Seeds Adaptive Optics Imaging of the Asymmetric Transition Disk Oph Irs 48 in Scattered Light

Follette, Katherine B.; Grady, C. A.; Swearingen, Jeremy R.; Sitko, Michael L.; Champney, Elizabeth H.; Marel, Nienke van der; Miki, Takami; Kuchner, Marc J.; Close, Laird M.; Muto, Takayuki; Mayama, Satoshi; McElwain, Michael W.; Fukagawa, Misato; Maaskant, K. M.; Min, M.; Russell, R. W.; Kudo, Tomoyuki; Kusakabe, Nobuhiko; Hashimoto, Jun; Abe, Lyu; Akiyama, Eiji; Brandner, W.; Brandt, Timothy D.; Carson, J.; Currie, Thayne; Egner, Sebastian; Feldt, M.; 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, G. R.; Kuzuhara, Masayuki; Kwon, Jungmi; Matsuo, Taro; Miyama, Shoken M.; Morino, Jun Ichi; Moro‐Martín, Amaya; Nishimura, Tetsuo; Pyo, Tae‐Soo; Serabyn, Eugene; Suenaga, Takuya; Shimada, Hiroshi; Suzuki, Ryuji; Takahashi, Yasuhiro; Takato, Naruhisa; Terada, Hiroshi; Thalmann, Christian; Tomono, Daigo; Turner, Edwin L.; Watanabe, Makoto; Wisniewski, John P.; Yamada, Tōru; Takami, Hideki; Usuda, Tomonori; Tamura, Motohide

doi:10.1088/0004-637x/798/2/132

Cited by 60 publications

(35 citation statements)

References 76 publications

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“…This morphology has been observed in a number of disks by comparing scattered light images (tracing µm-sized grains that are coupled to the gas well) and millimeter interferometric images (e.g., Garufi et al 2013;Tsukagoshi et al 2014;Follette et al 2015). More specifically, de Juan Ovelar et al (2013) simulated visible and millimeter images of disks with a cavity carved by planets with different masses and orbital radii.…”

Section: Cavity and Inner Rimmentioning

confidence: 90%

“…An additional possibility to keep in mind is that the polarized signal deriving from the disk surface is blended with the contribution from halo particles. Speculatively, this contribution may be significant in highly inclined systems as suggested by the notion that sharp, prominent features like spirals and annular gaps are hardly observed in polarized light from inclined disks (see, e.g., Hashimoto et al 2012;Takami et al 2013;Follette et al 2015;Thalmann et al 2015).…”

Section: Disk Interaction With Planet Bmentioning

confidence: 99%

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The SPHERE view of the planet-forming disk around HD 100546

Garufi

Quanz

Schmid

et al. 2016

A&A

122

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Context. The mechanisms governing planet formation are not fully understood. A new era of high-resolution imaging of protoplanetary disks has recently started, thanks to new instruments such as SPHERE, GPI, and ALMA. The planet formation process can now be directly studied by imaging both planetary companions embedded in disks and their effect on disk morphology. Aims. We image disk features that could be potential signs of planet-disk interaction with unprecedented spatial resolution and sensitivity. Two companion candidates have been claimed in the disk around the young Herbig Ae/Be star HD 100546. Thus, this object serves as an excellent target for our investigation of the natal environment of giant planets. Methods. We exploit the power of extreme adaptive optics operating in conjunction with the new high-contrast imager SPHERE to image HD 100546 in scattered light. We obtained the first polarized light observations of this source in the visible (with resolution as fine as 2 AU) and new H and K band total intensity images that we analyzed with the  package.Results. The disk shows a complex azimuthal morphology, where multiple scattering of photons most likely plays an important role. High brightness contrasts and arm-like structures are ubiquitous in the disk. A double-wing structure (partly due to angular differential imaging processing) resembles a morphology newly observed in inclined disks. Given the cavity size in the visible (11 AU), the CO emission associated to the planet candidate c might arise from within the circumstellar disk. We find an extended emission in the K band at the expected location of b. The surrounding large-scale region is the brightest in scattered light. There is no sign of any disk gap associated to b.

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Section: Cavity and Inner Rimmentioning

confidence: 90%

Section: Disk Interaction With Planet Bmentioning

confidence: 99%

The SPHERE view of the planet-forming disk around HD 100546

Garufi

Quanz

Schmid

et al. 2016

A&A

122

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“…Instead, they will pile up around the vortex centre to form a ring structure. Such anti-correlation between small and big dust may be able to explain the discrepancy of azimuthal structure between submm and near-IR scattered light observations for Oph IR 48 (Follette et al 2015).…”

Section: Range Of Dust Sizesmentioning

confidence: 94%

Survival and structure of dusty vortices in protoplanetary discs

Crnkovic-Rubsamen

Zhu

Stone

2015

Monthly Notices of the Royal Astronomical Society

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We have studied the impact of dust feedback on the survival and structure of vortices in protoplanetary discs using 2-D shearing box simulations with Lagrangian dust particles. We consider dust with a variety of sizes (stopping time t s = 102 Ω −1 ), from fully coupled with the gas to the decoupling limit. We find that a vortex is destroyed by dust feedback when the total dust-to-gas mass ratio within the vortex is larger than 30-50%, independent of the dust size. The dust distribution can still be asymmetric in some cases after the vortex has been destroyed. With smaller amounts of dust, a vortex can survive for at least 100 orbits, and the maximum dust surface density within the vortex can be more than 100 times larger than the gas surface density, potentially facilitating planetesimal formation. On the other hand, in these stable vortices, small (t s < Ω −1 ) and large (t s Ω −1 ) dust grains concentrate differently and affect the gas dynamics in different ways. The distribution of large dust is more elongated than that of small dust. Large dust (t s Ω −1 ) concentrates in the centre of the vortex and feedback leads to turn-over in vorticity towards the centre, forming a quiescent region within an anticyclonic vortex. Such a turn-over is absent if the vortex is loaded with small grains. We demonstrate that, in protoplanetary discs where both large and small dust grains are present and under the right condition, the concentration of large dust towards the vortex centre can lead to a quiescent centre, repelling the small dust and forming a small dust ring around the vortex centre. Such anticorrelations between small and large dust within vortices may explain the discrepancy between ALMA and near-IR scattered light observations in the asymmetric region of transitional discs.

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“…Development of large millimeter interferometers and high-resolution NIR Adaptive Optics (AO) systems have since enabled resolved images of centrally cleared regions in transitional disks at both millimeter and NIR wavelengths. Evidence of ubiquitous disk asymmetries (e.g., van der Marel et al 2013;Follette et al 2015) and recent confirmation of embedded accreting objects in these disks Sallum et al 2015a) have lent significant fodder to the hypothesis that transitional disk cavities are a result of ongoing planet formation (Owen 2016), at least in some cases.…”

Section: Introductionmentioning

confidence: 99%

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

Follette

Rameau

Dong

et al. 2017

Self Cite

107

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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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Seeds Adaptive Optics Imaging of the Asymmetric Transition Disk Oph Irs 48 in Scattered Light

Cited by 60 publications

References 76 publications

The SPHERE view of the planet-forming disk around HD 100546

The SPHERE view of the planet-forming disk around HD 100546

Survival and structure of dusty vortices in protoplanetary discs

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

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