Disks and Outflows in the Intermediate-mass Star Forming Region NGC 2071 IR
| Autor: | Yu Cheng, John J. Tobin, Yao-Lun Yang, Merel L. R. van ’t Hoff, Sarah I. Sadavoy, Mayra Osorio, Ana Karla Díaz-Rodríguez, Guillem Anglada, Nicole Karnath, Patrick D. Sheehan, Zhi-Yun Li, Nickalas Reynolds, Nadia M. Murillo, Yichen Zhang, S. Thomas Megeath, Łukasz Tychoniec |
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| Přispěvatelé: | Ministerio de Ciencia e Innovación (España), European Commission, National Science Foundation (US) |
| Rok vydání: | 2022 |
| Předmět: | |
| DOI: | 10.48550/arxiv.2205.15108 |
| Popis: | This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited. 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 (0farcs2) 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 C18O, H2CO, SO, SO2, and complex organic molecules like CH3OH, 13CH3OH, and CH3OCHO. 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⊙. IRS1 has a central mass of 3–5 M⊙ 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 H2 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. © 2022. The Author(s). Published by the American Astronomical Society. Support for this work was provided by the NSF through the Grote Reber Fellowship Program (to Y.C.) administered by Associated Universities, Inc./National Radio Astronomy Observatory. J.J.T. acknowledges funding from NSF grant AST-1814762. Y.-L.Y. acknowledges the support of the Virginia Initiative of Cosmic Origins (VICO) Postdoctoral Fellowship. M.L.R.H. acknowledges support from the Michigan Society of Fellows. Z.-Y.L. is supported in part by NASA 80NSSC20K0533 and NSF AST-1815784. G.A. and M.O. acknowledge support from the Spanish MINECO/AEI through the AYA2017-84390-C2 grant (co-funded by FEDER), MCIN/AEI/10.13039/501100011033 through the PID2020-114461GB-I00 and from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709). M.O. also acknowledges financial support from the Consejería de Transformación Económica, Industria, Conocimiento y Universidades of the Junta de Andalucía, and the European Regional Development Fund from the European Union through the grant P20-00880. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.00041.S and ADS/JAO.ALMA #2018.1.01038.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST 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. |
| Databáze: | OpenAIRE |
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