Resolving the Gap and Au-Scale Asymmetries in the Pre-Transitional Disk of V1247 Orionis

Kraus, Stefan; Ireland, Michael; Sitko, Michael L.; Monnier, John D.; Calvet, Nuria; Espaillat, Catherine; Grady, C. A.; Harries, Tim J.; Hönig, S. F.; Russell, R. W.; Swearingen, Jeremy R.; Werren, Chelsea; Wilner, David J.

doi:10.1088/0004-637x/768/1/80

Cited by 47 publications

(90 citation statements)

References 81 publications

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“…Kraus et al (2013) analysed the (pre-)transitional disk V1247 Ori, a source that is relatively similar to HD 135344B. To fit V1247 Ori near-IR and mid-IR interferometry data, Kraus et al suggest a disk structure where the innermost disk is composed of a mixture of carbon (50%) and silicate (50%) grains at 0.19 < R < 0.34 AU, and a mass of 10 −7 M carbon dust grains inside 0.3 < R < 46 AU.…”

Section: Discussionmentioning

confidence: 99%

“…This suggests that what is observed is likely a change in the dust size distribution inside the cavity . Near-IR interferometry provides evidence of dust emission (and inhomogeneities) inside the dust cavity of transition disks (e.g., Kraus et al 2013). Furthermore, recent ALMA observations have spatially resolved gas inside the cavity of transition disks (Casassus et al 2013;Bruderer et al 2013).…”

Section: Introductionmentioning

confidence: 99%

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Constraining the structure of the transition disk HD 135344B (SAO 206462) by simultaneous modeling of multiwavelength gas and dust observations

Carmona

Pinte

Thi

et al. 2014

A&A

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Context. Constraining the gas and dust disk structure of transition disks, particularly in the inner dust cavity, is a crucial step toward understanding the link between them and planet formation. HD 135344B is an accreting (pre-)transition disk that displays the CO 4.7 µm emission extending tens of AU inside its 30 AU dust cavity. Aims. We constrain HD 135344B's disk structure from multi-instrument gas and dust observations. Methods. We used the dust radiative transfer code MCFOST and the thermochemical code ProDiMo to derive the disk structure from the simultaneous modeling of the spectral energy distribution (SED), VLT/CRIRES CO P(10) 4.75 µm, Herschel/PACS [O ] 63 µm, Spitzer/IRS, and JCMT 12 CO J = 3−2 spectra, VLTI/PIONIER H-band visibilities, and constraints from (sub-)mm continuum interferometry and near-IR imaging. Results. We found a disk model able to describe the current gas and dust observations simultaneously. This disk has the following structure. (1) To simultaneously reproduce the SED, the near-IR interferometry data, and the CO ro-vibrational emission, refractory grains (we suggest carbon) are present inside the silicate sublimation radius (0.08 < R < 0.2 AU). (2) The dust cavity (R < 30 AU) is filled with gas, the surface density of the gas inside the cavity must increase with radius to fit the CO ro-vibrational line profile, a small gap of a few AU in the gas distribution is compatible with current data, and a large gap of tens of AU in the gas does not appear likely. (4) The gas-to-dust ratio inside the cavity is >100 to account for the 870 µm continuum upper limit and the CO P(10) line flux.(5) The gas-to-dust ratio in the outer disk (30 < R < 200 AU) is <10 to simultaneously describe the [O ] 63 µm line flux and the CO P(10) line profile. (6) In the outer disk, most of the gas and dust mass should be located in the midplane, and a significant fraction of the dust should be in large grains. Conclusions. Simultaneous modeling of the gas and dust is required to break the model degeneracies and constrain the disk structure. An increasing gas surface density with radius in the inner cavity echoes the effect of a migrating jovian planet in the disk structure. The low gas mass (a few Jupiter masses) throughout the HD 135344B disk supports the idea that it is an evolved disk that has already lost a large portion of its mass.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Constraining the structure of the transition disk HD 135344B (SAO 206462) by simultaneous modeling of multiwavelength gas and dust observations

Carmona

Pinte

Thi

et al. 2014

A&A

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“…The NIRC2 data were reduced using the pipeline described previously in and Kraus et al (2013), providing calibrated closure phases. In order to record the instrument transfer function, we bracketed the science star observations with observations of two unresolved calibrators.…”

Section: Observationsmentioning

confidence: 99%

“…Notes. Column 1: Target; Column 2: Association; Column 3: Distance; Column 4: Spectral Type; Column 5: Visual Extinction; Column 6: Effective Temperature; Column 7: Stellar Mass; Column 8: Stellar Luminosity; Column 9: Stellar Radius; Column 10: Literature References: (1) Bouvier & Appenzeller (1992), (2) Kenyon et al (1998), (9) Kraus et al (2013), (10) Loinard et al (2008), (11) Merín et al (2010), (12) Reipurth et al (1996), (13) We expect no significant asymmetric signal within these stars so use them to form a crude test statistic for our threshold of 4σ. Fitting a poisson distribution we find a confidence level of 88% for a 4σ and more than 95% for 4.5σ.…”

Section: Binary Model Approachmentioning

confidence: 99%

Sparse aperture masking interferometry survey of transitional discs

Willson

Kraus

Kluska

et al. 2016

A&A

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Context. Transitional discs are a class of circumstellar discs around young stars with extensive clearing of dusty material within their inner regions on 10s of au scales. One of the primary candidates for this kind of clearing is the formation of planet(s) within the disc that then accrete or clear their immediate area as they migrate through the disc. Aims. The goal of this survey was to search for asymmetries in the brightness distribution around a selection of transitional disc targets. We then aimed to determine whether these asymmetries trace dynamically-induced structures in the disc or the gap-opening planets themselves. Methods. Our sample included eight transitional discs. Using the Keck/NIRC2 instrument we utilised the Sparse Aperture Masking (SAM) interferometry technique to search for asymmetries indicative of ongoing planet formation. We searched for close-in companions using both model fitting and interferometric image reconstruction techniques. Using simulated data, we derived diagnostics that helped us to distinguish between point sources and extended asymmetric disc emission. In addition, we investigated the degeneracy between the contrast and separation that appear for marginally resolved companions. Results. We found FP Tau to contain a previously unseen disc wall, and DM Tau, LkHα330, and TW Hya to contain an asymmetric signal indicative of point source-like emission. We placed upper limits on the contrast of a companion in RXJ1842.9-3532 and V2246 Oph. We ruled the asymmetry signal in RXJ1615.3-3255 and V2062 Oph to be false positives. In the cases where our data indicated a potential companion we computed estimates for the value of M cṀc and found values in the range of 10 −5 − 10 −3 M 2 J yr −1 . Conclusions. We found significant asymmetries in four targets. Of these, three were consistent with companions. We resolved a previously unseen gap in the disc of FP Tau extending inwards from approximately 10 au.

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“…During our two pointings on TYC 8241 2652 1, we recorded a total of 1110 interferograms with a detector integration time of 1 s. The on-source observations were interlayed with observations on the calibrator star HD 105316 to calibrate instrumental closure phase effects. The NACO data were reduced using our data reduction pipeline that was already used in various earlier studies (e.g., Ireland & Kraus 2008;Kraus & Ireland 2012;Kraus et al 2013), providing absolute calibrated visibilities and closure phases.…”

Section: Vlt/naco Sparse Aperture Masking Interferometrymentioning

confidence: 99%