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1. Radial decoupling of small and large dust grains in the transitional disk RX J1615.3-3255

Author

Kooistra, Robin, Kamp, Inga, Fukagawa, Misato, Ménard, Francois, Momose, Munetake, Tsukagoshi, Takashi, Kudo, Tomoyuki, Kusakabe, Nobuhiko, Hashimoto, Jun, Abe, Lyu, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph C., Egner, Sebastian E., Feldt, Markus, Goto, Miwa, Grady, Carol A., 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, Currie, Thayne, Akiyama, Eiji, Mayama, Satoshi, Follette, Katherine B., and Nakagawa, Takao

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We present H-band (1.6 {\mu}m) scattered light observations of the transitional disk RX J1615.3-3255, located in the ~1 Myr old Lupus association. From a polarized intensity image, taken with the HiCIAO instrument of the Subaru Telescope, we deduce the position angle and the inclination angle of the disk. The disk is found to extend out to 68 $\pm$ 12 AU in scattered light and no clear structure is observed. Our inner working angle of 24 AU does not allow us to detect a central decrease in intensity similar to that seen at 30 AU in the 880 {\mu}m continuum observations. We compare the observations with multiple disk models based on the Spectral Energy Distribution (SED) and submm interferometry and find that an inner rim of the outer disk at 30 AU containing small silicate grains produces a polarized intensity signal which is an order of magnitude larger than observed. We show that a model in which the small dust grains extend smoothly into the cavity found for large grains is closer to the actual H-band observations. A comparison of models with different dust size distributions suggests that the dust in the disk might have undergone significant processing compared to the interstellar medium., Comment: 8 pages, 7 figures, 4 tables. Accepted for publication in A&A

Published
2016
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2. Extreme Asymmetry in the Disk of V1247 Ori

Author

Ohta, Yurina, Fukagawa, Misato, Sitko, Michael L., Muto, Takayuki, Kraus, Stefan, Grady, Carol A., Wisniewski, John P., Swearingen, Jeremy R., Shibai, Hiroshi, Sumi, Takahiro, Hashimoto, Jun, Kudo, Tomoyuki, Kusakabe, Nobuhiko, Momose, Munetake, Okamoto, Yoshiko, Kotani, Takayuki, Takami, Michihiro, Currie, Thayne, Thalmann, Christian, Janson, Markus, Akiyama, Eiji, Follette, Katherine B., Mayama, Satoshi, Abe, Lyu, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph C., Egner, Sebastian E., Feldt, Markus, Goto, Miwa, Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko S., Henning, Thomas, Hodapp, Klaus W., Ishii, Miki, Iye, Masanori, 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, Hideki, Takato, Naruhisa, Terada, Hiroshi, Tomono, Daigo, Turner, Edwin L., Usuda, Tomonori, Watanabe, Makoto, Yamada, Toru, and Tamura, Motohide

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

We present the first near-infrared scattered-light detection of the transitional disk around V1247 Ori, which was obtained using high-resolution polarimetric differential imaging observations with Subaru/HiCIAO. Our imaging in the H band reveals the disk morphology at separations of ~0.14"-0.86" (54-330 au) from the central star. The polarized intensity (PI) image shows a remarkable arc-like structure toward the southeast of the star, whereas the fainter northwest region does not exhibit any notable features. The shape of the arm is consistent with an arc of 0.28" $\pm$ 0.09" in radius (108 au from the star), although the possibility of a spiral arm with a small pitch angle cannot be excluded. V1247 Ori features an exceptionally large azimuthal contrast in scattered, polarized light; the radial peak of the southeastern arc is about three times brighter than the northwestern disk measured at the same distance from the star. Combined with the previous indication of an inhomogeneous density distribution in the gap at $\lesssim$46 au, the notable asymmetry in the outer disk suggests the presence of unseen companions and/or planet-forming processes ongoing in the arc., Comment: 21 pages, 5 figures, accepted for publication in PASJ

Published
2016
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3. Near-IR High-Resolution Imaging Polarimetry of the SU Aur Disk: Clues for Tidal Tails?

Author

de Leon, Jerome, Takami, Michihiro, Karr, Jennifer L., Hashimoto, Jun, Kudo, Tomoyuki, Sitko, Michael, Mayama, Satoshi, Kusakabe, Nobuyuki, Akiyama, Eiji, Liu, Hauyu Baobab, Usuda, Tomonori, Abe, Lyu, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph, Currie, Thayne, Egner, Sebastian E., Feldt, Markus, Follette, Katherine, Grady, Carol A., Goto, Miwa, Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko, 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, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Watanabe, Makoto, Wisniewski, John P., Yamada, Toru, Takami, Hideki, and Tamura, Motohide

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

We present new high-resolution ($\sim$0\farcs09) $H$-band imaging observations of the circumstellar disk around the T Tauri star SU Aur. Our observations with Subaru-HiCIAO have revealed the presence of scattered light as close as 0\farcs15 ($\sim$20 AU) to the star. Within our image, we identify bright emission associated with a disk with a minimum radius of $\sim$90 AU, an inclination of $\sim$35\degr from the plane of the sky, and an approximate P.A. of 15\degr for the major axis. We find a brightness asymmetry between the northern and southern sides of the disk due to a non-axisymmetric disk structure. We also identify a pair of asymmetric tail structures extending east and west from the disk. The western tail extends at least 2\farcs5 (350 AU) from the star, and is probably associated with a reflection nebula previously observed at optical and near-IR wavelengths. The eastern tail extends at least 1\arcsec (140 AU) at the present signal-to-noise. These tails are likely due to an encounter with an unseen brown dwarf, but our results do not exclude the explanation that these tails are outflow cavities or jets., Comment: 12 pages, 3 figures, accepted by ApJ

Published
2015
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4. SEEDS Adaptive Optics Imaging of the Asymmetric Transition Disk Oph IRS 48 in Scattered Light

Author

Follette, Katherine B., Grady, Carol A., Swearingen, Jeremy R., Sitko, Michael L., Champney, Elizabeth H., van der Marel, Nienke, Takami, Michihiro, Kuchner, Marc J., Close, Laird M., Muto, Takayuki, Mayama, Satoshi, McElwain, Michael W., Fukagawa, Misato, Maaskant, Koen, Min, Michiel, Russell, Ray W., Kudo, Tomoyuki, Kusakabe, Nobuhiko, Hashimoto, Jun, Abe, Lyu, Akiyama, Eiji, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph, Currie, Thayne, Egner, Sebastian E., Feldt, Markus, Goto, Miwa, Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko, Henning, Thomas, Hodapp, Klaus, Ishii, Miki, Iye, Masanori, Janson, Markus, Kandori, Ryo, Knapp, Gillian R., Kuzuhara, Masayuki, Kwon, Jungmi, Matsuo, Taro, Miyama, Shoken, Morino, Jun-Ichi, Moro-Martin, Amaya, Nishimura, Tetsuo, Pyo, Tae-Soo, Serabyn, Eugene, Suenaga, Takuya, Suto, Hiroshi, Suzuki, Ryuji, Takahashi, Yasuhiro, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Watanabe, Makoto, Wisniewski, John P., Yamada, Toru, Takami, Hideki, Usuda, Tomonori, and Tamura, Motohide

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

We present the first resolved near infrared imagery of the transition disk Oph IRS 48 (WLY 2-48), which was recently observed with ALMA to have a strongly asymmetric sub-millimeter flux distribution. H-band polarized intensity images show a $\sim$60AU radius scattered light cavity with two pronounced arcs of emission, one from Northeast to Southeast and one smaller, fainter and more distant arc in the Northwest. K-band scattered light imagery reveals a similar morphology, but with a clear third arc along the Southwestern rim of the disk cavity. This arc meets the Northwestern arc at nearly a right angle, revealing the presence of a spiral arm or local surface brightness deficit in the disk, and explaining the East-West brightness asymmetry in the H-band data. We also present 0.8-5.4$\mu$m IRTF SpeX spectra of this object, which allow us to constrain the spectral class to A0$\pm$1 and measure a low mass accretion rate of 10$^{-8.5}$M$_{\odot}$/yr, both consistent with previous estimates. We investigate a variety of reddening laws in order to fit the mutliwavelength SED of Oph IRS 48 and find a best fit consistent with a younger, higher luminosity star than previous estimates., Comment: Accepted by ApJ. 19 pages, 15 figures

Published
2014
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5. Indications of M-dwarf Deficits in the Halo and Thick Disk of the Galaxy

Author

Konishi, Mihoko, Shibai, Hiroshi, Sumi, Takahiro, Fukagawa, Misato, Matsuo, Taro, Samland, Matthias S., Yamamoto, Kodai, Sudo, Jun, Itoh, Yoichi, Arimoto, Nobuo, Kajisawa, Masaru, Abe, Lyu, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph, Currie, Thayne, Egner, Sebastian E., Feldt, Markus, Goto, Miwa, Grady, Carol A., Guyon, Olivier, Hashimoto, Jun, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko S., Henning, Thomas, Hodapp, Klaus W., Ishii, Miki, Iye, Masanori, Janson, Markus, Kandori, Ryo, Knapp, Gillian R., Kudo, Tomoyuki, Kusakabe, Nobuhiko, Kuzuhara, Masayuki, Kwon, Jungmi, McElwain, Michael W., Miyama, Shoken, Morino, Jun-Ichi, Moro-Martín, Amaya, Nishimura, Tetsuo, Pyo, Tae-Soo, Serabyn, Eugene, Suenaga, Takuya, Suto, Hiroshi, Suzuki, Ryuji, Takahashi, Yasuhiro H., Takami, Hideki, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Usuda, Tomonori, Watanabe, Makoto, Wisniewski, John P., Yamada, Toru, and Tamura, Motohide

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

We compared the number of faint stars detected in deep survey fields with the current stellar distribution model of the Galaxy and found that the detected number in the H band is significantly smaller than the predicted number. This indicates that M-dwarfs, the major component, are fewer in the halo and the thick disk. We used archived data of several surveys in both the north and south field of GOODS (Great Observatories Origins Deep Survey), MODS in GOODS-N, and ERS and CANDELS in GOODS-S. The number density of M-dwarfs in the halo has to be 20+/-13% relative to that in the solar vicinity, in order for the detected number of stars fainter than 20.5 mag in the H band to match with the predicted value from the model. In the thick disk, the number density of M-dwarfs must be reduced (52+/-13%) or the scale height must be decreased (~600 pc). Alternatively, overall fractions of the halo and thick disks can be significantly reduced to achieve the same effect, because our sample mainly consists of faint M-dwarfs. Our results imply that the M-dwarf population in regions distant from the Galactic plane is significantly smaller than previously thought. We then discussed the implications this has on the suitability of the model predictions for the prediction of non-companion faint stars in direct imaging extrasolar planet surveys by using the best-fit number densities., Comment: 22 pages, 9 figures, accepted for Publications of the Astronomical Society of Japan

Published
2014
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6. Surface Geometry of Protoplanetary Disks Inferred From Near-Infrared Imaging Polarimetry

Author

Takami, Michihiro, Hasegawa, Yasuhiro, Muto, Takayuki, Gu, Pin-Gao, Dong, Ruobing, Karr, Jennifer L., Hashimoto, Jun, Kusakabe, Nobuyuki, Chapillon, Edwige, Tang, Ya-Wen, Itoh, Youchi, Carson, Joseph, Follette, Katherine B., Mayama, Satoshi, Sitko, Michael, Janson, Markus, Grady, Carol A., Kudo, Tomoyuki, Akiyama, Eiji, Kwon, Jungmi, Takahashi, Yasuhiro, Suenaga, Takuya, Abe, Lyu, Brandner, Wolfgang, Brandt, Timothy D., Currie, Thayne, Egner, Sebastian E., Feldt, Markus, Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko, Henning, Thomas, Hodapp, Klaus W., Honda, Mitsuhiko, Ishii, Miki, Iye, Masanori, Kandori, Ryo, Knapp, Gillian R., Kuzuhara, Masayuki, McElwain, Michael W., Matsuo, Taro, Miyama, Shoken, Morino, Jun-Ichi, Moro-Martin, Amaya, Nishimura, Tetsuo, Pyo, Tae-Soo, Serabyn, Eugene, Suto, Hiroshi, Suzuki, Ryuji, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Wisniewski, John P., Watanabe, Makoto, Yamada, Toru, Takami, Hideki, Usuda, Tomonori, and Tamura, Motohide

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We present a new method of analysis for determining the surface geometry of five protoplanetary disks observed with near-infrared imaging polarimetry using Subaru-HiCIAO. Using as inputs the observed distribution of polarized intensity (PI), disk inclination, assumed properties for dust scattering, and other reasonable approximations, we calculate a differential equation to derive the surface geometry. This equation is numerically integrated along the distance from the star at a given position angle. We show that, using these approximations, the local maxima in the PI distribution of spiral arms (SAO 206462, MWC 758) and rings (2MASS J16042165-2130284, PDS 70) are associated with local concave-up structures on the disk surface. We also show that the observed presence of an inner gap in scattered light still allows the possibility of a disk surface that is parallel to the light path from the star, or a disk that is shadowed by structures in the inner radii. Our analysis for rings does not show the presence of a vertical inner wall as often assumed in studies of disks with an inner gap. Finally, we summarize the implications of spiral and ring structures as potential signatures of ongoing planet formation., Comment: 35 pages, 13 figures, 7 tables, accepted by ApJ

Published
2014
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7. High-Resolution Submillimeter and Near-Infrared Studies of the Transition Disk around Sz 91

Author

Tsukagoshi, Takashi, Momose, Munetake, Hashimoto, Jun, Kudo, Tomoyuki, Andrews, Sean, Saito, Masao, Kitamura, Yoshimi, Ohashi, Nagayoshi, Wilner, David, Kawabe, Ryohei, Abe, Lyu, Akiyama, Eiji, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph, Currie, Thayne, Egner, Sebastian E., Goto, Miwa, Grady, Carol, Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko, Henning, Thomas, Hodapp, Klaus W., Ishii, Miki, Iye, Masanori, Janson, Markus, Kandori, Ryo, Knapp, Gillian R., Kusakabe, Nobuhiko, Kuzuhara, Masayuki, Kwon, Jungmi, McElwain, Mike, Matsuo, Taro, Mayama, Satoshi, Miyama, Shoken, Morino, Jun-ichi, Moro-Martín, Amaya, Nishimura, Tetsuro, Pyo, Tae-Soo, Serabyn, Eugene, Suenaga, Takuya, Suto, Hiroshi, Suzuki, Ryuji, Takahashi, Yasuhiro, Takami, Hideki, Takami, Michihiro, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Usuda, Tomonori, Watanabe, Makoto, Wisniewski, John P., Yamada, Toru, and Tamura, Motohide

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

To reveal the structures of a transition disk around a young stellar object in Lupus, Sz 91, we have performed aperture synthesis 345 GHz continuum and CO(3--2) observations with the Submillimeter Array ($\sim1\arcsec$--3$\arcsec$ resolution), and high-resolution imaging of polarized intensity at the $K_s$-band by using the HiCIAO instrument on the Subaru Telescope ($0\farcs25$ resolution). Our observations successfully resolved the inner and outer radii of the dust disk to be 65 AU and 170 AU, respectively, which indicates that Sz 91 is a transition disk source with one of the largest known inner holes. The model fitting analysis of the spectral energy distribution reveals an H$_2$ mass of $2.4\times10^{-3}$ $M_\sun$ in the cold ($T<$30 K) outer part at $653\times10^{-9}$ $M_\sun$) of hot ($T\sim$180 K) dust possibly remains inside the inner hole of the disk. The structure of the hot component could be interpreted as either an unresolved self-luminous companion body (not directly detected in our observations) or a narrow ring inside the inner hole. Significant CO(3--2) emission with a velocity gradient along the major axis of the dust disk is concentrated on the Sz 91 position, suggesting a rotating gas disk with a radius of 420 AU. The Sz 91 disk is possibly a rare disk in an evolutionary stage immediately after the formation of protoplanets because of the large inner hole and the lower disk mass than other transition disks studied thus far.

Published
2014
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8. Direct Imaging Search for Extrasolar Planets in the Pleiades

Author

Yamamoto, Kodai, Matsuo, Taro, Shibai, Hiroshi, Itoh, Yoichi, Konishi, Mihoko, Sudo, Jun, Tanii, Ryoko, Fukagawa, Misato, Sumi, Takahiro, Kudo, Tomoyuki, Hashimoto, Jun, Kusakabe, Nobuhiko, Abe, Lyu, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph, Currie, Thayne, Egner, Sebastian E., Feldt, Markus, Goto, Miwa, Grady, Carol, Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko, Henning, Thomas, Hodapp, Klaus, Ishii, Miki, Iye, Masanori, Janson, Markus, Kandori, Ryo, Knapp, Gillian R., Kuzuhara, Masayuki, Kwon, Jungmi, McElwain, Mike, Miyama, Shoken, Morino, Jun-Ichi, Moro-Martin, Amaya, Nishikawa, June, Nishimura, Tetsuo, Pyo, Tae-Soo, Serabyn, Eugene, Suto, Hiroshi, Suzuki, Ryuji, Takami, Michihiro, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Wisniewski, John, Watanabe, Makoto, Yamada, Toru, Takami, Hideki, Usuda, Tomonori, and Tamura, Motohide

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We carried out an imaging survey for extrasolar planets around stars in the Pleiades (125 Myr, 135 pc) in the $H$ and $K_{S}$ bands using HiCIAO combined with the adaptive optics, AO188, on the Subaru telescope. We found 13 companion candidates fainter than 14.5 mag in the $H$ band around 9 stars. Five of these 13 were confirmed to be background stars by measurement of their proper motion. One was not found in the second epoch observation, and thus was not a background or companion object. One had multi-epoch image, but the precision of its proper motion was not sufficient to conclude whether it was background object. Four other candidates are waiting for second epoch observations to determine their proper motion. Finally, the remaining 2 were confirmed to be 60 $M_{J}$ brown dwarf companions orbiting around HD 23514 (G0) and HII 1348 (K5) respectively, as had been reported in previous studies. In our observations, the average detection limit for a point source was 20.3 mag in the $H$ band beyond 1''.5 from the central star. On the basis of this detection limit, we calculated the detection efficiency to be 90% for a planet with 6 to 12 Jovian masses and a semi-major axis of 50--1000 AU. For this we extrapolated the distribution of planet mass and semi-major axis derived from RV observations and adopted the planet evolution model of Baraffe et al. (2003). As there was no detection of a planet, we estimated the frequency of such planets to be less than 17.9% ($2\sigma$) around one star of the Pleiades cluster., Comment: 30 pages, 5 figures, accepted for publication in PASJ

Published
2013
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9. High-Contrast Near-Infrared Imaging Polarimetry of the Protoplanetary Disk around RY Tau

Author

Takami, Michihiro, Karr, Jennifer L., Hashimoto, Jun, Kim, Hyosun, Wisnewski, John, Henning, Thomas, Grady, Carol A., Kandori, Ryo, Hodapp, Klaus W., Kudo, Tomoyuki, Kusakabe, Nobuhiko, Chou, Mei-Yin, Itoh, Yoichi, Momose, Munetake, Mayama, Satoshi, Currie, Thayne, Follette, Katherine B., Kwon, Jungmi, Abe, Lyu, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph, Egner, Sebastian E., Feldt, Markus, Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko, Ishii, Miki, Iye, Masanori, Janson, Markus, Knapp, Gillian R., Kuzuhara, Masayuki, McElwain, Michael W., Matsuo, Taro, Miyama, Shoken, Morino, Jun-Ichi, Moro-Martin, Amaya, Nishimura, Tetsuo, Pyo, Tae-Soo, Serabyn, Eugene, Suto, Hiroshi, Suzuki, Ryuji, 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

We present near-infrared coronagraphic imaging polarimetry of RY Tau. The scattered light in the circumstellar environment was imaged at H-band at a high resolution (~0".05) for the first time, using Subaru-HiCIAO. The observed polarized intensity (PI) distribution shows a butterfly-like distribution of bright emission with an angular scale similar to the disk observed at millimeter wavelengths. This distribution is offset toward the blueshifted jet, indicating the presence of a geometrically thick disk or a remnant envelope, and therefore the earliest stage of the Class II evolutionary phase. We perform comparisons between the observed PI distribution and disk models with: (1) full radiative transfer code, using the spectral energy distribution (SED) to constrain the disk parameters; and (2) monochromatic simulations of scattered light which explore a wide range of parameters space to constrain the disk and dust parameters. We show that these models cannot consistently explain the observed PI distribution, SED, and the viewing angle inferred by millimeter interferometry. We suggest that the scattered light in the near-infrared is associated with an optically thin and geometrically thick layer above the disk surface, with the surface responsible for the infrared SED. Half of the scattered light and thermal radiation in this layer illuminates the disk surface, and this process may significantly affect the thermal structure of the disk., Comment: 35 pages, 14 figures, 7 tables, accepted for publication in Astrophysical Journal

Published
2013
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10. Mapping H-band Scattered Light Emission in the Mysterious SR21 Transitional Disk

Author

Follette, Katherine B., Tamura, Motohide, Hashimoto, Jun, Whitney, Barbara, Grady, Carol, Close, Laird, Andrews, Sean M., Kwon, Jungmi, Wisniewski, John, Brandt, Timothy D., Mayama, Satoshi, Kandori, Ryo, Dong, Ruobing, Abe, Lyu, Brandner, Wolfgang, Carson, Joseph, Currie, Thayne, Egner, Sebastian E., Feldt, Markus, Goto, Miwa, Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko, Henning, Thomas, Hodapp, Klaus, Ishii, Miki, Iye, Masanori, Janson, Markus, Knapp, Gillian R., Kudo, Tomoyuki, Kusakabe, Nobuhiko, Kuzuhara, Masayuki, McElwain, Michael W., Matsuo, Taro, Miyama, Shoken, Morino, Jun-Ichi, Moro-Martin, Amaya, Nishimura, Tetsuo, Pyo, Tae-Soo, Serabyn, Eugene, Suto, Hiroshi, Suzuki, Ryuji, Takami, Michihiro, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Watanabe, Makoto, Yamada, Toru, Takami, Hideki, and Usuda, Tomonori

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We present the first near infrared (NIR) spatially resolved images of the circumstellar transitional disk around SR21. These images were obtained with the Subaru HiCIAO camera, adaptive optics and the polarized differential imaging (PDI) technique. We resolve the disk in scattered light at H-band for stellocentric 0.1"

Published
2013
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11. A Common Proper Motion Stellar Companion to HAT-P-7

Author

Narita, Norio, Takahashi, Yasuhiro H., Kuzuhara, Masayuki, Hirano, Teruyuki, Suenaga, Takuya, Kandori, Ryo, Kudo, Tomoyuki, Sato, Bun'ei, Suzuki, Ryuji, Ida, Shigeru, Nagasawa, Makiko, Abe, Lyu, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph, Egner, Sebastian E., Feldt, Markus, Goto, Miwa, Grady, Carol A., Guyon, Olivier, Hashimoto, Jun, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko S., Henning, Thomas, Hodapp, Klaus W., Ishii, Miki, Iye, Masanori, Janson, Markus, Knapp, Gillian R., Kusakabe, Nobuhiko, Kwon, Jungmi, Matsuo, Taro, Mayama, Satoshi, McElwain, Michael W., Miyama, Shoken, Morino, Jun-Ichi, Moro-Martin, Amaya, Nishimura, Tetsuo, Pyo, Tae-Soo, Serabyn, Eugene, Suto, Hiroshi, Takami, Michihiro, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Watanab, Makoto, Wisniewski, John P., Yamada, Toru, Takami, Hideki, Usuda, Tomonori, and Tamara, Motohide

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

We report that HAT-P-7 has a common proper motion stellar companion. The companion is located at $\sim3.9$ arcsec to the east and estimated as an M5.5V dwarf based on its colors. We also confirm the presence of the third companion, which was first reported by Winn et al. (2009), based on long-term radial velocity measurements. We revisit the migration mechanism of HAT-P-7b given the presence of those companions, and propose sequential Kozai migration as a likely scenario in this system. This scenario may explain the reason for an outlier in the discussion of the spin-orbit alignment timescale for HAT-P-7b by Albrecht et al. (2012)., Comment: 5 pages, 4 figures, 2 tables, PASJ Letters in press

Published
2012
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12. Search for Outer Massive Bodies around Transiting Planetary Systems: Candidates of Faint Stellar Companions around HAT-P-7

Author

Narita, Norio, Kudo, Tomoyuki, Bergfors, Carolina, Nagasawa, Makiko, Thalmann, Christian, Sato, Bun'ei, Suzuki, Ryuji, Kandori, Ryo, Janson, Markus, Goto, Miwa, Brandner, Wolfgang, Ida, Shigeru, Abe, Lyu, Carson, Joseph, Egner, Sebastian E., Feldt, Markus, Golota, Taras, Guyon, Olivier, Hashimoto, Jun, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko S., Henning, Thomas, Hodapp, Klaus W., Ishii, Miki, Knapp, Gillian R., Kusakabe, Nobuhiko, Kuzuhara, Masayuki, Matsuo, Taro, McElwain, Michael W., Miyama, Shoken, Morino, Jun-Ichi, Moro-Martin, Amaya, Nishimura, Tetsuo, Pyo, Tae-Soo, Serabyn, Eugene, Suenaga, Takuya, Suto, Hiroshi, Takahashi, Yasuhiro, Takami, Michihiro, Takato, Naruhisa, Terada, Hiroshi, Tomono, Daigo, Turner, Edwin L., Watanabe, Makoto, Yamada, Toru, Takami, Hideki, Usuda, Tomonori, and Tamura, Motohide

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

We present results of direct imaging observations for HAT-P-7 taken with the Subaru HiCIAO and the Calar Alto AstraLux. Since the close-in transiting planet HAT-P-7b was reported to have a highly tilted orbit, massive bodies such as giant planets, brown dwarfs, or a binary star are expected to exist in the outer region of this system. We show that there are indeed two candidates for distant faint stellar companions around HAT-P-7. We discuss possible roles played by such companions on the orbital evolution of HAT-P-7b. We conclude that as there is a third body in the system as reported by Winn et al. (2009, ApJL, 763, L99), the Kozai migration is less likely while planet-planet scattering is possible., Comment: 8 pages, 3 figures, 2 tables, PASJ in press

Published
2010
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13. Radial decoupling of small and large dust grains in the transitional disk RX J1615.3-3255

Author

Kooistra, Robin, Kamp, Inga, Fukagawa, Misato, Menard, Francois, Momose, Munetake, Tsukagoshi, Takashi, Kudo, Tomoyuki, Kusakabe, Nobuhiko, Hashimoto, Jun, Abe, Lyu, Brandner, Wolfgang, Brandt, Timothy D, Carson, Joseph C, Egner, Sebastian E, Feldt, Markus, Goto, Miwa, Grady, Carol A, 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, Currie, Thayne, Akiyama, Eiji, Mayama, Satoshi, Follette, Katherine B, and Nakagawa, Takao

Subjects
Astrophysics
Abstract

We present H-band (1.6 micron) scattered light observations of the transitional disk RX J1615.3-3255, located in the approx. 1 Myr old Lupus association. From a polarized intensity image, taken with the HiCIAO instrument of the Subaru Telescope, we deduce the position angle and the inclination angle of the disk. The disk is found to extend out to 68 +/- 12 AU in scattered light and no clear structure is observed. Our inner working angle of 24 AU does not allow us to detect a central decrease in intensity similar to that seen at 30 AU in the 880 m continuum observations. We compare the observations with multiple disk models based on the spectral energy distribution (SED) and submm interferometry and find that an inner rim of the outer disk at 30 AU containing small silicate grains produces a polarized intensity signal which is an order of magnitude larger than observed. We show that a model in which the small dust grains extend smoothly into the cavity found for large grains is closer to the actual H-band observations. A comparison of models with different dust size distributions suggests that the dust in the disk might have undergone significant processing compared to the interstellar medium.

Published
2017
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15. High-contrast imaging of ϵ Eridani with ground-based instruments

Author

Mizuki, Toshiyuki, Yamada, Toru, Carson, Joseph C., Kuzuhara, Masayuki, Nakagawa, Takao, Nishikawa, June, Sitko, Michael L., Kudo, Tomoyuki, Kusakabe, Nobuhiko, Hashimoto, Jun, Abe, Lyu, Brander, W., Brandt, Timothy D., Egner, Sebastian E., Feldt, Markus, Goto, Miwa, Grady, Carol A., 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., Kwon, Jungmi, Matsuo, Taro, McElwain, Michael W., Miyama, Shoken, Morino, Junichi, Moro-Martín, Amaya, Nishimura, Tetsuro, Pyo, Tae-Soo, Serabyn, Eugene, Suenaga, Takuya, Suto, Hiroshi, Suzuki, Ryuji, Takahashi, Yasuhiro H., Takami, Michihiro, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Turner, Edwin L., Watanabe, Makoto, Wisniewski, John P., Takami, Hideki, Usuda, Tomonori, and Tamura, Motohide

Subjects
Planets and satellites: general, Instrumentation: adaptive optics, Techniques: image processing, Astrophysics::Solar and Stellar Astrophysics, Stars: individual:ϵ Eridani, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, general, Techniques: image processing [Planets and satellites], Astrophysics::Galaxy Astrophysics
Abstract

ϵ Eridani is one of the nearest solar-type stars. Its proximity and relatively young age allow high-contrast imaging observations to achieve sensitivities to planets at narrow separations down to an inner radius of ~5 AU. Previous observational studies of the system report a dust disk with asymmetric morphology as well as a giant planet with large orbital eccentricity, which may require another massive companion to induce the peculiar morphology and to enhance the large orbital eccentricity. In this paper, we report results from deep high-contrastimaging observations to detect the previously reported planet and search for other unseen less massive companions with Subaru/HiCIAO, Gemini-South/NICI, and VLT/NACO. No positive detection was made, but high-contrast measurements with the CH4S narrow-band filter of HiCIAO achieved sensitivities at 14.7 mag differential magnitude level, at an angular separation of 1.0″. In terms of planetary mass, as determined by cooling evolutionary models, the highest sensitivities were achieved by the Lp broad-band filter of NACO, resulting in sensitivities corresponding to 1.8, 2.8, and 4.5 Mjup at the projected separation of 3 AU, if 200, 400, and 800 Myr is assumed for the age of the system, respectively. We also discuss origins of the dust disk from the detection sensitivity in the planetary mass and find that a less massive eccentric planet is preferred for disk stirring, which is consistent with the orbital parameters of ϵ Eri b claimed from the previous long-term radial velocity monitoring., Astronomy & Astrophysics, 595, ISSN:0004-6361, ISSN:1432-0746

Published
2016

16. Extreme asymmetry in the polarized disk of V1247 Orionis

Author

Ohta, Yurina, Fukagawa, Misato, Sitko, Michael L., Muto, Takayuki, Kraus, Stefan, Grady, Carol A., Wisniewski, John P., Swearingen, Jeremy R., Shibai, Hiroshi, Sumi, Takahiro, Hashimoto, Jun, Kudo, Tomoyuki, Kusakabe, Nobuhiko, Momose, Munetake, Okamoto, Yoshiko, Kotani, Takayuki, Takami, Michihiro, Currie, Thayne, Thalmann, Christian, Janson, Markus, Akiyama, Eiji, Follette, Katherine B., Mayama, Satoshi, Abe, Lyu, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph C., Egner, Sebastian E., Feldt, Markus, Goto, Miwa, Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko S., Henning, Thomas, Hodapp, Klaus W., Ishii, Miki, Iye, Masanori, 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, Hideki, Takato, Naruhisa, Terada, Hiroshi, Tomono, Daigo, Turner, Edwin L., Usuda, Tomonori, Watanabe, Makoto, Yamada, Toru, Tamura, Motohide, Ohta, Yurina, Fukagawa, Misato, Sitko, Michael L., Muto, Takayuki, Kraus, Stefan, Grady, Carol A., Wisniewski, John P., Swearingen, Jeremy R., Shibai, Hiroshi, Sumi, Takahiro, Hashimoto, Jun, Kudo, Tomoyuki, Kusakabe, Nobuhiko, Momose, Munetake, Okamoto, Yoshiko, Kotani, Takayuki, Takami, Michihiro, Currie, Thayne, Thalmann, Christian, Janson, Markus, Akiyama, Eiji, Follette, Katherine B., Mayama, Satoshi, Abe, Lyu, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph C., Egner, Sebastian E., Feldt, Markus, Goto, Miwa, Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko S., Henning, Thomas, Hodapp, Klaus W., Ishii, Miki, Iye, Masanori, 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, Hideki, Takato, Naruhisa, Terada, Hiroshi, Tomono, Daigo, Turner, Edwin L., Usuda, Tomonori, Watanabe, Makoto, Yamada, Toru, and Tamura, Motohide

Abstract

We present the first near-infrared scattered-light detection of the transitional disk around V1247 Ori, which was obtained using high-resolution polarimetric differential imaging observations with Subaru/HiCIAO. Our imaging in the H band reveals the disk morphology at separations of similar to 0.'' 14-0.'' 86 (54-330 au) from the central star. The polarized intensity image shows a remarkable arc-like structure toward the southeast of the star, whereas the fainter northwest region does not exhibit any notable features. The shape of the arm is consistent with an arc of 0.'' 28 +/- 0.'' 09 in radius (108 au from the star), although the possibility of a spiral arm with a small pitch angle cannot be excluded. V1247 Ori features an exceptionally large azimuthal contrast in scattered, polarized light; the radial peak of the southeastern arc is about three times brighter than the northwestern disk measured at the same distance from the star. Combined with the previous indication of an inhomogeneous density distribution in the gap at less than or similar to 46 au, the notable asymmetry in the outer disk suggests the presence of unseen companions and/or planet-forming processes ongoing in the arc.

Published
2016
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17. NAOMI: a low-order adaptive optics system for the VLT interferometer

Author

Gonté, Frédéric Yves J., additional, Alonso, Jaime, additional, Aller-Carpentier, Emmanuel, additional, Andolfato, Luigi, additional, Berger, Jean-Philippe, additional, Cortes, Angela, additional, Delplancke-Strobele, Françoise, additional, Donaldson, Rob, additional, Dorn, Reinhold J., additional, Dupuy, Christophe, additional, Egner, Sebastian E., additional, Huber, Stefan, additional, Hubin, Norbert, additional, Kirchbauer, Jean-Paul, additional, Le Louarn, Miska, additional, Lilley, Paul, additional, Jolley, Paul, additional, Martis, Alessandro, additional, Paufique, Jérôme, additional, Pasquini, Luca, additional, Quentin, Jutta, additional, Ridings, Robert, additional, Reyes, Javier, additional, Shchkaturov, Pavel, additional, Suarez, Marcos, additional, Phan Duc, Thanh, additional, Valdes, Guillermo, additional, Woillez, Julien, additional, Le Bouquin, Jean-Baptiste, additional, Beuzit, Jean-Luc, additional, Rochat, Sylvain, additional, Vérinaud, Christophe, additional, Moulin, Thibaut, additional, Delboulbé, Alain, additional, Michaud, Laurence, additional, Correia, Jean-Jacques, additional, Roux, Alain, additional, Maurel, Didier, additional, Stadler, Eric, additional, and Magnard, Yves, additional

Published
2016
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18. SEEDS ADAPTIVE OPTICS IMAGING OF THE ASYMMETRIC TRANSITION DISK OPH IRS 48 IN SCATTERED LIGHT

Author

Follette, Katherine B., Grady, Carol A., Swearingen, Jeremy R., Sitko, Michael L., Champney, Elizabeth H., van der Marel, Nienke, Takami, Michihiro, Kuchner, Marc J., Close, Laird M., Muto, Takayuki, Mayama, Satoshi, McElwain, Michael W., Fukagawa, Misato, Maaskant, Koen, Min, Michiel, Russell, Ray W., Kudo, Tomoyuki, Kusakabe, Nobuhiko, Hashimoto, Jun, Abe, Lyu, Akiyama, Eiji, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph, Currie, Thayne, Egner, Sebastian E., Feldt, Markus, Goto, Miwa, Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko, Henning, Thomas, Hodapp, Klaus, Ishii, Miki, Iye, Masanori, Janson, Markus, Kandori, Ryo, Knapp, Gillian R., Kuzuhara, Masayuki, Kwon, Jungmi, Matsuo, Taro, Miyama, Shoken, Morino, Jun-Ichi, Moro-Martin, Amaya, Nishimura, Tetsuo, Pyo, Tae-Soo, Serabyn, Eugene, Suenaga, Takuya, Suto, Hiroshi, Suzuki, Ryuji, Takahashi, Yasuhiro, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Watanabe, Makoto, Wisniewski, John P., Yamada, Toru, Takami, Hideki, Usuda, Tomonori, Tamura, Motohide, Follette, Katherine B., Grady, Carol A., Swearingen, Jeremy R., Sitko, Michael L., Champney, Elizabeth H., van der Marel, Nienke, Takami, Michihiro, Kuchner, Marc J., Close, Laird M., Muto, Takayuki, Mayama, Satoshi, McElwain, Michael W., Fukagawa, Misato, Maaskant, Koen, Min, Michiel, Russell, Ray W., Kudo, Tomoyuki, Kusakabe, Nobuhiko, Hashimoto, Jun, Abe, Lyu, Akiyama, Eiji, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph, Currie, Thayne, Egner, Sebastian E., Feldt, Markus, Goto, Miwa, Guyon, Olivier, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko, Henning, Thomas, Hodapp, Klaus, Ishii, Miki, Iye, Masanori, Janson, Markus, Kandori, Ryo, Knapp, Gillian R., Kuzuhara, Masayuki, Kwon, Jungmi, Matsuo, Taro, Miyama, Shoken, Morino, Jun-Ichi, Moro-Martin, Amaya, Nishimura, Tetsuo, Pyo, Tae-Soo, Serabyn, Eugene, Suenaga, Takuya, Suto, Hiroshi, Suzuki, Ryuji, Takahashi, Yasuhiro, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Watanabe, Makoto, Wisniewski, John P., Yamada, Toru, Takami, Hideki, Usuda, Tomonori, and Tamura, Motohide

Abstract

We present the first resolved near-infrared imagery of the transition disk Oph IRS 48 (WLY 2-48), which was recently observed with ALMA to have a strongly asymmetric submillimeter flux distribution. H-band polarized intensity images show a similar to 60 AU radius scattered light cavity with two pronounced arcs of emission, one from northeast to southeast and one smaller, fainter, and more distant arc in the northwest. K-band scattered light imagery reveals a similar morphology, but with a clear third arc along the southwestern rim of the disk cavity. This arc meets the northwestern arc at nearly a right angle, revealing the presence of a spiral arm or local surface brightness deficit in the disk, and explaining the east-west brightness asymmetry in the H-band data. We also present 0.8-5.4 mu m IRTF SpeX spectra of this object, which allow us to constrain the spectral class to A0 +/- 1 and measure a low mass accretion rate of 10(-8.5) M-circle dot yr(-1), both consistent with previous estimates. We investigate a variety of reddening laws in order to fit the multiwavelength spectral energy distribution of Oph IRS 48 and find a best fit consistent with a younger, higher luminosity star than previous estimates., AuthorCount:63

Published
2015
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19. High-Resolution Submillimeter and Near-infrared Studies of the Transition Disk around Sz 91

Author

塚越, 崇, 百瀬, 宗武, 橋本, 淳, 工藤, 智幸, Andrews, Sean, 齋藤, 正雄, 北村, 良実, 大橋, 永芳, Wilner, David, 川辺, 良平, Abe, Lyu, 秋山, 永治, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph, Currie, Thayne, Egner, Sebastian E., 後藤, 美和, Grady, Carol, Guyon, Olivier, 早野, 裕, 林, 正彦, 林, 左絵子, Henning, Thomas, Hodapp, Klaus W., 石井, 未来, 家, 正則, Janson, Markus, 神鳥, 亮, Knapp, Gillian R., Tsukagoshi, Takashi, Momose, Munetake, Hashimoto, Jun, Kudo, Tomoyuki, Saito, Masao, Kitamura, Yoshimi, Ohashi, Nagayoshi, Kawabe, Ryohei, Akiyama, Eiji, Goto, Miwa, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko, Ishii, Miki, Iye, Masanori, Kandori, Ryo, 塚越, 崇, 百瀬, 宗武, 橋本, 淳, 工藤, 智幸, Andrews, Sean, 齋藤, 正雄, 北村, 良実, 大橋, 永芳, Wilner, David, 川辺, 良平, Abe, Lyu, 秋山, 永治, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph, Currie, Thayne, Egner, Sebastian E., 後藤, 美和, Grady, Carol, Guyon, Olivier, 早野, 裕, 林, 正彦, 林, 左絵子, Henning, Thomas, Hodapp, Klaus W., 石井, 未来, 家, 正則, Janson, Markus, 神鳥, 亮, Knapp, Gillian R., Tsukagoshi, Takashi, Momose, Munetake, Hashimoto, Jun, Kudo, Tomoyuki, Saito, Masao, Kitamura, Yoshimi, Ohashi, Nagayoshi, Kawabe, Ryohei, Akiyama, Eiji, Goto, Miwa, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko, Ishii, Miki, Iye, Masanori, and Kandori, Ryo

Abstract

著者人数: 58名, Accepted: 2014-01-16

Published
2015

20. NEAR-IR HIGH-RESOLUTION IMAGING POLARIMETRY OF THE SU Aur DISK: CLUES FOR TIDAL TAILS?

Author

Leon, Jerome de, primary, Takami, Michihiro, additional, Karr, Jennifer L., additional, Hashimoto, Jun, additional, Kudo, Tomoyuki, additional, Sitko, Michael, additional, Mayama, Satoshi, additional, Kusakabe, Nobuyuki, additional, Akiyama, Eiji, additional, Liu, Hauyu Baobab, additional, Usuda, Tomonori, additional, Abe, Lyu, additional, Brandner, Wolfgang, additional, Brandt, Timothy D., additional, Carson, Joseph, additional, Currie, Thayne, additional, Egner, Sebastian E., additional, Feldt, Markus, additional, Follette, Katherine, additional, Grady, Carol A., additional, Goto, Miwa, additional, Guyon, Olivier, additional, Hayano, Yutaka, additional, Hayashi, Masahiko, additional, Hayashi, Saeko, 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, Martin, Amaya Moro-, additional, Nishimura, Tetsuo, additional, Pyo, Tae-Soo, additional, Serabyn, Eugene, additional, Suenaga, Takuya, additional, Suto, Hiroshi, additional, Suzuki, Ryuji, additional, Takahashi, Yasuhiro, additional, Takato, Naruhisa, additional, Terada, Hiroshi, additional, Thalmann, Christian, additional, Tomono, Daigo, additional, Turner, Edwin L., additional, Watanabe, Makoto, additional, Wisniewski, John P., additional, Yamada, Toru, additional, Takami, Hideki, additional, and Tamura, Motohide, additional

Published
2015
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21. SEEDS ADAPTIVE OPTICS IMAGING OF THE ASYMMETRIC TRANSITION DISK OPH IRS 48 IN SCATTERED LIGHT

Author

Follette, Katherine B., primary, Grady, Carol A., additional, Swearingen, Jeremy R., additional, Sitko, Michael L., additional, Champney, Elizabeth H., additional, van der Marel, Nienke, additional, Takami, Michihiro, additional, Kuchner, Marc J, additional, Close, Laird M., additional, Muto, Takayuki, additional, Mayama, Satoshi, additional, McElwain, Michael W., additional, Fukagawa, Misato, additional, Maaskant, Koen, additional, Min, Michiel, additional, Russell, Ray W., additional, Kudo, Tomoyuki, additional, Kusakabe, Nobuhiko, additional, Hashimoto, Jun, additional, Abe, Lyu, additional, Akiyama, Eiji, additional, Brandner, Wolfgang, additional, Brandt, Timothy D., additional, Carson, Joseph, additional, Currie, Thayne, additional, Egner, Sebastian E., additional, Feldt, Markus, additional, Goto, Miwa, additional, Guyon, Olivier, additional, Hayano, Yutaka, additional, Hayashi, Masahiko, additional, Hayashi, Saeko, additional, Henning, Thomas, additional, Hodapp, Klaus, 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, 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, additional, Takato, Naruhisa, additional, Terada, Hiroshi, additional, Thalmann, Christian, additional, Tomono, Daigo, additional, Turner, Edwin L., additional, Watanabe, Makoto, additional, Wisniewski, John P., additional, Yamada, Toru, additional, Takami, Hideki, additional, Usuda, Tomonori, additional, and Tamura, Motohide, additional

Published
2015
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22. Multi-Conjugate Adaptive Optics for LINC-NIRVANA : Laboratory Tests of a Ground-Layer Adaptive Optics System and Virtical Turbulence Measurements at Mt. Graham

Author

Egner, Sebastian E.

Subjects
520 Astronomy and allied sciences
Abstract

Turbulence in Earth's atmosphere severely limits the image quality of ground-based telescopes. With the technique of Adaptive Optics, the induced distortions of the light can be measured and corrected in real-time, regaining nearly diffraction-limited performance. Unfortunately, when using a single guide star to measure the distortions, the correction is only useful within a small angular area centered on the guide star. The first part of this thesis presents a laboratory setup, which uses four guide stars to measure the turbulence-induced distortions and one deformable mirror to correct the most turbulent layer. With such a Layer-Oriented Ground-Layer Adaptive Optics (GLAO) system, the area of useful correction is significantly increased. The system is characterized in static and dynamic operation, and the influence of non-conjugated turbulent layers, the effect of brightness variations of the guide-stars and the impact of misalignments are studied. Furthermore, calibration strategies and the performance of the Kalman control algorithm are examined. The second part of this thesis focuses on SCIDAR measurements of the atmospheric turbulence above Mt. Graham. This dataset provides for the first time a statistical and thorough analysis of the vertical turbulence structure above the LBT site. Based on 16 nights of measurements, spread over one year, Mt. Graham appears to be an excellent site for an astronomical observatory. By extending an analytical model, describing the filtering of the turbulence-induced distortions by an AO system, we calculate performance expectations of the LINC-NIRVANA instrument. In particular, the optimal conjugation heights of the deformable mirrors are studied. Furthermore, we present a new method to measure the atmospheric turbulence near the ground with 40 times increased vertical resolution, compared to standard SCIDAR. First on-sky results demonstrate the power of this technique.

Published
2006
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23. SURFACE GEOMETRY OF PROTOPLANETARY DISKS INFERRED FROM NEAR-INFRARED IMAGING POLARIMETRY

Author

Takami, Michihiro, primary, Hasegawa, Yasuhiro, additional, Muto, Takayuki, additional, Gu, Pin-Gao, additional, Dong, Ruobing, additional, Karr, Jennifer L., additional, Hashimoto, Jun, additional, Kusakabe, Nobuyuki, additional, Chapillon, Edwige, additional, Tang, Ya-Wen, additional, Itoh, Youchi, additional, Carson, Joseph, additional, Follette, Katherine B., additional, Mayama, Satoshi, additional, Sitko, Michael, additional, Janson, Markus, additional, Grady, Carol A., additional, Kudo, Tomoyuki, additional, Akiyama, Eiji, additional, Kwon, Jungmi, additional, Takahashi, Yasuhiro, additional, Suenaga, Takuya, additional, Abe, Lyu, additional, Brandner, Wolfgang, additional, Brandt, Timothy D., additional, Currie, Thayne, additional, Egner, Sebastian E., additional, Feldt, Markus, additional, Guyon, Olivier, additional, Hayano, Yutaka, additional, Hayashi, Masahiko, additional, Hayashi, Saeko, additional, Henning, Thomas, additional, Hodapp, Klaus W., additional, Honda, Mitsuhiko, additional, Ishii, Miki, additional, Iye, Masanori, additional, Kandori, Ryo, additional, Knapp, Gillian R., additional, Kuzuhara, Masayuki, additional, McElwain, Michael W., additional, Matsuo, Taro, additional, Miyama, Shoken, additional, Morino, Jun-Ichi, additional, Moro-Martin, Amaya, additional, Nishimura, Tetsuo, additional, Pyo, Tae-Soo, additional, Serabyn, Eugene, additional, Suto, Hiroshi, additional, Suzuki, Ryuji, additional, Takato, Naruhisa, additional, Terada, Hiroshi, additional, Thalmann, Christian, additional, Tomono, Daigo, additional, Turner, Edwin L., additional, Wisniewski, John P., additional, Watanabe, Makoto, additional, Yamada, Toru, additional, Takami, Hideki, additional, Usuda, Tomonori, additional, and Tamura, Motohide, additional

Published
2014
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24. HIGH-RESOLUTION SUBMILLIMETER AND NEAR-INFRARED STUDIES OF THE TRANSITION DISK AROUND Sz 91

Author

Tsukagoshi, Takashi, primary, Momose, Munetake, additional, Hashimoto, Jun, additional, Kudo, Tomoyuki, additional, Andrews, Sean, additional, Saito, Masao, additional, Kitamura, Yoshimi, additional, Ohashi, Nagayoshi, additional, Wilner, David, additional, Kawabe, Ryohei, additional, Abe, Lyu, additional, Akiyama, Eiji, additional, Brandner, Wolfgang, additional, Brandt, Timothy D., additional, Carson, Joseph, additional, Currie, Thayne, additional, Egner, Sebastian E., additional, Goto, Miwa, additional, Grady, Carol, additional, Guyon, Olivier, additional, Hayano, Yutaka, additional, Hayashi, Masahiko, additional, Hayashi, Saeko, additional, Henning, Thomas, additional, Hodapp, Klaus W., additional, Ishii, Miki, additional, Iye, Masanori, additional, Janson, Markus, additional, Kandori, Ryo, additional, Knapp, Gillian R., additional, Kusakabe, Nobuhiko, additional, Kuzuhara, Masayuki, additional, Kwon, Jungmi, additional, McElwain, Mike, additional, Matsuo, Taro, additional, Mayama, Satoshi, additional, Miyama, Shoken, additional, Morino, Jun-ichi, additional, Moro-Martín, Amaya, additional, Nishimura, Tetsuro, additional, Pyo, Tae-Soo, additional, Serabyn, Eugene, additional, Suenaga, Takuya, additional, Suto, Hiroshi, additional, Suzuki, Ryuji, additional, Takahashi, Yasuhiro, additional, Takami, Hideki, additional, Takami, Michihiro, additional, Takato, Naruhisa, additional, Terada, Hiroshi, additional, Thalmann, Christian, additional, Tomono, Daigo, additional, Turner, Edwin L., additional, Usuda, Tomonori, additional, Watanabe, Makoto, additional, Wisniewski, John P., additional, Yamada, Toru, additional, and Tamura, Motohide, additional

Published
2014
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25. HIGH-CONTRAST NEAR-INFRARED IMAGING POLARIMETRY OF THE PROTOPLANETARY DISK AROUND RY TAU

Author

Takami, Michihiro, primary, Karr, Jennifer L., additional, Hashimoto, Jun, additional, Kim, Hyosun, additional, Wisniewski, John, additional, Henning, Thomas, additional, Grady, Carol A., additional, Kandori, Ryo, additional, Hodapp, Klaus W., additional, Kudo, Tomoyuki, additional, Kusakabe, Nobuhiko, additional, Chou, Mei-Yin, additional, Itoh, Yoichi, additional, Momose, Munetake, additional, Mayama, Satoshi, additional, Currie, Thayne, additional, Follette, Katherine B., additional, Kwon, Jungmi, additional, Abe, Lyu, additional, Brandner, Wolfgang, additional, Brandt, Timothy D., additional, Carson, Joseph, additional, Egner, Sebastian E., additional, Feldt, Markus, additional, Guyon, Olivier, additional, Hayano, Yutaka, additional, Hayashi, Masahiko, additional, Hayashi, Saeko, additional, Ishii, Miki, additional, Iye, Masanori, additional, Janson, Markus, additional, Knapp, Gillian R., additional, Kuzuhara, Masayuki, additional, McElwain, Michael W., additional, Matsuo, Taro, additional, Miyama, Shoken, additional, Morino, Jun-Ichi, additional, Moro-Martin, Amaya, additional, Nishimura, Tetsuo, additional, Pyo, Tae-Soo, additional, Serabyn, Eugene, additional, Suto, Hiroshi, additional, Suzuki, Ryuji, additional, Takato, Naruhisa, additional, Terada, Hiroshi, additional, Thalmann, Christian, additional, Tomono, Daigo, additional, Turner, Edwin L., additional, Watanabe, Makoto, additional, Yamada, Toru, additional, Takami, Hideki, additional, Usuda, Tomonori, additional, and Tamura, Motohide, additional

Published
2013
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26. MAPPINGH-BAND SCATTERED LIGHT EMISSION IN THE MYSTERIOUS SR21 TRANSITIONAL DISK

Author

Follette, Katherine B., primary, Tamura, Motohide, additional, Hashimoto, Jun, additional, Whitney, Barbara, additional, Grady, Carol, additional, Close, Laird, additional, Andrews, Sean M., additional, Kwon, Jungmi, additional, Wisniewski, John, additional, Brandt, Timothy D., additional, Mayama, Satoshi, additional, Kandori, Ryo, additional, Dong, Ruobing, additional, Abe, Lyu, additional, Brandner, Wolfgang, additional, Carson, Joseph, additional, Currie, Thayne, additional, Egner, Sebastian E., additional, Feldt, Markus, additional, Goto, Miwa, additional, Guyon, Olivier, additional, Hayano, Yutaka, additional, Hayashi, Masahiko, additional, Hayashi, Saeko, additional, Henning, Thomas, additional, Hodapp, Klaus, additional, Ishii, Miki, additional, Iye, Masanori, additional, Janson, Markus, additional, Knapp, Gillian R., additional, Kudo, Tomoyuki, additional, Kusakabe, Nobuhiko, additional, Kuzuhara, Masayuki, additional, McElwain, Michael W., additional, Matsuo, Taro, additional, Miyama, Shoken, additional, Morino, Jun-Ichi, additional, Moro-Martin, Amaya, additional, Nishimura, Tetsuo, additional, Pyo, Tae-Soo, additional, Serabyn, Eugene, additional, Suto, Hiroshi, additional, Suzuki, Ryuji, additional, Takami, Michihiro, additional, Takato, Naruhisa, additional, Terada, Hiroshi, additional, Thalmann, Christian, additional, Tomono, Daigo, additional, Turner, Edwin L., additional, Watanabe, Makoto, additional, Yamada, Toru, additional, Takami, Hideki, additional, and Usuda, Tomonori, additional

Published
2013
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27. High-Resolution Near-Infrared Polarimetry of a Circumstellar Disk around UX Tau A

Author

Tanii, Ryoko, primary, Itoh, Yoichi, additional, Kudo, Tomoyuki, additional, Hioki, Tomonori, additional, Oasa, Yumiko, additional, Gupta, Ranjan, additional, Sen, Asoke K., additional, Wisniewski, John P., additional, Muto, Takayuki, additional, Grady, Carol A., additional, Hashimoto, Jun, additional, Fukagawa, Misato, additional, Mayama, Satoshi, additional, Hornbeck, Jeremy, additional, Sitko, Michael L., additional, Russell, Ray W., additional, Werren, Chelsea, additional, CurÉ, Michel, additional, Currie, Thayne, additional, Ohashi, Nagayoshi, additional, Okamoto, Yoshiko, additional, Momose, Munetake, additional, Honda, Mitsuhiko, additional, Inutsuka, Shu-ichi, additional, Takeuchi, Taku, additional, Dong, Ruobing, additional, Abe, Lyu, additional, Brandner, Wolfgang, additional, Brandt, Timothy D., additional, Carson, Joseph, additional, Egner, Sebastian E., additional, Feldt, Markus, additional, Fukue, Tsubasa, 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, Kusakabe, Nobuhiko, additional, Kuzuhara, Masayuki, additional, Matsuo, Taro, additional, Mcelwain, Michael W., additional, Miyama, Shoken, additional, Morino, Jun-ichi, additional, Moro-MartÍn, Amaya, additional, Nishimura, Tetsuro, additional, Pyo, Tae-Soo, additional, Serabyn, Eugene, additional, Suto, Hiroshi, additional, Suzuki, Ryuji, additional, Takami, Michihiro, additional, Takato, Naruhisa, additional, Terada, Hiroshi, additional, Thalmann, Christian, additional, Tomono, Daigo, additional, Turner, Edwin L., additional, Watanabe, Makoto, additional, Yamada, Toru, additional, Takami, Hideki, additional, Usuda, Tomonori, additional, and Tamura, Motohide, additional

Published
2012
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28. A Common Proper Motion Stellar Companion to HAT-P-7

Author

Narita, Norio, primary, Takahashi, Yasuhiro H., additional, Kuzuhara, Masayuki, additional, Hirano, Teruyuki, additional, Suenaga, Takuya, additional, Kandori, Ryo, additional, Kudo, Tomoyuki, additional, Sato, Bun'ei, additional, Suzuki, Ryuji, additional, Ida, Shigeru, additional, Nagasawa, Makiko, additional, Abe, Lyu, additional, Brandner, Wolfgang, additional, Brandt, Timothy D., additional, Carson, Joseph, additional, Egner, Sebastian E., additional, Feldt, Markus, additional, Goto, Miwa, additional, Grady, Carol A., additional, Guyon, Olivier, additional, Hashimoto, Jun, 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, Knapp, Gillian R., additional, Kusakabe, Nobuhiko, additional, Kwon, Jungmi, additional, Matsuo, Taro, additional, Mayama, Satoshi, additional, Mcelwain, Michael W., additional, Miyama, Shoken M., additional, Morino, Jun-Ichi, additional, Moro-Martin, Amaya, additional, Nishimura, Tetsuo, additional, Pyo, Tae-Soo, additional, Serabyn, Eugene, additional, Suto, Hiroshi, 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 P., additional, Yamada, Toru, additional, Takami, Hideki, additional, Usuda, Tomonori, additional, and Tamura, Motohide, additional

Published
2012
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29. Commissioning status of Subaru laser guide star adaptive optics system

Author

Hayano, Yutaka, primary, Takami, Hideki, additional, Oya, Shin, additional, Hattori, Masayuki, additional, Saito, Yoshihiko, additional, Watanabe, Makoto, additional, Guyon, Olivier, additional, Minowa, Yosuke, additional, Egner, Sebastian E., additional, Ito, Meguru, additional, Garrel, Vincent, additional, Colley, Stephen, additional, Golota, Taras, additional, and Iye, Masanori, additional

Published
2010
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30. Search for Outer Massive Bodies around Transiting Planetary Systems: Candidates of Faint Stellar Companions around HAT-P-7

Author

Narita, Norio, primary, Kudo, Tomoyuki, additional, Bergfors, Carolina, additional, Nagasawa, Makiko, additional, Thalmann, Christian, additional, Sato, Bun’ei, additional, Suzuki, Ryuji, additional, Kandori, Ryo, additional, Janson, Markus, additional, Goto, Miwa, additional, Brandner, Wolfgang, additional, Ida, Shigeru, additional, Abe, Lyu, additional, Carson, Joseph, additional, Egner, Sebastian E., additional, Feldt, Markus, additional, Golota, Taras, additional, Guyon, Olivier, additional, Hashimoto, Jun, additional, Hayano, Yutaka, additional, Hayashi, Masahiko, additional, Hayashi, Saeko S., additional, Henning, Thomas, additional, Hodapp, Klaus W., additional, Ishii, Miki, additional, Knapp, Gillian R., additional, Kusakabe, Nobuhiko, additional, Kuzuhara, Masayuki, additional, Matsuo, Taro, additional, McElwain, Michael W., additional, Miyama, Shoken M., 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, Takahashi, Yasuhiro Haruhi, additional, Takami, Michihiro, additional, Takato, Naruhisa, additional, Terada, Hiroshi, additional, Tomono, Daigo, additional, Turner, Edwin L., additional, Watanabe, Makoto, additional, Yamada, Toru, additional, Takami, Hideki, additional, Usuda, Tomonori, additional, and Tamura, Motohide, additional

Published
2010
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34. LINC-NIRVANA: how to get a 23-m wavefront nearly flat

Author

Gaessler, Wolfgang, primary, Ragazzoni, Roberto, additional, Herbst, Thomas M., additional, Andersen, David R., additional, Arcidiacono, Carmelo, additional, Baumeister, Harald, additional, Beckmann, Udo, additional, Behrend, Jan, additional, Bertram, Thomas, additional, Bizenberger, Peter, additional, Bohnhardt, Hermann, additional, Briegel, F., additional, Diolaiti, Emiliano, additional, Driebe, Thomas M., additional, Eckhardt, A., additional, Egner, Sebastian E., additional, Farinato, Jacopo, additional, Heininger, Matthias, additional, K’rster, M., additional, Laun, Werner, additional, Ligori, Sebastiano, additional, Naranjo, Vianak, additional, Nussbaum, Edmund, additional, Rix, Hans-Walter, additional, Rohloff, Ralf-Rainer, additional, Salinari, Piero, additional, Soci, Roberto, additional, Storz, Clemens, additional, Straubmeier, Christian, additional, Vernet-Viard, Elise, additional, Weigelt, Gerd P., additional, Weiss, Robert, additional, and Xu, Wenli, additional

Published
2004
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35. LINC-NIRVANA: mechanical challanges of the MCAO wavefront sensor

Author

Soci, Roberto, primary, Ragazzoni, Roberto, additional, Herbst, Thomas M., additional, Farinato, Jacopo, additional, Gaessler, Wolfgang, additional, Baumeister, Harald, additional, Rohloff, Ralf-Rainer, additional, Diolaiti, Emiliano, additional, Xu, Wenli, additional, Andersen, David R., additional, Egner, Sebastian E., additional, Arcidiacono, Carmelo, additional, Lombini, Matteo, additional, Ebert, Monica, additional, Boehm, Armin, additional, Muench, Norbert, additional, and Xompero, Marco, additional

Published
2004
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39. LINC-NIRVANA: the single arm MCAO experiment.

Author

Egner, Sebastian E., Gaessler, Wolfgang, Herbst, Tom M., Ragazzoni, Roberto, Stuik, Remko, Andersen, D. A., Arcidiacono, C., Baumeister, H., Beckmann, U., Behrend, J., Bertram, T., Bizenberger, P., Boehnhardt, H., Diolaiti, E., Driebe, T., Eckhardt, A., Farinato, J., Kuerster, M., Laun, W., and Ligori, S.

Published
2004
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40. MAPPING H-BAND SCATTERED LIGHT EMISSION IN THE MYSTERIOUS SR21 TRANSITIONAL DISK.

Author

KATHERINE B. FOLLETTE, MOTOHIDE TAMURA, JUN HASHIMOTO, WHITNEY, BARBARA, GRADY, CAROL, LAIRD CLOSE, ANDREWS, SEAN M., KWON, JUNGMI, WISNIEWSKI, JOHN, BRANDT, TIMOTHY D., SATOSHI MAYAMA, KANDORI, RYO, DONG, RUOBING, ABE, LYU, BRANDNER, WOLFGANG, CARSONS, JOSEPH, CURRIE, THAYNE, EGNER, SEBASTIAN E., FELDT, MARKUS, and GOTO, MIWA

Subjects
LIGHT scattering, PROTOPLANETARY disks, POLARIMETRY, SUBMILLIMETER waves, SPECTRAL energy distribution
Abstract

We present the first near infrared (NIR) spatially resolved images of the circumstellar transitional disk around SR21. These images were obtained with the SubaruHiCIAOcamera, adaptive optics, and the polarized differential imaging technique. We resolve the disk in scattered light at H-band for stellocentric 0."⩽1 r ⩽ 0.6 (12 ≲ r ≲ 75AU). We compare our results with previously published spatially resolved 880 μm continuum Submillimeter Array images that show an inner r ≲ 36AU cavity in SR21. Radiative transfer models reveal that the large disk depletion factor invoked to explain SR21's sub-mm cavity cannot be "universal" for all grain sizes. Even significantly more moderate depletions (δ = 0.1, 0.01 relative to an undepleted disk) than those that reproduce the sub-mm cavity (δ ~ 10-6) are inconsistent with our H-band images when they are assumed to carry over to small grains, suggesting that surface grains scattering in the NIR either survive or are generated by whatever mechanism is clearing the disk midplane. In fact, the radial polarized intensity profile of our H-band observations is smooth and steeply inwardly-increasing (r-3), with no evidence of a break at the 36AU sub-mm cavity wall. We hypothesize that this profile is dominated by an optically thin disk envelope or atmosphere component.We also discuss the compatibility of our data with the previously postulated existence of a sub-stellar companion to SR21 at r ~ 10-20AU, and find that we can neither exclude nor verify this scenario. This study demonstrates the power of multiwavelength imaging of transitional disks to inform modeling efforts, including the debate over precisely what physical mechanism is responsible for clearing these disks of their large midplane grains [ABSTRACT FROM AUTHOR]

Published
2013
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41. NAOMI: a low-order adaptive optics system for the VLT interferometer

Author

Malbet, Fabien, Creech-Eakman, Michelle J., Tuthill, Peter G., Gonté, Frédéric Yves J., Alonso, Jaime, Aller-Carpentier, Emmanuel, Andolfato, Luigi, Berger, Jean-Philippe, Cortes, Angela, Delplancke-Strobele, Françoise, Donaldson, Rob, Dorn, Reinhold J., Dupuy, Christophe, Egner, Sebastian E., Huber, Stefan, Hubin, Norbert, Kirchbauer, Jean-Paul, Le Louarn, Miska, Lilley, Paul, Jolley, Paul, Martis, Alessandro, Paufique, Jérôme, Pasquini, Luca, Quentin, Jutta, Ridings, Robert, Reyes, Javier, Shchkaturov, Pavel, Suarez, Marcos, Phan Duc, Thanh, Valdes, Guillermo, Woillez, Julien, Le Bouquin, Jean-Baptiste, Beuzit, Jean-Luc, Rochat, Sylvain, Vérinaud, Christophe, Moulin, Thibaut, Delboulbé, Alain, Michaud, Laurence, Correia, Jean-Jacques, Roux, Alain, Maurel, Didier, Stadler, Eric, and Magnard, Yves

Published
2016
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42. Indications of M-dwarf deficits in the halo and thick disk of the Galaxy

Author

Konishi, Mihoko, Shibai, Hiroshi, Sumi, Takahiro, Fukagawa, Misato, Matsuo, Taro, Samland, Matthias S., Yamamoto, Kodai, Sudo, Jun, Itoh, Yoichi, Arimoto, Nobuo, Kajisawa, Masaru, Abe, Lyu, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph, Currie, Thayne, Egner, Sebastian E., Feldt, Markus, Goto, Miwa, Grady, Carol A., Guyon, Olivier, Hashimoto, Jun, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko S., Henning, Thomas, Hodapp, Klaus W., Ishii, Miki, Iye, Masanori, Janson, Markus, Kandori, Ryo, Knapp, Gillian R., Kudo, Tomoyuki, Kusakabe, Nobuhiko, Kuzuhara, Masayuki, Kwon, Jungmi, McElwain, Michael W., Miyama, Shoken, Morino, Jun-Ichi, Moro-Martín, Amaya, Nishimura, Tetsuo, Pyo, Tae-Soo, Serabyn, Eugene, Suenaga, Takuya, Suto, Hiroshi, Suzuki, Ryuji, Takahashi, Yasuhiro H., Takami, Hideki, Takato, Naruhisa, Terada, Hiroshi, Thalmann, Christian, Tomono, Daigo, Turner, Edwin L., Usuda, Tomonori, Watanabe, Makoto, Wisniewski, John P., Yamada, Toru, and Tamura, Motohide

Abstract

We compared the number of faint stars detected in deep survey fields with the current stellar distribution model of the Galaxy and found that the detected number in the Hband is significantly smaller than the predicted number. This indicates that M-dwarfs, the major component, are fewer in the halo and the thick disk. We used archived data of several surveys in both the north and south field of GOODS (Great Observatories Origins Deep Survey), MODS (MOIRCS Deep Survey) in GOODS-N, and ERS (Early Release Science) and CANDELS (Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey) in GOODS-S. The number density of M-dwarfs in the halo has to be 20% ± 13% relative to that in the solar vicinity, in order for the detected number of stars fainter than 20.5 mag in the Hband to match with the predicted value from the model. In the thick disk, the number density of M-dwarfs must be reduced (52% ± 13%) or the scale height must be decreased (∼ 600 pc). Alternatively, overall fractions of the halo and thick disks can be significantly reduced to achieve the same effect, because our sample mainly consists of faint M-dwarfs. Our results imply that the M-dwarf population in regions distant from the Galactic plane is significantly smaller than previously thought. We then discussed the implications this has on the suitability of the model predictions for the prediction of non-companion faint stars in direct imaging extrasolar planet surveys by using the best-fitting number densities.

Published
2015
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