Disks and Outflows in the Intermediate-mass Star-forming Region NGC 2071 IR

DOI: 
10.3847/1538-4357/ac7464
Publication date: 
08/07/2022
Main author: 
Cheng, Yu
IAA authors: 
Osorio, Mayra;Anglada, Guillem
Authors: 
Cheng, Yu;Tobin, John J.;Yang, Yao-Lun;van't Hoff, Merel L. R.;Sadavoy, Sarah I.;Osorio, Mayra;Díaz-Rodríguez, Ana Karla;Anglada, Guillem;Karnath, Nicole;Sheehan, Patrick D.;Li, Zhi-Yun;Reynolds, Nickalas;Murillo, Nadia M.;Zhang, Yichen;Megeath, S. Thomas;Tychoniec, Łukasz
Journal: 
The Astrophysical Journal
Refereed: 
Yes
Publication type: 
Article
Volume: 
933
Pages: 
178
Abstract: 
We present Atacama Large Millimeter Array band 6/7 (1.3 mm/0.87 mm) and Very Large Array Ka-band (9 mm) observations toward NGC 2071 IR, an intermediate-mass star-forming region. We characterize the continuum and associated molecular line emission toward the most luminous protostars, i.e., IRS1 and IRS3, on ~100 au (0.″2) scales. IRS1 is partly resolved in the millimeter and centimeter continuum, which shows a potential disk. IRS3 has a well-resolved disk appearance in the millimeter continuum and is further resolved into a close binary system separated by ~40 au at 9 mm. Both sources exhibit clear velocity gradients across their disk major axes in multiple spectral lines including C<SUP>18</SUP>O, H<SUB>2</SUB>CO, SO, SO<SUB>2</SUB>, and complex organic molecules like CH<SUB>3</SUB>OH, <SUP>13</SUP>CH<SUB>3</SUB>OH, and CH<SUB>3</SUB>OCHO. We use an analytic method to fit the Keplerian rotation of the disks and give constraints on physical parameters with a Markov Chain Monte Carlo routine. The IRS3 binary system is estimated to have a total mass of 1.4-1.5 M <SUB>⊙</SUB>. IRS1 has a central mass of 3-5 M <SUB>⊙</SUB> based on both kinematic modeling and its spectral energy distribution, assuming that it is dominated by a single protostar. For both IRS1 and IRS3, the inferred ejection directions from different tracers, including radio jet, water maser, molecular outflow, and H<SUB>2</SUB> emission, are not always consistent, and for IRS1 these can be misaligned by ~50°. IRS3 is better explained by a single precessing jet. A similar mechanism may be present in IRS1 as well but an unresolved multiple system in IRS1 is also possible.
Database: 
ADS
SCOPUS
URL: 
https://ui.adsabs.harvard.edu/#abs/2022ApJ...933..178C/abstract
ADS Bibcode: 
2022ApJ...933..178C
Keywords: 
Protostars;Protoplanetary disks;Stellar jets;Star formation;1302;1300;1607;1569;Astrophysics - Astrophysics of Galaxies