ALMA OBSERVATIONS OF CIRCUMSTELLAR DISKS IN THE UPPER SCORPIUS OB ASSOCIATION

By S. Barenfeld, J. Carpenter, L. Ricci, Andrea Isella. 2016

140 citations recorded by the source corpus.

We present ALMA observations of 106 G-, K-, and M-type stars in the Upper Scorpius OB Association hosting circumstellar disks. With these data, we measure the 0.88 mm continuum and 12CO J = 3–2 line fluxes of disks around low-mass (0.14–1.66 M⊙) stars at an age of 5–11 Myr. Of the 75 primordial disks in the sample, 53 are detected in the dust continuum and 26 in CO. Of the 31 disks classified as debris/evolved transitional disks, five are detected in the continuum and none in CO. The lack of CO emission in approximately half of the disks with detected continuum emission can be explained if CO is optically thick but has a compact emitting area (≲40 au), or if the CO is heavily depleted by a factor of at least ∼1000 relative to interstellar medium abundances and is optically thin. The continuum measurements are used to estimate the dust mass of the disks. We find a correlation between disk dust mass and stellar host mass consistent with a power-law relation of . Disk dust masses in Upper Sco are compared to those measured in the younger Taurus star-forming region to constrain the evolution of disk dust mass. We find that the difference in the mean of between Taurus and Upper Sco is 0.64 ± 0.09, such that Mdust/M* is lower in Upper Sco by a factor of ∼4.5.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d85c271b844b2c9f715e840bc7e586fc19a8a1d4

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Citations in the corpus

A millimeter Continuum Size–Luminosity Relationship for Protoplanetary Disks (2017, methodology): “…2007), and study how they vary with time (Mathews et al. 2012; Williams et al. 2013; Carpenter et al. 2014; Ansdell et al. 2015; Cieza et al. 2015; Barenfeld et al. 2016), environment (Jensen et al. 1994, 1996; Harris et al. 2012; Akeson & Jensen 2014; Mann & Williams 2009, 2010; Mann et al.…”
The Disk Substructures at High Angular Resolution Project (DSHARP). II. Characteristics of Annular Substructures (2018, unknown): “…209 (Huang et al. 2017; Fedele et al. 2018), DoAr 25 (Cox et al. 2017), Elias 24 (Cieza et al. 2017; Cox et al. 2017; Dipierro et al. 2018), Elias 27 (Pérez et al. 2016), HD 142666 (Rubinstein et al. 2018), HD 143006 (Barenfeld et al. 2016), and HD 163296 (Zhang et al. 2016; Isella et al. 2016).”
Why do protoplanetary disks appear not massive enough to form the known exoplanet population? (2018, background): “…to near-infrared spectroscopic surveys, are showing that the mass of the dust content of protoplanetary disks increases with stellar mass following a steeper than linear relation and decreases with time (e.g., Ansdell et al. 2016; Pascucci et al. 2016; Barenfeld et al. 2016; Ansdell et al. 2017).”
A STEEPER THAN LINEAR DISK MASS–STELLAR MASS SCALING RELATION (2016, methodology): “At ∼10Myr the deficit amounts to more than a factor of 5 as shown by the UpperSco region.”
An ALMA Survey of Protoplanetary Disks in the σ Orionis Cluster (2017, methodology): “…Myr at ∼150 pc; Comerón 2008; Alcalá et al. 2014) with continuum and line sensitivities corresponding to Mdust∼0.3 M⊕ and Mgas∼1.0 MJup, respectively; Barenfeld et al. (2016), who observed 106 disks in the more evolved Upper Sco region (∼5–10 Myr at 145 pc; Preibisch et al. 2002; Pecaut et…”
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).”
On the diversity and statistical properties of protostellar discs (2018, background): “26 that the observed distributions of disc radii for the Orion Nebula Cluster and for Taurus/Ophiuchus are very similar, despite the stellar densities being very different.”
ALMA Survey of Lupus Protoplanetary Disks. II. Gas Disk Radii (2018, background): “…I (Pascucci et al. 2016) regions, with those of the intermediate-aged (∼3–5 Myr) σ Orionis cluster (Ansdell et al. 2017) and the evolved (∼5–10 Myr) Upper Sco association (Barenfeld et al. 2016), reveal a clear decline in disk dust mass (Mdust) with age (see Figure 8 in Ansdell et al. 2017).”