Millimeter imaging of HD 163296: probing the disk structure and kinematics

By Andrea Isella, L. Testi, A. Natta, R. Neri, D. Wilner, C. Qi. 2007

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We present new multi-wavelength millimeter interferometric observations of the Herbig Ae star HD 163296 obtained with the IRAM/PBI, SMA and VLA arrays both in continuum and in the 12 CO, 13 CO and C 18 O emission lines. Gas and dust properties have been obtained comparing the observations with self-consistent disk models for the dust and CO emission. The circumstellar disk is resolved both in the continuum and in CO. We find strong evidence that the circumstellar material is in Keplerian rotation around a central star of 2.6 $M_\odot$. The disk inclination with respect to the line of sight is 46° ± 4° with a position angle of 128° ± 4°. The slope of the dust opacity measured between 0.87 and 7 mm ( β = 1) confirms the presence of mm/cm-size grains in the disk midplane. The dust continuum emission is asymmetric and confined inside a radius of 200 AU while the CO emission extends up to 540 AU. The comparison between dust and CO temperature indicates that CO is present only in the disk interior. Finally, we obtain an increasing depletion of CO isotopomers from 12 CO to 13 CO and C 18 O. We argue that these results support the idea that the disk of HD 163296 is strongly evolved. In particular, we suggest that there is a strong depletion of dust relative to gas outside 200 AU; this may be due to the inward migration of large bodies that form in the outer disk or to clearing of a large gap in the dust distribution by a low mass companion.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/e686200c59e9f28a0f731ef7737a722853984b41

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Citations in the corpus

Gas and Dust Emission at the Outer Edge of Protoplanetary Disks (2008, background): “As Isella et al. (2007) demonstrate, the 2 discrepancy in outer radii derived from the dust and gas is not simply an issue of sensitivity; the observations were sufficiently sensitive to detect emission from the powerlaw dust disk if it did extend to the radius indicated by the CO emission.”
On the diversity and statistical properties of protostellar discs (2018, background): “…and dust are observed it is common for the radius 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…”
STRUCTURE AND EVOLUTION OF PRE-MAIN-SEQUENCE CIRCUMSTELLAR DISKS (2009, methodology): “This radius is in very good agreement with the gas extent inferred from the CO line emission but it is twice as large as the disk outer radius implied by the same observations if a power law surface density disk model is adopted (Isella et al. 2007).”
EMPIRICAL CONSTRAINTS ON TURBULENCE IN PROTOPLANETARY ACCRETION DISKS (2010, background): “TW Hya is a 10Myr-old transition disk with an inner cavity of ∼4AU radius, while HD 163296 is a primordial disk with an inner radius consistent with the expected ∼0.4AU extent of the dust destruction zone (see, e.g., Isella et al. 2007).”
PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS (2009, background): “…sensitivity and resolution have shown that this power-law+cut-off behavior yields inconsistent results for the location of Rout: the optically thin continuum emission indicates a significantly smaller Rout than the optically thick molecular line emission (Piétu et al. 2005; Isella et al. 2007).”
Protoplanetary Disks and Their Evolution (2011, background): “A curious problem arose in that the size of the gas disk, as observed in rotational lines of CO, was found to significantly exceed the size of the continuum image (Isella et al. 2007; Piétu, Guilloteau & Dutrey 2005).”
WEAK TURBULENCE IN THE HD 163296 PROTOPLANETARY DISK REVEALED BY ALMA CO OBSERVATIONS (2015, background): “Unless otherwise specified, we assume Mgas= 0.09Me (Isella et al. 2007).”
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.”
Unveiling the gas-and-dust disk structure in HD 163296 using ALMA observations (2013, methodology): “It is known that grain growth occurs in this disk, as reported by Isella et al. (2007) based on the slope of the dust opacity law in the interval 0.87−7 mm. Related to the inward migration, models predict the gas drag to be more efficient in intermediate sized dust particles, with small grains…”
ALMA Survey of Lupus Protoplanetary Disks. II. Gas Disk Radii (2018, background): “…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).”
Molecules with ALMA at Planet-forming Scales (MAPS). I. Program Overview and Highlights (2021, background): “HD 163296 is one of the most well-studied Herbig Ae star-disk system at millimeter wavelengths due to its relative proximity and massive disk; it is estimated to contain 0.1–0.5 M (Isella et al. 2007; Tilling et al. 2012; Muro-Arena et al. 2018; Powell et al. 2019; Kama et al. 2020).”
THE TW Hya DISK AT 870 μm: COMPARISON OF CO AND DUST RADIAL STRUCTURES (2011, unknown): “A few studies used simple models to fit the millimeter continuum (dust) and CO line (gas) emission independently, finding inconsistent structures where the dust is much more compact than the gas (Piétu et al. 2005; Isella et al. 2007).”
A Three-dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk Using DCO+ (2017, methodology): “SMA observations of the 1.3mm continuum by Isella et al. (2007) measure a flux of 705 ± 12 mJy.”
A SPATIALLY RESOLVED VERTICAL TEMPERATURE GRADIENT IN THE HD 163296 DISK (2013, methodology): “Note that the asymmetries in the 12CO J = 3–2 line emission effectively resolve the absolute disk spin orientation (Piétu et al. 2007), so our P.A. and inclinations differ by ∼180◦ from the models presented by Isella et al. (2007) and Qi et al. (2011).”