TY - JOUR
T1 - The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. VI. Insights from Radiative Transfer Modeling
AU - Sheehan, Patrick D.
AU - Tobin, John J.
AU - Looney, Leslie W.
AU - Megeath, S. Thomas
N1 - Funding Information:
The authors would like to thank the anonymous referee for feedback that helped to focus and improve the manuscript. P.D.S. would also like to thank Leonardo Testi and the referee for pointing him to the protostellar evolutionary tracks used in Section , which added an interesting new piece of analysis to the work. P.D.S. is supported by a National Science Foundation Astronomy & Astrophysics Postdoctoral Fellowship under award No. 2001830. J.J.T. acknowledges support from NSF AST-1814762 and past support from the Homer L. Dodge Endowed Chair at the University of Oklahoma. L.W.L. acknowledges support from NSF AST-1910364 and AST-2108794. This work used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant No. ACI-1548562, for the majority of the computing done. Additional computing was performed at the OU Supercomputing Center for Education and Research (OSCER) at the University of Oklahoma (OU), when needed. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.00041.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/4/1
Y1 - 2022/4/1
N2 - We present Markov Chain Monte Carlo radiative transfer modeling of a joint ALMA 345 GHz and spectral energy distribution data set for a sample of 97 protostellar disks from the VLA and ALMA Nascent Disk and Multiplicity Survey of Orion Protostars. From this modeling, we derive disk and envelope properties for each protostar, allowing us to examine the bulk properties of a population of young protostars. We find that disks are small, with a median dust radius of 29.4-2.7+4.1 au and a median dust mass of 5.8-2.7+4.6 M + . We find no statistically significant difference between most properties of Class 0, Class I, and flat-spectrum sources with the exception of envelope dust mass and inclination. The distinction between inclination is an indication that the Class 0/I/flat-spectrum system may be difficult to tie uniquely to the evolutionary state of protostars. When comparing with Class II disk dust masses in Taurus from similar radiative transfer modeling, we further find that the trend of disk dust mass decreasing from Class 0 to Class II disks is no longer present, though it remains unclear whether such a comparison is fair owing to differences in star-forming region and modeling techniques. Moreover, the disks we model are broadly gravitationally stable. Finally, we compare disk masses and radii with simulations of disk formation and find that magnetohydrodynamical effects may be important for reproducing the observed properties of disks.
AB - We present Markov Chain Monte Carlo radiative transfer modeling of a joint ALMA 345 GHz and spectral energy distribution data set for a sample of 97 protostellar disks from the VLA and ALMA Nascent Disk and Multiplicity Survey of Orion Protostars. From this modeling, we derive disk and envelope properties for each protostar, allowing us to examine the bulk properties of a population of young protostars. We find that disks are small, with a median dust radius of 29.4-2.7+4.1 au and a median dust mass of 5.8-2.7+4.6 M + . We find no statistically significant difference between most properties of Class 0, Class I, and flat-spectrum sources with the exception of envelope dust mass and inclination. The distinction between inclination is an indication that the Class 0/I/flat-spectrum system may be difficult to tie uniquely to the evolutionary state of protostars. When comparing with Class II disk dust masses in Taurus from similar radiative transfer modeling, we further find that the trend of disk dust mass decreasing from Class 0 to Class II disks is no longer present, though it remains unclear whether such a comparison is fair owing to differences in star-forming region and modeling techniques. Moreover, the disks we model are broadly gravitationally stable. Finally, we compare disk masses and radii with simulations of disk formation and find that magnetohydrodynamical effects may be important for reproducing the observed properties of disks.
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U2 - 10.3847/1538-4357/ac574d
DO - 10.3847/1538-4357/ac574d
M3 - Article
AN - SCOPUS:85128845585
SN - 0004-637X
VL - 929
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 76
ER -