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1. Revisiting planetary systems in the Okayama Planet Search Program: A new long-period planet, RV astrometry joint analysis, and a multiplicity-metallicity trend around evolved stars.

Author

Teng, Huan-Yu, Sato, Bun'ei, Kuzuhara, Masayuki, Takarada, Takuya, Omiya, Masashi, Harakawa, Hiroki, Izumiura, Hideyuki, Kambe, Eiji, Yilmaz, Mesut, Bikmaev, Ilfan, Selam, Selim O, Brandt, Timothy D, Xiao, Guang-Yao, Yoshida, Michitoshi, Itoh, Yoichi, Ando, Hiroyasu, Kokubo, Eiichiro, and Ida, Shigeru

Subjects
STARS, PLANETARY systems, STELLAR activity, GAS giants, ASTROMETRY, ORIGIN of planets, PLANETARY mass
Abstract

In this study, we revisit 32 planetary systems around evolved stars observed within the framework of the Okayama Planet Search Program (OPSP) and its collaborative framework of the East Asian Planet Search Network to search for additional companions and investigate the properties of stars and giant planets in multiple-planet systems. With our latest radial velocities obtained from Okayama Astrophysical Observatory, we confirm an additional giant planet in the wide orbit of the 75 Cet system (⁠|$P_{\rm {c}} = 2051.62_{-40.47}^{+45.98}\ \rm {d}$|⁠ , |$M_{\rm {c}}\sin i=0.912_{-0.090}^{+0.088}\,\,M_{\rm {J}}$|⁠ , and |$a_{\rm {c}}=3.929_{-0.058}^{+0.052}\ \rm {au}$|⁠), along with five stars exhibiting long-term radial velocity accelerations, which indicates massive companions in the wide orbits. We also find that the radial velocity variations of several planet-harboring stars may indicate additional planet candidates, stellar activities, or other understudied sources. These stars include ϵ Tau, 11 Com, 24 Boo, 41 Lyn, 14 And, HD 32518, and ω Ser. We further constrain the orbital configuration of the HD 5608, HD 14067, HD 120084, and HD 175679 systems by combining radial velocities with astrometry, as their host central stars exhibit significant astrometric accelerations. For other systems, we simply refine their orbital parameters. Moreover, our study indicates that the OPSP planet-harboring stars are more metal poor compared to the currently known planet-harboring stars, and this is likely due to the B − V color upper limit at 1.0 for star selection in the beginning of the survey. Finally, by investigating the less massive giant planets (<5  M J) around currently known planet-harboring evolved stars, we find that metallicity positively correlates with the multiplicity and total planet mass of the system, which can be evidence for the core-accretion planet formation model. [ABSTRACT FROM AUTHOR]

Published
2023
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2. The Nearby Evolved Stars Survey – I. JCMT/SCUBA-2 Submillimeter Detection of the Detached Shell of U Antliae

Author

Dharmawardena, Thavisha E, Kemper, Francisca, Srinivasan, Sundar, Scicluna, Peter, Marshal, Jonathan P, Wouterloot, Jan G. A, Greaves, Jane, Goldman, Steven R, Loon, Jacco Th. van, Matsuura, Mikako, McDonald, Iain, He, Jinhua, Zijlstra, Albert A, Toal´a, Jes´us A, Wallstr¨om, Sofia H. J, Kim, Hyosun, Trejo, Alfonso, Ventura, Paolo, Lagadec, Eric, Boyer, Martha L, Liu, Tie, Rau, Gioia, Izumiura, Hideyuki, Cami, Jan, Holland, Wayne, Jones, Olivia, and Shinnaga, Hiroko

Subjects
Astrophysics
Abstract

We present the highest resolution single-dish submillimetre observations of the detached shell source U Antliae to date. The observations were obtained at 450 and 850μm with SCUBA-2 instrument on the James Clerk Maxwell Telescope as part of the Nearby Evolved Stars Survey. The emission at 850μm peaks at 40 arcsec with hints of a second peak seen at ∼20 arcsec. The emission can be traced out to a radius of 56 arcsec at a 3σ level. The outer peak observed at 850μm aligns well with the peak observed at Herschel/PACS wavelengths. With the help of spectral energy distribution fitting and radiative transfer calculations of multiple-shell models for the circumstellar envelope, we explore the various shell structures and the variation of grain sizes along the in the circumstellar envelope. We determine a total shell dust mass of (2.0 ± 0.3) × 10−5 M⊙ and established that the thermal pulse that gave rise to the detached shell occurred 3500 ± 500 yr ago.

Published
2019
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3. The Spin Temperature of NH 3 in Comet C/1999S4 (LINEAR)

Author

Kawakita, Hideyo, Watanabe, Jun-ichi, Ando, Hiroyasu, Aoki, Wako, Fuse, Tetsuharu, Honda, Satoshi, Izumiura, Hideyuki, Kajino, Toshitaka, Kambe, Eiji, Kawanomoto, Satoshi, Noguchi, Kunio, Okita, Kiichi, Sadakane, Kozo, Takada-Hidai, Masahide, Takeda, Yoichi, Usuda, Tomonori, Watanabe, Etsuji, and Yoshida, Michitoshi

Published
2001

4. Optical IFU Observations of GOALS Sample with KOOLS-IFU on Seimei Telescope: Initial results of 9 U/LIRGs at $z <$ 0.04

Author

Toba, Yoshiki, Yamada, Satoshi, Matsubayashi, Kazuya, Terao, Koki, Moriya, Aoi, Ueda, Yoshihiro, Ohta, Kouji, Hashiguchi, Aoi, Himoto, Kazuharu G., Izumiura, Hideyuki, Joh, Kazuma, Kato, Nanako, Koyama, Shuhei, Maehara, Hiroyuki, Misato, Rana, Noboriguchi, Akatoki, Ogawa, Shoji, Ota, Naomi, Shibata, Mio, Tamada, Nozomu, Yanagawa, Anri, Yonekura, Naoki, Nagao, Tohru, Akiyama, Masayuki, Kajisawa, Masaru, and Matsuoka, Yoshiki

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present ionized gas properties of 9 local ultra/luminous infrared galaxies (U/LIRGs) at $z, Comment: 12 pages, 8 figures, and 2 tables, accepted for publication in PASJ

Published
2022

5. close-in planet orbiting giant star HD 167768.

Author

Teng, Huan-Yu, Sato, Bun'ei, Kunitomo, Masanobu, Takarada, Takuya, Omiya, Masashi, Harakawa, Hiroki, Xiao, Guang-Yao, Liu, Yu-Juan, Izumiura, Hideyuki, Kambe, Eiji, Yoshida, Michitoshi, Itoh, Yoichi, Ando, Hiroyasu, Kokubo, Eiichiro, and Ida, Shigeru

Subjects
PLANETARY orbits, HOT Jupiters, STELLAR orbits, OBSERVATORIES, VELOCITY measurements
Abstract

We report the detection of a giant planet orbiting the G-type giant star HD 167768 from radial velocity measurements using the High Dispersion Echelle Spectrograph (HIDES) at Okayama Astrophysical Observatory (OAO). HD 167768 has a mass of |$1.08_{-0.12}^{+0.14}\, M_{\odot }$|⁠ , a radius of |$9.70_{-0.25}^{+0.25}\, R_{\odot }$|⁠ , a metallicity of |$[\mbox{Fe}/\mbox{H}]=-0.67_{-0.08}^{+0.09}$|⁠ , and a surface gravity of |$\log g = 2.50_{-0.06}^{+0.06}$|⁠. The planet orbiting the star is a warm Jupiter, having a period of |$20.6532_{-0.0032}^{+0.0032}\:\mbox{d}$|⁠ , a minimum mass of |$0.85_{-0.11}^{+0.12}\, M_{\rm {J}}$|⁠ , and an orbital semimajor axis of |$0.1512_{-0.0063}^{+0.0058}\:\mbox{au}$|⁠. The planet has one of the shortest orbital periods among those ever found around deeply evolved stars (log  g < 3.5) using radial velocity methods. The equilibrium temperature of the planet is 1874 K, as high as a hot Jupiter. The radial velocities show two additional regular variations at 41 d and 95 d, suggesting the possibility of outer companions in the system. Follow-up monitoring will enable validation of the periodicity. We also calculated the orbital evolution of HD 167768 b and found that the planet will be engulfed within 0.15 Gyr. [ABSTRACT FROM AUTHOR]

Published
2023
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6. Optical IFU observations of GOALS sample with KOOLS-IFU on Seimei Telescope: Initial results of nine U/LIRGs at z < 0.04.

Author

Toba, Yoshiki, Yamada, Satoshi, Matsubayashi, Kazuya, Terao, Koki, Moriya, Aoi, Ueda, Yoshihiro, Ohta, Kouji, Hashiguchi, Aoi, Himoto, Kazuharu G, Izumiura, Hideyuki, Joh, Kazuma, Kato, Nanako, Koyama, Shuhei, Maehara, Hiroyuki, Misato, Rana, Noboriguchi, Akatoki, Ogawa, Shoji, Ota, Naomi, Shibata, Mio, and Tamada, Nozomu

Subjects
ACTIVE galactic nuclei, SUPERMASSIVE black holes, GALAXY mergers, TELESCOPES, IONIZED gases, MERGERS & acquisitions
Abstract

We present ionized gas properties of nine local ultra/luminous infrared galaxies (U/LIRGs) at z < 0.04 through Integral Field Unit (IFU) observations with KOOLS-IFU on the Seimei Telescope. The observed targets are drawn from the Great Observatories All-sky LIRG Survey (GOALS), covering a wide range of merger stages. We successfully detect emission lines such as Hβ, [O  iii ]λ5007, Hα, [N  ii ]λλ6549, 6583, and [S  ii ]λλ6717, 6731 with a spectral resolution of R = 1500–2000, which provides (i) a spatially resolved (∼200–700 pc) moment map of ionized gas and (ii) diagnostics for an active galactic nucleus (AGN) within the central ∼3–11 kpc in diameter for our sample. We find that the [O  iii ] outflow that is expected to be driven by an AGN tends to be stronger (i) towards the galactic center and (ii) as a sequence of the merger stage. In particular, the outflow strength in the late-stage (stage D) mergers is about 1.5 times stronger than that in the early-state (stage B) mergers, which indicates that galaxy mergers could induce AGN-driven outflow and play an important role in the co-evolution of galaxies and supermassive black holes. [ABSTRACT FROM AUTHOR]

Published
2022
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7. trio of giant planets orbiting evolved star HD 184010.

Author

Teng, Huan-Yu, Sato, Bun'ei, Takarada, Takuya, Omiya, Masashi, Harakawa, Hiroki, Nagasawa, Makiko, Hasegawa, Ryo, Izumiura, Hideyuki, Kambe, Eiji, Yoshida, Michitoshi, Itoh, Yoichi, Ando, Hiroyasu, Kokubo, Eiichiro, and Ida, Shigeru

Subjects
GAS giants, PLANETARY orbits, PLANETARY mass, PLANETARY systems, ORBITS (Astronomy), RED giants
Abstract

We report the discovery of a triple-giant-planet system around an evolved star HD 184010 (HR 7421, HIP 96016). This discovery is based on observations from Okayama Planet Search Program, a precise radial velocity survey, undertaken at Okayama Astrophysical Observatory between 2004 April and 2021 June. The star is K0 type and located at the beginning of the red giant branch. It has a mass of |$1.35_{-0.21}^{+0.19}\, M_{\odot }$|⁠ , a radius of |$4.86_{-0.49}^{+0.55} R_{\odot }$|⁠ , and a surface gravity log  g of |$3.18_{-0.07}^{+0.08}$|⁠. The planetary system is composed of three giant planets in a compact configuration: the planets have minimum masses of |$M_{\rm {b}}\sin i = 0.31_{-0.04}^{+0.03}\, M_{\rm {J}}$|⁠ , |$M_{\rm {c}}\sin i = 0.30_{-0.05}^{+0.04}\, M_{\rm {J}}$|⁠ , and |$M_{\rm {d}}\sin i = 0.45_{-0.06}^{+0.04}\, M_{\rm {J}}$|⁠ , and orbital periods of |$P_{\rm {b}}=286.6_{-0.7}^{+2.4}\:$| d, |$P_{\rm {c}}=484.3_{-3.5}^{+5.5}\:$| d, and |$P_{\rm {d}}=836.4_{-8.4}^{+8.4}\:$| d, respectively, which are derived from a triple Keplerian orbital fit to three sets of radial velocity data. The ratio of orbital periods are close to P d :  P c :  P b ∼ 21 : 12 : 7, which means the period ratios between neighboring planets are both lower than 2 : 1. The dynamical stability analysis reveals that the planets should have near-circular orbits. The system could remain stable over 1 Gyr, initialized from co-planar orbits, low eccentricities (e = 0.05), and planet masses equal to the minimum mass derived from the best-fitting circular orbit fitting. Besides, the planets are not likely in mean motion resonance. The HD 184010 system is unique: it is the first system discovered to have a highly evolved star (log  g < 3.5 cgs) and more than two giant planets all with intermediate orbital periods (102 < P < 103 d). [ABSTRACT FROM AUTHOR]

Published
2022
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9. Thirty Millimeter Telescope.

Author

Ita, Yoshifusa, Ichikawa, Takashi, Tsutsui, Hironori, Hanaue, Takumi, Komiyama, Takahiro, Onozato, Hiroki, Iwamatsu, Atsushi, Morita, Ryosuke, Habasaki, Yuta, Amemiya, Ryuto, Hanawa, Miho, Yanagisawa, Kenshi, Izumiura, Hideyuki, and Nakada, Yoshikazu

Subjects
PHOTOMETRY, TELESCOPES, VARIABLE stars, ASTRONOMICAL surveys
Abstract

A near-infrared telescope with an effective aperture diameter of 30 mm has been developed. The primary objective of the development is to observe northern bright stars in the J , H , and K s bands and provide accurate photometric data on those stars. The second objective is to observe a belt-like region along the northern Galactic plane (| b | ≤ 5° and δ ≥ −30°) repeatedly, to monitor bright variable stars there. The telescope has been in use since 2016 December. The purpose of this paper is to describe the design and operational performances of the telescope, the photometric calibration methods, and our scientific goals. We show that the telescope has the ability to provide photometry with an uncertainty of less than |$5\%$| for stars brighter than 7, 6.5, and 6 mag in the J , H , and K s bands, respectively. The repeatability of the photometric measurements for the same star is better than |$1\%$| for bright stars. Our observations will provide accurate photometry on bright stars that are lacking in the Two Micron Sky Survey and the Two Micron All-Sky Survey. Repeated observations at a good cadence will also reveal their nature in terms of variability in the near-infrared. [ABSTRACT FROM AUTHOR]

Published
2022
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10. Surface brightness correction for compact extended sources observed by the AKARI Far-Infrared Surveyor in the slow-scan mode

Author

Tomasino, Rachael L., Fullard, Andrew, Ueta, Toshiya, Takita, Satoshi, Izumiura, Hideyuki, Shirahata, Mai, Yamamura, Issei, and Matsuura, Shuji

Subjects
techniques: photometric, techniques: image processing, methods: observational, infrared: general, methods: data analysis
Abstract

第4回「あかり」国際会議 (2017年10月17-20日. 東京大学), 文京区, 東京, The 4th AKARI International Conference: The Cosmic Wheel and the Legacy of the AKARI archive: from galaxies and stars to planets and life (October 17-20, 2017. The University of Tokyo), Bunkyo-ku, Tokyo, Japan, We introduce a general-purpose surface brightness correction method for compact extended sources imaged in the slow-scan pointed-observation mode of the Far-Infrared Surveyor (FIS) aboard the AKARI infrared astronomical satellite. Our method recovers correct surface brightness maps by rescaling archived raw FIS maps using the surface-brightness-dependent inverse FIS response function. The flux of a target source is then automatically corrected for as the simple sum of surface brightnesses within the adopted target perimeter (i.e., standard contour photometry). This correction method is contrasted with the previous aperture photometry method for point sources, which directly corrects for the target flux with a flux-dependent scaling law. The new surface brightness correction method is applicable to objects of any shape from unresolved point sources to resolved extended objects, as long as the target is not deemed diffuse, i.e., the total extent of the target source does not exceed much more than a single FIS scan width of about 10 min. The new correction method takes advantage of the well-defined shape (i.e., the scale-invariance) of the point spread function, which enables us to adopt a power-law FIS response function. We analyze the point source photometric calibrator data using the FIS AKARI Slow-Scan Tool and constrain the parameters of the adopted power-law FIS response function. We conclude that the photometric accuracy of the new correction method is better than 10% error based on comparisons with the expected fluxes of the photometric calibrators, and that resulting fluxes without the present correction method can lead to differences more than a factor of two., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730026053, レポート番号: JAXA-SP-17-009E

Published
2018

11. Flux Calibration of the AKARI Far-Infrared Surveyor FIS Data for Extended Emission Sources

Author

Tomasino, Rachael L., Ueta, Toshiya, Yamamura, Issei, and Izumiura, Hideyuki

Abstract

SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe (June 18-21, 2013. Ito Hall, the University of Tokyo), Bunkyou-ku, Tokyo, Japan, We present the preliminary results of the flux calibration for extended sources observed with the Far-Infrared Surveyor (FIS) onboard the AKARI satellite. The circumstellar shells of evolved stars (particularly of AGB and post-AGB stars) retain the fossil record of their mass loss in the form of dust/gas density distributions and these shells have the potential to verify/constrain many theoretical aspects of stellar evolution and mass loss. Hence, it is critical to have an accurate surface brightness and flux calibration. The FIS has four photometric bands between 50-180 μm with two types of Ge:Ga array detectors. The Ge:Ga array is long known to have a slow transient response and FIS has already been characterized for point sources. To calibrate for extended sources, we used a method in which photometry is done in a contour aperture of the 3σ detection threshold above the background to encompass more than the PSF core. We show that the revised slow transient corrections for the short wavelength band have a similar functional form as for the point source corrections, whereas for the long wavelength band two distinct functional forms dependent on the source brightness., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730027055, レポート番号: JAXA-SP-17-010E

Published
2018

13. Regular radial velocity variations in nine G- and K-type giant stars: Eight planets and one planet candidate.

Author

Teng, Huan-Yu, Sato, Bun'ei, Takarada, Takuya, Omiya, Masashi, Harakawa, Hiroki, Izumiura, Hideyuki, Kambe, Eiji, Takeda, Yoichi, Yoshida, Michitoshi, Itoh, Yoichi, Ando, Hiroyasu, and Kokubo, Eiichiro

Subjects
PLANETS, GAS giants, VELOCITY, GIANT stars
Abstract

We report the detection of radial velocity (RV) variations in nine evolved G- and K-type giant stars. The observations were conducted at Okayama Astrophysical Observatory. Planets or planet candidates can best explain these regular variations. However, a coincidence of near 280 d variability among five of them prevents us from fully ruling out stellar origins for some of the variations, since all nine stars behave similarly in stellar properties. In the planet hypotheses for the RV variations, the planets (including one candidate) may survive close to the boundary of the so-called "planet desert" around evolved stars, having orbital periods between 255 and 555 d. Besides, they are the least-massive giant planets detected around G- and K-type giant stars, with minimum masses between 0.45  M J and 1.34  M J. We further investigated other hypotheses for our detection, yet none of them can better explain regular RV variation. With our detection, we can be convinced that year-long regular variation with amplitude down to 15 m s−1 for G- and K-type giant stars is detectable. Moreover, we performed simulations to further confirm the detectability of planets around these stars. Finally, we explored giant planets around intermediate-mass stars, and likewise found a four-Jupiter-mass gap (e.g. Santos et al. 2017, A&A, 603, A30), which is probably a boundary of the giant planet population. [ABSTRACT FROM AUTHOR]

Published
2022
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14. Optical spectroscopic observations of a symbiotic star MWC 560 in the mass accumulation phase.

Author

Ando, Kazuko, Fukuda, Naoya, Sato, Bunei, Maehara, Hiroyuki, and Izumiura, Hideyuki

Subjects
STAR observations, VELOCITY, ABSORPTION
Abstract

There are about a dozen symbiotic stars known to produce high-velocity jets during outbursts. MWC 560 (V694 Mon) is a symbiotic star that seems to show a permanent jet. After showing an unexpected brightening in 2018 November, it has continued to brighten until 2021 and is currently in the brightest state ever. We have been conducting long-term high-dispersion spectroscopic monitoring of this object since 2016 March. An emission wing with v FWHM ≈ 700 km s−1 in the hydrogen Balmer line at an unexpected brightening event in 2018 was reported by Ando et al. (2021 , PASJ, 73, L1). In subsequent continuous observations, this emission wing was no longer seen on 2019 February 6. The absorption lines seen in the hydrogen Balmer lines are gradually deepening and spreading to the slower side of the velocity, and the outflow velocity is becoming slower. The expanding component generated by the outburst was initially observed in the emission wing just after the 2018 outburst, got gradually cooler, and was observed in the absorption line after 2019. [ABSTRACT FROM AUTHOR]

Published
2021
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15. WISE J180956.27-330500.2: A Candidate AGB star with Ongoing Episodic Mass Loss

Author

Gandhi, Poshak, Ladjal, Djazia, GarciaLario, Pedro, Yamamura, Issei, Takita, Satoshi, Ueta, Toshiya, Matsunaga, Noriyuki, and Izumiura, Hideyuki

Abstract

SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe (June 18-21, 2013. Ito Hall, the University of Tokyo), Bunkyou-ku, Tokyo, Japan, Results of infrared photometries and dust shell modeling of a peculiar object WISE J180956.27-330500.2 are presented. The object has shown a significant time variation of its SED in the last 30 years. The variation is understood as a formation and expansion of massive dust shell since late 1990’s. The object was suspected to be a red star in the optical wavelengths before the mass ejection, which allows us to hypothesize that the object is possibly the first example of the AGB star just experiencing an episodic mass loss after a thermal pulse. Observation of this object with SPICA after some 10 years from now will bring us an important clue to understand the stellar evolution and mass loss, as well as the chemistry in the thick circumstellar envelopes., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730027058, レポート番号: JAXA-SP-17-010E

Published
2018

17. The Spin Temperature of NH3 in Comet C/1999S4 (LINEAR)

Author

Kawakita, Hideyo, Watanabe, Jun-ichi, Ando, Hiroyasu, Aoki, Wako, Fuse, Tetsuharu, Honda, Satoshi, Izumiura, Hideyuki, Kajino, Toshitaka, Kambe, Eiji, Kawanomoto, Satoshi, Noguchi, Kunio, Okita, Kiichi, Sadakane, Kozo, Sato, Bun'ei, Takada-Hidai, Masahide, Takeda, Yoichi, Usuda, Tomonori, Watanabe, Etsuji, and Yoshida, Michitoshi

Published
2001

18. Optical spectroscopic monitoring of the symbiotic star MWC 560 before and after the 2018 unpredicted brightening.

Author

Ando, Kazuko, Fukuda, Naoya, Akazawa, Hidehiko, Sato, Bunei, Hasegawa, Ryo, Koizumi, Yohei, Omiya, Masashi, Harakawa, Hiroki, Kambe, Eiji, Maehara, Hiroyuki, and Izumiura, Hideyuki

Subjects
DWARF novae, RED giants, NOVAE (Astronomy), CATACLYSMIC variable stars, ASTRONOMERS, ABSORPTION
Abstract

MWC 560 (V694 Mon) is classified as a symbiotic binary consisting of a white dwarf and an M5III red giant. In this object, a very- high-speed component, thought to be a jet, has been reported in the hydrogen Balmer line. We have been conducting long-term spectroscopic monitoring since the brightening in 2016 February. An irregular rebrightening was reported by Goranskij et al. (2018 , Astronomer's Telegram, 12227), who also showed that the high-velocity absorption component was not seen on 2018 November 16. Our low-resolution spectroscopic observations showed no high-velocity absorption component on 2018 November 14, and wide emission lines in Balmer line region (Hα, Hβ). However, high-resolution spectroscopy revealed the presence of slow, weak absorbing components and an emission wing on 2018 December 25. MWC 560 began to brighten in 2018 November, and it is gradually brightening as of 2020 April 14. For the absorption component, we propose a shell expansion of a classical symbiotic nova that occurred in 2016. During the 2018 brightening a new emission wing with v FWHM ≈ 700 km s−1 was confirmed, which could be triggered by disk instability like a dwarf nova. This paper summarizes the results of long-term monitoring observations and the recent changes in MWC 560. [ABSTRACT FROM AUTHOR]

Published
2021
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19. AKARI Mission Program: Excavating Mass Loss History in Extended Dust Shells of Evolved Stars (MLHES) I. Far-IR Photometry

Author

Torres, Andrew J., Tomasino, Rachael L., Ueta, Toshiya, Izumiura, Hideyuki, Yamamura, Issei, and Takita, Satoshi

Subjects
Infrared, media_common.quotation_subject, FOS: Physical sciences, stars: AGB and post-AGB, circumstellar matter, 01 natural sciences, surveys, 0103 physical sciences, Surface brightness, infrared: stars, 010303 astronomy & astrophysics, Image resolution, Solar and Stellar Astrophysics (astro-ph.SR), media_common, Physics, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Stars, Photometry (astronomy), Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Sky, Circumstellar dust, stars: mass-loss, Data reduction
Abstract

We performed a far-IR imaging survey of the circumstellar dust shells of 144 evolved stars as a mission programme of the AKARI infrared astronomical satellite using the Far-Infrared Surveyor (FIS) instrument. With this survey, we deliver far-IR surface brightness distributions of roughly 10' x 40' or 10' x 20' areas of the sky around the target evolved stars in the four FIS bands at 65, 90, 140, and 160 microns. Our objectives are to characterize the far-IR surface brightness distributions of the cold dust component in the circumstellar dust shells, from which we derive the amount of cold dust grains as low as 20 K and empirically establish the history of the early mass loss history. In this first installment of the series, we introduce the project and its aims, describe the observations, data reduction, and surface brightness correction process, and present the entire data set along with the results of integrated photometry measurements (i.e., the central source and circumstellar dust shell altogether). We find that (1) far-IR emission is detected from all but one object at the spatial resolution about 30" - 50" in the corresponding bands, (2) roughly 60 - 70 % of the target sources show some extension, (3) previously unresolved nearby objects in the far-IR are now resolved around 28 target sources, (4) the results of photometry measurements are reasonable with respect to the entries in the AKARI/FIS Bright Source Catalogue, despite the fact that the targets are assumed to be point-sources when catalogue flux densities were computed, and (5) an IR two-color diagram would place the target sources in a roughly linear distribution that may correlate with the age of the circumstellar dust shell and can potentially be used to identify which targets are more extended than others., To be published in PASJ AKARI Special Issue: 25 pages, 5 figures, 5 tables (and 28 supplementary figures available only in PASJ on-line)

Published
2018

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

Author

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

Subjects
Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, quasars: individual(SDSS J110006.07+442144.3), 01 natural sciences, law.invention, 010309 optics, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, relativistic processes, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, accretion, accretion disks, Near-infrared spectroscopy, quasars: supermassive black holes, Astronomy and Astrophysics, Light curve, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Accretion (astrophysics), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, Flare
Abstract

著者人数: 83名, Accepted: 2017-07-13, 資料番号: SA1170168000

Published
2017

25. Long-term Near-infrared Brightening of Nonvariable OH/IR Stars.

Author

Kamizuka, Takafumi, Nakada, Yoshikazu, Yanagisawa, Kenshi, Ohsawa, Ryou, Ita, Yoshifusa, Izumiura, Hideyuki, Mito, Hiroyuki, Onozato, Hiroki, Asano, Kentaro, Ueta, Toshiya, and Miyata, Takashi

Subjects
CIRCUMSTELLAR matter, STELLAR mass, NEAR infrared radiation, STELLAR luminosity function, DUST, DUST explosions
Abstract

Nonvariable OH/IR stars are thought to have just left the asymptotic giant branch (AGB) phase. In this conventional picture, they must still show strong circumstellar extinction caused by the dust ejected during the AGB phase, and the extinction is expected to decrease over time because of the dispersal of the circumstellar dust after the cessation of stellar mass loss. The reduction of extinction makes the stars become apparently brighter and bluer with time, especially in the near-infrared (NIR) range. We look for such long-term brightening of nonvariable OH/IR stars by using 2MASS, UKIDSS, and OAOWFC survey data. As such, we obtain multiepoch NIR data taken over a 20 yr period (1997–2017) for 6 of 16 nonvariable OH/IR stars, and all 6 objects are found to be brightening. The K-band brightening rate of five objects ranges from 0.010 to 0.130 mag yr−1, which is reasonably explained with the conventional picture. However, one OH/IR star, OH 31.0−0.2, shows a rapid brightening, which cannot be explained only by the dispersal of the dust shell. Multicolor (J-, H-, and K-band) data are obtained for three objects, OH 25.1−0.3, OH 53.6−0.2, and OH 77.9+0.2. Surprisingly, none of them appears to have become bluer, and OH 53.6−0.2 is found to have reddened at a rate of 0.013 mag yr−1 in (J – K). Our findings suggest other mechanisms such as rapid changes in stellar properties (temperature or luminosity) or a generation of a new batch of dust grains. [ABSTRACT FROM AUTHOR]

Published
2020
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26. The Seimei telescope project and technical developments.

Author

Kurita, Mikio, Kino, Masaru, Iwamuro, Fumihide, Ohta, Kouji, Nogami, Daisaku, Izumiura, Hideyuki, Yoshida, Michitoshi, Matsubayashi, Kazuya, Kuroda, Daisuke, Nakatani, Yoshikazu, Yamamoto, Kodai, Tsutsui, Hironori, Iribe, Masatsugu, Jikuya, Ichiro, Ohtani, Hiroshi, Shibata, Kazunari, Takahashi, Keisuke, Tokoro, Hitoshi, Maihara, Toshinori, and Nagata, Tetsuya

Subjects
OPTICAL telescopes, TELESCOPES, ASTRONOMICAL observatories, GENETIC algorithms, TIME management, OPTICS
Abstract

An overview of the Seimei telescope, a 3.8 m optical infrared telescope located on Mt. Chikurinji in the Okayama prefecture of Japan, is presented. Seimei is a segmented-mirror telescope whose primary mirror consists of 18 petal-shaped segments. The telescope tube supporting the thin segmented mirrors is structurally incorporated within large arc-rails providing the elevation axis. The tube has a light-weight homologous structure designed with a genetic algorithm. The total weight of the telescope tube, including 1.4-ton optics, is only 8 tons. By virtue of its light weight, the telescope is able to point at an object anywhere in the observable sky within one minute. The telescope is operated by Kyoto University in collaboration with the National Astronomical Observatory of Japan (NAOJ). Half of the telescope time is used by Kyoto University. The remaining time is open to the Japanese astronomical community. NAOJ is responsible for the management of the open-use time, including handling of the observation proposals. The telescope is now regularly performing scientific observations on the basis of a variety of proposals. [ABSTRACT FROM AUTHOR]

Published
2020
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29. 小惑星(893)Leopoldinaの光度曲線

Author

Kuroda, Daisuke, Yoshikawa, Makoto, Yanagisawa, Kenshi, Shimizu, Yasuhiro, Nagayama, Shogo, Inata, Motoko, Hattori, Takashi, Okita, Kiichi, Koyano, Hisashi, and Izumiura, Hideyuki

Subjects
小惑星(893)Leopoldina, ガンマ線バースト, 多色カメラ, lightcurve, multi-color camera, Okayama Astrophysical Observatory, 望遠鏡, telescope, 岡山天体物理観測所, Asteroid (893) Leopoldina, gamma ray burst, 残光, 光学フィルター, optical filter, 光度曲線, afterglow
Abstract

A 0.5 m telescope with a multi-color camera at the Okayama Astrophysical Observatory has been developed for the observation of the optical afterglow of a gamma ray burst and lightcurve of asteroids. This camera can observe objects through a V, R and I band at the same time. Reported is the result of the test observation of an asteroid (893) Leopoldina by this telescope with a single color camera. The rotational period of this asteroid was found as 12.60 hours. This asteroid probably owns a satellite from the previous observation (Dunham, 1997). The multi-color CCD photometry of several asteroids with satellite will be carried out., 資料番号: AA0047898062

Published
2004

30. The Herschel Planetary Nebula Survey (HerPlaNS). I. Data overview and analysis demonstration with NGC 6781

Author

Ladjal, D., Exter, K. M., Szczerba, R., Siodmiak, N., Aleman, I., van, Hoof P. A. M., Kastner, J. H., Montez, Jr. R., McDonald, I., Wittkowski, M., Sandin, C., Ramstedt, S., DeMarco, O., Villaver, E., Chu, Y.-H., Vlemmings, W., Sahai, R., Lopez, J. A., Balick, B., Zijlstra, A., Tielens, A. G. G. M., Rattray, R. E., Behar, E., Blackman, E. G., Hebden, K., Hora, J. L., Murakawa, K., Nordhaus, J., Nordon, R., Ueta, Toshiya, Otsuka, M., Izumiura, Hideyuki, and Yamamura, Issei

Subjects
Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Spatial distribution, 01 natural sciences, Spectral line, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, planetary nebulae: general, Spectroscopy, 010303 astronomy & astrophysics, infrared: stars, Astrophysics::Galaxy Astrophysics, Physics, Nebula, 010308 nuclear & particles physics, White dwarf, Astronomy and Astrophysics, Mass ratio, Planetary nebula, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), stars: winds, Halo, Astrophysics::Earth and Planetary Astrophysics
Abstract

著者人数: 33名, Accepted: 2014-03-14, 資料番号: SA1140080000

Published
2014

32. The ISO-SWS Spectrum of NML Cyg

Author

Justtanont, K., de, Jong T., Helmich, F. P., Waters, L. B. F. M., de, Graauw T., Loup, C., Beintema, D. A., Lahuis, F., Roelfsema, P.R., Valentijn, E.A., Izumiura, Hideyuki, and Yamamura, Issei

Abstract

著者人数: 12名, Accepted: 1996-08-02, 資料番号: SA1003920000

Published
1996

38. Mass Loss History of the AGB star, R Cas

Author

Ueta, Toshiya, Stencel, Robert E., Yamamura, Issei, Izumiura, Hideyuki, Nakada, Yoshikazu, Matsuura, Mikako, Ita, Yoshifusa, Tanabe, Toshihiko, Fukushi, Hinako, Matsunaga, Noriyuki, Mito, Hiroyuki, and Speck, Angela K.

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

We report here on the discovery of an extended far-infrared shell around the AGB star, R Cassiopeia, made by AKARI and Spitzer. The extended, cold circumstellar shell of R Cas spans nearly 3 arcmin and is probably shaped by interaction with the interstellar medium. This report is one of several studies of well-resolved mass loss histories of AGB stars under AKARI and Spitzer observing programs labeled "Excavating Mass Loss History in Extended Dust Shells of Evolved Stars (MLHES)"., Poster contribution, to be published in the proceedings of the conference "AKARI, a light to illuminate the misty Universe" held at University of Tokyo, Japan, 16-19 February 2009

Published
2009

39. The space infrared telescope for cosmology and astrophysics: SPICA A joint mission between JAXA and ESA

Author

SWINYARD, Bruce, NAKAGAWA, Takao, MERKEN, Patrick, ROYER, Pierre, SOUVERIJNS, Tim, VANDENBUSSCHE, Bart, WAELKENS, Christoffel, DAVIS, Peter, DI FRANCESCO, James, HALPERN, Mark, HOUDE, Martin, JOHNSTONE, Doug, JONCAS, Gilles, NAYLOR, David, PLUME, Rene, SCOTT, Douglas, ABERGEL, A., BENSAMMAR, S., BRAINE, J., BUAT, V., BURGARELLA, D., CAIS, Ph., DOLE, H., DUBAND, L., ELBAZ, D., GERIN, M., GIARD, M., GOICOECHEA, J., JOBLIN, C., JONES, A., KNEIB, J. P., LAGACHE, Guilaine, MADDEN, S., PONS, R., PAJOT, F., RAMBAUD, D., RAVERA, L., RISTORCELLI, I., RODRIGUEZ, L., VIVES, S., ZAVAGNO, Annie, GEIS, Norbert, KRAUSE, Oliver, LUTZ, Dieter, POGLITSCH, Albrecht, RAAB, Walfried, STEGMAIER, Jutta, STURM, Eckhard, TUFFS, Richard, LEE, Hyung Mok, KOO, Bon-Chul, IM, Myungshin, PAK, Soojong, HAN, Wonyong, PARK, Jang-Hyun, NAM, Uk-Won, JIN, Ho, LEE, Dae-Hee, YUK, In-Soo, LEE, Sungho, AIKAWA, Yuri, ARIMOTO, Nobuo, DOI, Yasuo, ENYA, Keigo, FUKAGAWA, Misato, FURUSHO, Reiko, HASEGAWA, Sunao, HAYASHI, Masahiko, HONDA KANAGAWA, Mitsuhiko, IDA, Shigeru, IMANISHI, MASATOSHI, INUTSUKA, Shu-Ichiro, IZUMIURA, Hideyuki, KAMAYA, Hideyuki, KANEDA, Hidehiro, KASUGA, Toshihiro, KATAZA, Hirokazu, KAWABATA, Koji, KAWADA, Mitsunobu, KAWAKITA, Hideyo, KII, Tsuneo, KODA, Jin, KODAMA, Tadayuki, KOKUBO, Eiichiro, KOMATSU, Keiji, MATSUHARA, Hideo, MATSUMOTO, Toshio, MATSUURA, Shuji, MIYATA, Takashi, MIYATA, Murakam, NAGATA, Hirohisa, NAGATA, Tetsuya, NAKAJIMA, Tadashi, NAOTO, Kobayashi, NISHI, Ryoichi, NODA, Atsushi, OKAMOTO, Atsushi, OKAMOTO, Yoshiko K., OMUKAI, Kazuyuki, ONAKA, Takashi, OOTSUBO, Takafumi, OUCHI, Masami, SAITO, Hirobumi, SATO, Yoichi, SAKO, Shigeyuki, SEKIGUCHI, Tomohiko, SHIBAI, Hiroshi, SUGITA, Hiroyuki, SUGITANI, Koji, SUSA, Hajime, PYO, Tae-Soo, TAMURA, Motohide, UEDA, Yoshihiro, UENO, Munetaka, WADA, Takehiko, WATANABE, Jun'Ichi, YAMADA, Toru, YAMAMURA, Issei, YOSHIDA, Naoki, YOSHIMI, Kitamura, YUI, Yukari, BENEDETTINI, Milena, CERULLI, Riccardo, DI GIORGIO, Anna, MOLINARI, Sergio, ORFEI, Renato, PEZZUTO, Stefano, PIAZZO, Lorenzo, SARACENO, Paolo, SPINOGLIO, Luigi, DE GRAAUW, Thijs, DE KORTE, Piet, HELMICH, Frank, HOEVERS, Henk, HUISMAN, Robert, SHIPMAN, Russell, VAN DER TAK, Floris, VAN DER WERF, Paul, WILD, Wolfgang, ACOSTA-PULIDO, Jose, CERNICHARO, Jose, HERREROS, Jose, MARTIN-PINTADO, Jesus, NAJARRO, Francisco, PEREZ-FOURMON, Ismael, RAMON PARDO, Juan, GOMEZ, Francisca, CASTRO RODRIGUEZ, Nieves, ADE, Peter, BARLOW, Mike, CLEMENTS, David, FERLET, Marc, FRASER, Helen, GRIFFIN, Douglas, GRIFFIN, Matthew, HARGRAVE, Peter, ISAAK, Kate, IVISON, Robert, MANSOUR, Malik, LANIESSE, Jonathan, MAUSKOPF, Phillip, MOROZOV, Dmitry, OLIVER, Seb, ORLANDO, Angiola, PAGE, Mathew, POPESCU, Cristina, SERJEANT, Stephen, SUDIWALA, Rashmi, RIGOPOULOU, Dimitra, WALKER, Ian, WHITE, Glenn, VITI, Serena, WINTER, Berend, BOCK, Jamie, BRADFORD, Matt, HARWIT, Martin, HOLMES, Warren, Institut Méditerranéen d'Ecologie et de Paléoécologie (IMEP), Université Paul Cézanne - Aix-Marseille 3-Centre National de la Recherche Scientifique (CNRS)-Avignon Université (AU)-Université de Provence - Aix-Marseille 1, Institute of Atomic Physics, Université de Roumanie, Groundwater Tracing Unit, Department of Geological Sciences, School of Environmental Sciences [Norwich], University of East Anglia [Norwich] (UEA), Institut de Recherche en Immunologie et en Cancérologie [UdeM-Montréal] (IRIC), Université de Montréal (UdeM), Department of Zoology, University of Otago [Dunedin, Nouvelle-Zélande], Transplantation Biology Group, Imperial College London, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), FORMATION STELLAIRE 2009, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Radioastronomie (LRA), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Processus mentaux et activation cérébrale, Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-IFR19-Institut National de la Santé et de la Recherche Médicale (INSERM), IFR des neurosciences de Lyon (IFNL), Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre Hospitalier le Vinatier [Bron]-Hospices Civils de Lyon (HCL)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, British Antarctic Survey (BAS), Natural Environment Research Council (NERC), Department of Radio and Space Science [Göteborg], Chalmers University of Technology [Göteborg], Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Services communs OMP (UMS 831), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Solar Influences Data Analysis Center [Brussels] (SIDC), Royal Observatory of Belgium [Brussels] (ROB), Propriétés Optiques des Matériaux et Applications (POMA), Centre National de la Recherche Scientifique (CNRS)-Université d'Angers (UA), Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies (UMR 6174) (FEMTO-ST), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physiology, The University of Hong Kong (HKU), School of Environmental Systems Engineering (SESE), The University of Western Australia (UWA), Centre for Water Research (CWR), Macaulay Institute, Centre Science des Matériaux et des Structures (SMS-ENSMSE), École des Mines de Saint-Étienne (Mines Saint-Étienne MSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Département Mécanique et Procédés d'Elaboration (MPE-ENSMSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-SMS, Department of Obstetrics and Gynecology [Stanford], Stanford Medicine, Stanford University-Stanford University, Korea Astronomy and Space Science Institute (KASI), Okayama University, Jack Baskin School of Engineering (UCSC), University of California [Santa Cruz] (UCSC), University of California-University of California, Adobe Systems Inc. (Adobe Advanced Technology Labs), Adobe Systems Inc., Defence Evaluation and Research Agency (DERA), Ministry of Defence (UK) (MOD)-Propulsion and Performance Department, Centre for Air Transport and the Environment (CATE), Manchester Metropolitan University (MMU), Department of Chemistry, Williams Hall-Kent State University, School of Earth and Atmospheric Sciences [Atlanta], Georgia Institute of Technology [Atlanta], Department of Earth and Planetary Sciences [Kobe], Kobe University, National Institute of Agro-Environmental Sciences (NIAES), Department of Earth System Science and Technology [Fukuoka] (ESST), Kyushu University [Fukuoka], Tokyo Institute of Technology [Tokyo] (TITECH), Department of Information and Communication Engineering, Graduate School of Information Science and Technology-The University of Tokyo (UTokyo), Department of Physics and Earth Sciences, University of the Ryukyus [Okinawa], Japan Agency for Marine-Earth Science and Technology (JAMSTEC), Center for Climate System Research [Kashiwa] (CCSR), The University of Tokyo (UTokyo), School of Humanities [Univ of Toyama], University of Toyama, Department of Mechanical System (Hiroshima University), Hiroshima University, High Temperature Plasma Center [Tokyo], Discrete Optimization Laboratory, Toyohashi University of Technology, Hatakeyama Laboratory, University of Electro-Communications [Tokyo] (UEC)-Tohoku University [Sendai], Institute of Industrial Science (IIS), Institut de génétique et biologie moléculaire et cellulaire (IGBMC), Université Louis Pasteur - Strasbourg I-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Science and Technology Research Center (MCC), Mitsubishi Chemical Corporation, Institute for Solid State Physics [Tokyo] (ISSP), University of Electro-Communications [Tokyo] (UEC), Faculty of Science and Engineering [Waseda], Waseda University, Department of Civil Engineering, Chuo University (Chuo University), Frontier Collaborative Research Center (FCRC), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Antarctic Research a European Network for Astrophysics (ARENA), Institut de biologie et chimie des protéines [Lyon] (IBCP), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), SRON Netherlands Institute for Space Research (SRON), Max-Planck-Institut für Radioastronomie (MPIFR), Departamento de Astrofísica Molecular e Infrarroja (DAMIR), Instituto de Estructura de la Materia (IEM), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire d'océanographie et de biogéochimie (LOB), Université de la Méditerranée - Aix-Marseille 2-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Ecosystèmes Littoraux et Cotiers, Université de Lille, Sciences et Technologies-Centre National de la Recherche Scientifique (CNRS), Royal Observatory Edinburgh (ROE), University of Edinburgh, Processus d'Activation Sélective par Transfert d'Energie Uni-électronique ou Radiatif (UMR 8640) (PASTEUR), Université Pierre et Marie Curie - Paris 6 (UPMC)-Département de Chimie - ENS Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Ecole Supérieure des Affaires (ESA), Université Pierre Mendès France - Grenoble 2 (UPMF), Service de Neurologie [CHU Pitié-Salpêtrière], IFR70-CHU Pitié-Salpêtrière [AP-HP], Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Neurologie et thérapeutique expérimentale, Institut National de la Santé et de la Recherche Médicale (INSERM)-IFR70-Université Pierre et Marie Curie - Paris 6 (UPMC), Department of Physics, University of Wales, Engineering Department, University of Cambridge [UK] (CAM), SLAC National Accelerator Laboratory (SLAC), Stanford University, Université Paul Cézanne - Aix-Marseille 3-Université de Provence - Aix-Marseille 1-Avignon Université (AU)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université de Lyon-Université de Lyon-Hospices Civils de Lyon (HCL)-Centre Hospitalier le Vinatier [Bron]-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université d'Angers (UA)-Centre National de la Recherche Scientifique (CNRS), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), University of California [Santa Cruz] (UC Santa Cruz), University of California (UC)-University of California (UC), Kyushu University, Waseda University [Tokyo, Japan], National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), Université Pierre et Marie Curie - Paris 6 (UPMC)-IFR70-Institut National de la Santé et de la Recherche Médicale (INSERM), Institut de Recherche en Immunologie et en Cancérologie (IRIC), Université de Montréal [Montréal], PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Services communs OMP - UMS 831 (UMS 831), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Toulouse III - Paul Sabatier (UT3), Royal Observatory of Belgium [Brussels], Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Technologie de Belfort-Montbeliard (UTBM), Division of Reproductive Biology, Stanford University [Stanford], Okayama University [Okayama], Graduate School of Information Science and Technology-The University of Tokyo, The University of Tokyo, Department of linguistic [Toyama], Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS), Service de neurologie 1 [CHU Pitié-Salpétrière], Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-CHU Pitié-Salpêtrière [APHP], Stanford Linear Accelerator Center (SLAC), Astronomy, Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), The University of Tokyo (UTokyo)-Graduate School of Information Science and Technology, Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-CHU Pitié-Salpêtrière [AP-HP], and Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Sorbonne Université (SU)

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Infrared telescope, UNIVERSE, Astrophysics, Spica, Astrophysics::Cosmology and Extragalactic Astrophysics, POLYCYCLIC AROMATIC-HYDROCARBON, 7. Clean energy, 01 natural sciences, Space missions, Cosmology, Space exploration, law.invention, STAR-FORMATION, 010309 optics, Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Spitzer Space Telescope, law, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Infrared astronomy, SPECTRUM, Spacecraft, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], SUBMILLIMETER GALAXIES, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, MODEL, SPITZER, PAHS, Space and Planetary Science, Infrared, Physics::Space Physics, IR, Astrophysics::Earth and Planetary Astrophysics, business, EMISSION
Abstract

International audience; The Space Infrared telescope for Cosmology and Astrophysics (SPICA) is planned to be the next space astronomy mission observing in the infrared. The mission is planned to be launched in 2017 and will feature a 3.5 m telescope cooled to 30 microns wavelength). We describe the scientific advances that will be made possible by this large increase in sensitivity and give details of the mission, spacecraft and focal plane conceptual design.

Published
2009

40. Development of iodine cells for Subaru HDS and Okayama HIDES. III. An improvement on radial velocity measurement technique

Author

Kambe, Eiji, Ando, Hiroyasu, Sato, Bun’ei, Izumiura, Hideyuki, Sekii, Takashi, Paulson, Diane B., Yanagisawa, Kenshi, Masuda, Seiji, Shibahashi, Hiromoto, Hatzes, Artie P., Martic, Milena, Lebrun, Jean-Claude, Mkrtichian, David E., Kiss, Laszlo L., Bruntt, Hans, O'Toole, Simon J., Bedding, Timothy R., Okayama Astrophysical Observatory (OAO), National Astronomical Observatory of Japan (NAOJ), Tokyo Institute of Technology [Tokyo] (TITECH), NASA Goddard Space Flight Center (GSFC), Tokushima Science Museum, Graduate School of Science [Tokyo], The University of Tokyo (UTokyo), Thüringer Landessternwarte Tautenburg (TLS), Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astronomical observatory of Odessa National University [Odessa], Odessa National I.I.Mechnikov University, School of Physics [Sydney], The University of Sydney, and Anglo-Australian Observatory (AAO)

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract

An improvement of the radial-velocity measurement accuracy is crucial for the detection of tiny stellar oscil- lations and exoplanets. Through the analysis of week-long extensive observations of solar-type stars (Procyon in 2000, 2002, and 2006/2007 and Cet in 2002 and 2006/2007), we have carefully examined, revised, and finely tuned the widely used multiple Gaussian IP fitting method for the spectrograph, HIDES. By determining a necessary and sufficient number of free parameters in the model as well as introducing an iterative process in the radial-velocity analysis, we can reach a precision of below 3 m s 1 , which is much smaller than the precision of 6 m s 1 officially announced so far for HIDES. We also make our technique refined for the 2002 McDonald Procyon data. Even with our revised method, slow radial velocity variations with an amplitude of about 10 m s 1 are left in the Procyon data. We emphasize that it is neither due to particular observing instruments nor radial-velocity analysis, and thus could be due to stellar origin. The analysis presented here makes the foundations of our next scientific analysis of the radial-velocity variations of Procyon, which will be presented in our forthcoming papers.

Published
2008

42. Korean-Japanese Planet Search Program: Substellar Companions around Intermediate-Mass Giants.

Author

Omiya, Masashi, Han, Inwoo, Izumiura, Hideyuki, Lee, Byeong-Cheol, Sato, Bun'ei, Kim, Kang-Min, Yoon, Tae Seog, Kambe, Eiji, Yoshida, Michitoshi, Masuda, Seiji, Toyota, Eri, Urakawa, Seitaro, and Takada-Hidai, Masahide

Subjects
DETECTION of extrasolar planets, GIANT stars, STELLAR mass, BROWN dwarf stars, SUPERGIANT stars, TELESCOPES, ASTRONOMICAL observatories
Abstract

A Korean-Japanese planet search program has been carried out using the 1.8m telescope at Bohyunsan Optical Astronomy Observatory (BOAO) in Korea, and the 1.88m telescope at Okayama Astrophysical Observatory (OAO) in Japan to search for planets around intermediate-mass giant stars. The program aims to show the properties of planetary systems around such stars by precise Doppler survey of about 190 G or K type giants together with collaborative surveys of the East-Asian Planet Search Network. So far, we detected two substellar companions around massive intermediate-mass giants in the Korean-Japanese planet search program. One is a brown dwarf-mass companion with 37.6 MJ orbiting a giant HD 119445 with 3.9 M⊙, which is the most massive brown dwarf companion among those found around intermediate-mass giants. The other is a planetary companion with 1.8 MJ orbiting a giant star with 2.4 M⊙, which is the lowest-mass planetary companion among those detected around giant stars with >1.9 M⊙. Plotting these systems on companion mass vs. stellar mass diagram, there seem to exist two unpopulated regions of substellar companions around giants with 1.5-3 M⊙ and planetary companions orbiting giants with 2.4-4 M⊙. The existence of these possible unpopulated regions supports a current characteristic view that more massive substellar companions tend to exist around more massive stars. [ABSTRACT FROM AUTHOR]

Published
2011
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43. HiCIAO: A High-contrast Instrument for the Next Generation Subaru Adaptive Optics.

Author

Suzuki, Ryuji, Tamura, Motohide, Suto, Hiroshi, Morino, Jun-ichi, Hashimoto, Jun, Kudo, Tomoyuki, Kandori, Ryo, Murakami, Naoshi, Nishikawa, Jun, Ukita, Nobuharu, Takami, Hideki, Guyon, Olivier, Nishimura, Tetsuo, Hayashi, Masahiko, Izumiura, Hideyuki, Abe, Lyu, Tavrov, Alexander, Jacobson, Shane, Stahlberger, Vern, and Yamada, Hubert

Subjects
ADAPTIVE optics, IMAGE stabilization, TELESCOPES, INFRARED radiation, IMAGING systems
Abstract

HiCIAO (the High-Contrast Instrument with Adaptive Optics) is a high-contrast instrument for the 8.2-meter Subaru Telescope. The instrument is a near-infrared camera which benefits from a new adaptive optics (AO) system on the Subaru Telescope (AO188). The instrument realizes the high contrast with a help of AO188, a classical Lyot coronagraph, and three differential imaging techniques (polarimetric, spectral, and angular). Besides the differential imaging modes, HiCIAO also offers a normal imaging mode which covers 20″×20″ FOV with 0.″01 pixel-1 resolution, and a pupil viewing mode for a precise alignment of the Lyot stop on the pupil image. The expected contrasts are 105.5 at 1.″0 separation and 104 at 0.″1 separation from a central star in the spectral differential imaging mode. The instrument is currently in its commissioning phase after the first-light observation in December 2008. This paper is an introductory review of the instrument. [ABSTRACT FROM AUTHOR]

Published
2009
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45. Dynamics of Stars in the Inner Galactic Bulge Revealed from SiO Maser Surveys.

Author

Wada, Keiichi, Combes, Françoise, Deguchi, Shuji, Fujii, Takahiro, Ita, Yoshifusa, Izumiura, Hideyuki, Kameya, Osamu, Miyazaki, Atsushi, Nakada, Yoshikazu, and Ideta, Makoto

Abstract

We surveyed ~300 MSX/2MASS infrared objects in the 7° × 2° area of the Galactic center in the ~43 GHz SiO maser lines, obtaining accurate radial velocities of ~160 detected objects. The longitude-velocity diagram of these objects reveals two conspicuous features: one indicating a linear velocity increase with longitude with l < 1.5°, which is likely to be associated with the inner bar, and the other having eccentric velocities with Vlsr >250 km s-1. Based on numerical simulations of stellar orbits in the Galactic bulge, we conclude that the latter feature is created as a result of a past star formation in the bulge, when the intersecting point of the x1 and x2 orbits was considerably outside of the present position. [ABSTRACT FROM AUTHOR]

Published
2008
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47. OPTICAL-TO-NEAR-INFRARED SIMULTANEOUS OBSERVATIONS FOR THE HOT URANUS GJ3470b: A HINT OF A CLOUD-FREE ATMOSPHERE.

Author

FUKUI, AKIHIKO, NARITA, NORIO, KUROSAKI, KENJI, IKOMA, MASAHIRO, YANAGISAWA, KENSHI, KURODA, DAISUKE, SHIMIZU, YASUHIRO, TAKAHASHI, YASUHIRO H., OHNUKI, HIROSHI, ONITSUKA, MASAHIRO, HIRANO, TERUYUKI, SUENAGA, TAKUYA, KAWAUCHI, KIYOE, NAGAYAMA, SHOGO, OHTA, KOUJI, YOSHIDA, MICHITOSHI, KAWAI, NOBUYUKI, and IZUMIURA, HIDEYUKI

Subjects
NEAR infrared radiation, ASTRONOMICAL photometry, NATURAL satellites, URANUS (Planet), DWARF stars
Abstract

We present optical (g', Rc, and Ic) to near-infrared (J) simultaneous photometric observations for a primary transit of GJ3470b, a Uranus-mass transiting planet around a nearby M dwarf, by using the 50 cm MITSuME telescope and the 188 cm telescope, both at the Okayama Astrophysical Observatory. From these data, we derive the planetary mass, radius, and density as 14.1±1.3 M⊙, 4.32-0.10+0.21 R⊕, and 0.94±0.12 g cm-3, respectively, thus confirming the low density that was reported by Demory et al. based on the Spitzer/IRAC 4.5 μm photometry (0.72-0.12+0.13 g cm-3). Although the planetary radius is about 10% smaller than that reported by Demory et al., this difference does not alter their conclusion that the planet possesses a hydrogen-rich envelope whose mass is approximately 10% of the planetary total mass. On the other hand, we find that the planet-to-star radius ratio (Rp/Rs ) in the J band (0.07577-0.00075+0.00072) is smaller than that in the Ic (0.0802±0.0013) and 4.5 μm (0.07806+0.00052 -0.00054) bands by 5.8%±2.0% and 2.9%±1.1%, respectively. A plausible explanation for the differences is that the planetary atmospheric opacity varies withwavelength due to absorption and/or scattering by atmospheric molecules.Although the significance of the observed Rp/Rs variations is low, if confirmed, this fact would suggest that GJ3470b does not have a thick cloud layer in the atmosphere. This property would offer a wealth of opportunity for future transmission-spectroscopic observations of this planet to search for certain molecular features, such as H2O, CH4, and CO, without being prevented by clouds. [ABSTRACT FROM AUTHOR]

Published
2013
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48. DENSE OPTICAL AND NEAR-INFRARED MONITORING OF CTA 102 DURING HIGH STATE IN 2012 WITH OISTER: DETECTION OF INTRA-NIGHT "ORPHAN POLARIZED FLUX FLARE".

Author

ITOH, RYOSUKE, FUKAZAWA, YASUSHI, TANAKA, YASUYUKI T., ABE, YUHEI, AKITAYA, HIROSHI, ARAI, AKIRA, HAYASHI, MASAHIKO, HORI, TAKAFUMI, ISOGAI, MIZUKI, IZUMIURA, HIDEYUKI, KAWABATA, KOJI S., KAWAI, NOBUYUKI, KURODA, DAISUKE, MIYANOSHITA, RYO, MORITANI, YUKI, MOROKUMA, TOMOKI, NAGAYAMA, TAKAHIRO, NAKAMOTO, JUMPEI, NAKAT, CHIKAKO, and OASA, YUMIKO

Published
2013
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