Abstract
We present Atacama Large Millimeter/submillimeter Array (0.87 mm) and Very Large Array (9 mm) observations toward OMC-2 FIR4 and OMC-2 FIR3 within the Orion integral-shaped filament, thought to be two of the nearest regions of intermediate-mass star formation. We characterize the continuum sources within these regions on ∼40 au (0.″1) scales and associated molecular line emission at a factor of ∼30 better resolution than previous observations at similar wavelengths. We identify six compact continuum sources within OMC-2 FIR4, four in OMC-2 FIR3, and one additional source just outside OMC-2 FIR4. This continuum emission is tracing the inner envelope and/or disk emission on less than 100 au scales. HOPS-108 is the only protostar in OMC-2 FIR4 that exhibits emission from high-excitation transitions of complex organic molecules (e.g., methanol and other lines) coincident with the continuum emission. HOPS-370 in OMC-2 FIR3, with L ∼ 360 L o˙, also exhibits emission from high-excitation methanol and other lines. The methanol emission toward these two protostars is indicative of temperatures high enough to thermally evaporate it from icy dust grains; overall, these protostars have characteristics similar to hot corinos. We do not identify a clear outflow from HOPS-108 in 12CO, but we find evidence of interaction between the outflow/jet from HOPS-370 and the OMC-2 FIR4 region. A multitude of observational constraints indicate that HOPS-108 is likely a low- to intermediate-mass protostar in its main mass accretion phase and is the most luminous protostar in OMC-2 FIR4. The high-resolution data presented here are essential for disentangling the embedded protostars from their surrounding dusty environments and characterizing them.
| Original language | English (US) |
|---|---|
| Article number | 6 |
| Journal | Astrophysical Journal |
| Volume | 886 |
| Issue number | 1 |
| DOIs | |
| State | Published - Nov 20 2019 |
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science
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The vla/alma nascent disk and multiplicity (vandam) survey of orion protostars. i. identifying and characterizing the protostellar content of the omc-2 fir4 and omc-2 fir3 regions. / Tobin, John J.; Megeath, S. Thomas; Hoff, Merel Van T.; Díaz-Rodríguez, Ana Karla; Reynolds, Nickalas; Osorio, Mayra; Anglada, Guillem; Furlan, Elise; Karnath, Nicole; Offner, Stella S.R.; Sheehan, Patrick D.; Sadavoy, Sarah I.; Stutz, Amelia M.; Fischer, William J.; Kama, Mihkel; Persson, Magnus; Francesco, James Di; Looney, Leslie W.; Watson, Dan M.; Li, Zhi Yun; Stephens, Ian; Chandler, Claire J.; Cox, Erin; Dunham, Michael M.; Kratter, Kaitlin; Kounkel, Marina; Mazur, Brian; Murillo, Nadia M.; Patel, Lisa; Perez, Laura; Segura-Cox, Dominique; Sharma, Rajeeb; Tychoniec, Łukasz; Wyrowski, Friedrich.
In: Astrophysical Journal, Vol. 886, No. 1, 6, 20.11.2019.Research output: Contribution to journal › Article › peer-review
}
TY - JOUR
T1 - The vla/alma nascent disk and multiplicity (vandam) survey of orion protostars. i. identifying and characterizing the protostellar content of the omc-2 fir4 and omc-2 fir3 regions
AU - Tobin, John J.
AU - Megeath, S. Thomas
AU - Hoff, Merel Van T.
AU - Díaz-Rodríguez, Ana Karla
AU - Reynolds, Nickalas
AU - Osorio, Mayra
AU - Anglada, Guillem
AU - Furlan, Elise
AU - Karnath, Nicole
AU - Offner, Stella S.R.
AU - Sheehan, Patrick D.
AU - Sadavoy, Sarah I.
AU - Stutz, Amelia M.
AU - Fischer, William J.
AU - Kama, Mihkel
AU - Persson, Magnus
AU - Francesco, James Di
AU - Looney, Leslie W.
AU - Watson, Dan M.
AU - Li, Zhi Yun
AU - Stephens, Ian
AU - Chandler, Claire J.
AU - Cox, Erin
AU - Dunham, Michael M.
AU - Kratter, Kaitlin
AU - Kounkel, Marina
AU - Mazur, Brian
AU - Murillo, Nadia M.
AU - Patel, Lisa
AU - Perez, Laura
AU - Segura-Cox, Dominique
AU - Sharma, Rajeeb
AU - Tychoniec, Łukasz
AU - Wyrowski, Friedrich
N1 - Funding Information: John J. Tobin S. Thomas Megeath Merel van’t Hoff Ana Karla D�az-Rodr�guez Nickalas Reynolds Mayra Osorio Guillem Anglada Elise Furlan Nicole Karnath Stella S. R. Offner Patrick D. Sheehan Sarah I. Sadavoy Amelia M. Stutz William J. Fischer Mihkel Kama Magnus Persson James Di Francesco Leslie W. Looney Dan M. Watson Zhi-Yun Li Ian Stephens Claire J. Chandler Erin Cox Michael M. Dunham Kaitlin Kratter Marina Kounkel Brian Mazur Nadia M. Murillo Lisa Patel Laura Perez Dominique Segura-Cox Rajeeb Sharma Łukasz Tychoniec Friedrich Wyrowski John J. Tobin S. Thomas Megeath Merel van’t Hoff Ana Karla D�az-Rodr�guez Nickalas Reynolds Mayra Osorio Guillem Anglada Elise Furlan Nicole Karnath Stella S. R. Offner Patrick D. Sheehan Sarah I. Sadavoy Amelia M. Stutz William J. Fischer Mihkel Kama Magnus Persson James Di Francesco Leslie W. Looney Dan M. Watson Zhi-Yun Li Ian Stephens Claire J. Chandler Erin Cox Michael M. Dunham Kaitlin Kratter Marina Kounkel Brian Mazur Nadia M. Murillo Lisa Patel Laura Perez Dominique Segura-Cox Rajeeb Sharma Łukasz Tychoniec Friedrich Wyrowski National Radio Astronomy Observatory, 520 Edgemont Rd., Charlottesville, VA 22903, USA Department of Physics and Astronomy, University of Toledo, Toledo, OH 43560, USA Leiden Observatory, Leiden University, P.O. Box 9513, 2300-RA Leiden, The Netherlands Instituto de Astrof�sica de Andaluc�a, CSIC, Glorieta de la Astronom�a s/n, E-18008 Granada, Spain Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, 440 W. Brooks St., Norman, OK 73019, USA IPAC, Mail Code 314-6, Caltech, 1200 E. California Blvd., Pasadena, CA 91125, USA The University of Texas at Austin, 2500 Speedway, Austin, TX, USA Harvard-Smithsonian Center for Astrophysics, 60 Garden St., MS 78, Cambridge, MA 02138, USA Departmento de Astronom�a, Universidad de Concepci�n, Casilla 160-C, Concepci�n, Chile Max-Planck-Institute for Astronomy, K�nigstuhl 17, D-69117 Heidelberg, Germany Space Telescope Science Institute, Baltimore, MD 21218, USA Institute of Astronomy, Madingley Rd., Cambridge CB3 OHA, UK Chalmers University of Technology, Department of Space, Earth and Environment, Sweden Herzberg Astronomy and Astrophysics Programs, National Research Council of Canada, 5071 West Saanich Rd., Victoria BC V9E 2E7, Canada Department of Astronomy, University of Illinois, Urbana, IL 61801, USA Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA Department of Astronomy, University of Virginia, Charlottesville, VA 22903, USA National Radio Astronomy Observatory, P.O. Box O, Socorro, NM 87801, USA Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208, USA Department of Physics, State University of New York Fredonia, Fredonia, NY 14063, USA University of Arizona, Steward Observatory, Tucson, AZ 85721, USA Department of Physics and Astronomy, Western Washington University, 516 High St., Bellingham, WA 98225, USA Departamento de Astronom�a, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile Max-Planck-Institut f�r extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching, Germany Max-Planck-Institut f�r Radioastronomie, Auf dem H�gel 69, D-53121, Bonn, Germany John J. Tobin, S. Thomas Megeath, Merel van’t Hoff, Ana Karla D�az-Rodr�guez, Nickalas Reynolds, Mayra Osorio, Guillem Anglada, Elise Furlan, Nicole Karnath, Stella S. R. Offner, Patrick D. Sheehan, Sarah I. Sadavoy, Amelia M. Stutz, William J. Fischer, Mihkel Kama, Magnus Persson, James Di Francesco, Leslie W. Looney, Dan M. Watson, Zhi-Yun Li, Ian Stephens, Claire J. Chandler, Erin Cox, Michael M. Dunham, Kaitlin Kratter, Marina Kounkel, Brian Mazur, Nadia M. Murillo, Lisa Patel, Laura Perez, Dominique Segura-Cox, Rajeeb Sharma, Łukasz Tychoniec and Friedrich Wyrowski 2019-11-20 2019-11-13 14:31:31 cgi/release: Article released bin/incoming: New from .zip National Science Foundation AST-1814762 yes We present Atacama Large Millimeter/submillimeter Array (0.87 mm) and Very Large Array (9 mm) observations toward OMC-2 FIR4 and OMC-2 FIR3 within the Orion integral-shaped filament, thought to be two of the nearest regions of intermediate-mass star formation. We characterize the continuum sources within these regions on ∼40 au (0.″1) scales and associated molecular line emission at a factor of ∼30 better resolution than previous observations at similar wavelengths. We identify six compact continuum sources within OMC-2 FIR4, four in OMC-2 FIR3, and one additional source just outside OMC-2 FIR4. This continuum emission is tracing the inner envelope and/or disk emission on less than 100 au scales. HOPS-108 is the only protostar in OMC-2 FIR4 that exhibits emission from high-excitation transitions of complex organic molecules (e.g., methanol and other lines) coincident with the continuum emission. HOPS-370 in OMC-2 FIR3, with L �∼�360 L ⊙ , also exhibits emission from high-excitation methanol and other lines. The methanol emission toward these two protostars is indicative of temperatures high enough to thermally evaporate it from icy dust grains; overall, these protostars have characteristics similar to hot corinos. We do not identify a clear outflow from HOPS-108 in 12 CO, but we find evidence of interaction between the outflow/jet from HOPS-370 and the OMC-2 FIR4 region. 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PY - 2019/11/20
Y1 - 2019/11/20
N2 - We present Atacama Large Millimeter/submillimeter Array (0.87 mm) and Very Large Array (9 mm) observations toward OMC-2 FIR4 and OMC-2 FIR3 within the Orion integral-shaped filament, thought to be two of the nearest regions of intermediate-mass star formation. We characterize the continuum sources within these regions on ∼40 au (0.″1) scales and associated molecular line emission at a factor of ∼30 better resolution than previous observations at similar wavelengths. We identify six compact continuum sources within OMC-2 FIR4, four in OMC-2 FIR3, and one additional source just outside OMC-2 FIR4. This continuum emission is tracing the inner envelope and/or disk emission on less than 100 au scales. HOPS-108 is the only protostar in OMC-2 FIR4 that exhibits emission from high-excitation transitions of complex organic molecules (e.g., methanol and other lines) coincident with the continuum emission. HOPS-370 in OMC-2 FIR3, with L ∼ 360 L o˙, also exhibits emission from high-excitation methanol and other lines. The methanol emission toward these two protostars is indicative of temperatures high enough to thermally evaporate it from icy dust grains; overall, these protostars have characteristics similar to hot corinos. We do not identify a clear outflow from HOPS-108 in 12CO, but we find evidence of interaction between the outflow/jet from HOPS-370 and the OMC-2 FIR4 region. A multitude of observational constraints indicate that HOPS-108 is likely a low- to intermediate-mass protostar in its main mass accretion phase and is the most luminous protostar in OMC-2 FIR4. The high-resolution data presented here are essential for disentangling the embedded protostars from their surrounding dusty environments and characterizing them.
AB - We present Atacama Large Millimeter/submillimeter Array (0.87 mm) and Very Large Array (9 mm) observations toward OMC-2 FIR4 and OMC-2 FIR3 within the Orion integral-shaped filament, thought to be two of the nearest regions of intermediate-mass star formation. We characterize the continuum sources within these regions on ∼40 au (0.″1) scales and associated molecular line emission at a factor of ∼30 better resolution than previous observations at similar wavelengths. We identify six compact continuum sources within OMC-2 FIR4, four in OMC-2 FIR3, and one additional source just outside OMC-2 FIR4. This continuum emission is tracing the inner envelope and/or disk emission on less than 100 au scales. HOPS-108 is the only protostar in OMC-2 FIR4 that exhibits emission from high-excitation transitions of complex organic molecules (e.g., methanol and other lines) coincident with the continuum emission. HOPS-370 in OMC-2 FIR3, with L ∼ 360 L o˙, also exhibits emission from high-excitation methanol and other lines. The methanol emission toward these two protostars is indicative of temperatures high enough to thermally evaporate it from icy dust grains; overall, these protostars have characteristics similar to hot corinos. We do not identify a clear outflow from HOPS-108 in 12CO, but we find evidence of interaction between the outflow/jet from HOPS-370 and the OMC-2 FIR4 region. A multitude of observational constraints indicate that HOPS-108 is likely a low- to intermediate-mass protostar in its main mass accretion phase and is the most luminous protostar in OMC-2 FIR4. The high-resolution data presented here are essential for disentangling the embedded protostars from their surrounding dusty environments and characterizing them.
UR - http://www.scopus.com/inward/record.url?scp=85077332268&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85077332268&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ab498f
DO - 10.3847/1538-4357/ab498f
M3 - Article
AN - SCOPUS:85077332268
VL - 886
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1
M1 - 6
ER -