Disks around T Tauri Stars with SPHERE (DARTTS-S). I. SPHERE/IRDIS Polarimetric Imaging of Eight Prominent T Tauri Disks*

Avenhaus, H.; Quanz, Sascha P.; Garufi, A.; Pérez, Sebastián; Casassus, S.; Pinte, C.; Bertrang, Gesa H.-M.; Cáceres, C.; Benisty, M.; Dominik, C.

doi:10.3847/1538-4357/aab846

Cited by 352 publications

(484 citation statements)

References 123 publications

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“…Such structures were indeed detected in a growing sample of disks in mmemission as well as in optical and near infrared scattered light (see e.g. Andrews et al 2018;Avenhaus et al 2018 for recent Based on observations performed with SPHERE/VLT under program ID 1100.C-0481(Q). examples).…”

Section: Introductionmentioning

confidence: 89%

Spirals inside the millimeter cavity of transition disk SR 21

Muro-Arena

Ginski

Dominik

et al. 2020

A&A

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Context. Hydrodynamical simulations of planet-disk interactions suggest that planets may be responsible for a number of the substructures frequently observed in disks in both scattered light and dust thermal emission. Despite the ubiquity of these features, direct evidence of planets embedded in disks and of the specific interaction features like spiral arms within planetary gaps still remain rare. Aims. In this study we discuss recent observational results in the context of hydrodynamical simulations in order to infer the properties of a putative embedded planet in the cavity of a transition disk. Methods. We imaged the transition disk SR 21 in H-band in scattered light with SPHERE/IRDIS and in thermal dust emission with ALMA band 3 (3 mm) observations at a spatial resolution of 0.1 . We combine these datasets with existing band 9 (430 µm) and band 7 (870 µm) ALMA continuum data. Results. The Band 3 continuum data reveals a large cavity and a bright ring peaking at 53 au strongly suggestive of dust trapping. The ring shows a pronounced azimuthal asymmetry, with a bright region in the north-west that we interpret as a dust over-density. A similarly-asymmetric ring is revealed at the same location in polarized scattered light, in addition to a set of bright spirals inside the mm cavity and a fainter spiral bridging the gap to the outer ring. These features are consistent with a number of previous hydrodynamical models of planet-disk interactions, and suggest the presence of a ∼1 M Jup planet at 44 au and PA=11deg. This makes SR21 the first disk showing spiral arms inside the mm cavity, as well as one for which the location of a putative planet can be precisely inferred. Conclusions. SR 21's main features in both scattered light and thermal emission are consistent with hydrodynamical predictions of planet-disk interactions. With the location of a possible planet being well-constrained by observations, it is an ideal candidate for follow-up observations to search for direct evidence of a planetary companion still embedded in its disk.

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Section: Introductionmentioning

confidence: 89%

Spirals inside the millimeter cavity of transition disk SR 21

Muro-Arena

Ginski

Dominik

et al. 2020

A&A

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“…3.1. To take into account the vertical origin of the molecular emission with simple geometrical considerations, we followed a technique commonly used by the near-IR community (de Boer et al 2016;Avenhaus et al 2018) that exploits the apparent displacement from the center of any ring raised above the midplane. We superimposed the shape of projected circular rings, varying their different vertical locations until the match with the observed shift between molecular and continuum emission was reached.…”

Section: Radial Distribution Of Dust and Gas Emissionmentioning

confidence: 99%

“…However, the millimeter observations by Guilloteau et al (2011) constrained the disk inclination to only ∼ 65 • , implying that the disk opening angle for small particles in the outer regions is larger than 90 • − 65 • = 25 • . In several Class II sources with more inclined disks, the star is not obscured by the disk (see, e.g., Pohl et al 2017;Langlois et al 2018;Avenhaus et al 2018). This implies that the earlytype SED of DG Tau B is due to its young evolutionary stage and not by a coincidental alignment of disk and line of sight.…”

Section: Introductionmentioning

confidence: 97%

“…The morphological characterization of dust grains in protoplanetary disks is much more advanced than that of molecular species. In fact, high-resolution images at either near-IR or (sub)millimeter wavelengths are currently available for more than a hundred sources (e.g., Garufi et al 2017;Avenhaus et al 2018;Andrews et al 2018;Long et al 2018). The vast majority of these objects are Class II sources (following Lada 1987), namely stars older than ∼1 Myr that are visible at optical wavelengths and show a spectral energy distribution (SED) composed of a stellar blackbody plus a substantial IR excess from the surrounding disk.…”

Section: Introductionmentioning

confidence: 99%

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ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT)

Garufi

Podio

Codella

et al. 2020

A&A

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The chemical composition of planets is determined by the distribution of the various molecular species in the protoplanetary disk at the time of their formation. To date, only a handful of disks have been imaged in multiple spectral lines with high spatial resolution. As part of a small campaign devoted to the chemical characterization of disk-outflow sources in Taurus, we report on new ALMA Band 6 (∼1.3 mm) observations with ∼0.15 (20 au) resolution toward the embedded young star DG Tau B. Images of the continuum emission reveals a dust disk with rings and, putatively, a leading spiral arm. The disk, as well as the prominent outflow cavities, are detected in CO, H 2 CO, CS, and CN; instead, they remain undetected in SO 2 , HDO, and CH 3 OH. From the absorption of the back-side outflow, we inferred that the disk emission is optically thick in the inner 50 au. This morphology explains why no line emission is detected from this inner region and poses some limitations toward the calculation of the dust mass and the characterization of the inner gaseous disk. The H 2 CO and CS emission from the inner 200 au is mostly from the disk, and their morphology is very similar. The CN emission significantly differs from the other two molecules as it is observed only beyond 150 au. This ring-like morphology is consistent with previous observations and the predictions of thermochemical disk models. Finally, we constrained the disk-integrated column density of all molecules. In particular, we found that the CH 3 OH/H 2 CO ratio must be smaller than ∼2, making the methanol non-detection still consistent with the only such ratio available from the literature (1.27 in TW Hya).

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“…VLT/SPHERE is a HCI system that has discovered two confirmed planets: HIP 65426b (Chauvin, G. et al 2017) and PDS 70b (Keppler et al 2018). It has also discovered a vast array of debris, protoplanetary, and circumstellar disks (e.g., Avenhaus et al 2018;Sissa, E. et al 2018). Operating with a tip/tilt deformable mirror (TTDM), a 41-by-41 high order deformable mirror (HODM), and a Shack-Hartmann wavefront sensor (SHWFS) sampling at 1380 Hz, the XAO system of VLT/SPHERE, SAXO delivers Strehl ratios greater than 90 % in the H band (Beuzit et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Robustness of prediction for extreme adaptive optics systems under various observing conditions

Kooten

Doelman

Kenworthy

2020

A&A

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Context. For high-contrast imaging (HCI) systems, such as VLT/SPHERE, the performance of the system at small angular separations is contaminated by the wind-driven halo in the science image. This halo is a result of the servo-lag error in the adaptive optics (AO) system due to the finite time between measuring the wavefront phase and applying the phase correction. One approach to mitigating the servo-lag error is predictive control. Aims. We aim to estimate and understand the potential on-sky performance that linear data-driven prediction would provide for VLT/SPHERE under various turbulence conditions. Methods. We used a linear minimum mean square error predictor and applied it to 27 different AO telemetry data sets from VLT/SPHERE taken over many nights under various turbulence conditions. We evaluated the performance of the predictor using residual wavefront phase variance as a performance metric. Results. We show that prediction always results in a reduction in the temporal wavefront phase variance compared to the current VLT/SPHERE AO performance. We find an average improvement factor of 5.1 in phase variance for prediction compared to the VLT/SPHERE residuals. When comparing to an idealised VLT/SPHERE, we find an improvement factor of 2.0. Under our 27 different cases, we find the predictor results in a smaller spread of the residual temporal phase variance. Finally, we show there is no benefit to including spatial information in the predictor in contrast to what might have been expected from the frozen flow hypothesis. A purely temporal predictor is best suited for AO on VLT/SPHERE. Conclusions. Linear prediction leads to a significant reduction in phase variance for VLT/SPHERE under a variety of observing conditions and reduces the servo-lag error. Furthermore, prediction improves the reliability of the AO system performance, making it less sensitive to different conditions.

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Disks around T Tauri Stars with SPHERE (DARTTS-S). I. SPHERE/IRDIS Polarimetric Imaging of Eight Prominent T Tauri Disks*

Cited by 352 publications

References 123 publications

Spirals inside the millimeter cavity of transition disk SR 21

Spirals inside the millimeter cavity of transition disk SR 21

ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT)

Robustness of prediction for extreme adaptive optics systems under various observing conditions

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