Direct Imaging of Fine Structures in Giant Planet-Forming Regions of the Protoplanetary Disk Around Ab Aurigae

Hashimoto, Jun; Tamura, Motohide; Muto, Takayuki; Kudo, Tomoyuki; Fukagawa, Misato; Fukue, T.; Goto, Miwa; Grady, C. A.; Henning, Th.; Hodapp, Klaus W.; Honda, Mitsuhiko; Inutsuka, Shu‐ichiro; Kokubo, Eiichiro; Knapp, G. R.; McElwain, Michael; Momose, Munetake; Ohashi, Nagayoshi; Okamoto, Y.; Takami, M.; Turner, Edwin L.; Wisniewski, John P.; Janson, Markus; Abe, Lyu; Brandner, W.; Carson, J.; Egner, Sebastian; Feldt, M.; Golota, Taras; Guyon, Olivier; Hayano, Yutaka; Hayashi, M.; Hayashi, Saeko S.; Ishii, Miki; Kandori, Ryo; Kusakabe, Nobuhiko; Matsuo, Taro; Mayama, Satoshi; Miyama, Shoken M.; Morino, Jun-Ichi; Moro‐Martín, Amaya; Nishimura, Tetsuro; Pyo, Tae‐Soo; Shimada, Hiroshi; Suzuki, Ryuji; Takato, Naruhisa; Terada, Hiroshi; Thalmann, Christian; Tomono, D.; Watanabe, Makoto; Yamada, Tōru; Takami, Hideki; Usuda, Tomonori

doi:10.1088/2041-8205/729/2/l17

Cited by 222 publications

(129 citation statements)

References 35 publications

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“…The southwest side is brighter than the northern side by a factor of ∼2 near the peaks (PI/I * ∼ 8 × 10 −7 and ∼3 × 10 −7 per pixel, respectively). The observed PI distribution, asymmetric with respect to the major axis of the disk, contrasts with the other disks observed in the SEEDS program (Hashimoto et al 2011Muto et al 2012;Kusakabe et al 2012;Tanii et al 2012;Mayama et al 2012;Grady et al 2013;Follette et al 2013), in which the PI distribution is generally symmetric. This indicates that RY Tau is associated with a geometrically thick disk or a remnant envelope, and therefore at a younger evolutionary stage than the others (see, e.g., Fischer et al 1994;Whitney et al 2003a).…”

Section: Observed Pi Distributioncontrasting

confidence: 63%

“…The data were reduced using the standard approach for polarimetric differential imaging (Hinkley et al 2009) as well as the other SEEDS studies (e.g., Hashimoto et al 2011Hashimoto et al , 2012Kusakabe et al 2012). The reduction was made using the Image Reduction and Analysis Facility (IRAF), 26 pyRAF, and python.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…Using coronagraphy, the ongoing survey "Strategic Explorations of Exoplanets and Disks with Subaru" (SEEDS; Tamura 2009) with Subaru/HiCIAO (Tamura et al 2006) and AO188 (Hayano et al 2004) has recently discovered structures in a number of protoplanetary disks (Thalmann et al 2010), in particular in the polarized intensity (hereafter PI) distribution in the near-infrared (Hashimoto et al 2011Muto et al 2012;Kusakabe et al 2012;Tanii et al 2012;Mayama et al 2012;Dong et al 2012a;Grady et al 2013;Follette et al 2013). PI imaging has been used for observations of most of the disks in the SEEDS program, since this suffers significantly less contamination from the stellar flux than the normal intensity I.…”

Section: Introductionmentioning

confidence: 99%

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High-Contrast Near-Infrared Imaging Polarimetry of the Protoplanetary Disk Around Ry Tau

Miki

Karr

Hashimoto

et al. 2013

ApJ

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We present near-infrared coronagraphic imaging polarimetry of RY Tau. The scattered light in the circumstellar environment was imaged at the 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.

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Section: Observed Pi Distributioncontrasting

confidence: 63%

Section: Observations and Data Reductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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High-Contrast Near-Infrared Imaging Polarimetry of the Protoplanetary Disk Around Ry Tau

Miki

Karr

Hashimoto

et al. 2013

ApJ

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“…5, 45 ,    and 67 . 5  were employed in order to allow for double difference polarized imaging (Kuhn et al 2001;Perrin et al 2004;Hinkley et al 2009;Hashimoto et al 2011), and the 60 s images were taken as four 15 s coadds in order to avoid saturating the inner region of the images.…”

Section: Gpi Datamentioning

confidence: 99%

Complex Spiral Structure in the HD 100546 Transitional Disk as Revealed by GPI and MagAO

et al. 2017

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We present optical and near-infrared high-contrast images of the transitional disk HD 100546 taken with the Magellan Adaptive Optics system (MagAO) and the Gemini Planet Imager (GPI). GPI data include both polarized intensity and total intensity imagery, and MagAO data are taken in Simultaneous Differential Imaging mode at Hα. The new GPI H-band total intensity data represent a significant enhancement in sensitivity and field rotation compared to previous data sets and enable a detailed exploration of substructure in the disk. The data are processed with a variety of differential imaging techniques (polarized, angular, reference, and simultaneous differential imaging) in an attempt to identify the disk structures that are most consistent across wavelengths, processing techniques, and algorithmic parameters. The inner disk cavity at 15 au is clearly resolved in multiple data sets, as are a variety of spiral features. While the cavity and spiral structures are identified at levels significantly distinct from the neighboring regions of the disk under several algorithms and with a range of algorithmic parameters, emission at the location of HD 100546 "c" varies from point-like under aggressive algorithmic parameters to a smooth continuous structure with conservative parameters, and is consistent with disk emission. Features identified in the HD 100546 disk bear qualitative similarity to computational models of a moderately inclined two-armed spiral disk, where projection effects and wrapping of the spiral arms around the star result in a number of truncated spiral features in forward-modeled images.

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“…Using PDI, SEEDS observations have discovered large central gaps 13,14 and spiral structures 15 in disks, which may point to unseen planets.…”

Section: Angular Differential Imaging (Adi)mentioning

confidence: 99%

CHARIS science: performance simulations for the Subaru Telescope's third-generation of exoplanet imaging instrumentation

Brandt¹,

McElwain

Janson

et al. 2014

SPIE Proceedings

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We describe the expected scientific capabilities of CHARIS, a high-contrast integral-field spectrograph (IFS) currently under construction for the Subaru telescope. CHARIS is part of a new generation of instruments, enabled by extreme adaptive optics (AO) systems (including SCExAO at Subaru), that promise greatly improved contrasts at small angular separation thanks to their ability to use spectral information to distinguish planets from quasistatic speckles in the stellar point-spread function (PSF). CHARIS is similar in concept to GPI and SPHERE, on Gemini South and the Very Large Telescope, respectively, but will be unique in its ability to simultaneously cover the entire near-infrared J, H, and K bands with a low-resolution mode. This extraordinarily broad wavelength coverage will enable spectral differential imaging down to angular separations of a few λ/D, corresponding to ∼0. 1. SCExAO will also offer contrast approaching 10 −5 at similar separations, ∼0. 1-0. 2. The discovery yield of a CHARIS survey will depend on the exoplanet distribution function at around 10 AU. If the distribution of planets discovered by radial velocity surveys extends unchanged to ∼20 AU, observations of ∼200 mostly young, nearby stars targeted by existing high-contrast instruments might find ∼1-3 planets. Carefully optimizing the target sample could improve this yield by a factor of a few, while an upturn in frequency at a few AU could also increase the number of detections. CHARIS, with a higher spectral resolution mode of R ∼ 75, will also be among the best instruments to characterize planets and brown dwarfs like HR 8799 cde and κ And b. We then use the thousands of mini spectra to reconstruct the data cube, the spectrum of each spatial element of the field-of-view.

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Direct Imaging of Fine Structures in Giant Planet-Forming Regions of the Protoplanetary Disk Around Ab Aurigae

Abstract: We report high-resolution 1.6 µm polarized intensity (P I) images of the circumstellar disk around the Herbig Ae star AB Aur at a radial distance of 22 AU (0. ′′ 15) up to 554 AU (3. ′′ 85),

Cited by 222 publications

References 35 publications

High-Contrast Near-Infrared Imaging Polarimetry of the Protoplanetary Disk Around Ry Tau

High-Contrast Near-Infrared Imaging Polarimetry of the Protoplanetary Disk Around Ry Tau

Complex Spiral Structure in the HD 100546 Transitional Disk as Revealed by GPI and MagAO

CHARIS science: performance simulations for the Subaru Telescope's third-generation of exoplanet imaging instrumentation

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