprimary disk, the lower limit of the ratio between the disk and the total flux is estimated to be 1.3 × 10-2. Asymmetries are seen in the surface brightness of this disk. Azimuthal asymmetry of the radial profile suggests that the companion has an effect on the distortion of the circumprimary disk. HD 150193 provides insight into the disk evolutionary process in binary systems.
Scientific journal
DOI：https://doi.org/10.1086/376685
DOI ID：10.1086/376685, ISSN：0004-637X, eISSN：1538-4357, ORCID：74077375, SCOPUS ID：0043156466 - Deep near-infrared surveys and young brown dwarf populations in star-forming regions
M Tamura; T Naoi; Y Oasa; Y Nakajima; C Nagashima; T Nagayama; D Baba; T Nagata; S Sato; D Kato; M Kurita; K Sugitani; Y Itoh; H Nakaya; A Pickles
BROWN DWARFS, Number：211, First page：87, Last page：90, 2003, [Reviewed]
We are currently conducting three kinds of IR surveys of star forming regions (SFRs) in order to seek for very low-mass young stellar populations. First is a deep JHKs-bands (simultaneous) survey with the SIRIUS camera on the IRSF 1.4m or the UH 2.2m telescopes. Second is a very deep JHKs survey with the CISCO IR camera on the Subaru 8.2m telescope. Third is a high resolution companion search around nearby YSOs with the CIAO adaptive optics coronagraph IR camera on the Subaru. In this contribution, we describe our SIRIUS camera and present preliminary results of the ongoing surveys with this new instrument.
ASTRONOMICAL SOC PACIFIC, English, Scientific journal
ISSN：0074-1809, Web of Science ID：WOS:000184043700018 - Subaru near-IR Coronagraphic Image of LkHα 198
Misato Fukagawa; Motohide Tamura; Hiroshi Suto; Yoichi Itoh; Koji Murakawa; Yumiko Oasa; Saeko S. Hayashi; Takahiro Naoi; Norio Kaifu; Yoshiyuki Doi
Publications of the Astronomical Society of Japan, Volume：54, Number：6, First page：969, Last page：973, 2002, [Reviewed]
High-resolution near-infrared imaging of a Herbig Ae/Be star LkHα 198 has been carried out using the coronagraphic camera CIAO (Coronagraphic Imager with Adaptive Optics) on the Subaru 8.2 m Telescope. Obtained images resolve the infrared companion (IRC) and an associated reflection nebula. The IRC exhibits near-infrared colors suggestive of a class I-like source. Faint nebulae associated with outflow activity and a bright flattened envelope are also found around the primary. Our observations provide morphological evidence of the IRC being an outflow source as well as the primary star.
Astronomical Society of Japan, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/54.6.969
DOI ID：10.1093/pasj/54.6.969, ISSN：0004-6264, ORCID：74077285, SCOPUS ID：0036944429 - Near-infrared Coronagraphy of the GG Tauri A binary system
Yoichi Itoh; Motohide Tamura; Saeko S. Hayashi; Yumiko Oasa; Misato Fukagawa; Norio Kaifu; Hiroshi Suto; Koji Murakawa; Yoshiyuki Doi; Noboru Ebizuka; Takahiro Naoi; Hideki Takami; Naruhisa Takato; Wolfgang Gaessler; Tomio Kanzawa; Yutaka Hayano; Yukiko Kamata; David Saint-Jacques; Masanori Iye
Publications of the Astronomical Society of Japan, Volume：54, Number：6, First page：963, Last page：967, 2002, [Reviewed]
The highest angular resolution near-infrared images of the GG Tau A binary system were obtained with the Coronagraphic Imager with Adaptive Optics (CIAO) mounted on the Subaru Telescope. The images show that its circumbinary disk is smooth and does not have 0″1 scale structures. Asymmetries in the surface brightness as well as a gap are also resolved. Combined with previous measurements of the stellar positions, our data indicate that the central binary is unlikely to have a large eccentricity. The fifth point source toward this double binary system is probably a background star, based on astrometric measurements.
Astronomical Society of Japan, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/54.6.963
DOI ID：10.1093/pasj/54.6.963, ISSN：0004-6264, ORCID：74077299, SCOPUS ID：0036934651 - Near infrared coronagraph images of IRC + 10216. Faint structures at 1-5″ from the central star
Murakawa, K.; Tamura, M.; Suto, H.; Itoh, Y.; Hayashi, S.S.; Oasa, Y.; Nakajima, Y.; Kaifu, N.; Yates, J.A.; Gledhill, T.M.; Richards, A.M.S.; Hough, J.H.; Kosugi, G.; Usuda, T.
Astronomy and Astrophysics, Volume：395, Number：1, 2002, [Reviewed]
Scientific journal
DOI：https://doi.org/10.1051/0004-6361:20021421
DOI ID：10.1051/0004-6361:20021421, ORCID：74077344, SCOPUS ID：0036852040 - Free Floating Planets〔和文〕—第2回宇宙科学シンポジウム ; 特別セッション:太陽系の起源と第二の地球探査
大朝 由美子
Volume：2, First page：251, Last page：254, Nov. 2001
Japanese
CiNii Articles ID：40005599026, CiNii Books ID：AA11571712 - Near-infrared observations of S 255-2: The heart of a massive YSO cluster
Yoichi Itoh; Motohide Tamura; Hiroshi Suto; Saeko S. Hayashi; Koji Murakawa; Yumiko Oasa; Yasushi Nakajima; Norio Kaifu; George Kosugi; Tomonori Usuda; Yoshiyuki Doi
Publications of the Astronomical Society of Japan, Volume：53, Number：3, First page：495, Last page：500, Jun. 2001, [Reviewed]
High-resolution near-infrared (J H K L′ M′) images of a massive star-forming region, S 255-2, were obtained with the Subaru Telescope and an infrared camera, CIAO. These images clearly resolve two sets of bipolar nebulae illuminated by two independent massive YSOs. A number of cluster member YSOs have been detected, including 3 new sources. Seven early-B type stars have been identified within 10pc of S 255-2
three are associated with extended optical H II regions. The variation in the appearance of these early-B type stars suggests an evolutionary sequence of massive stars in the S 255 region.
Astronomical Society of Japan, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/53.3.495
DOI ID：10.1093/pasj/53.3.495, ISSN：0004-6264, ORCID：74077304, SCOPUS ID：0035948353 - A Near-Infrared Imaging Survey of the Lupus 3 Dark Cloud: A Modest Cluster of Low-Mass, Pre–Main-Sequence Stars
Yasushi Nakajima; Motohide Tamura; Yumiko Oasa; Tadashi Nakajima
Volume：119, Number：2, First page：873, Last page：881, Feb. 2000
We present the first report on results of a near-infrared imaging survey of the Lupus 3 dark cloud. This cloud is known to be associated with a modest cluster of T Tauri stars from a previous optical Hα emission-line star survey. The survey covers 7' × 11', which corresponds to a projected area of ~0.35 × 0.55 pc at a distance of 150 pc. Mapping was carried out at J, H, and Ks, to 10 σ limiting magnitudes of J = 17.0, H = 16.5, and Ks = 15.5. A total of 229 sources brighter than Ks < 15.8 were detected at all bands with a 90% completeness limit. Source classification is performed based on the near-infrared colors. Ten sources are candidates of Lada's Class II pre–main-sequence (PMS) stars, as they have a color excess that cannot be explained by reddening resulting from interstellar dust. We also identified 11 Class I–like candidates that were not detected at J and have a large color excess (H-Ks ≥ 2), which is unlikely to arise from extinction in the Lupus dark cloud. There are four subclusters in this survey area of which three are embedded and mainly consist of the Class I–like candidates. The average density of PMS stars is around 500 pc-3, suggesting the presence of a modest cluster of embedded PMS stars. We estimate masses of the Class II candidates with aid of an evolutionary model of PMS stars. Ten of them have masses less than 0.08 M⊙ if we assume their age to be 106 yr. Hence, we consider them to be young brown dwarf (YBD) candidates. The relative population of YBDs in the Lupus 3 dark cloud is larger than in the Taurus.
DOI：https://doi.org/10.1086/301222
DOI：https://doi.org/10.3847/1538-4357/aba43d_references_DOI_LZ2BWNEYHTQi4qL7dWf8qzTVgHs
DOI ID：10.1086/301222, ISSN：0004-6256 - A Deep Near‐Infrared Survey of the Chamaeleon I Dark Cloud Core
Yumiko Oasa; Motohide Tamura; Koji Sugitani
Volume：526, Number：1, First page：336, Last page：343, Nov. 1999
We have carried out a deep near-infrared imaging survey to search for low-mass young stellar objects (YSOs) in the densest star-forming core of the Chamaeleon I dark cloud. Our observations cover an area of 30 arcmin2, including an early B9 star (HD 97300) and an outflow source (HM 23). The 10 σ limiting magnitudes are 18.1, 17.0, and 16.2 mag at J, H, and K, respectively, which is sensitive enough to provide a census of the embedded stellar population down to substellar objects in the cloud. Source classification is performed based on the near-infrared (NIR) color-color diagram. Many of the YSO candidates with NIR excesses are more than 7 mag fainter than typical T Tauri stars in the same cloud. Some of them are even fainter than the known brown dwarfs in the Pleiades. The luminosities of newly identified YSO candidates and the recent evolutionary models for very low mass objects suggest that they appear to be substellar, if their typical age is assumed to be similar to that of classic T Tauri stars or, namely, 1 Myr with an upper limit of 10 Myr. Therefore it is highly likely that young brown dwarfs form in this molecular cloud core. The J-band luminosity function of the YSO candidates does not appear to turn over down to the completeness limit. In the Chamaeleon I dark cloud core, stars form in a clustered mode characterized by both a high star formation efficiency and high stellar density such as in the ρ Oph core.
DOI：https://doi.org/10.1086/307964
DOI：https://doi.org/10.1093/pasj/psu016_references_DOI_EceHn8alEbd8ke6Ku7J3ZEUinrX
DOI ID：10.1086/307964, ISSN：0004-637X, eISSN：1538-4357, CiNii Articles ID：30017607139, CiNii Books ID：AA00553242 - 若い褐色矮星
伊藤 洋一; 大朝 由美子
Volume：92, Number：5, First page：257, Last page：264, May 1999
資料形態 : テキストデータ プレーンテキスト
コレクション : 国立国会図書館デジタルコレクション > デジタル化資料 > 雑誌
Japanese
ISSN：0374-2466, CiNii Articles ID：10002148615, CiNii Books ID：AN00154555 - Isolated and Companion Young Brown Dwarfs in the Taurus and Chamaeleon Molecular Clouds
Motohide Tamura; Yoichi Itoh; Yumiko Oasa; Tadashi Nakajima
Volume：282, Number：5391, First page：1095, Last page：1097, Nov. 1998
DOI：https://doi.org/10.1126/science.282.5391.1095
DOI：https://doi.org/10.1051/0004-6361/202243850_references_DOI_7BzztEGp9vvSs0HxC9u01fbL9Gi
DOI ID：10.1126/science.282.5391.1095, ISSN：0036-8075, eISSN：1095-9203, PubMed ID：9804541 - Very Low-Luminosity Objects in Star-Forming Regions
Alan T. Tokunaga; Yoichi Itoh; Motohide Tamura; Yumiko Oasa; Koji Sugitani
Volume：11, First page：423, Last page：424, Jan. 1998
DOI：https://doi.org/10.1017/s1539299600021626
DOI ID：10.1017/s1539299600021626, ISSN：1539-2996
- 教員養成系学生を対象としたぐんま天文台150cm望遠鏡を用いた観測実習
大朝由美子; 橋本修; 田口光
Volume：2024, 2024
ISSN：1347-0639, J-Global ID：202402213368431660 - ペルセウス座分子雲Barnard1領域における若い超低質量天体の近赤外測光探査
小柳香; 大朝由美子; 金井昂大
Volume：2024, 2024
ISSN：1347-0639, J-Global ID：202402224539883784 - OISTER連携観測で明らかになったStarlink’s Visorsatの反射光低減効果
堀内貴史; 花山秀和; 大石雅寿; 中岡竜也; 高橋隼; 山中雅之; 野上大作; 大朝由美子; 村田勝寛; 高木聖子
Volume：2023, 2023
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山下真依; 伊藤洋一; 高木悠平; 大朝由美子
Volume：2023, 2023
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金井昂大; 大朝由美子; 高橋英則; 橋本修
Volume：2023, 2023
ISSN：1347-0639, J-Global ID：202302242014449826 - 高校生・大学生を対象としたプラネタリウム番組制作を通した天文教育の実践報告(1)
小田達功; 大朝由美子
Volume：2023, 2023
ISSN：1347-0639, J-Global ID：202302242106078026 - 高校生・大学生を対象としたプラネタリウム番組制作を通した天文教育の実践報告(2)
大朝由美子; 小田達功
Volume：2023, 2023
ISSN：1347-0639, J-Global ID：202302254057248610 - Lupus領域の前主系列星に付随する原始惑星系円盤の進化時間
高木悠平; 伊藤洋一; 大朝由美子
Volume：2023, 2023
ISSN：1347-0639, J-Global ID：202302254111713727 - 史上最大規模の矮新星アウトバースト:MASTER OT J030227.28+191754.5
反保雄介; 磯貝桂介; 小路口直冬; 加藤太一; 伊藤潤平; 野上大作; 木邑真理子; 大朝由美子; 村田勝寛; 堀内貴史; 中岡竜也; 高橋隼; 松本桂; 酒向重行
Volume：2023, 2023
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大朝由美子; 奥田大翔; 小柳香
Volume：2023, 2023
ISSN：1347-0639, J-Global ID：202302221586036570 - 前主系列星の正確な有効温度の決定と微弱な彩層輝線の検出
山下真依; 伊藤洋一; 高木悠平; 大朝由美子
Volume：2023, 2023
ISSN：1347-0639, J-Global ID：202302237698196670 - 太陽型の前主系列星の彩層活動と黒点・フレアによる光度変動の調査
山下真依; 伊藤洋一; 高木悠平; 大朝由美子
Volume：2023, 2023
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村田勝寛; 太田耕司; 野上大作; 高橋幸弘; 齊藤大晶; 大朝由美子; 土居守; 瀧田怜; 谷津陽一; 高橋一郎; 金田英宏; 楠根貴成; 伊藤洋一; 高橋隼; 川端弘治; 中岡竜也; 永山貴宏; 泉浦秀行; 花山秀和; 早津夏己
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大朝由美子; 熊澤希珠; 金井昂大; 石岡千寛
Volume：2022, 2022
ISSN：1347-0639, J-Global ID：202202259505248554 - 太陽型の零歳主系列星における活動性と黒点による光度変化
山下真依; 伊藤洋一; 大朝由美子
Volume：2022, 2022
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金井昂大; 大朝由美子; 大出康平; 大出康平; 高木悠平
Volume：2022, 2022
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山下真依; 伊藤洋一; 高木悠平; 大朝由美子
Volume：2022, 2022
ISSN：1347-0639, J-Global ID：202202237294632428 - 10年目のSaCRA望遠鏡:埼玉大学におけるさまざまな形態での教育利用や星空観望会
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Volume：2022, 2022
ISSN：1347-0639, J-Global ID：202202245183723629 - Spitzer IRAC Colors of Nebulae Associated with Star-Forming Regions
Yoichi Itoh; Yumiko Oasa
Volume：09, Number：01, First page：39, Last page：50, 2019
Star-forming regions are often associated with nebulosity. In this study, we
investigated infrared diffuse emission in Spitzer IRAC images. The infrared
nebula L1527 traces outflows emanating from a low-mass protostar. The nebular
color is consistent with the color of a stellar photosphere with large
extinction. Nebulae around the HII region W5-East are bright in the infrared.
These colors are consistent with the model color of dust containing polycyclic
aromatic hydrocarbon (PAH). The strength of ultraviolet irradiation of the
nebulae and the small dust fraction were deduced from the infrared colors of
the nebulae. We found that the edges of the nebulae are irradiated by strong
ultraviolet radiation and have abundant small dust. Dust at the surface of the
molecular cloud is thought to be destroyed by ultraviolet radiation from an
early-type star.
DOI：https://doi.org/10.4236/ijaa.2019.91004
DOI ID：10.4236/ijaa.2019.91004, ISSN：2161-4717, eISSN：2161-4725, arXiv ID：arXiv:2006.00221 - ドップラーシフト法による連星系の系外惑星探査
豊田英里; 松山浩子; 浦川聖太郎; 木村真二; 大朝由美子; 伊藤洋一; 佐藤文衛; 向井正
日本惑星科学会秋季講演会予稿集, Volume：2005, First page：87, 2005
Japanese
DOI：https://doi.org/10.14909/jsps.2005f.0.87.0
DOI ID：10.14909/jsps.2005f.0.87.0, J-Global ID：200902271369386137 - Coronagraph Imager with Adaptive Optics (CIAO): Description and first results
M Tamura; H Suto; Y Itoh; N Ebizuka; Y Doi; K Murakawa; SS Hayashi; Y Oasa; H Takami; N Kaifu
OPTICAL AND IR TELESCOPE INSTRUMENTATION AND DETECTORS, PTS 1 AND 2, Volume：4008, First page：1153, Last page：1161, 2000
We describe a near-infrared coronagraphic camera built for use with the Subaru 8.2-m telescope and its adaptive optics system. The purpose of this instrument CIAO (Coronagraph Imager with Adaptive Optics) is to obtain high-resolution (0.06 arcsec at 2 micron) images of faint objects in close vicinity of bright objects at infrared wavelengths. Such a desire is strong in astronomy, especially in the study of companion brown dwarfs and extra-solar planets, circumstellar disks around both young stellar objects and main-sequence stars, jets and outflows from both young stars and evolved stars, circumnuclear regions around AGNs, and host galaxies of QSOs. CIAO is a 1-5 micron camera with two focal plate scales: 22 milli-arcsec/pixel and 11 milli-arcsec/pixel. The camera is equipped with the standard broad-band filters (zJHKKsL'M') as well as a number of narrow-band filters. Choice of masks, filters and camera lenses and optical alignment with collimator and detector are made with cryogenic motors. CIAO utilizes one ALLADIN II (1024x1024 InSb) "science"-grade detector array manufactured by SBRC. Occulting masks whose diameter ranges from 0.1 to 3 arcsec and several types of pupil masks are selectable, all cooled down to about 60 K and the detector is cooled to about 30 K. Also available are a R less than or similar to 1000 grism with coronagraphic slits and a polarimetric module. We also present preliminary results from the first commissioning run (without the adaptive optics system) at the Subaru telescope.
SPIE-INT SOC OPTICAL ENGINEERING, English
ISSN：0277-786X, Web of Science ID：WOS:000089706500121
- 天文宇宙検定公式問題集 : 天文宇宙博士 : 1級
天文宇宙検定委員会
Apr. 2024
Japanese, Total pages：157p
CiNii Books：http://ci.nii.ac.jp/ncid/BD06654752
ISBN：9784769917038, CiNii Books ID：BD06654752 - 天文宇宙検定公式問題集 : 銀河博士 : 2級
天文宇宙検定委員会
Apr. 2024
Japanese, Total pages：177p
CiNii Books：http://ci.nii.ac.jp/ncid/BD06654785
ISBN：9784769917045, CiNii Books ID：BD06654785 - 星博士ジュニア
天文宇宙検定委員会
Mar. 2023
Japanese, Total pages：133p
CiNii Books：http://ci.nii.ac.jp/ncid/BD00984357
ISBN：9784769916949, CiNii Books ID：BD00984357 - 天文宇宙検定公式テキスト《2級 銀河博士》 2023～2024年版
大朝由美子ほか天文宇宙検定委員会 編
恒星社厚生閣, Mar. 2023
Japanese, Total pages：158p
CiNii Books：http://ci.nii.ac.jp/ncid/BD00984266
ISBN：9784769916925, CiNii Books ID：BD00984266 - 天文宇宙検定公式テキスト《3級 星空博士》 2023～2024年版
大朝由美子ほか天文宇宙検定委員会 編
恒星社厚生閣, Mar. 2023
Japanese, Total pages：133p
CiNii Books：http://ci.nii.ac.jp/ncid/BD00984288
ISBN：9784769916932, CiNii Books ID：BD00984288 - 世界で一番美しい太陽系図鑑―太陽から惑星や衛星、準惑星、彗星まで
マーカス チャウン(著)、大朝 由美子(監修)
誠文堂新光社, Feb. 2023
Japanese, Total pages：224p
CiNii Books：http://ci.nii.ac.jp/ncid/BD00790372
ISBN：9784416523520, CiNii Books ID：BD00790372 - 星空の図鑑〈2023年-2031年〉―月ごとに星や星座の見方がわかる
ウィル ゲイター(著)、ジャイルズ スパロウ(著)、大朝 由美子(監修)
誠文堂新光社, Jan. 2023
Japanese, Total pages：128p
CiNii Books：http://ci.nii.ac.jp/ncid/BD00390884
ISBN：9784416523209, CiNii Books ID：BD00390884 - 天文宇宙検定公式問題集 4級 星博士ジュニア 2022-2023年
大朝由美子、福江純ほか天文宇宙検定委員会
恒星社厚生閣, Jul. 2022
Total pages：140
ISBN：9784769916826 - 天文宇宙検定公式問題集 3級星空博士 2022-2023年
大朝由美子、福江純ほか天文宇宙検定委員会
恒星社厚生閣, Jul. 2022
Total pages：182
ISBN：9784769916819 - 天文宇宙検定公式問題集 1級 天文宇宙博士 2022-2023年
大朝由美子、福江純ほか天文宇宙検定委員会
恒星社厚生閣, Jul. 2022
Total pages：153
ISBN：9784769916796 - 天文宇宙検定公式問題集 2級 銀河博士 2022-2023年
大朝由美子、福江純ほか天文宇宙検定委員会
恒星社厚生閣, Jul. 2022
Japanese, Total pages：177p
CiNii Books：http://ci.nii.ac.jp/ncid/BC15678492
ISBN：9784769916802, CiNii Books ID：BC15678492 - すべての人の天文学
岡村定矩、芝井広、大朝由美子ほか
日本評論社, Mar. 2022
Japanese, Total pages：iii, 257p
CiNii Books：http://ci.nii.ac.jp/ncid/BC13856920
ISBN：9784535789463, CiNii Books ID：BC13856920 - すべての人の天文学
縣, 秀彦; 大山, 真満; 大朝, 由美子; 工藤, 哲洋; 岡村, 定矩; 芝井, 広
Mar. 2022
Japanese, Total pages：iii, 257p
CiNii Books：http://ci.nii.ac.jp/ncid/BC13200157
ISBN：9784535789463, CiNii Books ID：BC13200157 - 星博士ジュニア
天文宇宙検定委員会
Jul. 2021
Japanese, Total pages：133p
CiNii Books：http://ci.nii.ac.jp/ncid/BC08839762
ISBN：9784769916697, CiNii Books ID：BC08839762 - 天文宇宙検定公式テキスト3級 星空博士〈2021～2022年版〉
大朝由美子ほか天文宇宙検定編集委員会
恒星社厚生閣, Jul. 2021
Japanese, Total pages：133p
CiNii Books：http://ci.nii.ac.jp/ncid/BC08839751
ISBN：9784769916680, CiNii Books ID：BC08839751 - 天文宇宙検定公式テキスト2級 銀河博士〈2021～2022年版〉
大朝由美子ほか天文宇宙検定編集委員会
恒星社厚生閣, Jul. 2021
Japanese, Total pages：158p
CiNii Books：http://ci.nii.ac.jp/ncid/BC09078220
ISBN：9784769916673, CiNii Books ID：BC09078220 - 天文宇宙検定公式問題集1級 天文宇宙博士〈2020～2021年版〉
大朝由美子ほか天文宇宙検定編集委員会
恒星社厚生閣, Jul. 2020
Japanese, Total pages：161p
CiNii Books：http://ci.nii.ac.jp/ncid/BC01265687
ISBN：9784769916499, CiNii Books ID：BC01265687 - 天文宇宙検定公式問題集4級 星博士ジュニア〈2020～2021年版〉
大朝由美子ほか天文宇宙検定編集委員会
恒星社厚生閣, Jul. 2020
Japanese, Total pages：139p
CiNii Books：http://ci.nii.ac.jp/ncid/BC01265712
ISBN：9784769916529, CiNii Books ID：BC01265712 - 天文宇宙検定公式問題集2級 銀河博士〈2020～2021年版〉
大朝由美子ほか天文宇宙検定編集委員会
恒星社厚生閣, Jul. 2020
Japanese, Total pages：173p
CiNii Books：http://ci.nii.ac.jp/ncid/BC01265698
ISBN：9784769916505, CiNii Books ID：BC01265698 - 天文宇宙検定公式問題集3級 星空博士〈2020～2021年版〉
大朝由美子ほか天文宇宙検定編集委員会
恒星社厚生閣, Jul. 2020
Japanese, Total pages：177p
CiNii Books：http://ci.nii.ac.jp/ncid/BC01265701
ISBN：9784769916512, CiNii Books ID：BC01265701 - 文部科学省検定済教科書 中学校理科用 理科の世界3
有馬朗人、大朝由美子ほか69名
大日本図書, Mar. 2020
Total pages：373
ISBN：9784477031774 - 文部科学省検定済教科書 中学校理科用 理科の世界2
有馬朗人、大朝由美子ほか69名
大日本図書, Mar. 2020
Total pages：317
ISBN：9784477031767 - 文部科学省検定済教科書 中学校理科用 理科の世界1
有馬朗人、大朝由美子ほか69名
大日本図書, Mar. 2020
Total pages：294
ISBN：9784477031750 - 極・宇宙を解く: 現代天文学演習
大朝由美子、福江 純, 沢 武文, 高橋 真聡ほか,
恒星社厚生閣, Feb. 2020
Japanese, Total pages：vi, 301p
CiNii Books：http://ci.nii.ac.jp/ncid/BB2983409X
ISBN：9784769916437, CiNii Books ID：BB2983409X - 天文宇宙検定公式テキスト3級 星空博士〈2019～2020年版〉
大朝由美子ほか天文宇宙検定編集委員会
恒星社厚生閣, Jun. 2019
Total pages：133
ISBN：9784769916376 - 天文宇宙検定公式テキスト2級 銀河博士〈2019～2020年版〉
大朝由美子ほか天文宇宙検定編集委員会
恒星社厚生閣, Jun. 2019
Total pages：158
ISBN：9784769916369 - 天文宇宙検定 4級 公式問題集 2018-2019
大朝由美子、福江純ほか天文宇宙検定委員会
恒星社厚生閣, Jul. 2018
Total pages：132
ISBN：9784769916253 - 天文宇宙検定公式問題集3級 星空博士〈2018～2019年版〉
大朝由美子ほか天文宇宙検定編集委員会
恒星社厚生閣, Jul. 2018
Total pages：166
ISBN：9784769916246 - 天文宇宙検定公式問題集2級 銀河博士〈2018～2019年版〉
大朝由美子ほか天文宇宙検定編集委員会
恒星社厚生閣, Jul. 2018
Total pages：174
ISBN：9784769916239 - 天文宇宙検定公式問題集1級 天文宇宙博士〈2018～2019年版〉
大朝由美子、沢武史、福江純、ほか天文宇宙検定編集委員会
恒星社厚生閣, Jul. 2018
Total pages：154
ISBN：9784769916222 - 天文宇宙検定公式テキスト3級星空博士 (2017年~2018年版)
大朝由美子、富田晃彦、冨田良雄、仲野誠、成田直、福江純、室井恭子, 天文宇宙検定編集委員会
恒星社厚生閣, May 2017
Total pages：134
ISBN：9784769916055 - 天文宇宙検定公式テキスト2級銀河博士 (2017年~2018年版)
大朝由美子、沢武史、富田晃彦、冨田良雄、福江純、松村雅文、室井恭子、吉富進、天文宇宙検定編集委員会
恒星社厚生閣, May 2017
Total pages：160
ISBN：9784769916048 - 天文宇宙検定 4級 公式問題集 2016-2017
大朝由美子、福江純ほか天文宇宙検定委員会
恒星社厚生閣, Aug. 2016
Total pages：128
ISBN：9784769915928 - 天文宇宙検定 3級 公式問題集2016-2017
天文宇宙検定委員会(大朝由美子含む)
恒星社厚生閣, Aug. 2016
Total pages：166
ISBN：9784769915911 - 天文宇宙検定 2級 公式問題集 2016-2017
天文宇宙検定委員会(大朝由美子含む)
恒星社厚生閣, Aug. 2016
Total pages：174
ISBN：9784769915904 - 天文宇宙検定 1級公式問題集 2016-2017
天文宇宙検定委員会(大朝由美子含む)
恒星社厚生閣, Aug. 2016
Total pages：150
ISBN：9784769915898 - 天文宇宙検定 3級 星空博士 公式テキスト 2015-2016
天文宇宙検定委員会(大朝由美子含む)
恒星社厚生閣, Jul. 2015
Total pages：132
ISBN：9784769915652 - 天文宇宙検定 2級 銀河博士 公式テキスト 2015-2016
天文宇宙検定委員会(大朝由美子含む)
恒星社厚生閣, Jul. 2015
Total pages：134
ISBN：9784769915645 - 文部科学省検定済教科書中学校理科用 新版理科の世界3年
有馬朗人、大朝由美子ほか61名
大日本図書, Mar. 2015
Total pages：333
ISBN：9784477027142 - 文部科学省検定済教科書中学校理科用 新版理科の世界2年
有馬朗人、大朝由美子ほか61名
大日本図書, Mar. 2015
Total pages：309
ISBN：9784477027135 - 文部科学省検定済教科書中学校理科用 新版理科の世界1年
有馬朗人、大朝由美子ほか61名
大日本図書, Mar. 2015
Total pages：285
ISBN：9784477027128 - 天文宇宙検定 1級 天文宇宙博士 公式問題集 2014-2015
天文宇宙検定委員会(大朝由美子含む)
恒星社厚生閣, Aug. 2014
Total pages：144
ISBN：9784769914778 - 天文宇宙検定 3級 星空博士 公式問題集 2014-2015
天文宇宙検定委員会(大朝由美子含む)
恒星社厚生閣, Aug. 2014
Japanese, Total pages：冊
CiNii Books：http://ci.nii.ac.jp/ncid/BB16495606
ISBN：9784769914792, CiNii Books ID：BB16495606 - 天文宇宙検定 4級 星博士ジュニア 公式問題集 2014-2015
福江 純,沢 武文大朝由美子含む)
恒星社厚生閣, Aug. 2014
Japanese, Total pages：冊
CiNii Books：http://ci.nii.ac.jp/ncid/BB16495752
ISBN：9784769914808, CiNii Books ID：BB16495752 - 天文宇宙検定2級公式問題集 2014－2015
大朝由美子、福江純、ほか天文宇宙検定委員会
恒星社厚生閣, Aug. 2014
Japanese, Total pages：冊
CiNii Books：http://ci.nii.ac.jp/ncid/BB16495366
ISBN：9784769914785, CiNii Books ID：BB16495366 - 超・宇宙を解く―現代天文学演習
大朝由美子、福江 純、沢 武文、高橋真聡、松本 桂、 濤崎智佳
恒星社厚生閣, Jul. 2014
Japanese, Total pages：vi, 286p
CiNii Books：http://ci.nii.ac.jp/ncid/BB15932104
ISBN：9784769914747, CiNii Books ID：BB15932104 - 天文宇宙検定 3級 星空博士 2013－2014
大朝由美子、富田晃彦、冨田良雄、仲野誠、成田直、福江純、室井恭子
恒星社厚生閣, May 2013
Total pages：128
ISBN：9784769913016 - 天文宇宙検定 2級銀河博士 2013-2014
大朝由美子、沢武史、時政典孝、富田晃彦、冨田良雄、福江純、松村雅文、室井恭子、吉富進
恒星社厚生閣, May 2013
Total pages：152
ISBN：9784769913023 - 星博士ジュニア
天文宇宙検定委員会
Aug. 2012
Japanese, Total pages：冊
CiNii Books：http://ci.nii.ac.jp/ncid/BB10622507
ISBN：9784769912743, CiNii Books ID：BB10622507 - 天文宇宙検定公式問題集《１級 天文宇宙博士》
大朝由美子、福江純、ほか天文宇宙検定委員会
恒星社厚生閣, Jul. 2012
Japanese, Total pages：冊
CiNii Books：http://ci.nii.ac.jp/ncid/BB10262081
ISBN：9784769912781, CiNii Books ID：BB10262081 - 天文宇宙検定 銀河博士 2011-2012年度版
大朝由美子、福江純ほか
恒星社厚生閣, Aug. 2011
Japanese, Total pages：冊
CiNii Books：http://ci.nii.ac.jp/ncid/BB06692677
ISBN：9784769912538, CiNii Books ID：BB06692677 - 天文宇宙検定 星空博士 2011-2012年度版
大朝由美子、富田晃彦、冨田良雄、仲野誠、成田直、福江純、室井恭子
恒星社厚生閣, Jun. 2011
Total pages：130
ISBN：4769912528 - 星空博士
天文宇宙検定委員会
Jun. 2011
Japanese, Total pages：冊
CiNii Books：http://ci.nii.ac.jp/ncid/BB06059233
ISBN：9784769912521, CiNii Books ID：BB06059233 - 天文宇宙検定公式テキスト《3級 星空博士》 2023～2024年版
大朝由美子ほか天文宇宙検定委員会 編
恒星社厚生閣
Total pages：136 - 天文宇宙検定公式テキスト《2級 銀河博士》 2023～2024年版
大朝由美子ほか天文宇宙検定委員会 編
恒星社厚生閣
Total pages：160 - 天文宇宙検定 星空博士
大朝由美子、富田晃彦、冨田良雄、仲野誠、成田直、福江純、室井恭子
恒星社厚生閣
Total pages：127 - 天文宇宙検定 銀河博士
大朝由美子、沢武史、時政典孝、富田晃彦、冨田良雄、福江純、松村雅文、室井恭子
恒星社厚生閣
Total pages：135 - 国立天文台
大朝由美子ほか
すばる＋TMTサイエンスブック2020ｰすばる望遠鏡とTMTで結ぶ新たな宇宙像ー
Total pages：90
- Formation of very low mass objects on various Clouds
Oasa Yumiko
web, Mar. 2024, [International conference] - 光・赤外線天文学大学間連携事業の教育事業について
高橋隼、大朝由美子
Web, Mar. 2024, [Domestic conference] - Ultimate-Study of Star Formation
Takagi Yuhei, Oasa Yumiko
web, Jan. 2024, [International conference] - ぐんま天文台150cm望遠鏡とMuSaSHI
大朝由美子
Web, Sep. 2023, [Domestic conference] - 前主系列星の正確な有効温度の決定と微弱な彩層輝線の検出
山下真依、伊藤洋一、高木悠平、大朝由美子
web, Sep. 2023, [Domestic conference] - 太陽型の前主系列星の彩層活動と黒点・フレアによる光度変動の調査
山下真依、伊藤洋一、高木悠平、大朝由美子
web, Sep. 2023, [Domestic conference] - 光赤外線大学間連携OISTER によるマルチメッセンジャー天文学
村田勝寛, 太田耕司, …大朝由美子ほか光赤外線大学間連携
web, Sep. 2023, [Domestic conference] - Report on practical astronomical education through planetarium program production for high school and university students
Oasa, Y., Oda, T.
Global Hands-on Universe, Aug. 2023, [International conference] - Research and education experience using the SaCRA telescope for teacher training undergraduate students
Oasa, Yumiko
Web, Aug. 2023, [International conference] - Measurement of starspots and chromospheric emission lines of pre-main-sequence stars
Yamashita, M., Itoh, Y., Takagi, Y., Oasa, Y.
Web, Aug. 2023, [International conference] - NIR Photometric/Spectroscopic Observations of Very Low-Mass Objects in R CrA Region
Kanai, T., Oasa, Y.,
Web, Aug. 2023, [International conference] - Optical and Infrared Synergetic Telescopes for Education and Research (OISTER) Project
Oasa, Y., Murata, K., OISTER collaboration team
Web, Aug. 2023, [International conference] - Revealing the Evolution Timescale of Protoplanetary Disks with High-resolution Spectroscopy
Takagi, Y.., Itoh, Y., Oasa, Y.
Web, Apr. 2023, [International conference] - Starspots, chromospheric emission lines, and flares of pre-main-sequence stars
Yamashita, M., Itoh, Y., Takagi, Y., Oasa, Y.
Web, Apr. 2023, [International conference] - A Deep NIR Survey of Very-low mass Objects in the R CrA Region
Kanai Takahiro, Oasa Yumiko
Web, Mar. 2023, [International conference] - 前主系列星の可視光高分散分光観測
山下 真依, 伊藤 洋一 , 高木 悠平, 大朝 由美子
Web, Mar. 2023, [Domestic conference] - 三波長同時撮像装置MuSaSHIのぐんま天文台150cm望遠鏡搭載と観測(2)
金井昂大, 大朝由美子, 高橋英則 , 橋本修
Web, Mar. 2023, [Domestic conference] - OISTER 連携観測で明らかになった Starlink’s Visorsat の反射光低減効果
堀内 貴史, 花山 秀和,大朝由美子ほか
Web, Mar. 2023, [Domestic conference] - Lupus 領域の前主系列星に付随する原始惑星系円盤の進化時間
高木悠平、伊藤洋一、大朝由美子
Web, Mar. 2023, [Domestic conference] - 星団形成領域 Corona Australis 分子雲内部のフィラメント状構造
深谷直史, 立原研悟, 大朝由美子ほか
Web, Mar. 2023, [Domestic conference] - 高校生・大学生を対象としたプラネタリウム番組制作を通した天文教育の実践報告（2）
大朝由美子、小田達功
Web, Mar. 2023, [Domestic conference] - 高校生・大学生を対象としたプラネタリウム番組制作を通した天文教育の実践報告 (1)
小田達功、大朝由美子
Web, Mar. 2023, [Domestic conference] - 若い太陽型星の可視光分光観測
山下 真依, 伊藤 洋一 , 高木 悠平, 大朝 由美子
Web, Feb. 2023, [Domestic conference] - 若い太陽型星の磁気活動の調査
山下 真依, 伊藤 洋一, 大朝 由美子
Web, Feb. 2023, [Domestic conference] - ALMA観測で探るCorona Australis分子雲におけるフィラメント状構造の性質
深谷直史, 立原研悟, 大朝由美子ほか
Web, Feb. 2023, [Domestic conference] - 三波長同時撮像装置MuSaSHIのぐんま天文台150cm望遠鏡搭載と観測
金井昂大, 大朝由美子, 高橋英則 , 橋本修
Web, Feb. 2023, [Domestic conference] - R CrA領域における超低質量天体の近赤外探査観測
金井 昂大, 大朝由美子
Web, Feb. 2023, [Domestic conference] - 教育事業について (短期滞在実習、装置開発支援)
高橋隼、大朝由美子
Web, Feb. 2023, [Domestic conference] - 埼玉大学SaCRA望遠鏡とぐんま天文台1.5m望遠鏡の現況報告
大朝由美子
Web, Feb. 2023, [Domestic conference] - R CrA領域における若い超低質量天体の近赤外探査観測
金井 昂大, 大朝由美子
Web, Feb. 2023, [Domestic conference] - Ultimate-Study of Star Formation
Oasa Yumiko, Takagi Yuhei
Jan. 2023, [International conference] - A Photometric/Spectroscopic Study of Very low-mass objects in R CrA with Subaru/MOIRCS
Kanai Takahiro, Oasa Yumiko
Web, Jan. 2023, [International conference] - 若い太陽型星の黒点とフレアによる変光の調査
山下 真依, 伊藤 洋一 , 高木 悠平, 大朝 由美子
Web, Dec. 2022, [Domestic conference] - 三波長同時撮像装置MuSaSHIの ぐんま天文台150cm望遠鏡 搭載と観測
金井昂大, 大朝由美子, 高橋英則 , 橋本修
Web, Dec. 2022, [Domestic conference] - クロージングリマーク：光赤天連の展望
大朝由美子
Nov. 2022, [Domestic conference] - 短期滞在実習プログラムについて
高橋隼、大朝由美子
web, Nov. 2022, [Domestic conference] - 余剰ファイバーを用いた PFS-星形成案
大朝由美子
Oct. 2022, [Domestic conference] - 埼玉大学SaCRA望遠鏡と光赤外大学連携事業の取り組み
大朝由美子
web, Oct. 2022, [Domestic conference] - R CrA 領域における若い超低質量天体の近赤外分光観測
金井 昂大, 大朝由美子, 大出康平, 高木悠平
Web, Sep. 2022, [Domestic conference] - 10 年目の SaCRA 望遠鏡：埼玉大学におけるさまざまな形態での教育利用や 星空観望会
大朝由美子, 金井昂大, 奥田大翔, 小柳香, 佐藤陸人, 中田伊織 (埼玉大学), 大島吾一, 高原佑典, 星久 樹, 佐藤太基, 石橋遥子, 潮田和俊, 柴田吉輝, 小田達功, 平塚雄一郎, 石岡千寛, 大出康平ほか埼玉大 学教育学部/大学院教育学研究科・理工学研究科天文学研究室 OB・OG
Web, Sep. 2022, [Domestic conference] - 前主系列星の彩層活動と黒点による光度変化の調査
山下 真依, 伊藤 洋一 , 高木 悠平, 大朝 由美子
Web, Sep. 2022, [Domestic conference] - 地上からのフォローアップ観測：OISTER
野上大作、大朝由美子ほかOISTERコンソーシアム
Web, Sep. 2022, [Domestic conference] - 光赤外線大学間連携における連携観測
山中雅之、大朝由美子、et al.
Web, Aug. 2022, [Domestic conference] - 多波長トランジット測光観測から探る系外惑星大気
大朝由美子,石岡千寛, 金井昂大, 高橋隼、伊藤洋一
Web, Aug. 2022, [Domestic conference] - Measurements of Dynamo Activity and Spots of Zero-Age Main-Sequence Stars with TESS
Yamashita, Mai, Itoh, Yoichi, Takagi, Yuhei, Oasa, Yumiko
Web, Jul. 2022, [International conference] - Activities and starspots of young solar-type stars
Yamashita, Mai, Itoh, Yoichi, Takagi, Yuhei, Oasa, Yumiko
Jul. 2022, [International conference] - 若い太陽型星における活動性と黒点による光度変化
山下 真依, 伊藤 洋一, 高木悠平, 大朝 由美子
Web, Mar. 2022, [Domestic conference] - 太陽型の零歳主系列星における活動性と黒点による光度変化
山下 真依, 伊藤 洋一, 大朝 由美子
Web, Mar. 2022, [Domestic conference] - ALMA ACA サーベイで探る Corona Australis 領域の星形成 (4)
西岡丈翔, 立原研悟, 大朝由美子ほか
Web, Mar. 2022, [Domestic conference] - ぐんま天文台 150cm 望遠鏡への三波長同時撮像装置 MuSaSHI の搭載と観測
金井昂大, 大朝由美子, 高橋英則, 橋本修
Web, Mar. 2022, [Domestic conference] - 埼玉大学 SaCRA 望遠鏡/MuSaSHI と 36cm 望遠鏡 を用いた、系外惑星の多波 長トランジット測光観測
大朝由美子,熊澤希珠,金井昂大,石岡千寛
Web, Mar. 2022, [Domestic conference] - 高銀緯分子雲MBM16,24 における深い可視分光探査観測
大朝由美子,佐々木優
Web, Mar. 2022, [Domestic conference] - 光・赤外大学間連携事業”OISTER”の現状と将来
大朝由美子
web, Dec. 2021, [Domestic conference] - 光赤外線大学間連携事業の活動報告
山中雅之,...大朝由美子,...ほか光赤外線大学間連携事業メンバー
日本天文学会春季年会予稿集, Mar. 2021, [Domestic conference] - 月面地球照の近赤外観測で検出された海の偏光
高橋隼,伊藤洋一,松尾太郎,大朝由美子, Yoonsoo P. Bach,石黒正晃
日本天文学会春季年会予稿集, Mar. 2021, [Domestic conference] - 超低光度前主系列星J162656.43-243超低光度前主系列星J162656.43-243301.5周囲のtransition diskのALMA観測II301.5周囲のtransition diskのALMA観測II
杉谷朱泉,高桑繁久,川邊良平,島尻芳人,塚越崇,中村文隆,田村元秀,大朝由美子,坪井陽子,富田賢吾,原千穂美
日本天文学会春季年会予稿集, Mar. 2021, [Domestic conference] - Lupus IとR CrAにおける若い超低質量天体の近赤外測光探査
金井昂大, 大朝由美子
日本天文学会春季年会予稿集, Mar. 2021, [Domestic conference] - 銀河面における前主系列星の広域探査観測
竹内媛香,大朝由美子,大出康平,木内穂貴,平塚雄一郎,本田敏志,伊藤洋一,高木悠平,橋本修
日本天文学会春季年会予稿集, Mar. 2021, [Domestic conference] - へび座分子雲における若い超低質量天体の近赤外分光観測る褐色矮星・惑星質量天体の近赤外測光探査観測
大出康平,大朝由美子,Malte Schramm,小田達功,中岡竜也,高木悠平,伊藤洋一
日本天文学会春季年会予稿集, Mar. 2021, [Domestic conference] - はえ座分子雲における褐色矮星・惑星質量天体の近赤外測光探査観測
大朝由美子, 伊佐勇亮,金井昂大
日本天文学会春季年会予稿集, Mar. 2021, [Domestic conference] - Lunar Earthshine Polarimetry in Near-Infrared: Signature of Ocean Glint
Takahashi Jun, Itoh Yoichi, Matsuo Taro, Oasa Yumiko, Yoonsoo P. Bach, Ishiguro Masateru
Web, Mar. 2021, [International conference] - Near-Infrared Photometry and Spectroscopy of Young Brown Dwarfs and Planetary-mass Objects in Serpens
Yumiko Oasa, Kohei Oide, Takumi Shigeyosi, Yuhei Takagi, Yoichi Itoh
Web, Mar. 2021, [International conference] - Mulit-wavelength SimultaneouS High throughput Imager and polarimeter (MuSaSHI) : development and its performance
Yumiko Oasa, Kazutoshi Ushioda, Yoshiki Shibata, Genta Seino, Masaru Kino, Hiroshi Akitaya
Proceedings of the SPIE, Dec. 2020, [International conference] - NICによる地球照偏光観測: 海の検出
高橋隼、伊藤洋一、松尾太郎、大朝由美子、Yoonsoo P. Bach、石黒正晃
(Web), Nov. 2020, [Domestic conference] - 低温度ガス惑星の多波長トランジット観測
宝田拓也, 大朝由美子, 石岡千寛, 大出康平, 金井昂大, 竹内媛香
(Web), Nov. 2020, [Domestic conference] - 埼玉大学SaCRA望遠鏡・観測装置と大学間連携観測の現況
大朝由美子
(Web), Nov. 2020, [Domestic conference] - 野辺山45m鏡FOREST受信機による銀河面COサーベイデータを用いた分子雲形成の観測的研究
中西裕之、藤田真司、立原研悟、泉奈津子、松尾光洋、梅本智文、大朝由美子、井上剛志
日本天文学会秋季年会予稿集, Sep. 2020, [Domestic conference] - ALMA ACAサーベイで探るCorona Australis領域の星形成(1):初期成果
立原研悟,山崎康正,徳田一起,藤城翔,金井昂大,大朝由美子,西合一矢,深川美里,町田正博
日本天文学会秋季年会予稿集, Sep. 2020, [Domestic conference] - 光赤外線大学間連携における連携観測
山中雅之、高木聖子、高橋隼、Malte Schramn、宝田拓也、大朝由美子、et al.
Web, Aug. 2020, [Domestic conference] - 光赤外線大学間連携における教育活動の報告
高橋隼,大朝由美子
Web, Aug. 2020, [Domestic conference] - 太陽系外惑星の多波長トランジット測光観測
石岡千寛、大朝由美子,宝田拓也, 高橋隼、伊藤洋一
Web, Aug. 2020, [Domestic conference] - 銀河面における前主系列星の広域探査観測
竹内媛香, 大朝由美子、木内穂貴,大出康平, 鵜澤由規,田村泰樹,平塚雄一郎,伊藤洋一,本田敏志,高木悠平
Web, Aug. 2020, [Domestic conference] - NRO銀河面サーベイプロジェクト（FUGIN):巨大分子雲複合体W43における高密度ガスと大質量星形成シナリオⅢ
河野樹人,立原研悟,,...大朝由美子ほかFUGINチーム
日本天文学会春季年会予稿集, Mar. 2020, [Domestic conference] - OISTERで実現したこと、いま目指すべき道
川端弘治,関口和寛,,...大朝由美子ほかOISTERコンソーシアム
日本天文学会春季年会予稿集, Mar. 2020, [Domestic conference] - 光赤外線大学間連携における観測企画運営委員会の活動と有機的連携の実現
山中雅之, 野上大作,...大朝由美子ほか光赤外線大学間連携関係者
日本天文学会春季年会予稿集, Mar. 2020, [Domestic conference] - BH X線連星MAXI J1820+070の2019年の再増光時における多波長観測（２）
安達稜, 村田勝寛…大朝由美子ほか光赤外線大学間連携メンバー
日本天文学会春季年会予稿集, Mar. 2020, [Domestic conference] - 科学ライブショー「ユニバース」におけるライブ天体観測
41. 亀谷和久、大朝由美子ほか科学ライブショー「ユニバース」関係者一同
日本天文学会春季年会予稿集, Mar. 2020, [Domestic conference] - 銀河面における前主系列星の可視分光探査観測
竹内媛香,大朝由美子, 木内穂貴,大出康平, 鵜澤由規,田村泰樹,平塚雄一郎,伊藤洋一,本田敏志,高木悠平
日本天文学会春季年会予稿集, Mar. 2020, [Domestic conference] - FU Ori型星V960 Monの高分散分光観測
高木悠平,本田敏志、高橋隼、伊藤洋一,新井彰,大朝由美子
日本天文学会春季年会予稿集, Mar. 2020, [Domestic conference] - 埼玉大学望遠鏡・装置制御系 “SaCRA システム”および 36cm 望遠鏡の改良
金井昂大, 鵜澤由規, 石岡千寛, 宝田拓也, 大朝由美子, 柴田吉輝, 秋田谷洋
日本天文学会春季年会予稿集, Mar. 2020, [Domestic conference] - 重力波観測ランO3におけるJ-GEMのすばるでの観測状況とTMTとの連携
大神隆幸, 冨永望…大朝由美子ほかJ-GEM Collaboration
日本天文学会秋季年会予稿集, Sep. 2019, [Domestic conference] - BH X線連星MAXI J1820+070の2019年の再増光時における多波長観測
安達稜, 村田勝寛…大朝由美子ほか光赤外線大学間連携メンバー
日本天文学会秋季年会予稿集, Sep. 2019, [Domestic conference] - 埼玉大学55cm望遠鏡SaCRA/MuSaSHIを用いた太陽系外惑星の多波長トランジット測光観測
石岡千寛,大朝由美子
天文・天体物理若手の会予稿集, Jul. 2019, [Domestic conference] - へび座分子雲における低質量YSOの近赤外分光観測
大出康平,大朝由美子
天文・天体物理若手の会予稿集, Jul. 2019, [Domestic conference] - 銀河面低密度領域における星形成の広域探査観測
竹内媛香,大朝由美子
天文・天体物理若手の会予稿集, Jul. 2019, [Domestic conference] - 近赤外広視野観測から探る褐色矮星・惑星質量天体とIMF
Yumiko Oasa
(Web), Jul. 2019, [International conference] - Investigation of the Initial Mass Function at Very Low-Mass Side: Is it universal?
Yumiko Oasa
(Web), Mar. 2019, [International conference] - NRO銀河面サーベイプロジェクト(FUGIN) :銀河面における分子雲中の高密度ガス質量比の定量
鳥居和史,藤田真司,西村淳,...大朝由美子ほかFUGINチーム
日本天文学会春季年会予稿集, Mar. 2019, [Domestic conference] - NRO銀河面サーベイプロジェクト(FUGIN):巨大分子雲複合体W43における高密度ガスとミニスターバーストII
河野樹人,立原研悟,藤田真司,西村淳,大浜晶生,…大朝由美子ほかFUGINチーム
日本天文学会春季年会予稿集, Mar. 2019, [Domestic conference] - 月食偏光の比較: 2014年10月8日と2015年4月4日
高橋 隼,伊藤 洋一,渡邉 誠,秋田谷 洋,高木 勝俊,川端 弘治,伊藤 亮介,大朝 由美子,石橋 遥子
日本天文学会春季年会予稿集, Mar. 2019, [Domestic conference] - RCrAにおける惑星質量天体/褐色矮星の近赤外測光探査観測
大朝由美子,金井昂大
日本天文学会春季年会予稿集, Mar. 2019, [Domestic conference] - SaCRA望遠鏡の自動観測・即時解析化に向けた環境構築
5. 秋田谷洋、大朝由美子
(Web), Dec. 2018, [Domestic conference] - 埼玉大学の大学間連携共同観測について
大朝由美子
(Web), Dec. 2018, [Domestic conference] - NRO銀河面サーベイプロジェクト(FUGIN)：銀経10°－20°でのホットコアカタログ
佐藤一樹,長谷川哲夫,梅本智文,…大朝由美子ほかFUGINチーム
日本天文学会秋季年会予稿集, Sep. 2018, [Domestic conference] - NRO銀河面サーベイプロジェクト(FUGIN) : Spitzer Bubble N4の星形成(2)
藤田真司,西村淳,河野樹人,立原研悟,大浜晶生,…大朝由美子ほかFUGINチーム
日本天文学会秋季年会予稿集, Sep. 2018, [Domestic conference] - 銀河面における前主系列星の広域探査
木内穂貴,大朝由美子,平塚雄一郎,伊藤洋一,本田敏志,高木悠平,松尾光洋
日本天文学会秋季年会予稿集, Sep. 2018, [Domestic conference] - Gaia 衛星データと分光観測に基づく高銀緯分子雲における星形成探査
大朝由美子,岩澤司季,木内穂貴,平塚雄一郎
日本天文学会秋季年会予稿集, Sep. 2018, [Domestic conference] - 埼玉大学SaCRA望遠鏡・装置と突発天体観測対応の現状
秋田谷洋、大朝由美子ほか計8名
(Web), Jul. 2018, [Domestic conference] - 銀河面における T タウリ型星の広域探査
大朝由美子 , 木内穂貴 , 平塚雄一郎, 中村一貴, 伊藤洋一 , 本田敏志, 高木悠平
日本天文学会春季年会予稿集, Mar. 2018, [Domestic conference] - 近赤外観測から探るへび座分子雲における超低質量天体形成
小田達功 , 大朝由美子, 佐藤太基
日本天文学会春季年会予稿集, Mar. 2018, [Domestic conference] - 高銀緯分子雲における星形成の分光探査観測 (2)
平塚雄一郎、大朝由美子、木内穂貴、伊藤洋一 、中岡竜也、川端美穂 、高木悠平 、山本宏昭
日本天文学会春季年会予稿集, Mar. 2018, [Domestic conference] - NRO 銀河面サーベイプロジェクト (FUGIN) : 爆発的星形成領域 W43 の CO 輝 線観測I
河野樹人 , 立原研悟 , 藤田真司 , 西村淳 , 大浜晶生 , 福井康雄...大朝由美子ほかFUGINチーム
日本天文学会春季年会予稿集, Mar. 2018, [Domestic conference] - NRO 銀河面サーベイプロジェクト (FUGIN) : Spitzer Bubble N4 の星形成
藤田真司 , 西村淳 , 河野樹人 , 立原研悟 , 大浜晶生 , 佐野栄俊 , 林克洋 , 榎谷玲依 , 吉池智史 , 堤大陸 , 大 河一貴 , 福井康雄...大朝由美子ほかFUGINチーム
日本天文学会春季年会予稿集, Mar. 2018, [Domestic conference] - NRO 銀河面サーベイプロジェクト (FUGIN): ホットコアの無バイアスサーベイ (2) 解析手法の改良と銀経10－20degの解析結果
佐藤一樹, 長谷川哲夫 , 梅本智文 , 南谷哲宏 , 鳥居和史 , 阪本成一...ほかFUGINチーム
日本天文学会春季年会予稿集, Mar. 2018, [Domestic conference] - 埼玉大学における中・高校生への天文学の研究体験指導 (2)
平塚雄一郎、大朝由美子、小田達功、木内穂貴
日本天文学会春季年会予稿集, Mar. 2018, [Domestic conference] - 埼玉大学の大学間連携の取り組み報告
大朝由美子
(Web), Dec. 2017, [Domestic conference] - 3波長同時偏光撮像装置“MuSaSHI”偏光観測ユニットの開発及び試験観測の状況
大朝由美子、清野玄太、荒沼佳純、平塚雄一郎、木内穂貴、潮田和俊、柴田吉輝、木野勝、秋田谷洋、伊藤洋一、高橋隼
(Web), Nov. 2017, [Domestic conference] - 岡山91cm望遠鏡を用いた銀河円盤部における前主系列星の近赤外変光探査観測
大朝由美子、伊藤茉由、柳澤顕史
(Web), Sep. 2017, [Domestic conference] - 高銀緯分子雲における星形成の分光探査観測
平塚雄一郎、大朝由美子、木内穂貴、伊藤洋一 、中岡竜也、川端美穂 、安部太晴、高木悠平 、山本宏昭
日本天文学会秋季年会予稿集, Sep. 2017, [Domestic conference] - NRO 銀河面サーベイプロジェクト (FUGIN) ：最終年度報告
梅本智文 , 南谷哲宏 , 鳥居和史 ,松尾光洋 , 長谷川哲夫 , 水野範和 , 廣田明彦 , 本間希樹 , Muller, E., 亀谷 和久 , 井上剛志,....大朝由美子ほか
日本天文学会秋季年会予稿集, Sep. 2017, [Domestic conference] - NRO 銀河面サーベイプロジェクト (FUGIN): 銀河系外縁部 (4)
松尾光洋 , 南谷哲宏 , 鳥居和史 , 梅本智文,中西裕之, 久野成夫, 西村淳 , 藤田真司 , 河野樹人, 山岸光義...大朝由美子ほかFUGINチーム
日本天文学会秋季年会予稿集, Sep. 2017, [Domestic conference] - NRO 銀河面サーベイプロジェクト (FUGIN): 銀河系内域における分子雲同定
齋藤弘雄 , 久野成夫, 梅本智文 , 鳥居和史 , 西村淳 , 長谷川哲夫 , 松尾光洋 , 南谷哲宏, 河野樹人 , 西村淳 , 藤田真司...大朝由美子ほかFUGINチーム
日本天文学会秋季年会予稿集, Sep. 2017, [Domestic conference] - NRO 銀河面サーベイプロジェクト (FUGIN): ホットコアの無バイアスサーベイ
佐藤一樹, 長谷川哲夫 , 梅本智文 , 南谷哲宏 , 鳥居和史, 久野成夫,半田利弘, 瀬田益道, 坪井昌人、大朝由美子ほかFUGINチーム
日本天文学会秋季年会予稿集, Sep. 2017, [Domestic conference] - OISTER Optical and Near-Infrared Monitoring Observations of a Peculiar Radio- Loud Active Galactic Nucleus SDSS J110006.07+442144.3
T. Morokuma, M. Tanaka, Y.T.Tanaka, R. Itoh.... Y. Oasa et al.
日本天文学会秋季年会予稿集, Sep. 2017, [Domestic conference] - 3 波長同時偏光撮像装置 “MuSaSHI” 偏光観測ユニットの開発
清野玄太、大朝由美子、荒沼佳純、平塚雄一郎、木内穂貴、潮田和俊、柴田吉輝、木野勝、秋田谷洋、伊藤洋一、高橋隼
日本天文学会秋季年会予稿集, Sep. 2017, [Domestic conference] - 全国の大学生を対象とした天文分野の理解度・意識の継続調査：理解度を高 める要因は何か？
大朝由美子、吉田康貴、埼玉大学教育学部/大学院理工学研 究科天文学研究室
日本天文学会秋季年会予稿集, Sep. 2017, [Domestic conference] - 埼玉大学における中・高校生への天文学の研究体験指導
小田達功 , 大朝由美子 , 平塚雄一郎
日本天文学会秋季年会予稿集, Sep. 2017, [Domestic conference] - 埼玉大学"SaCRA"望遠鏡を用いた分光観測体験
平塚雄一郎、大朝由美子、宮川遼太、木内穂高
(Web), Mar. 2017, [Domestic conference] - OrionB 分子雲における超低質量天体の近赤外広域測光探査観測
大朝由美子,北島隆太郎,渡邊千夏
日本天文学会春季年会予稿集, Mar. 2017, [Domestic conference] - へび座分子雲における超低質量天体の観測的研究
小田達功、大朝由美子
日本天文学会春季年会予稿集, Mar. 2017, [Domestic conference] - 高銀緯分子雲 における星形成の探査観測
平塚雄一郎、大朝由美子、伊藤洋一、山本宏昭
日本天文学会春季年会予稿集, Mar. 2017, [Domestic conference] - FU Ori 型星 V960Mon の中分散分光モニター観測
高木悠平、本田敏志、高橋隼、森鼻久美子、伊藤洋一、大朝由美子
日本天文学会春季年会予稿集, Mar. 2017, [Domestic conference] - 星形成領域 Ophiuchus, Lupus I,Orion B,Serpens,S106 における近赤外赤化則
渡邊千夏 , 大朝由美子 , 小田達則 , 北島隆太郎 , 星久樹 , 前原雄太 , 榎本藍子
日本天文学会春季年会予稿集, Mar. 2017, [Domestic conference] - FUGIN: W51 領域における CO multi-line 解析 (2)
藤田真司、久野成夫、梅本智文 ・・・大朝由美子ほか
日本天文学会春季年会予稿集, Mar. 2017, [Domestic conference] - FUGIN: 銀河系外縁部 (3)
松尾光洋、南谷哲宏、鳥居和史 ・・・大朝由美子ほかFUGINチーム
日本天文学会春季年会予稿集, Mar. 2017, [Domestic conference] - FUGIN: 大質量星形成領域 W33 の CO 輝線観測 III
河野樹人 , 立原研悟 , 大濱晶生 ・・・大朝由美子ほかFUGINチーム
日本天文学会春季年会予稿集, Mar. 2017, [Domestic conference] - 光赤外観測による銀河面/高銀緯分子雲の星形成探査
大朝由美子
(Web), Mar. 2017, [Domestic conference] - 教員養成学部における太陽観測実習の授業実践とその評価（１）
大朝由美子,矢治健太郎
日本天文学会春季年会予稿集, Mar. 2017, [Domestic conference] - 教員養成学部における太陽観測実習の授業実践とその評価（２）
矢治健太郎、大朝由美子
日本天文学会春季年会予稿集, Mar. 2017, [Domestic conference] - 埼玉大学望遠鏡・制御系“ SaCRA システム”の現状
柴田吉輝、大朝由美子、清水孝志、清野玄太、宮川遼太、潮田和俊、木野勝
(Web), Nov. 2016, [Domestic conference] - 高銀緯分子雲における星形成の探査観測
平塚雄一郎、大朝由美子
(Web), Nov. 2016, [Domestic conference] - 埼玉大学"SaCRA"望遠鏡・観測装置の現況報告
大朝由美子
(Web), Nov. 2016, [Domestic conference] - UH/UKIRTの移行
伊藤洋一、大朝由美子
(Web), Sep. 2016, [Domestic conference] - S106領域の近赤外広域測光探査観測
大朝由美子、小田達功、馬場優芽乃
日本天文学会秋季年会予稿集, Sep. 2016, [Domestic conference] - 埼玉大学望遠鏡・装置制御系“ SaCRA システム”による多波長複数装置 同時観測
柴田吉輝、清水孝志、清野玄太、宮川遼太、大朝由美子、潮田和俊、木野勝
日本天文学会秋季年会予稿集, Sep. 2016, [Domestic conference] - 極超新星における史上初めての強いヘリウムの検出
山中雅之 , 中岡竜也, 田中雅臣 ・・・大朝由美子ほか
日本天文学会秋季年会予稿集, Sep. 2016, [Domestic conference] - Near-Infrared Observations of Young Brown Dwarfs and Planetary-Mass Objects: Is their initial mass functions universal?
Yumiko Oasa
in print, Jul. 2016, [International conference] - Investigation of the Initial Masss Functions at Low-Mass End: Is it uniform?
Yumiko Oasa
(Web), Jun. 2016, [International conference] - Subaru Near-Infrared Spectroscopy of Young Brown Dwarfs and Planetary-Mass Objects
Yumiko Oasa
(Web), May 2016, [International conference] - 小型エシェル分光器の開発
大朝由美子 , 窪田悠 , 潮田和俊 , 柴田吉輝 , 宮川遼太, 高原祐典, 海老塚昇 , 渡辺和明
日本天文学会春季年会予稿集, Mar. 2016, [Domestic conference] - 外縁天体表面の水氷結晶度測定
寺居剛, 伊藤洋一 ,大朝由美子, 古 荘玲子,渡部潤一
日本天文学会春季年会予稿集, Mar. 2016, [Domestic conference] - おうし座分子雲に属する原始惑星系円盤の散逸過程
高木悠平、伊藤洋一 ,大朝由美子
日本天文学会春季年会予稿集, Mar. 2016, [Domestic conference] - 光赤外線大学間連携事業における共通自動即時測光パイプラインの開発
斉藤 嘉彦, 諸隈 智貴, 渡辺 誠, 大朝由美子ほか計12名
日本天文学会春季年会予稿集, Mar. 2016, [Domestic conference] - 埼玉大学 55cm 望遠鏡 SaCRA の同時測光分光観測システム構築I) の開発
柴田吉輝 , 大朝由美子 , 潮田和俊 , 窪田悠, 石橋遥子, 居倉聖, 木野勝
日本天文学会春季年会予稿集, Mar. 2016, [Domestic conference] - 3 波長同時偏光撮像装置 (MuSaSHI) の開発
潮田和俊 , 大朝由美子 , 柴田吉輝 , 窪田悠,清野玄太,石橋遥子, 居倉聖, 木野勝
日本天文学会春季年会予稿集, Mar. 2016, [Domestic conference] - 日本における公開天文台と天文教育との連携
李銀知 , 小倉康 ,大朝由美子
日本天文学会春季年会予稿集, Mar. 2016, [Domestic conference] - 小型エシェル分光器の開発
大朝由美子 , 窪田悠 , 潮田和俊 , 柴田吉輝 , 宮川遼太, 高原祐典, 海老塚昇 , 渡辺和明
(Web), Feb. 2016, [Domestic conference] - 三波長同時偏光撮像装置の開発
柴田吉輝 , 大朝由美子 , 潮田和俊 , 窪田悠, 石橋遥子, 居倉聖, 木野勝
(Web), Dec. 2015, [Domestic conference] - 三波長同時偏光撮像装置の開発
潮田和俊 , 大朝由美子 , 柴田吉輝 , 窪田悠,清野玄太,石橋遥子, 居倉聖, 木野勝
(Web), Dec. 2015, [Domestic conference] - 光赤外観測から探る星形成
大朝由美子
(Web), Nov. 2015, [Domestic conference] - 埼玉大学の大学間連携活動報告
大朝由美子
(Web), Nov. 2015, [Domestic conference] - 光赤外線天文学大学間連携による教育プログラム
大朝由美子
(Web), Nov. 2015, [Domestic conference] - "Is the substellar IMF universal?"
大朝由美子
(Web), Sep. 2015, [Domestic conference] - おおかみ座の遷移円盤天体における高解像度近赤外線偏光観測
工藤智幸 、田村元秀 、橋本淳 ・・・大朝由美子ほかすばる望遠鏡 /HiCAIO/AO188 team
日本天文学会秋季年会予稿集, Sep. 2015, [Domestic conference] - NRO 銀河面サーベイプロジェクト： 2014 年度進捗
梅本智文 , 南谷哲宏 , 西村淳 ・・・大朝由美子ほか
日本天文学会秋季年会予稿集, Sep. 2015, [Domestic conference] - 3 波長同時偏光撮像装置の開発
潮田和俊 , 大朝由美子 , 柴田吉輝 , 窪田悠 , 石橋遥子, 居倉聖, 木野勝
日本天文学会秋季年会予稿集, Sep. 2015, [Domestic conference] - 高銀緯分子雲における形成探査
大朝由美子、平塚雄一郎,源川
日本天文学会秋季年会予稿集, Sep. 2015, [Domestic conference] - UH88日本人時間の現況と課題
大朝由美子
2015年度岡山天体物理観測所・第25回光赤外ユーザーズミーティング 収録, Aug. 2015, [Domestic conference] - UH88日本人時間の現況と課題
大朝由美子
2015年度岡山天体物理観測所・第25回光赤外ユーザーズミーティング 収録, Aug. 2015, [Domestic conference] - The Initial Masss Functions at Low Masses: Is it Universal?
Yumiko Oasa
(Web), Jun. 2015, [International conference] - すばる望遠鏡戦略枠観測「 SEEDS 」による原始惑星系円盤および系外惑 星探査 V
工藤智幸 , 田村元秀 , 臼田知史・・・大朝由美子他SEEDs/HiCIAO/AO188 チーム
日本天文学会春季年会予稿集, Mar. 2015, [Domestic conference] - 埼玉大学 55cm 望遠鏡観測システムの自動化と基本特性調査
石橋遥子 , 大朝由美子 , 潮田和俊 , 居倉聖 , 星久樹 , 佐藤太基 , 前原雄太、 斉藤嘉彦、内海洋輔
日本天文学会春季年会予稿集, Mar. 2015, [Domestic conference] - 可視三色同時偏光撮像装置の開発
大朝由美子、潮田和俊、石橋遥子、居倉聖、木野勝
日本天文学会春季年会予稿集, Mar. 2015, [Domestic conference] - へびつかい座分子雲における若い惑星質量天体の探査観測
大朝由美子、星久樹、伊藤洋一
日本天文学会春季年会予稿集, Mar. 2015, [Domestic conference] - おおかみ座分子雲 I における超低質量天体形成
大朝由美子、前原雄太、星久樹、佐藤太基
日本天文学会春季年会予稿集, Mar. 2015, [Domestic conference] - 超低質量天体形成の赤外線観測
大朝由美子
Jan. 2015, [Domestic conference] - へびつかい座分子雲における若い惑星質量天体の探査観測
星久樹、大朝由美子
(Web), Sep. 2014, [Domestic conference] - すばる8.2m望遠鏡／MOIRCSを用いたへび座分子雲における若い超低質量天体の探査観測
佐藤太基,大朝由美子
(Web), Sep. 2014, [Domestic conference] - すばる望遠鏡を用いたS106における若い褐色矮星・惑星質量天体の分光観測
大朝由美子、高原佑典
(Web), Sep. 2014, [Domestic conference] - 星・惑星形成分野の将来展望
高見道弘、大朝由美子ほか2020年代の光赤外線天文学星惑星系形成チーム
(Web), Sep. 2014, [Domestic conference] - 若い小惑星族の高速自転小惑星候補の観測
吉田二美, Z.-Y.Lin, O.A.Burkhonov,Sh.A.Egamberdiyev,K.E.Ergashev・・大朝 由美子ほか光赤外線大学間連携観測チーム
日本天文学会秋季年会予稿集, Sep. 2014, [Domestic conference] - 光赤外線大学間連携における超新星爆発のToO観測状況報告II
山中雅之, 川端弘治, 高木勝俊, 秋田谷洋・・大朝由美子ほか光赤 外線大学間連携観測チーム
日本天文学会秋季年会予稿集, Sep. 2014, [Domestic conference] - OISTER・すざくによる 2FGL J2339.6-0532の観測
谷津陽一, 橘優太郎, 大内遥河, 有元誠, 斉藤嘉彦, 河合誠之・・大朝由美子ほ か光赤外線大学間連携観測チーム
日本天文学会秋季年会予稿集, Sep. 2014, [Domestic conference] - 光赤外大学間連携とかなた望遠鏡による Narrow Line Seyfert 1 Galaxy 1H̃0323+342の可視観測
田中康之、伊藤亮介、秋田谷洋、植村誠、深沢泰司、井上芳幸、土居明広、大 朝由美子ほか光赤外線大学間連携観測チーム
日本天文学会秋季年会予稿集, Sep. 2014, [Domestic conference] - 光赤外線大学間連携OISTER チームによるNova Delphini 2013 = V339 Del のToO観測
関口和寛, 神戸栄治, 柳澤顕史, 福井暁彦, 泉浦秀行, 黒田大介, 大朝由美子 ほか 光・赤外線天文学大学間連携観測チーム
Sep. 2014, [Domestic conference] - 可視・近赤外撮像データに対する測光パイプラインの開発
斉藤 嘉彦, 諸隈 智貴, 渡辺誠, 大朝由美子, 村田勝寛, 野上大作, 高橋隼, 秋 田谷洋, 永山貴宏, 黒田大介, 関口和寛, 光・赤外線天文学大学間連携観測 チーム
Sep. 2014, [Domestic conference] - 光赤外線大学間連携による観測教育ネットワークOISTER
黒田大介, 関口和寛、渡辺誠, 大朝由美子, 諸隈智貴, 斉藤嘉彦, 村田勝寛, 野上大作, 高橋隼, 秋田谷洋, 永山貴宏, 光・赤外線天文学大学間連携観測 チーム,
Sep. 2014, [Domestic conference] - 大学間連携望遠鏡によるガンマ線バーストの観測
河合誠之、斎藤嘉彦、谷津陽一、黒田大介、花山秀和、柳澤顕史、大朝由美子 ほか光赤外線大学間連携観測チーム
日本天文学会秋季年会予稿集, Sep. 2014, [Domestic conference] - 光赤外線大学間連携を通じた矮新星観測とその成果
大島誠人, 野上大作, 加藤太一, 秋田谷洋, 川端弘治, 植村誠, 橋本修, 新井 彰、花山秀和, 永山貴宏、坂田脩一郎, 大朝由美子ほか光赤外線大学間連携 観測チーム
日本天文学会秋季年会予稿集, Sep. 2014, [Domestic conference] - 大学間連携によるAGNジェットの多波長観測
短周期彗星209P/LINEARの光赤外線天文学大学間連携による観測
日本天文学会秋季年会予稿集, Sep. 2014, [Domestic conference] - 短周期彗星209P/LINEARの光赤外線天文学大学間連携による観測
石黒正晃、黒田大介、花山秀和、高橋隼、 高木悠平 、森鼻久美子、本田敏 志、新井彰・・・大朝由美子ほか光赤外線大学間連携観測チーム
日本天文学会秋季年会予稿集, Sep. 2014, [Domestic conference] - 光赤外線大学間連携観測の円滑な遂行に向けた環境整備
秋田谷洋, 渡辺誠, 大朝由美子, 諸隈智貴, 斉藤嘉彦, 村田勝寛, 野上大作, 高橋隼, 永山貴宏, 黒田大介, 関口和寛, 光・赤外線天文学大学間連携観測 チーム
日本天文学会秋季年会予稿集, Sep. 2014, [Domestic conference] - 埼玉大学55cm望遠鏡観測システムの自動化と性能評価試験
石橋遥子,大朝由美子,潮田和俊,居倉聖,星久樹,佐藤太基,前原雄太,斉 藤嘉彦,内海洋輔
日本天文学会秋季年会予稿集, Sep. 2014, [Domestic conference] - Class-I 超低光度天体 L1709-5 に対する観測的研究
原 千穂美, 川辺 良平, 中村 文隆, 島尻 芳人, 大朝 由美
日本天文学会秋季年会予稿集, Sep. 2014, [Domestic conference] - へびつかい座分子雲に属する前主系列星の円盤進化タイムスケール
高木悠平、伊藤洋一、新井彰、蔡承亨、大朝由美子
日本天文学会秋季年会予稿集, Sep. 2014, [Domestic conference] - 海外の天文教育との比較と大学生の天文分野における意識調査
佐藤太基,大朝由美子
日本天文学会秋季年会予稿集, Sep. 2014, [Domestic conference] - 光・赤外線天文学大学間連携による短期滞在実習プログラムの実施II
大朝由美子、高橋隼、高木悠平、本田敏志、秋田谷洋、黒田大介、泉浦秀行、 筒井寛典、関口和寛、橋本修、渡辺誠、諸隈智貴、斉藤嘉彦、村田勝寛 、野上 大作、永山貴宏、光赤外線天文学大学間連携観測チーム
日本天文学会秋季年会予稿集, Sep. 2014, [Domestic conference] - UH88望遠鏡日本人時間の報告と今後の運用方針について
大朝由美子
2014年度岡山天体物理観測所・第25回光赤外ユーザーズミーティング 収録, Aug. 2014, [Domestic conference] - Free Floating Planets and Initial Masss Functions
Yumiko Oasa
(Web), Aug. 2014, [International conference] - 光赤外線大学間連携におけるIc型超新星SN 2013geの初期観測報告
山中雅之(甲南大学), 川端弘治, 高木勝俊, 秋田谷洋・・大朝由美子ほか光赤 外線大学間連携観測チーム
日本天文学会秋季年会予稿集, Jul. 2014, [Domestic conference] - Observation campaign for the near-Earth object 2012 DA_{14} in Japan
Urakawa, S.; Terai, T.; Takahashi, J.; Fujii, M.; Hanayama, H.; Yoshida, F.; Hoshi, H.; Sato, T.; Ushioda, K.; Oasa, Y.; Arai, A.; Honda, S.; Takagi, Y.; Itoh, Y.; Ishiguro, M.
(Web), Jul. 2014, [International conference] - V339 Del=Nova Delphini 2013 の光赤外線大学間連携ToO観測
関口和寛、ほか光赤外線大学間連携OISTERチーム一同
日本天文学会春季年会予稿集, Mar. 2014, [Domestic conference] - すばる8.2ｍ望遠鏡/MOIRCSを用いたへび座分子雲における若い超低質量天体の探査観測
佐藤太基、大朝由美子
日本天文学会春季年会予稿集, Mar. 2014, [Domestic conference] - すばる望遠鏡を用いたS106における若い超低光度天体の分光観測
高原 佑典、大朝由美子、伊藤洋一
日本天文学会春季年会予稿集, Mar. 2014, [Domestic conference] - へびつかい座分子雲における若い惑星質量天体の探査観測
星久樹、大朝由美子、工藤智幸、伊藤洋一
日本天文学会春季年会予稿集, Mar. 2014, [Domestic conference] - すばる望遠鏡戦略枠観測「SEEDS」による原始惑星系円盤および系外惑星探査V
工藤智幸ほかSEEDS/HiCIAO/AO188 team (大朝由美子含)
日本天文学会春季年会予稿集, Mar. 2014, [Domestic conference] - 光・赤外線大学間連携による短期滞在実習プログラムの実施
大朝由美子、高橋隼、黒田大介、秋田谷洋、面高俊宏、斉藤嘉彦、永山貴宏、野上大作、諸隈智貴、渡辺誠、関口和寛、林正彦
日本天文学会春季年会予稿集, Mar. 2014, [Domestic conference] - Earthshine Polarimetry to Extract Signatures of Earth-like Atmosphere and Surface
Takahashi, J., Itoh, Y., Akitaya, H., Okazaki, A., Kawabata, K., Oasa, Y., Isogai, M., Niwa, T.
Proceedings of the conference American Geophysical Union, Fall Meeting 2013, Dec. 2013, [International conference] - Is the Initial Mass Function Universal?
Yumiko Oasa
(Web), Dec. 2013, [International conference] - Polarimetric Signatures of the Earth Extracted from Earthshine Observations
Takahashi, J., Itoh, Y., Akitaya, H., Okazaki, A., Kawabata, K., Oasa, Y., Isogai, M., Niwa, T.
Proceedings of the conference International Astrobiology Workshop 2013, Nov. 2013, [International conference] - Investigating the stellar parameters of pre-main sequence stars with TMT
Yuhei Takagi, Yoichi, Itoh, Yumiko Oasa
(Web), Oct. 2013, [International conference] - NIR observations of young brown dwarfs and planetary mass objects
Yumiko Oasa
(Web), Oct. 2013, [International conference] - すばる望遠鏡戦略枠観測「SEEDS」による原始惑星系円盤および系外惑星探査IV
田村元秀ほかSEEDS/HiCIAO/AO188 team (大朝由美子含)
日本天文学会秋季年会予稿集, Sep. 2013, [Domestic conference] - おおかみ座分子雲における超低質量天体探査観測
大朝由美子、榎本藍子、中里佳織
日本天文学会秋季年会予稿集, Sep. 2013, [Domestic conference] - 光赤外線大学間連携事業によるIRSFへのガンマ線バースト即時観測システムの導入とその初期観測結果
永山貴宏 、西山正吾、黒田大介、斉藤嘉彦、渡辺誠、秋田谷洋、野上大作、面高俊宏、諸隈智貴、大朝由美子、高橋隼、光赤外線大学間連携事業
日本天文学会秋季年会予稿集, Sep. 2013, [Domestic conference] - UH88望遠鏡を用いた高銀緯分子雲HLCG92-35におけるTタウリ型星探査
大朝由美子
2013年度岡山天体物理観測所・第24回光赤外ユーザーズミーティング 収録, Aug. 2013, [Domestic conference] - UH88日本人時間の報告と今後について
大朝由美子
2013年度岡山天体物理観測所・第24回光赤外ユーザーズミーティング 収録, Aug. 2013, [Domestic conference] - Diversity of Star/Planet Formation with Subaru/GLAO
Yumiko Oasa
(Web), Jun. 2013, [International conference] - すばる望遠鏡戦略枠観測「SEEDS」による原始惑星系円盤および系外惑星探査III
工藤智幸ほかSEEDS/HiCIAO/AO188 team (大朝由美子含)
日本天文学会春季年会予稿集, Mar. 2013, [Domestic conference] - 君も今日から太陽研究者！ - ひので衛星データを使って解析体験実習 –
矢治健太郎、川村教一、大山真満、大朝由美子ほか
日本天文学会春季年会予稿集, Mar. 2013, [Domestic conference] - 地球照観測から得られた地球の偏光分光特性
高橋 隼, 伊藤洋一, 岡崎彰, 秋田谷洋, 川端弘治,大朝由美子, 磯貝瑞希
日本天文学会春季年会予稿集, Mar. 2013, [Domestic conference] - 小惑星2012 DA14地球大接近時の連続測光観測
寺居剛, 大朝由美子,大島吾一,荒谷健太,星久樹,榎本藍子,佐藤太基,高井大地,中里佳織,潮田和俊
日本天文学会春季年会予稿集, Mar. 2013, [Domestic conference] - 高分散分光観測によるおうし座分子雲中の円盤進化タイムスケールの解明
高木 悠平、伊藤 洋一、大朝由美子
日本天文学会春季年会予稿集, Mar. 2013, [Domestic conference] - すばる望遠鏡を用いた若い超低光度天体の分光観測
高原 佑典、大朝由美子、伊藤洋一
日本天文学会春季年会予稿集, Mar. 2013, [Domestic conference] - へびつかい座分子雲L1709領域における若い惑星質量天体の探査
星久樹、大朝由美子、工藤智幸、伊藤洋一
日本天文学会春季年会予稿集, Mar. 2013, [Domestic conference] - 高銀緯分子雲HLCG92-35に対するT Tauri型星の探査
大島吾一、大朝由美子
日本天文学会春季年会予稿集, Mar. 2013, [Domestic conference] - 埼玉大学望遠鏡を用いた星空観望会の報告
大朝由美子、大島吾一、高原佑典、星久樹、荒谷健太、榎本藍子、佐藤太基、高井大地、中里佳織、加藤卓磨、鈴木愛理、他埼玉大学教育学部天文学研究室一同
日本天文学会春季年会予稿集, Mar. 2013, [Domestic conference] - 太陽観測用小型分光器の製作と応用
坂江隆志、大朝 由美子、花岡庸一郎
Mar. 2013, [Domestic conference] - 太陽観測用小型分光器の製作と応用
坂江隆志、大朝由美子、花岡庸一郎
日本天文学会春季年会予稿集, Mar. 2013, [Domestic conference] - SEEDSプロジェクトによる原始惑星系円盤の偏光撮像観測
工藤智幸ほかSEEDS/HiCIAO/AO188 team (大朝由美子含)
日本天文学会秋季年会予稿集, Sep. 2012, [Domestic conference] - へびつかい座分子雲における深い近赤外撮像観測
大朝由美子、星久樹、工藤智幸、伊藤洋一
日本天文学会秋季年会予稿集, Sep. 2012, [Domestic conference] - UH2.2m望遠鏡日本人時間の報告
大朝由美子
Aug. 2012, [Domestic conference] - 近赤外偏光観測によるTタウリ型連星系に対する原始惑星系円盤の探査
谷井良子、伊藤洋一、工藤智幸、Ranjan Gupta、Asoke Sen、大朝由美子他SEEDSグループ
日本天文学会春季年会予稿集, Mar. 2012 - すばる望遠鏡戦略枠観測「SEEDS」による原始惑星系円盤および系外惑星探査II
工藤智幸ほかSEEDS/HiCIAO/AO188 team (大朝由美子含)
日本天文学会春季年会予稿集, Mar. 2012 - GG Tauに付随する周連星円盤の近赤外線観測
伊藤洋一、谷井良子、大朝由美子他SEEDSプロジェクト
日本天文学会春季年会予稿集, Mar. 2012 - 系外惑星への応用にむけた地球照の偏光分光観測
高橋 隼, 伊藤洋一, 岡崎彰, 秋田谷洋, 川端弘治,大朝由美子, 磯貝瑞希
日本天文学会春季年会予稿集, Mar. 2012 - ひので衛星と高校・公開天文台・科学館との太陽共同観測データアーカイブの活用
矢治健太郎、大山真満、大朝由美子ほか
日本天文学会春季年会予稿集, Mar. 2012 - Young Brown Dwarfs and Planetary-Mass Objects with Disks in NGC1333
Yumiko Oasa
"Formation and early evolution of very low mass stars and brown dwarfs", Oct. 2011, [Domestic conference] - TMT時代の星・惑星形成
大朝由美子
Sep. 2011, [Domestic conference] - すばる望遠鏡戦略枠観測「SEEDS」による原始惑星系円盤および系外惑星探査
工藤智幸ほかSEEDS/HiCIAO/AO188 team (大朝由美子含)
日本天文学会秋季年会予稿集, Sep. 2011 - へび座分子雲に付随する前主系列星候補天体の近赤外多天体分光観測
伊藤洋一、大朝由美子、太田耕司、岩室史英、秋山正幸、田村直之ほかFMOSチーム
日本天文学会秋季年会予稿集, Sep. 2011 - 若い褐色矮星の可視／赤外多波長測光観測：円盤の可能性
大朝由美子、立澤麻衣、田中宗親、伊藤洋一
日本天文学会秋季年会予稿集, Sep. 2011 - 「教員養成の立場からの天文教育の実態と課題」
大朝 由美子
Jun. 2011 - 2009年皆既日食で用いた船上観測のための可視光赤外線観測装置
伊藤洋一、向井正、寺居剛、高橋隼、奥田治之、大朝由美子、猿楽祐樹
日本天文学会春季年会予稿集, Mar. 2010, [Domestic conference] - すばるまでの星惑星形成とTMT時代の星惑星形成
Oasa, Yumiko
光赤天連シンポジウム『30m地上超大型望遠鏡TMTによる天文学の新展開』, Oct. 2009, [Domestic conference] - 可視Iバンド高分散分光観測による前主系列星の年齢決定
高木悠平、伊藤洋一、大朝由美子
日本天文学会秋季年会予稿集, Sep. 2009, [Domestic conference] - ペルセウス座分子雲に付随する低質量YSOの可視中分散分光観測
伊藤洋一、Ranjan Gupta、大朝由美子、Asoke Sen、田中宗親、寺居剛、中岡正奈
日本天文学会秋季年会予稿集, Sep. 2009, [Domestic conference] - Tタウリ型連星FS Tauriに付随する原始惑星系の観測的研究
日置智紀、伊藤洋一、大朝由美子、深川美里
日本天文学会秋季年会予稿集, Sep. 2009, [Domestic conference] - 誘発的星形成領域BRC13の近赤外撮像観測
林実幸、伊藤洋一、丹羽隆裕、大朝由美子、柳澤顕史
日本天文学会秋季年会予稿集, Sep. 2009, [Domestic conference] - 若い超低質量天体の赤外測光/分光観測
大朝由美子、田中宗親、伊藤洋一
日本天文学会秋季年会予稿集, Sep. 2009, [Domestic conference] - ミリ波による誘発的星形成領域BRC14の詳細観測
丹羽隆裕、立原研悟、伊藤洋一、大朝由美子、砂田和良、杉谷光司
日本天文学会秋季年会予稿集, Sep. 2009, [Domestic conference] - ほ座分子雲に付随するブライトリム分子雲BRC57の近赤外線撮像観測
田中温子、伊藤洋一、大朝由美子
日本天文学会秋季年会予稿集, Sep. 2009, [Domestic conference] - Young Substellar Objects in NGC 1333
Oasa,Y.,Tanaka,M., Itoh, Y.
May 2009, [Domestic conference] - 埼玉大学SaCRA望遠鏡とぐんま天文台1.5m望遠鏡の現況報告
大朝由美子
Web, [Domestic conference] - 10 年目の SaCRA 望遠鏡：埼玉大学におけるさまざまな形態での教育利用や 星空観望会
大朝由美子, 奥田大翔, 小柳香, 吉田康貴ほか埼玉大学教育学部/大学院教育学研究科・理工学研究科天文学研究室
Web, [Domestic conference] - 10 年目の SaCRA 望遠鏡：埼玉大学におけるさまざまな形態での教育利用や 星空観望会
大朝由美子, 金井昂大, 奥田大翔, 小柳香, 佐藤陸人, 中田伊織 (埼玉大学), 大島吾一, 高原佑典, 星久 樹, 佐藤太基, 石橋遥子, 潮田和俊, 柴田吉輝, 小田達功, 平塚雄一郎, 石岡千寛, 大出康平ほか埼玉大 学教育学部/大学院教育学研究科・理工学研究科天文学研究室 OB・OG
Web, [Domestic conference] - 埼玉大学の2021年度活動報告
大朝由美子
web, [Domestic conference] - 光・赤外大学間連携観測による STARLINK Visorsat の多波長の等級測定
堀内 貴史, 花山 秀和, 大石 雅寿, 大朝 由美子ほか
Web, [Domestic conference] - ALMA ACA サーベイで探る Corona Australis 領域の星形成 (3)
西岡丈翔, 立原研悟, 山崎康正, 徳田一起, 大西利和, 金井昂大, 大朝由美子ほか
Web, [Domestic conference] - 太陽系外惑星大気の多波長トランジット観測
熊澤希珠、大朝由美子
天文・天体物理若手の会予稿集, [Domestic conference] - Lupus IとR CrAにおける若い超低質量天体の近赤外測光探査
石岡千寛,金井昂大,大朝由美子,宝田拓也,高橋隼,伊藤洋一
日本天文学会春季年会予稿集, [Domestic conference] - 短期滞在実習について
高橋隼,大朝由美子
(Web), [Domestic conference] - FU Ori型星V960 Monの分光観測
高木悠平,本田敏志、高橋隼、伊藤洋一,新井彰,大朝由美子
Web, [Domestic conference] - 埼玉大学55cm望遠鏡SaCRA/MuSaSHIを用いた系外惑星の多波長トランジット測光観測
石岡千寛,大朝由美子
日本天文学会秋季年会予稿集, [Domestic conference] - R CrA領域における若い超低質量天体の近赤外測光探査
金井昂大,大朝由美子
日本天文学会春季年会予稿集, [Domestic conference] - BH X線連星MAXI J1820+070の2019年の再増光時における多波長観測
安達稜, 村田勝寛…大朝由美子ほか光赤外線大学間連携メンバー
日本天文学会秋季年会予稿集, [Domestic conference] - BH X線連星MAXI J1820+070の2019年の再増光時における多波長観測
安達稜, 村田勝寛…大朝由美子ほか光赤外線大学間連携メンバー
日本天文学会秋季年会予稿集, [Domestic conference] - 埼玉大学55cm望遠鏡SaCRA/MuSaSHIを用いた系外惑星の多波長トランジット測光観測
石岡千寛,大朝由美子
日本天文学会秋季年会予稿集, [Domestic conference] - R CrA領域における若い超低質量天体の近赤外測光探査
金井昂大,大朝由美子
日本天文学会秋季年会予稿集, [Domestic conference] - 銀河面低密度領域における星形成の広域探査観測
大朝由美子, 竹内媛香, 木内穂貴,大出康平, 鵜澤由規,田村泰樹,平塚雄一郎,伊藤洋一,本田敏志,高木悠平
日本天文学会秋季年会予稿集, [Domestic conference] - BH X線連星MAXI J1820+070の2019年の再増光時における多波長観測
安達稜, 村田勝寛…大朝由美子ほか光赤外線大学間連携メンバー
日本天文学会秋季年会予稿集, [Domestic conference] - BH X線連星MAXI J1820+070の2019年の再増光時における多波長観測
安達稜, 村田勝寛…大朝由美子ほか光赤外線大学間連携メンバー
日本天文学会秋季年会予稿集, [Domestic conference] - BH X線連星MAXI J1820+070の2019年の再増光時における多波長観測
安達稜, 村田勝寛…大朝由美子ほか光赤外線大学間連携メンバー
日本天文学会秋季年会予稿集, [Domestic conference] - BH X線連星MAXI J1820+070の2019年の再増光時における多波長観測
安達稜, 村田勝寛…大朝由美子ほか光赤外線大学間連携メンバー
日本天文学会秋季年会予稿集, [Domestic conference] - BH X線連星MAXI J1820+070の2019年の再増光時における多波長観測
安達稜, 村田勝寛…大朝由美子ほか光赤外線大学間連携メンバー
日本天文学会秋季年会予稿集, [Domestic conference] - R CrA領域における若い超低質量天体の近赤外測光探査R CrA領域における若い超低質量天体の近赤外測光探査
金井昂大,大朝由美子
天文・天体物理若手の会予稿集, [Domestic conference] - 変光に基づく前主系列星の探査
伊藤洋一 , 冨田堅太郎 , 松永典之 , 大朝由美子
日本天文学会秋季年会予稿集, [Domestic conference] - 全国の大学生を対象とした天文分野の理解度調査報告体探査観測
大朝由美子、佐藤太基,前原雄太,塩田真彩,矢治健太郎
日本天文学会秋季年会予稿集, [Domestic conference] - 低活性彗星 209P/LINEAR の可視・近赤外偏光観測
黒田大介 , 石黒正晃 ,・・・大朝由美子ほか計27名
日本天文学会春季年会予稿集, [Domestic conference] - 低活性彗星 209P/LINEAR の可視・近赤外偏光観測
黒田大介 , 石黒正晃 ,・・・大朝由美子ほか計27名
日本天文学会春季年会予稿集, [Domestic conference] - 原子ガス定量における低密度領域のダストの星間減光と放射の非相関性
佐伯駿,山本宏昭,立原研悟,林克洋,福井康雄,大朝由美子
日本天文学会春季年会予稿集, [Domestic conference] - 高銀緯分子雲 MBM01,02,03,32 における深い可視分光探査観測
平塚雄一郎、大朝由美子
日本天文学会秋季年会予稿集, [Domestic conference] - 埼玉大学望遠鏡・装置制御系“ SaCRA システム”による多波長複数装置 同時観測
柴田吉輝、大朝由美子、清水孝志、清野玄太、中村一貴、宮川遼太、潮田和俊、木野勝、川野元
日本天文学会秋季年会予稿集, [Domestic conference] - FUGIN: シェル状の速度構造をもつ分子ガス
津田裕也、小野寺幸子、田中邦彦 ・・・大朝由美子ほかFUGINチーム
日本天文学会春季年会予稿集, [Domestic conference] - NRO 銀河面サーベイプロジェクト： 2015年度進捗
梅本智文 , 南谷哲宏 , 鳥居和史 ・・・大朝由美子ほか
日本天文学会秋季年会予稿集, [Domestic conference] - 星・惑星形成班検討最終報告
高見道弘、大朝由美子ほか2020年代の光赤外線天文学星惑星系形成チーム
(Web), [Domestic conference]
■ Research projects
- Development of a compact all-sky camera system and construction of an astronomy/weather observation education program
Japan Society for the Promotion of Science, Grants-in-Aid for Scientific Research, Grant-in-Aid for Scientific Research (C), 01 Apr. 2017 - 31 Mar. 2023
Oasa Yumiko, Saitama University
Grant amount(Total)：4810000, Direct funding：3700000, Indirect funding：1110000
This work aims to achieve a hands-on and experiential understanding of astronomy which is often considered difficult for observation and experimentation. To this end, we have developed cost-effective, compact, and high-performance all-sky camera systems, weather observation instruments, and educational materials for astronomy and meteorology. Despite the significant challenges imposed by the COVID-19 pandemic on practical application and educational activities, we have successfully developed content that can be utilized in primary and secondary education astronomy and meteorology classes through the internet and ICT devices.
Additionally, a survey and detailed analysis of understanding and interest in astronomy indicated that observational experiences and hands-on learning utilizing telescopes and studying "earth science （basic）" in high school significantly enhance both knowledge and comprehension.
Grant number：17K00960 - Evolution timescale of young stars
Japan Society for the Promotion of Science, Grants-in-Aid for Scientific Research, Grant-in-Aid for Young Scientists (B), 01 Apr. 2014 - 31 Mar. 2019
Takagi Yuhei; Itoh Yoichi; Oasa Yumiko; Honda Satoshi; Arai Akira
Grant amount(Total)：2860000, Direct funding：2200000, Indirect funding：660000
Age determination of young stars is crucial for the understanding of the evolution of young stars and protoplanetary disks. An original age determination method based on high-resolution spectroscopy was used to discuss the evolution timescale of protoplanetary disks, and I found that the disk lifetime depends on the nature of the star-forming regions.
Spectroscopic monitoring observations of FU Ori type star V960 Mon was also conducted to understand the evolution of protoplanetary disks during the FU Ori outburst. The variation in obtained spectra shows the change of effective temperature and the surface gravity of the disk during the outburst, indicating the physical evolution of the protoplanetary disk.
Grant number：26870507 - Observational Study of various extrasolar planets
Japan Society for the Promotion of Science, Grants-in-Aid for Scientific Research, Grant-in-Aid for Young Scientists (B), 2006 - 2008
OASA Yumiko, Kobe University
Grant amount(Total)：3600000, Direct funding：3300000, Indirect funding：300000
Grant number：18740279 - -
Competitive research funding - -
Competitive research funding