The VLA/ALMA Nascent Disk And Multiplicity (VANDAM) Survey of Orion Protostars. V. A Characterization of Protostellar Multiplicity

The VLA/ALMA Nascent Disk And Multiplicity (VANDAM) Survey of Orion Protostars. V. A Characterization of Protostellar Multiplicity

Abstract We characterize protostellar multiplicity in 20 Current address: Niels Bohr Institute, University of Copenhagen, Øster Voldgade 5–7, DK-1350, Copenhagen K, Denmark. the Orion molecular clouds using Atacama Large Millimeter/submillimeter Array 0.87 mm and Very Large Array 9 mm continuum su...

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Bibliographic Details
Published in:The Astrophysical journal 2022-01, Vol.925 (1), p.39
Main Authors: Tobin, John J., Offner, Stella S. R., Kratter, Kaitlin M., Megeath, S. Thomas, Sheehan, Patrick D., Looney, Leslie W., Diaz-Rodriguez, Ana Karla, Osorio, Mayra, Anglada, Guillem, Sadavoy, Sarah I., Furlan, Elise, Segura-Cox, Dominique, Karnath, Nicole, van ’t Hoff, Merel L. R., van Dishoeck, Ewine F., Li, Zhi-Yun, Sharma, Rajeeb, Stutz, Amelia M., Tychoniec, Łukasz
Format: Article
Language:eng
Subjects:
Arrays
Astrophysics
Density
Fragmentation
Molecular clouds
Multiple stars
Polls & surveys
Protostars
Radio interferometry
Radio telescopes
Separation
Star formation
Stars
Young stellar objects
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Summary:Abstract We characterize protostellar multiplicity in 20 Current address: Niels Bohr Institute, University of Copenhagen, Øster Voldgade 5–7, DK-1350, Copenhagen K, Denmark. the Orion molecular clouds using Atacama Large Millimeter/submillimeter Array 0.87 mm and Very Large Array 9 mm continuum surveys toward 328 protostars. These observations are sensitive to projected spatial separations as small as ∼20 au, and we consider source separations up to 10 4 au as potential companions. The overall multiplicity fraction (MF) and companion fraction (CF) for the Orion protostars are 0.30 ± 0.03 and 0.44 ± 0.03, respectively, considering separations from 20 to 10 4 au. The MFs and CFs are corrected for potential contamination by unassociated young stars using a probabilistic scheme based on the surface density of young stars around each protostar. The companion separation distribution as a whole is double peaked and inconsistent with the separation distribution of solar-type field stars, while the separation distribution of Flat Spectrum protostars is consistent solar-type field stars. The multiplicity statistics and companion separation distributions of the Perseus star-forming region are consistent with those of Orion. Based on the observed peaks in the Class 0 separations at ∼100 au and ∼10 3 au, we argue that multiples with separations 10 3 au to
ISSN:0004-637X
1538-4357