ALMA SURVEY OF LUPUS PROTOPLANETARY DISKS. I. DUST AND GAS MASSES

By M. Ansdell, Jonathan P. Williams, N. Marel, J. Carpenter, G. Guidi, M. Hogerheijde, G. Mathews, C. Manara, A. Miotello, A. Natta and 5 more. 2016

336 citations recorded by the source corpus.

We present the first high-resolution sub-millimeter survey of both dust and gas for a large population of protoplanetary disks. Characterizing fundamental properties of protoplanetary disks on a statistical level is critical to understanding how disks evolve into the diverse exoplanet population. We use the Atacama Large Millimeter/Submillimeter Array (ALMA) to survey 89 protoplanetary disks around stars with in the young (1–3 Myr), nearby (150–200 pc) Lupus complex. Our observations cover the 890 μm continuum and the 13CO and C18O 3–2 lines. We use the sub-millimeter continuum to constrain to a few Martian masses (0.2–0.4 M⊕) and the CO isotopologue lines to constrain to roughly a Jupiter mass (assuming an interstellar medium (ISM)-like abundance). Of 89 sources, we detect 62 in continuum, 36 in 13CO, and 11 in C18O at significance. Stacking individually undetected sources limits their average dust mass to Lunar masses (0.03 M⊕), indicating rapid evolution once disk clearing begins. We find a positive correlation between and M*, and present the first evidence for a positive correlation between and M*, which may explain the dependence of giant planet frequency on host star mass. The mean dust mass in Lupus is 3× higher than in Upper Sco, while the dust mass distributions in Lupus and Taurus are statistically indistinguishable. Most detected disks have and gas-to-dust ratios , assuming an ISM-like abundance; unless CO is very depleted, the inferred gas depletion indicates that planet formation is well underway by a few Myr and may explain the unexpected prevalence of super-Earths in the exoplanet population.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/77323849055ec9bfa0300c29dcc6f3aeea0f544a

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Citations in the corpus

A millimeter Continuum Size–Luminosity Relationship for Protoplanetary Disks (2017, background): “…et al. 2016), environment (Jensen et al. 1994, 1996; Harris et al. 2012; Akeson & Jensen 2014; Mann & Williams 2009, 2010; Mann et al. 2014), and stellar host mass (Andrews et al. 2013; Mohanty et al. 2013; Carpenter et al. 2014; Ansdell et al. 2016; Barenfeld et al. 2016; Pascucci et al. 2016).”
X-shooter spectroscopy of young stellar objects in Lupus (2017, background): “2-392302 has a most probable transitional disk (see Ansdell et al. 2016; Alcalá et al. 2017 for details).”
The Disk Substructures at High Angular Resolution Project (DSHARP). II. Characteristics of Annular Substructures (2018, methodology): “Dust disk radii To assess how substructure characteristics relate to disk size, we also compute the radius of the millimeter disk, Rdust, for each source using a “curve-of-growth”type method similar to that described in Ansdell et al. (2016).”
The Disk Substructures at High Angular Resolution Project (DSHARP). I. Motivation, Sample, Calibration, and Overview (2018, background): “′′3) resolution for selection (Andrews et al. 2009, 2010; Ansdell et al. 2016; Barenfeld et al. 2016).”
Why do protoplanetary disks appear not massive enough to form the known exoplanet population? (2018, methodology): “Finally, the disk masses are obtained by rescaling the disk masses reported by Ansdell et al. (2016) and Pascucci et al. (2016) for the new distances, and are reported in Col. 5 of Tables A.1 and A.2.”
A STEEPER THAN LINEAR DISK MASS–STELLAR MASS SCALING RELATION (2016, background): “…using rotational lines from CO isotopologues have claimed gas-to-dust ratios well below the ISM value in young disks (Williams & Best 2014; Ansdell et al. 2016), detailed physico-chemical disk models need to be carried out to properly account for isotope-selective processes (Miotello et…”
An ALMA Survey of Protoplanetary Disks in the σ Orionis Cluster (2017, methodology): “…2 01 7 2 Recent observations suggest that the inherited ISM ratio may actually decrease by an order of magnitude after just a few Myr of evolution (Williams & Best 2014; Ansdell et al. 2016), although these calculations may be underestimated due to carbon depletion (e.g., Miotello et al. 2016b).”
One Solution to the Mass Budget Problem for Planet Formation: Optically Thick Disks with Dust Scattering (2019, background): “The mean mass is ∼15 M⊕ for Lupus (Ansdell et al. 2016), Taurus (Andrews et al. 2013), and Ophiuchus (Cieza et al. 2019) young ar X iv :1 90 4.”
On the diversity and statistical properties of protostellar discs (2018, methodology): “In Lupus, Tazzari et al. (2017) give the number of systems that they are unable to determine disc radii for, but there is no indication of completeness in the studies of Andrews et al. (2009, 2010) and Tripathi et al. (2017).”
A Three-dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk Using DCO+ (2017, background): “Recent work has brought into question standard assumptions about the gas-to-dust mass ratio, CO/H2, and C18O/CO (Bergin et al. 2013; Miotello et al. 2014; Ansdell et al. 2016; Kama et al. 2016), raising the possibility of a significant deviation from our assumed disk mass.”
ALMA Survey of Lupus Protoplanetary Disks. II. Gas Disk Radii (2018, methodology): “In the first paper of this series (Ansdell et al. 2016; hereafter Paper I), we used ALMA to observe a nearcomplete sample of protoplanetary disks in the Lupus star-forming region in the 890 µm (Band 7) continuum as well as the 13CO and C18O J = 3–2 isotopologue lines.”