Dust properties across the CO snowline in the HD 163296 disk from ALMA and VLA observations

Guidi, Greta; Tazzari, Marco; Testi, L.; Gregorio-Monsalvo, I. de; Chandler, C. J.; Pérez, Laura; Isella, Andrea; Natta, A.; Ortolani, S.; Henning, Thomas; Corder, Stuartt; Linz, H.; Andrews, Sean M.; Wilner, David J.; Ricci, Luca; Carpenter, John M.; Sargent, Anneila I.; Mundy, Lee G.; Storm, Shaye; Calvet, Nuria; Dullemond, C. P.; Greaves, J. S.; Lazio, Joseph; Deller, Adam T.; Kwon, Woojin

doi:10.1051/0004-6361/201527516

Cited by 58 publications

(65 citation statements)

References 62 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…, so we assumed uniform priors from 0-10 au and 10-20 au, with the probability of h 10 au 0 > equal to one-third of the probability of h 10 au 0 < We also assumed a constant dust opacity throughout the disk. Previous multi-wavelength studies of disks at millimeter and centimeter wavelengths suggested radial variations in dust opacity due to grain growth (Isella et al 2010a; Banzatti Guilloteau et al 2011;Pérez et al 2012Pérez et al , 2015Trotta et al 2013;Menu et al 2014;ALMA Partnership et al 2015;Guidi et al 2016;Tazzari et al 2016). Similar radial variations may be present in our Upper Sco disks, and, in fact, are predicted by models of dust transport and evolution (e.g., Dullemond & Dominik 2005;Birnstiel et al 2010).…”

Section: Continuum Modelingsupporting

confidence: 85%

Measurement of Circumstellar Disk Sizes in the Upper Scorpius OB Association with ALMA

Barenfeld

Carpenter

Sargent

et al. 2017

ApJ

100

144

View full text Add to dashboard Cite

We present detailed modeling of the spatial distributions of gas and dust in 57 circumstellar disks in the Upper Scorpius OB Association observed with ALMA at submillimeter wavelengths. We fit power-law models to the dust surface density and CO J=3-2 surface brightness to measure the radial extent of dust and gas in these disks. We found that these disks are extremely compact: the 25 highest signal-to-noise disks have a median dust outer radius of 21 au, assuming an R 1 -dust surface density profile. Our lack of CO detections in the majority of our sample is consistent with these small disk sizes assuming the dust and CO share the same spatial distribution. Of seven disks in our sample with well-constrained dust and CO radii, four appear to be more extended in CO, although this may simply be due to the higher optical depth of the CO. Comparison of the Upper Sco results with recent analyses of disks in Taurus, Ophiuchus, and Lupus suggests that the dust disks in Upper Sco may be approximately three times smaller in size than their younger counterparts, although we caution that a more uniform analysis of the data across all regions is needed. We discuss the implications of these results for disk evolution.

show abstract

Section: Continuum Modelingsupporting

confidence: 85%

Measurement of Circumstellar Disk Sizes in the Upper Scorpius OB Association with ALMA

Barenfeld

Carpenter

Sargent

et al. 2017

ApJ

100

144

View full text Add to dashboard Cite

show abstract

“…Previous ALMA observations showed that the continuum emission has a local maximum at about 90 A.U. [24], suggesting a dusty ring at a distance that corresponds to the frost line for CO molecules [25]. Recently, we have imaged the HD 163296 disk with ALMA at 0.2 00 angular resolution, a factor of 3 higher than previous observations and corresponding to a physical scale of 25 A.U.…”

mentioning

confidence: 82%

Ringed Structures of the HD 163296 Protoplanetary Disk Revealed by ALMA

et al. 2016

View full text Add to dashboard Cite

We present Atacama Large Millimeter and Submillimeter Array observations of the protoplanetary disk around the Herbig Ae star HD 163296 that trace the spatial distribution of millimeter-sized particles and cold molecular gas on spatial scales as small as 25 astronomical units (A.U.). The image of the disk recorded in the 1.3 mm continuum emission reveals three dark concentric rings that indicate the presence of dust depleted gaps at about 60, 100, and 160 A.U. from the central star. The maps of the 12 CO, 13 CO, and C 18 O J ¼ 2 − 1 emission do not show such structures but reveal a change in the slope of the radial intensity profile across the positions of the dark rings in the continuum image. By comparing the observations with theoretical models for the disk emission, we find that the density of CO molecules is reduced inside the middle and outer dust gaps. However, in the inner ring there is no evidence of CO depletion. From the measurements of the dust and gas densities, we deduce that the gas-to-dust ratio varies across the disk and, in particular, it increases by at least a factor 5 within the inner dust gap compared to adjacent regions of the disk. The depletion of both dust and gas suggests that the middle and outer rings could be due to the gravitational torque exerted by two Saturn-mass planets orbiting at 100 and 160 A.U. from the star. On the other hand, the inner dust gap could result from dust accumulation at the edge of a magnetorotational instability dead zone, or from dust opacity variations at the edge of the CO frost line. Observations of the dust emission at higher angular resolution and of molecules that probe dense gas are required to establish more precisely the origins of the dark rings observed in the HD 163296 disk.

show abstract

“…It is expected that the small dust grains seen in scattered light should be well-coupled with the gas for young disks, suggesting that the use of this surface density distribution is justified here. (See also the recent work by Guidi et al 2016 andPohl et al 2017 for HD 163296 and T Cha, respectively). The scale height is also defined as a power law in radius by…”

Section: Radiative Transfer Modeling With Mcfostmentioning

confidence: 95%

Hubble Space Telescope Scattered-light Imaging and Modeling of the Edge-on Protoplanetary Disk ESO-Hα 569

Wolff

Perrin

Stapelfeldt

et al. 2017

ApJ

View full text Add to dashboard Cite

We present new Hubble Space Telescope (HST) Advanced Camera for Surveys observations and detailed models for a recently discovered edge-on protoplanetary disk around ESO-Hα569 (a low-mass T Tauri star in the Cha I star-forming region). Using radiative transfer models, we probe the distribution of the grains and overall shape of the disk (inclination, scale height, dust mass, flaring exponent, and surface/volume density exponent) by model fitting to multiwavelength (F606W and F814W) HST observations together with a literature-compiled spectral energy distribution. A new tool set was developed for finding optimal fits of MCFOST radiative transfer models using the MCMC code emcee to efficiently explore the high-dimensional parameter space. It is able to selfconsistently and simultaneously fit a wide variety of observables in order to place constraints on the physical properties of a given disk, while also rigorously assessing the uncertainties in those derived properties. We confirm that ESO-Hα569 is an optically thick nearly edge-on protoplanetary disk. The shape of the disk is well-described by a flared disk model with an exponentially tapered outer edge, consistent with models previously advocated on theoretical grounds and supported by millimeter interferometry. The scattered-light images and spectral energy distribution are best fit by an unusually high total disk mass (gas+dust assuming a ratio of 100:1) with a disk-tostar mass ratio of 0.16.

show abstract

Dust properties across the CO snowline in the HD 163296 disk from ALMA and VLA observations

Cited by 58 publications

References 62 publications

Measurement of Circumstellar Disk Sizes in the Upper Scorpius OB Association with ALMA

Measurement of Circumstellar Disk Sizes in the Upper Scorpius OB Association with ALMA

Ringed Structures of the HD 163296 Protoplanetary Disk Revealed by ALMA

Hubble Space Telescope Scattered-light Imaging and Modeling of the Edge-on Protoplanetary Disk ESO-Hα 569

Contact Info

Product

Resources

About