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50 results on '"OKAMOTO, Yoshiko K."'

1. The Fundamental Stellar Parameters of FGK Stars in the SEEDS Survey

Author

Rich, Evan A., Wisniewski, John P., McElwain, Michael W., Hashimoto, Jun, Kudo, Tomoyuki, Kusakabe, Nobuhiko, Okamoto, Yoshiko K., Abe, Lyu, Akiyama, Eiji, Brandner, Wolfgang, Brandt, Timothy D., Cargile, Phillip, Carson, Joseph C., Currie, Thayne M, Egner, Sebastian, Feldt, Markus, Fukagawa, Misato, Goto, Miwa, Grady, Carol A., Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko S., Hebb, Leslie, Helminiak, Krzysztof G., Henning, Thomas, Hodapp, Klaus W., Ishii, Miki, Iye, Masanori, Janson, Markus, Kandori, Ryo, Knapp, Gillian R., Kuzuhara, Masayuki, Kwon, Jungmi, Matsuo, Taro, Mayama, Satoshi, Miyama, Shoken, Momose, Munetake, Morino, Jun-Ichi, Moro-Martin, Amaya, Nakagawa, Takao, Nishimura, Tetsuo, Oh, Daehyeon, Pyo, Tae-Soo, Schlieder, Joshua, Serabyn, Eugene, Sitko, Michael L., Suenaga, Takuya, Suto, Hiroshi, Suzuki, Ryuji, Takahashi, Yasuhiro H., Takami, Michihiro, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Watanabe, Makoto, Yamada, Toru, Takami, Hideki, Usuda, Tomonori, and Tamura, Motohide

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Large exoplanet surveys have successfully detected thousands of exoplanets to-date. Utilizing these detections and non-detections to constrain our understanding of the formation and evolution of planetary systems also requires a detailed understanding of the basic properties of their host stars. We have determined the basic stellar properties of F, K, and G stars in the Strategic Exploration of Exoplanets and Disks with Subaru (SEEDS) survey from echelle spectra taken at the Apache Point Observatory's 3.5m telescope. Using ROBOSPECT to extract line equivalent widths and TGVIT to calculate the fundamental parameters, we have computed Teff, log(g), vt, [Fe/H], chromospheric activity, and the age for our sample. Our methodology was calibrated against previously published results for a portion of our sample. The distribution of [Fe/H] in our sample is consistent with that typical of the Solar neighborhood. Additionally, we find the ages of most of our sample are $< 500 Myrs$, but note that we cannot determine robust ages from significantly older stars via chromospheric activity age indicators. The future meta-analysis of the frequency of wide stellar and sub-stellar companions imaged via the SEEDS survey will utilize our results to constrain the occurrence of detected co-moving companions with the properties of their host stars., Comment: 22 Pages, 10 Figures, 5 Tables. Published in MNRAS

Published
2017
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2. Constraining the Movement of the Spiral Features and the Locations of Planetary Bodies within the AB Aur System

Author

Lomax, Jamie R., Wisniewski, John P., Grady, Carol A., McElwain, Michael W., Hashimoto, Jun, Kudo, Tomoyuki, Kusakabe, Nobuhiko, Okamoto, Yoshiko K., Fukagawa, Misato, Abe, Lyu, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph C., Currie, Thayne M., Egner, Sebastian, Feldt, Markus, Goto, Miwa, Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko S., Henning, Thomas, Hodapp, Klaus W., Inoue, Akio, Ishii, Miki, Iye, Masanori, Janson, Markus, Kandori, Ryo, Knapp, Gillian R., Kuzuhara, Masayuki, Kwon, Jungmi, Matsuo, Taro, Mayama, Satoshi, Miyama, Shoken, Momose, Munetake, Morino, Jun-Ichi, Moro-Martin, Amaya, Nishimura, Tetsuo, Pyo, Tae-Soo, Schneider, Glenn H, Serabyn, Eugene, Sitko, Michael L., Suenaga, Takuya, Suto, Hiroshi, Suzuki, Ryuji, Takahashi, Yasuhiro H., Takami, Michihiro, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Watanabe, Makoto, Yamada, Toru, Takami, Hideki, Usuda, Tomonori, and Tamura, Motohide

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present new analysis of multi-epoch, H-band, scattered light images of the AB Aur system. We used a Monte Carlo, radiative transfer code to simultaneously model the system's SED and H-band polarized intensity imagery. We find that a disk-dominated model, as opposed to one that is envelope dominated, can plausibly reproduce AB Aur's SED and near-IR imagery. This is consistent with previous modeling attempts presented in the literature and supports the idea that at least a subset of AB Aur's spirals originate within the disk. In light of this, we also analyzed the movement of spiral structures in multi-epoch H-band total light and polarized intensity imagery of the disk. We detect no significant rotation or change in spatial location of the spiral structures in these data, which span a 5.8 year baseline. If such structures are caused by disk-planet interactions, the lack of observed rotation constrains the location of the orbit of planetary perturbers to be >47 AU., Comment: 8 pages, 3 figures, 1 table, Accepted to ApJ

Published
2016
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3. Detailed structure of the outer disk around HD 169142 with polarized light in H-band

Author

Momose, Munetake, Morita, Ayaka, Fukagawa, Misato, Muto, Takayuki, Takeuchi, Taku, Hashimoto, Jun, Honda, Mitsuhiko, Kudo, Tomoyuki, Okamoto, Yoshiko K., Kanagawa, Kazuhiro D., Tanaka, Hidekazu, Grady, Carol A., Sitko, Michael L., Akiyama, Eiji, Currie, Thayne, Follette, Katherine B., Mayama, Satoshi, Kusakabe, Nobuhiko, Abe, Lyu, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph C., Egner, Sebastian, Feldt, Markus, Goto, Miwa, Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko S., Henning, Thomas, Hodapp, Klaus W., Ishii, Miki, Iye, Masanori, Janson, Markus, Kandori, Ryo, Knapp, Gillian R., Kuzuhara, Masayuki, Kwon, Jungmi, Matsuo, Taro, McElwain, Michael W., Miyama, Shoken, Morino, Jun-Ichi, Moro-Martin, Amaya, Nishimura, Tetsuo, Pyo, Tae-Soo, Serabyn, Eugene, Suenaga, Takuya, Suto, Hiroshi, Suzuki, Ryuji, Takahashi, Yasuhiro H., Takami, Michihiro, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Watanabe, Makoto, Wisniewski, John, Yamada, Toru, Takami, Hideki, Usuda, Tomonori, and Tamura, Motohide

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Coronagraphic imagery of the circumstellar disk around HD 169142 in H-band polarized intensity (PI) with Subaru/HiCIAO is presented. The emission scattered by dust particles at the disk surface in 0.2" <= r <= 1.2", or 29 <= r <= 174 AU, is successfully detected. The azimuthally-averaged radial profile of the PI shows a double power-law distribution, in which the PIs in r=29-52 AU and r=81.2-145 AU respectively show r^{-3}-dependence. These two power-law regions are connected smoothly with a transition zone (TZ), exhibiting an apparent gap in r=40-70 AU. The PI in the inner power-law region shows a deep minimum whose location seems to coincide with the point source at \lambda = 7 mm. This can be regarded as another sign of a protoplanet in TZ. The observed radial profile of the PI is reproduced by a minimally flaring disk with an irregular surface density distribution or with an irregular temperature distribution or with the combination of both. The depletion factor of surface density in the inner power-law region (r< 50 AU) is derived to be <= 0.16 from a simple model calculation. The obtained PI image also shows small scale asymmetries in the outer power-law region. Possible origins for these asymmetries include corrugation of the scattering surface in the outer region, and shadowing effect by a puffed up structure in the inner power-law region., Comment: 26 pages, 7 figures, accepted for publication in PASJ

Published
2015
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4. Thirty Meter Telescope Detailed Science Case: 2015

Author

Skidmore, Warren, Dell'Antonio, Ian, Fukugawa, Misato, Goswami, Aruna, Hao, Lei, Jewitt, David, Laughlin, Greg, Steidel, Charles, Hickson, Paul, Simard, Luc, Schöck, Matthias, Treu, Tommaso, Cohen, Judith, Anupama, G. C., Dickinson, Mark, Harrison, Fiona, Kodama, Tadayuki, Lu, Jessica R., Macintosh, Bruce, Malkan, Matt, Mao, Shude, Narita, Norio, Sekiguchi, Tomohiko, Subramaniam, Annapurni, Tanaka, Masaomi, Tian, Feng, A'Hearn, Michael, Akiyama, Masayuki, Ali, Babar, Aoki, Wako, Bagchi, Manjari, Barth, Aaron, Bhalerao, Varun, Bradac, Marusa, Bullock, James, Burgasser, Adam J., Chapman, Scott, Chary, Ranga-Ram, Chiba, Masashi, Cooper, Michael, Cooray, Asantha, Crossfield, Ian, Currie, Thayne, Das, Mousumi, Dewangan, G. C., de Grijs, Richard, Do, Tuan, Dong, Subo, Evslin, Jarah, Fang, Taotao, Fang, Xuan, Fassnacht, Christopher, Fletcher, Leigh, Gaidos, Eric, Gal, Roy, Ghez, Andrea, Giavalisco, Mauro, Grady, Carol A., Greathouse, Thomas, Gogoi, Rupjyoti, Guhathakurta, Puragra, Ho, Luis, Hasan, Priya, Herczeg, Gregory J., Honda, Mitsuhiko, Imanishi, Masa, Inami, Hanae, Iye, Masanori, Kalirai, Jason, Kamath, U. S., Kane, Stephen, Kashikawa, Nobunari, Kasliwal, Mansi, Kasliwal, Vishal, Kirby, Evan, Konopacky, Quinn M., Lepine, Sebastien, Li, Di, Li, Jianyang, Liu, Junjun, Liu, Michael C., Lopez-Rodriguez, Enrigue, Lotz, Jennifer, Lubin, Philip, Macri, Lucas, Maeda, Keiichi, Marchis, Franck, Marois, Christian, Marscher, Alan, Martin, Crystal, Matsuo, Taro, Max, Claire, McConnachie, Alan, McGough, Stacy, Melis, Carl, Meyer, Leo, Mumma, Michael, Muto, Takayuki, Nagao, Tohru, Najita, Joan R., Navarro, Julio, Pierce, Michael, Prochaska, Jason X., Oguri, Masamune, Ojha, Devendra K., Okamoto, Yoshiko K., Orton, Glenn, Otarola, Angel, Ouchi, Masami, Packham, Chris, Padgett, Deborah L., Pandey, Shashi Bhushan, Pilachowsky, Catherine, Pontoppidan, Klaus M., Primack, Joel, Puthiyaveettil, Shalima, Ramirez-Ruiz, Enrico, Reddy, Naveen, Rich, Michael, Richter, Matthew J., Schombert, James, Sen, Anjan Ananda, Shi, Jianrong, Sheth, Kartik, Srianand, R., Tan, Jonathan C., Tanaka, Masayuki, Tanner, Angelle, Tominaga, Nozomu, Tytler, David, U, Vivian, Wang, Lingzhi, Wang, Xiaofeng, Wang, Yiping, Wilson, Gillian, Wright, Shelley, Wu, Chao, Wu, Xufeng, Xu, Renxin, Yamada, Toru, Yang, Bin, Zhao, Gongbo, and Zhao, Hongsheng

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The TMT Detailed Science Case describes the transformational science that the Thirty Meter Telescope will enable. Planned to begin science operations in 2024, TMT will open up opportunities for revolutionary discoveries in essentially every field of astronomy, astrophysics and cosmology, seeing much fainter objects much more clearly than existing telescopes. Per this capability, TMT's science agenda fills all of space and time, from nearby comets and asteroids, to exoplanets, to the most distant galaxies, and all the way back to the very first sources of light in the Universe. More than 150 astronomers from within the TMT partnership and beyond offered input in compiling the new 2015 Detailed Science Case. The contributing astronomers represent the entire TMT partnership, including the California Institute of Technology (Caltech), the Indian Institute of Astrophysics (IIA), the National Astronomical Observatories of the Chinese Academy of Sciences (NAOC), the National Astronomical Observatory of Japan (NAOJ), the University of California, the Association of Canadian Universities for Research in Astronomy (ACURA) and US associate partner, the Association of Universities for Research in Astronomy (AURA)., Comment: 203 pages, 10 Mb. Full resolution version available at http://www.tmt.org/science-case/

Published
2015
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5. Physical Relation of Source I to IRc2 in the Orion KL Region

Author

Okumura, Shin-ichiro, Yamashita, Takuya, Sako, Shigeyuki, Miyata, Takashi, Honda, Mitsuhiko, Kataza, Hirokazu, and Okamoto, Yoshiko K.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

We present mid-infrared narrow-band images of the Orion BN/KL region, and N-band low-resolution spectra of IRc2 and the nearby radio source "I." The distributions of the silicate absorption strength and the color temperature have been revealed with a sub-arcsecond resolution. The detailed structure of the 7.8 micron/12.4 micron color temperature distribution was resolved in the vicinity of IRc2. A mid-infrared counterpart to source I has been detected as a large color temperature peak. The color temperature distribution shows an increasing gradient from IRc2 toward source I, and no dominant temperature peak is seen at IRc2. The spectral energy distribution of IRc2 could be fitted by a two-temperature component model, and the "warmer component" of the infrared emission from IRc2 could be reproduced by scattering of radiation from source I. IRc2 itself is not self-luminous, but is illuminated and heated by an embedded luminous young stellar object located at source I., Comment: 20 pages, 11 figures. Minor corrections had been done in the ver.2. Accepted for publication in PASJ

Published
2011
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6. Direct detection of a flared disk around a young massive star HD200775 and its 10 to 1000AU scale properties

Author

Okamoto, Yoshiko K., Kataza, Hirokazu, Honda, M., Fujiwara, H., Momose, M., Ohashi, N., Fujiyoshi, T., Sakon, I., Sako, S., Yamashita, T., Miyata, T., and Onaka, T.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

We made mid-infrared observations of the 10Msun Herbig Be star HD200775 with the Cooled Mid-Infrared Camera and Spectrometer (COMICS) on the 8.2m Subaru Telescope. We discovered diffuse emission of an elliptical shape extended in the north-south direction inabout 1000AU radius around unresolved excess emission. The diffuse emission is perpendicular to the cavity wall formed by the past outflow activity and is parallel to the projected major axis of the central close binary orbit. The centers of the ellipse contours of the diffuse emission are shifted from the stellar position and the amount of the shift increases as the contour brightness level decreases. The diffuse emission is well explained in all of geometry, size, and configuration by an inclined flared disk where only its surface emits the mid-infrared photons. Our results give the first well-resolved infrared disk images around a massive star and strongly support that HD200775 is formed through the disk accretion. The disk survives the main accretion phase and shows a structure similar to that around lower-mass stars with 'disk atmosphere'. At the same time, the disk also shows properties characteristic to massive stars such as photoevaporation traced by the 3.4mm free-free emission and unusual silicate emission with a peak at 9.2micron, which is shorter than that of many astronomical objects. It provides a good place to compare the disk properties between massive and lower-mass stars., Comment: 18 pages, 8 figures, accepted by The Astrophysical Journal

Published
2009
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7. Si and Fe depletion in Galactic star-forming regions observed by the Spitzer Space Telescope

Author

Okada, Yoko, Onaka, Takashi, Miyata, Takashi, Okamoto, Yoshiko K., Sakon, Itsuki, Shibai, Hiroshi, and Takahashi, Hidenori

Subjects
Astrophysics
Abstract

We report the results of the mid-infrared spectroscopy of 14 Galactic star-forming regions with the high-resolution modules of the Infrared Spectrograph (IRS) on board the Spitzer Space Telescope. We detected [SiII] 35um, [FeII] 26um, and [FeIII] 23um as well as [SIII] 33um and H2 S(0) 28um emission lines. Using the intensity of [NII] 122um or 205um and [OI] 146um or 63um reported by previous observations in four regions, we derived the ionic abundance Si+/N+ and Fe+/N+ in the ionized gas and Si+/O0 and Fe+/O0 in the photodissociation gas. For all the targets, we derived the ionic abundance of Si+/S2+ and Fe2+/S2+ for the ionized gas. Based on photodissociation and HII region models the gas-phase Si and Fe abundance are suggested to be 3-100% and <8% of the solar abundance, respectively, for the ionized gas and 16-100% and 2-22% of the solar abundance, respectively, for the photodissociation region gas. Since the [FeII] 26um and [FeIII] 23um emissions are weak, the high sensitivity of the IRS enables to derive the gas-phase Fe abundance widely in star-forming regions. The derived gas-phase Si abundance is much larger than that in cool interstellar clouds and that of Fe. The present study indicates that 3-100% of Si atoms and <22% of Fe atoms are included in dust grains which are destroyed easily in HII regions, probably by the UV radiation. We discuss possible mechanisms to account for the observed trend; mantles which are photodesorbed by UV photons, organometallic complexes, or small grains., Comment: 43 pages with 7 figures, accepted in Astrophysical Journal

Published
2008
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8. The Asymmetric Thermal Emission of Protoplanetary Disk Surrounding HD 142527 Seen by Subaru/COMICS

Author

Fujiwara, Hideaki, Honda, Mitsuhiko, Kataza, Hirokazu, Yamashita, Takuya, Onaka, Takashi, Fukagawa, Misato, Okamoto, Yoshiko K., Miyata, Takashi, Sako, Shigeyuki, Fujiyoshi, Takuya, and Sakon, Itsuki

Subjects
Astrophysics
Abstract

Mid-infrared (MIR) images of the Herbig Ae star HD 142527 were obtained at 18.8 and 24.5 micron with the Subaru/COMICS. Bright extended arc-like emission (outer disk) is recognized at r=0.85" together with a strong central source (inner disk) and a gap around r=0.6" in the both images. Thermal emission of the eastern side is much brighter than that of the western side in the MIR. We estimate the dust size as a few micron from the observed color of the extended emission and the distance from the star. The dust temperature T and the optical depth tau of the MIR emitting dust are also derived from the two images as T=82+/-1K, tau=0.052+/-0.001 for the eastern side and T=85+/-3K, tau=0.018+/-0.001 for the western side. The observed asymmetry in the brightness can be attributed to the difference in the optical depth of the MIR emitting dust. To account for the present observations, we propose an inclined disk model, in which the outer disk is inclined along the east-west direction with the eastern side being in the far side and the inner rim of the outer disk in the eatern side is exposed directly to us. The proposed model can successfully account for the MIR observations as well as near-infrared (NIR) images of the scattering light, in which the asymmetry is seen in the opposite sense and the forward scattering light (near side -- western side) is brighter., Comment: 5 figures, published in ApJ Letters

Published
2007
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9. Ionization of Polycyclic Aromatic Hydrocarbon Molecules around the Herbig Ae/Be environment

Author

Sakon, Itsuki, Okamoto, Yoshiko K., Kataza, Hirokazu, Onaka, Takashi, Kaneda, Hidehiro, and Honda, Mitsuhiko

Subjects
Astrophysics
Abstract

We present the results of mid-infrared N-band spectroscopy of the Herbig Ae/Be system MWC1080 using the Cooled Mid-Infrared Camera and Spectrometer (COMICS) on board the 8m Subaru Telescope. The MWC1080 has a geometry such that the diffuse nebulous structures surround the central Herbig B0 type star. We focus on the properties of polycyclic aromatic hydrocarbons (PAHs) and PAH-like species, which are thought to be the carriers of the unidentified infrared (UIR) bands in such environments. A series of UIR bands at 8.6, 11.0, 11.2, and 12.7um is detected throughout the system and we find a clear increase in the UIR 11.0um/11.2um ratio in the vicinity of the central star. Since the UIR 11.0um feature is attributed to a solo-CH out-of-plane wagging mode of cationic PAHs while the UIR 11.2um feature to a solo-CH out-of-plane bending mode of neutral PAHs, the large 11.0um/11.2um ratio directly indicates a promotion of the ionization of PAHs near the central star., Comment: accepted for publication in Advances in Geoscience

Published
2007
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10. Crystalline Silicate Feature of the Vega-like star HD145263

Author

Honda, Mitsuhiko, Kataza, Hirokazu, Okamoto, Yoshiko K., Miyata, Takashi, Yamashita, Takuya, Sako, Shigeyuki, Fujiyoshi, Takuya, Ito, Meguru, Okada, Yoko, Sakon, Itsuki, and Onaka, Takashi

Subjects
Astrophysics
Abstract

We have observed the 8-13 $\mu$m spectrum (R$\sim$250) of the Vega-like star candidate HD145263 using Subaru/COMICS. The spectrum of HD145263 shows the broad trapezoidal silicate feature with the shoulders at 9.3 $\mu$m and 11.44 $\mu$m, indicating the presence of crystalline silicate grains. This detection implies that crystalline silicate may also be commonly present around Vega-like stars. The 11.44 $\mu$m feature is slightly shifted to a longer wavelength compared to the usual 11.2-3 $\mu$m crystalline forsterite feature detected toward Herbig Ae/Be stars and T Tauri stars. Although the peak shift due to the effects of the grain size can not be ruled out, we suggest that Fe-bearing crystalline olivine explains the observed peak wavelength fairly well. Fe-bearing silicates are commonly found in meteorites and most interplanetary dust particles, which originate from planetesimal-like asteroids. According to studies of meteorites, Fe-bearing silicate must have been formed in asteroidal planetesimals, supporting the scenario that dust grains around Vega-like stars are of planetesimal origin, if the observed 11.44 $\mu$m peak is due to Fe-bearing silicates., Comment: accepted for Publication in ApJL

Published
2004
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11. Detection of crystalline silicates around the T Tauri star Hen 3-600A

Author

Honda, Mitsuhiko, Kataza, Hirokazu, Okamoto, Yoshiko K., Miyata, Takashi, Yamashita, Takuya, Sako, Shigeyuki, Takubo, Shinya, and Onaka, Takashi

Subjects
Astrophysics
Abstract

We have carried out mid-infrared N-band spectroscopic observations of the T Tauri star Hen 3-600A in the TW Hydra association with the COMICS on the 8.2m Subaru Telescope and found structured features in its spectrum. These structured features are well explained by a combination of crystalline forsterite, crystalline enstatite, silica and glassy olivine grains. Among intermediate-mass young stellar objects (YSOs), crystalline silicates have already been detected, but no firm detection has been reported so far for low-mass YSOs such as T Tauri stars. This is the first clear detection of crystalline silicates in low-mass YSOs and shows that the crystallization event occurs even in the protoplanetary disk of low-mass YSOs in the T Tauri phase. The physical processes leading to the inferred dust composition in the Hen3-600A system may be analogous to those occured in the early epoch of the Solar system., Comment: 13 pages,3 figures,1 table, ApJ Letter accepted

Published
2003
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12. Constraining the Movement of the Spiral Features and the Locations of Planetary Bodies Within the AB Aur System

Author

Lomax, Jamie R, Wisniewski, John P, Grady, Carol A, McElwain, Michael W, Hashimoto, Jun, Kudo, Tomoyuki, Kusakabe, Nobuhiko, Okamoto, Yoshiko K, Fukagawa, Misato, and Abe, Lyu

Subjects
Astrophysics
Abstract

We present a new analysis of multi-epoch, H-band, scattered light images of the AB Aur system. We use a Monte Carlo radiative transfer code to simultaneously model the systems spectral energy distribution (SED) and H-band polarized intensity (PI) imagery. We find that a disk-dominated model, as opposed to one that is envelope dominated, can plausibly reproduce AB Aurs SED and near-IR imagery. This is consistent with previous modeling attempts presented in the literature and supports the idea that at least a subset of AB Aurs spirals originate within the disk. In light of this, we also analyzed the movement of spiral structures in multi-epoch H-band total light and PI imagery of the disk. We detect no significant rotation or change in spatial location of the spiral structures in these data, which span a 5.8-year baseline. If such structures are caused by disk planet interactions, the lack of observed rotation constrains the location of the orbit of planetary perturbers to be 47 au.

Published
2016
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13. The fundamental stellar parameters of FGK stars in the SEEDS survey Norman, OK 73071, USA

Author

Rich, Evan A., Wisniewski, John P., McElwain, Michael W., Okamoto, Yoshiko K., Abe, Lyu, Akiyama, Eiji, Brandner, Wolfgang, Brandt, Timothy D., Cargile, Phillip, Carson, Joseph C., Currie, Thayne M., Egner, Sebastian, Feldt, Markus, Fukagawa, Misato, Grady, Carol A., Guyon, Olivier, Hebb, Leslie, Helminiak, Krzysztof G., Henning, Thomas, Hodapp, Klaus W., Janson, Markus, Knapp, Gillian R., Momose, Munetake, Moro-Martin, Amaya, Oh, Daehyeon, Pyo, Tae-Soo, Schlieder, Joshua, Serabyn, Eugene, Sitko, Michael L., Suenaga, Takuya, Takahashi, Yasuhiro H., Takami, Michihiro, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Hashimoto, Jun, Kudo, Tomoyuki, Kusakabe, Nobuhiko, Goto, Miwa, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko S., Ishii, Miki, Iye, Masanori, Kandori, Ryo, Kuzuhara, Masayuki, Kwon, Jungmi, Matsuo, Taro, Mayama, Satoshi, Miyama, Shoken, Morino, Jun-Ichi, Nakagawa, Takao, Nishimura, Tetsuo, Suto, Hiroshi, Suzuki, Ryuji, Takato, Naruhisa, Terada, Hiroshi, Watanabe, Makoto, Yamada, Toru, Takami, Hideki, Usuda, Tomonori, and Tamura, Motohide

Subjects
Physics, 010504 meteorology & atmospheric sciences, stars: abundances, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Planetary system, 01 natural sciences, Exoplanet, Spectral line, law.invention, Telescope, Stars, Space and Planetary Science, Observatory, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, stars: fundamental parameters, 010303 astronomy & astrophysics, planetary systems, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Line (formation)
Abstract

著者人数: 62名, Accepted: 2017-08-08, 資料番号: SA1170166000

Published
2017

14. No high-mass protostars in the silhouette young stellar object M17-SO1

Author

Sako, Shigeyuki, Yamashita, Takuya, Kataza, Hirokazu, Miyata, Takashi, Okamoto, Yoshiko K., Honda, Mitsuhiko, Fujiyoshi, Takuya, Terada, Hiroshi, Kamazaki, Takeshi, Jiang, Zhibo, Hanawa, Tomoyuki, and Onaka, Takashi

Subjects
Environmental issues, Science and technology, Zoology and wildlife conservation
Abstract

Author(s): Shigeyuki Sako (corresponding author) [1, 2, 3]; Takuya Yamashita [1, 2]; Hirokazu Kataza [4]; Takashi Miyata [3]; Yoshiko K. Okamoto [5]; Mitsuhiko Honda [1, 2, 4]; Takuya Fujiyoshi [2]; [...]

Published
2005
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17. The fundamental stellar parameters of FGK stars in the SEEDS survey Norman, OK 73071, USA

Author

Rich, Evan A., Wisniewski, John P., McElwain, Michael W., Hashimoto, Jun, Kudo, Tomoyuki, Kusakabe, Nobuhiko, Okamoto, Yoshiko K., Abe, Lyu, Akiyama, Eiji, Brandner, Wolfgang, Brandt, Timothy D., Cargile, Phillip, Carson, Joseph C., Currie, Thayne M., Egner, Sebastian, Feldt, Markus, Fukagawa, Misato, Goto, Miwa, Grady, Carol A., Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko S., Hebb, Leslie, Helminiak, Krzysztof G., Henning, Thomas, Hodapp, Klaus W., Ishii, Miki, Iye, Masanori, Janson, Markus, Kandori, Ryo, Knapp, Gillian R., Kuzuhara, Masayuki, Kwon, Jungmi, Matsuo, Taro, Mayama, Satoshi, Miyama, Shoken, Momose, Munetake, Morino, Jun-Ichi, Moro-Martin, Amaya, Nakagawa, Takao, Nishimura, Tetsuo, Oh, Daehyeon, Pyo, Tae-Soo, Schlieder, Joshua, Serabyn, Eugene, Sitko, Michael L., Suenaga, Takuya, Suto, Hiroshi, Suzuki, Ryuji, Takahashi, Yasuhiro H., Takami, Michihiro, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Watanabe, Makoto, Yamada, Toru, Takami, Hideki, Usuda, Tomonori, Tamura, Motohide, 橋本, 淳, 工藤, 智幸, 日下部, 展彦, 後藤, 美和, 早野, 裕, 林, 正彦, 林, 左絵子, 石井, 未来, 家, 正則, 神鳥, 亮, 葛原, 昌幸, 權, 靜美, 松尾, 太郎, 真山, 聡, 観山, 正見, 森野, 潤一, 中川, 貴雄, 西村, 徹朗, 周藤, 浩士, 鈴木, 竜二, 高遠, 徳尚, 寺田, 宏, 渡辺, 誠, 山田, 亨, 高見, 英樹, 臼田, 知史, 田村, 元秀, Rich, Evan A., Wisniewski, John P., McElwain, Michael W., Hashimoto, Jun, Kudo, Tomoyuki, Kusakabe, Nobuhiko, Okamoto, Yoshiko K., Abe, Lyu, Akiyama, Eiji, Brandner, Wolfgang, Brandt, Timothy D., Cargile, Phillip, Carson, Joseph C., Currie, Thayne M., Egner, Sebastian, Feldt, Markus, Fukagawa, Misato, Goto, Miwa, Grady, Carol A., Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko S., Hebb, Leslie, Helminiak, Krzysztof G., Henning, Thomas, Hodapp, Klaus W., Ishii, Miki, Iye, Masanori, Janson, Markus, Kandori, Ryo, Knapp, Gillian R., Kuzuhara, Masayuki, Kwon, Jungmi, Matsuo, Taro, Mayama, Satoshi, Miyama, Shoken, Momose, Munetake, Morino, Jun-Ichi, Moro-Martin, Amaya, Nakagawa, Takao, Nishimura, Tetsuo, Oh, Daehyeon, Pyo, Tae-Soo, Schlieder, Joshua, Serabyn, Eugene, Sitko, Michael L., Suenaga, Takuya, Suto, Hiroshi, Suzuki, Ryuji, Takahashi, Yasuhiro H., Takami, Michihiro, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Watanabe, Makoto, Yamada, Toru, Takami, Hideki, Usuda, Tomonori, Tamura, Motohide, 橋本, 淳, 工藤, 智幸, 日下部, 展彦, 後藤, 美和, 早野, 裕, 林, 正彦, 林, 左絵子, 石井, 未来, 家, 正則, 神鳥, 亮, 葛原, 昌幸, 權, 靜美, 松尾, 太郎, 真山, 聡, 観山, 正見, 森野, 潤一, 中川, 貴雄, 西村, 徹朗, 周藤, 浩士, 鈴木, 竜二, 高遠, 徳尚, 寺田, 宏, 渡辺, 誠, 山田, 亨, 高見, 英樹, 臼田, 知史, and 田村, 元秀

Abstract

著者人数: 62名, Accepted: 2017-08-08

Published
2018

18. Resolved 24.5 micron emission from massive young stellar objects

Author

De, Wit W. J., Hoare, M. G., Oudmaijer, R. D., Fujiyoshi, Takuya, Honda, Mitsuhiko, Kataza, Hirokazu, Miyata, Takashi, Okamoto, Yoshiko K., Onaka, Takashi, Sako, Shigeyuki, and Yamashita, Takuya

Subjects
Physics, stars: formation, Star formation, Young stellar object, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Scale (descriptive set theory), Astrophysics, stars: early-type, ISM: clouds, Flattening, stars: imaging, Space and Planetary Science, Radiative transfer, Angular resolution, infrared: stars, Envelope (waves)
Abstract

Massive young stellar objects (MYSO) are surrounded by massive dusty envelopes. Our aim is to establish their density structure on scales of ~1000 AU, i.e. a factor 10 increase in angular resolution compared to similar studies performed in the (sub)mm. We have obtained diffraction-limited (0.6") 24.5 micron images of 14 well-known massive star formation regions with Subaru/COMICS. The images reveal the presence of discrete MYSO sources which are resolved on arcsecond scales. For many sources, radiative transfer models are capable of satisfactorily reproducing the observations. They are described by density powerlaw distributions (n(r) ~ r^(-p)) with p = 1.0 +/-0.25. Such distributions are shallower than those found on larger scales probed with single-dish (sub)mm studies. Other sources have density laws that are shallower/steeper than p = 1.0 and there is evidence that these MYSOs are viewed near edge-on or near face-on, respectively. The images also reveal a diffuse component tracing somewhat larger scale structures, particularly visible in the regions S140, AFGL 2136, IRAS 20126+4104, Mon R2, and Cep A. We thus find a flattening of the MYSO envelope density law going from ~10 000 AU down to scales of ~1000 AU. We propose that this may be evidence of rotational support of the envelope (abridged)., Comment: 21 pages, accepted for A&A

Published
2009

19. A Red Supergiant Nebula at 25 μm: Arcsecond-Scale Mass-Loss Asymmetries of μ Cephei

Author

de, Wit W. J., Oudmaijer, R. D., Hoare, M. G., Fujiyoshi, Takuya, Honda, Mitsuhiko, Kataza, Hirokazu, Miyata, Takashi, Okamoto, Yoshiko K., Onaka, Takashi, Sako, Shigeyuki, and Yamashita, Takuya

Subjects
Physics, Nebula, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, stars: individual (μ Cephei), supergiants, Astrophysics::Cosmology and Extragalactic Astrophysics, Radius, Astrophysics, Wavelength, Supernova, Stars, Space and Planetary Science, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, Spectral energy distribution, Red supergiant, Astrophysics::Earth and Planetary Astrophysics, stars: evolution, stars: mass loss, Astrophysics::Galaxy Astrophysics
Abstract

We present diffraction limited (0.6") 24.5micron Subaru/COMICS images of the red supergiant mu Cep. We report the detection of a circumstellar nebula, that was not detected at shorter wavelengths. It extends to a radius of at least 6" in the thermal infrared. On these angular scales, the nebula is roughly spherical, in contrast, it displays a pronounced asymmetric morphology closer in. We simultaneously model the azimuthally averaged intensity profile of the nebula and the observed spectral energy distribution using spherical dust radiative transfer models. The models indicate a constant mass-loss process over the past 1000 years, for mass-loss rates a few times 10^(-7) Msun/yr. This work supports the idea that at least part of the asymmetries in shells of evolved massive stars and supernovae may be due to the mass-loss process in the red supergiant phase.

Published
2008

20. Mid-Infrared Observations of Planetary Nebula BD +30 3639: Evolution and Distribution of Unidentified IR Band Carriers*

Author

Matsumoto, Hiroko, Sakon, Itsuki, Onaka, Takashi, Sako, Shigeyuki, Miyata, Takashi, Kataza, Hirokazu, Okada, Yoko, Okamoto, Yoshiko K., Honda, Mitsuhiko, Yamashita, Takuya, Takahashi, Hidenori, and Fujiyoshi, Takuya

Subjects
infrared: ISM, planetary nebulae: general, dust, extinction, infrared: stars, planetary nebulae: individual (BD +30 3639)
Abstract

資料番号: PAIS08059000

Published
2008

22. Detailed structure of the outer disk around HD169142 with polarized light in H-band

Author

Momose, Munetake, Morita, Ayaka, Fukagawa, Misato, Muto, Takayuki, Takeuchi, Taku, Hashimoto, Jun, Honda, Mitsuhiko, Kudo, Tomoyuki, Okamoto, Yoshiko K., Kanagawa, Kazuhiro D., Tanaka, Hidekazu, Grady, Carol A., Sitko, Michael L., Akiyama, Eiji, Currie, Thayne, Follette, Katherine B., Mayama, Satoshi, Kusakabe, Nobuhiko, Abe, Lyu, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph C., Egner, Sebastian, Feldt, Markus, Goto, Miwa, Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko S., Henning, Thomas, Hodapp, Klaus W., Ishii, Miki, Iye, Masanori, Janson, Markus, Kandori, Ryo, Knapp, Gillian R., Kuzuhara, Masayuki, Kwon, Jungmi, Matsuo, Taro, McElwain, Michael W., Miyama, Shoken, Morino, Jun-Ichi, Moro-Martin, Amaya, Nishimura, Tetsuo, Pyo, Tae-Soo, Serabyn, Eugene, Suenaga, Takuya, Suto, Hiroshi, Suzuki, Ryuji, Takahashi, Yasuhiro H., Takami, Michihiro, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Watanabe, Makoto, Wisniewski, John, Yamada, Toru, Takami, Hideki, Usuda, Tomonori, Tamura, Motohide, Momose, Munetake, Morita, Ayaka, Fukagawa, Misato, Muto, Takayuki, Takeuchi, Taku, Hashimoto, Jun, Honda, Mitsuhiko, Kudo, Tomoyuki, Okamoto, Yoshiko K., Kanagawa, Kazuhiro D., Tanaka, Hidekazu, Grady, Carol A., Sitko, Michael L., Akiyama, Eiji, Currie, Thayne, Follette, Katherine B., Mayama, Satoshi, Kusakabe, Nobuhiko, Abe, Lyu, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph C., Egner, Sebastian, Feldt, Markus, Goto, Miwa, Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko S., Henning, Thomas, Hodapp, Klaus W., Ishii, Miki, Iye, Masanori, Janson, Markus, Kandori, Ryo, Knapp, Gillian R., Kuzuhara, Masayuki, Kwon, Jungmi, Matsuo, Taro, McElwain, Michael W., Miyama, Shoken, Morino, Jun-Ichi, Moro-Martin, Amaya, Nishimura, Tetsuo, Pyo, Tae-Soo, Serabyn, Eugene, Suenaga, Takuya, Suto, Hiroshi, Suzuki, Ryuji, Takahashi, Yasuhiro H., Takami, Michihiro, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Watanabe, Makoto, Wisniewski, John, Yamada, Toru, Takami, Hideki, Usuda, Tomonori, and Tamura, Motohide

Abstract

Coronagraphic imagery of the circumstellar disk around HD 169142 in H-band polarized intensity (PI) with Subaru/HiCIAO is presented. The emission scattered by dust particles at the disk surface in 0.2 <= r <= 1.2, or 29 <= r <= 174 AU, is successfully detected. The azimuthally-averaged radial profile of the PI shows a double power-law distribution, in which the PIs in r=29-52 AU and r=81.2-145 AU respectively show r(-3)-dependence. These two power-law regions are connected smoothly with a transition zone (TZ), exhibiting an apparent gap in r=40-70 AU. The PI in the inner power-law region shows a deep minimum whose location seems to coincide with the point source at lambda = 7 mm. This can be regarded as another sign of a protoplanet in TZ. The observed radial profile of the PI is reproduced by a minimally flaring disk with an irregular surface density distribution or with an irregular temperature distribution or with the combination of both. The depletion factor of surface density in the inner power-law region (r<50 AU) is derived to be >= 0.16 from a simple model calculation. The obtained PI image also shows small scale asymmetries in the outer power-law region. Possible origins for these asymmetries include corrugation of the scattering surface in the outer region, and shadowing effect by a puffed up structure in the inner power-law region.

Published
2015
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23. Detailed structure of the outer disk around HD 169142 with polarized light inH-band

Author

Momose, Munetake, primary, Morita, Ayaka, additional, Fukagawa, Misato, additional, Muto, Takayuki, additional, Takeuchi, Taku, additional, Hashimoto, Jun, additional, Honda, Mitsuhiko, additional, Kudo, Tomoyuki, additional, Okamoto, Yoshiko K., additional, Kanagawa, Kazuhiro D., additional, Tanaka, Hidekazu, additional, Grady, Carol A., additional, Sitko, Michael L., additional, Akiyama, Eiji, additional, Currie, Thayne, additional, Follette, Katherine B., additional, Mayama, Satoshi, additional, Kusakabe, Nobuhiko, additional, Abe, Lyu, additional, Brandner, Wolfgang, additional, Brandt, Timothy D., additional, Carson, Joseph C., additional, Egner, Sebastian, additional, Feldt, Markus, additional, Goto, Miwa, additional, Guyon, Olivier, additional, Hayano, Yutaka, additional, Hayashi, Masahiko, additional, Hayashi, Saeko S., additional, Henning, Thomas, additional, Hodapp, Klaus W., additional, Ishii, Miki, additional, Iye, Masanori, additional, Janson, Markus, additional, Kandori, Ryo, additional, Knapp, Gillian R., additional, Kuzuhara, Masayuki, additional, Kwon, Jungmi, additional, Matsuo, Taro, additional, McElwain, Michael W., additional, Miyama, Shoken, additional, Morino, Jun-Ichi, additional, Moro-Martin, Amaya, additional, Nishimura, Tetsuo, additional, Pyo, Tae-Soo, additional, Serabyn, Eugene, additional, Suenaga, Takuya, additional, Suto, Hiroshi, additional, Suzuki, Ryuji, additional, Takahashi, Yasuhiro H., additional, Takami, Michihiro, additional, Takato, Naruhisa, additional, Terada, Hiroshi, additional, Thalmann, Christian, additional, Tomono, Daigo, additional, Turner, Edwin L., additional, Watanabe, Makoto, additional, Wisniewski, John, additional, Yamada, Toru, additional, Takami, Hideki, additional, Usuda, Tomonori, additional, and Tamura, Motohide, additional

Published
2015
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24. 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

26. A trial production of the image slicer unit for next generation infrared instruments and the assembly of the evaluation system of the pseudo slit image quality

Author

Sakon, Itsuki, additional, Onaka, Takashi, additional, Kataza, Hirokazu, additional, Okamoto, Yoshiko K., additional, Honda, Mitsuhiko, additional, Tokoro, Hitoshi, additional, Fujishiro, Naofumi, additional, Ikeda, Yuji, additional, Nakagawa, Hiroyuki, additional, Kirino, Okiharu, additional, Mitsui, Kenji, additional, and Okada, Norio, additional

Published
2014
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28. Mid-infrared Imaging of the Transitional Disk of HD 169142: Measuring the Size of the Gap

Author

Maaskant, Koen, Waters, L. B. F. M., Dominik, C., Tielens, A. G. G. M., Mulders, G. D., Min, M., Honda, Mitsuhiko, Okamoto, Yoshiko K., Kataza, Hirokazu, Fukagawa, Misato, Yamashita, Takuya, Fujiyoshi, Takuya, Miyata, Takashi, Sako, Shigeyuki, Sakon, Itsuki, Fujiwara, Hideaki, Onaka, Takashi, and Low Energy Astrophysics (API, FNWI)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Star (graph theory), Astrophysics - Astrophysics of Galaxies, law.invention, Atmospheric radiative transfer codes, Space and Planetary Science, law, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, Hydrostatic equilibrium, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

著者人数: 17名, Accepted: 2012-04-17, 資料番号: SA1004161000

Published
2012

29. Diffuse 18 $\mu$m Emission around TYC 3159-6-1 Discovered by the AKARI MIR All-Sky Survey

Author

Takita, Satoshi, primary, Kitamura, Yoshimi, additional, Kataza, Hirokazu, additional, Ishihara, Daisuke, additional, Ueno, Munetaka, additional, Fujiwara, Hideaki, additional, Ikeda, Norio, additional, Kawamura, Akiko, additional, Murakami, Hiroshi, additional, Okamoto, Yoshiko K., additional, Onaka, Takashi, additional, Oyabu, Shinki, additional, Sakon, Itsuki, additional, and Takahashi, Hidenori, additional

Published
2009
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31. Detailed structure of the outer disk around HD169142 with polarized light in H-band.

Author

Munetake MOMOSE, Ayaka MORITA, Misato FUKAGAWA, Takayuki MUTO, Taku TAKEUCHI, Jun HASHIMOTO, Mitsuhiko HONDA, Tomoyuki KUDO, OKAMOTO, Yoshiko K., KANAGAWA, Kazuhiro D., Hidekazu TANAKA, GRADY, Carol A., SITKO, Michael L., Eiji AKIYAMA, Thayne CURRIE, FOLLETTE, Katherine B., MAYAMA, Satoshi, Nobuhiko KUSAKABE, Lyu ABE, and BRANDNER, Wolfgang

Subjects
CIRCUMSTELLAR matter, SCATTERING (Physics), PROTOPLANETARY disks, PROTO-planetary nebulae, ASTRONOMICAL research
Abstract

Coronagraphic imagery of the circumstellar disk around HD169142 in H-band polarized intensity (PI) with Subaru/HiCIAO is presented. The emission scattered by dust particles at the disk surface in 0".2 ≤ r ≤ 1".2, or 29 ≤ r ≤ 174 au, is successfully detected. The azimuthally averaged radial profile of the PI shows a double power-law distribution, in which the PIs in r=29-52 au and r=81.2-145 au respectively show r-3 dependence. These two power-law regions are connected smoothly with a transition zone (TZ), exhibiting an apparent gap in r = 40-70 au. The PI in the inner power-law region shows a deep minimum whose location seems to coincide with the point source at λ = 7mm. This can be regarded as another sign of a protoplanet in the TZ. The observed radial profile of the PI is reproduced by aminimally flaring disk with an irregular surface density distribution, an irregular temperature distribution, or with a combination of both. The depletion factor of surface density in the inner power-law region (r < 50 au) is derived to be ≥0.16 from a simple model calculation. The obtained PI image also shows small-scale asymmetries in the outer power-law region. Possible origins for these asymmetries include corrugation of the scattering surface in the outer region, and a shadowing effect by a puffed-up structure in the inner power-law region. [ABSTRACT FROM AUTHOR]

Published
2015
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34. Ground-based Mid-Infrared Spectroscopy of Faint Standard Stars in the North Ecliptic Polar Region for theASTRO-FInfrared Camera

Author

Ishihara, Daisuke, primary, Onaka, Takashi, additional, Kataza, Hirokazu, additional, Miyata, Takashi, additional, Okamoto, Yoshiko K., additional, Yamashita, Takuya, additional, Sako, Sigeyuki, additional, Honda, Mitsuhiko, additional, Okada, Yoko, additional, Fujiyoshi, Takuya, additional, and Cohen, Martin, additional

Published
2006
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36. Crystalline Silicate Feature of the Vega-like Star HD 145263

Author

Honda, Mitsuhiko, primary, Kataza, Hirokazu, additional, Okamoto, Yoshiko K., additional, Miyata, Takashi, additional, Yamashita, Takuya, additional, Sako, Shigeyuki, additional, Fujiyoshi, Takuya, additional, Ito, Meguru, additional, Okada, Yoko, additional, Sakon, Itsuki, additional, and Onaka, Takashi, additional

Published
2004
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37. The 10 Micron Spectra of Comet C/2002 V1 (NEAT) and C/2001 RX14 (LINEAR)

Author

Honda, Mitsuhiko, primary, Watanabe, Jun‐ichi, additional, Yamashita, Takuya, additional, Kataza, Hirokazu, additional, Okamoto, Yoshiko K., additional, Miyata, Takashi, additional, Sako, Shigeyuki, additional, Fujiyoshi, Takuya, additional, Kawakita, Hideyo, additional, Furusho, Reiko, additional, Kinoshita, Daisuke, additional, Sekiguchi, Tomohiko, additional, Ootsubo, Takafumi, additional, and Onaka, Takashi, additional

Published
2004
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39. Developing new data acquisition devices for COMICS

Author

Sako, Shigeyuki, primary, Kataza, Hirokazu, additional, Miyata, Takashi, additional, Okamoto, Yoshiko K., additional, Takubo, Shinya, additional, Honda, Mitsuhiko, additional, Onaka, Takashi, additional, and Yamashita, Takuya, additional

Published
2003
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47. K3-50A: An Ultracompact H II Region Ionized by a Massive Stellar Cluster

Author

Okamoto, Yoshiko K., Kataza, Hirokazu, Yamashita, Takuya, Miyata, Takashi, Sako, Shigeyuki, Takubo, Shinya, Honda, Mitsuhiko, and Onaka, Takashi

Abstract

We have made imaging and spectroscopic observations of the ultracompact H II region K3-50A with a spatial resolution of 0.''4 using a new mid-infrared instrument, the Cooled Mid-Infrared Camera and Spectrometer, on the 8.2 m Subaru Telescope. The spectra show thermal dust emission, 9.7 mm silicate absorption, and fine-structure line emissions of [Ne II] at 12.8 mm, [Ar III] at 8.99 mm, and [S IV] at 10.51 mm. From the maps of the continuum, line emissions, and/or derived dust parameters, we identify eight mid-infrared sources in K3-50A. Especially the central [Ne II] emission has been resolved into two peaks clearly. The ionization condition is investigated with the line flux ratios I([Ar III])/I([Ne II]) and I([S IV])/I([Ne II]). It is suggested that the spectral types of the ionizing stars in K3-50A correspond to B0-O8 V, which is much later than O5.5 V, the type estimated from radio continuum observations under a single-star assumption. The three line fluxes suggest a number of Ne+ ions greater than what is ionized by a single star of any spectral type, but the numbers of Ar2+ and S3+ are similar to that formed by a single O8-O9 V star and that by a single O7-O9 V star, respectively. From these features as well as the dust temperature and the correspondence of each identified source with the near-infrared source, we propose that K3-50A is excited by at least two (possibly three) ionizing stars. This is the first convincing example that a massive stellar cluster is ionizing an ultracompact H II region.

Published
2003

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