Alma survey of lupus protoplanetary disks. I. Dust and gas masses

Journal Article · Thu Sep 01 04:00:00 EDT 2016 · Astrophysical Journal

DOI:https://doi.org/10.3847/0004-637X/828/1/46· OSTI ID:22868731

Ansdell, M.; Williams, J. P.; Marel, N. van der ^[1]; Carpenter, J. M. ^[2]; Guidi, G.; Natta, A.; Testi, L. ^[3]; Hogerheijde, M.; Miotello, A.; Van Dishoeck, E. F.; Van Terwisga, S. E. ^[4]; Mathews, G. S. ^[5]; Manara, C. F. ^[6]; Oliveira, I. ^[7]; Tazzari, M. ^[8]

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1. Institute for Astronomy, University of Hawai‘i at Mānoa, Honolulu, HI (United States)
2. California Institute of Technology, 1200 East California Blvd, Pasadena, CA 91125 (United States)
3. INAF-Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze (Italy)
4. Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden (Netherlands)
5. Department of Physics and Astronomy, University of Hawaii, Honolulu, HI 96822 (United States)
6. Scientific Support Office, Directorate of Science, European Space Research and Technology Centre (ESA/ESTEC), Keplerlaan 1, 2201 AZ Noordwijk (Netherlands)
7. Observatório Nacional/MCTI, Rio de Janeiro, 20921-400 (Brazil)
8. European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching bei München (Germany)

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 M{sub ∗}>0.1 M{sub ⊙} in the young (1–3 Myr), nearby (150–200 pc) Lupus complex. Our observations cover the 890 μm continuum and the {sup 13}CO and C{sup 18}O 3–2 lines. We use the sub-millimeter continuum to constrain M{sub dust} to a few Martian masses (0.2–0.4 M {sub ⊕}) and the CO isotopologue lines to constrain M{sub gas} to roughly a Jupiter mass (assuming an interstellar medium (ISM)-like [CO]/[H{sub 2}] abundance). Of 89 sources, we detect 62 in continuum, 36 in {sup 13}CO, and 11 in C{sup 18}O at >3σ significance. Stacking individually undetected sources limits their average dust mass to ≲6 Lunar masses (0.03 M {sub ⊕}), indicating rapid evolution once disk clearing begins. We find a positive correlation between M{sub dust} and M {sub *}, and present the first evidence for a positive correlation between M{sub gas} and M {sub *}, 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 M{sub gas}≲1 M{sub Jup} and gas-to-dust ratios <100, assuming an ISM-like [CO]/[H{sub 2}] 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.

• OSTI ID: 22868731
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 828; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
CARBON MONOXIDE
CORRELATIONS
COSMIC DUST
ELEMENT ABUNDANCE
HYDROGEN
MASS
MASS DISTRIBUTION
PROTOPLANETS
PROTOSTARS
RESOLUTION
SATELLITES
STAR EVOLUTION
STARS