Unveiling the gas-and-dust disk structure in HD 163296 using ALMA observations

By I. Gregorio-Monsalvo, F. Ménard, W. Dent, C. Pinte, C. L'opez, P. Klaassen, A. Hales, P. Cortés, M. Rawlings, K. Tachihara and 13 more. 2013

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Aims. The aim of this work is to study the structure of the protoplan etary disk surrounding the Herbig Ae star HD 163296. Methods. We have used high-resolution and high-sensitivity ALMA observations of the CO(3‐2) emission line and the continuum at 850µm, as well as the 3- dimensional radiative transfer code MCFOST to model the data presented in this work. Results. The CO(3‐2) emission unveils for the first time at sub-millim eter frequencies the vertical structure details of a gaseou s disk in Keplerian rotation, showing the back- and the front-side of a flared disk. Continuum emission at 850 µm reveals a compact dust disk with a 240 AU outer radius and a surface brightness profil e that shows a very steep decline at radius larger than 125 AU. The gaseous disk is more than two times larger than the dust disk, with a similar critical radius but with a shallower radial pr ofile. Radiative transfer models of the continuum data confirms the need for a s harp outer edge to the dust disk. The models for the CO(3‐2) channel map require the disk to be slightly more geometrically thick than previous models suggested, and that the temperature at which CO gas becomes depleted (frozen-out) from the outer regions of the disk midplane is T < 20 K, in agreement with previous studies.

Subfields: Astronomy and Astrophysics, Spectroscopy

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Citations in the corpus

A millimeter Continuum Size–Luminosity Relationship for Protoplanetary Disks (2017, methodology): “…Definition High quality observations of disk continuum emission have previously been modeled with “broken power-law” (e.g., Andrews et al. 2012; de Gregorio-Monsalvo et al. 2013; Hogerheijde et al. 2016) or “similarity solution” 0.1 1 % / arcsec 5 4 3 2 1 0 1 lo g I ν (% ) / J y a rc se c−…”
Direct mapping of the temperature and velocity gradients in discs Imaging the vertical CO snow line around IM Lupi (2017, background): “While already suggested by previous ALMA observations (e.g. de Gregorio-Monsalvo et al. 2013; Rosenfeld et al. 2013, for HD 163296), this is the first direct, model-independent measurement of the altitude of the CO layers.”
Molecules with ALMA at Planet-forming Scales (MAPS). I. Program Overview and Highlights (2021, background): “…SMA, and ALMA projects (e.g., Thi et al. 2004; Qi et al. 2011; Öberg et al. 2011b; Rosenfeld et al. 2013; Klaassen et al. 2013; Mathews et al. 2013; de Gregorio-Monsalvo et al. 2013; Flaherty et al. 2015; Huang et al. 2017; Salinas et al. 2017; Guzmán et al. 2018; Booth et al. 2019; Bergner et…”
Kinematic Evidence for an Embedded Protoplanet in a Circumstellar Disk (2018, background): “…not as obvious in the Band 7 Early-Science data due to the limited spatial resolution, the deformation of the isovelocity curve is present and could already be seen, with the benefit of hindsight from our Band 6 detection, in de Gregorio-Monsalvo et al. (2013) and Rosenfeld et al. (2013, their Fig.”
On the diversity and statistical properties of protostellar discs (2018, background): “…of the gas disc to be larger than that of the (sub-)mm dust disc (e.g. Piétu et al. 2007, 2014; Isella et al. 2007; Panić et al. 2009; Andrews et al. 2012; Rosenfeld et al. 2013; de Gregorio-Monsalvo et al. 2013; Walsh et al. 2014; Pineda et al. 2014; Cleeves et al. 2016; Barenfeld et al. 2017).”
Turbulence in the TW Hya Disk (2018, background): “Recent ALMA observations have spatially resolved the CO molecular layers within the disks around HD 163296 (Rosenfeld et al. 2013; de Gregorio-Monsalvo et al. 2013), HD 34282 (van 10 der Plas et al. 2017), IM Lup (Pinte et al. 2018), and the edge-on ’Flying Saucer’ (Dutrey et al. 2017) supporting…”
On planet formation in HL Tau (2015, result): “…et al. 2007; Kwon et al. 2011, 2015), these assume that the dust is co-located with the gas, whereas we expect settling and radial inward migration to produce a more compact dust disc, consistent with observations in other systems (Andrews et al. 2012; de Gregorio-Monsalvo et al. 2013).”
Accretion disks in luminous young stellar objects (2015, background): “…couple of 100s of au in radius (Guilloteau et al., 2013) and they are often found to be in Keplerian rotation, allowing dynamical estimates of the central star mass (e.g. for MWC 480 and HD 163296: Simon et al., 2001; Isella et al., 2007; Qi et al., 2013; de Gregorio-Monsalvo et al., 2013; see Fig.”
Dust Evolution and the Formation of Planetesimals (2016, background): “…revealed radial variations in the dust-to-gas ratio in several disks (e.g., Panić et al. 2009; Andrews et al. 2012; Isella et al. 2012; de Gregorio-Monsalvo et al. 2013; Rosenfeld et al. 2013) and resolved multi-wavelength observations indicate also radial variations in the dust…”
ALMA Survey of Lupus Protoplanetary Disks. II. Gas Disk Radii (2018, methodology): “…effects (Guilloteau & Dutrey 1998; Facchini et al. 2017), can also make the dust disk appear smaller than the gas disk at sub-mm/mm wavelengths, as seen for several individual disks (Isella et al. 2007; Panić et al. 2009; Andrews et al. 2012; de Gregorio-Monsalvo et al. 2013; Cleeves et al. 2016).”
WEAK TURBULENCE IN THE HD 163296 PROTOPLANETARY DISK REVEALED BY ALMA CO OBSERVATIONS (2015, methodology): “…both the dust and the gas (Hughes et al. 2008) including the different apparent radii for the gas and dust disk, although recent evidence suggests that in some systems the dust disks are smaller than the gaseous component (Andrews et al. 2012; de Gregorio-Monsalvo et al. 2013; Walsh et al. 2014).”
A Three-dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk Using DCO+ (2017, background): “De Gregorio-Monsalvo et al. (2013) are also able to reproduce much of the CO emission with an irradiated disk model.”
The Disk Substructures at High Angular Resolution Project (DSHARP). I. Motivation, Sample, Calibration, and Overview (2018, background): “…line emission have led to suggestions that the mass ratio of solids relative to gas also varies with radius (higher closer to the star; Panić et al. 2009; Andrews et al. 2012; de Gregorio-Monsalvo et al. 2013; Rosenfeld et al. 2013; Zhang et al. 2014; Facchini et al. 2017; Ansdell et al. 2018).”
ALMA unveils rings and gaps in the protoplanetary system HD 169142: signatures of two giant protoplanets (2017, background): “This dichotomy is also observed in other systems that are observed at high angular resolution, such as LkCa 15 (Isella et al. 2012), HD 163296 (de Gregorio-Monsalvo et al. 2013), HD 100546 (Walsh et al. 2014), and HD 97048 (Walsh et al. 2016; van der Plas et al. 2017).”