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| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| Online Access: | https://arxiv.org/abs/2407.17249 |
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| author | Gavino, Sacha Jørgensen, Jes K. Sharma, Rajeeb Yang, Yao-Lun Li, Zhi-Yun Tobin, John J. Ohashi, Nagayoshi Takakuwa, Shigehisa Plunkett, Adele Kwon, Woojin de Gregorio-Monsalvo, Itziar Lin, Zhe-Yu Daniel Santamaría-Miranda, Alejandro Aso, Yusuke Sai, Jinshi Aikawa, Yuri Tomida, Kengo Koch, Patrick M. Lee, Jeong-Eun Lee, Chang Won Lai, Shih-Ping Looney, Leslie W. Narayanan, Suchitra Phuong, Nguyen Thi Thieme, Travis J. Hoff, Merel L. R. van 't Willians, Jonathan P. Yen, Hsi-Wei |
| author_facet | Gavino, Sacha Jørgensen, Jes K. Sharma, Rajeeb Yang, Yao-Lun Li, Zhi-Yun Tobin, John J. Ohashi, Nagayoshi Takakuwa, Shigehisa Plunkett, Adele Kwon, Woojin de Gregorio-Monsalvo, Itziar Lin, Zhe-Yu Daniel Santamaría-Miranda, Alejandro Aso, Yusuke Sai, Jinshi Aikawa, Yuri Tomida, Kengo Koch, Patrick M. Lee, Jeong-Eun Lee, Chang Won Lai, Shih-Ping Looney, Leslie W. Narayanan, Suchitra Phuong, Nguyen Thi Thieme, Travis J. Hoff, Merel L. R. van 't Willians, Jonathan P. Yen, Hsi-Wei |
| contents | We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of the binary Class 0 protostellar system BHR 71 IRS1 and IRS2 as part of the Early Planet Formation in Embedded Disks (eDisk) ALMA Large Program. We describe the $^{12}$CO ($J$=2--1), $^{13}$CO ($J$=2--1), C$^{18}$O ($J$=2--1), H$_2$CO ($J=3_{2,1}$--$2_{2,0}$), and SiO ($J$=5--4) molecular lines along with the 1.3 mm continuum at high spatial resolution ($\sim$0.08" or $\sim$5 au). Dust continuum emission is detected toward BHR 71 IRS1 and IRS2, with a central compact component and extended continuum emission. The compact components are smooth and show no sign of substructures such as spirals, rings or gaps. However, there is a brightness asymmetry along the minor axis of the presumed disk in IRS1, possibly indicative of an inclined geometrically and optically thick disk-like component. Using a position-velocity diagram analysis of the C$^{18}$O line, clear Keplerian motions were not detected toward either source. If Keplerian rotationally-supported disks are present, they are likely deeply embedded in their envelope. However, we can set upper limits of the central protostellar mass of 0.46 M$_\odot$ and 0.26 M$_\odot$ for BHR 71 IRS1 and BHR 71 IRS2, respectively. Outflows traced by $^{12}$CO and SiO are detected in both sources. The outflows can be divided into two components, a wide-angle outflow and a jet. In IRS1, the jet exhibits a double helical structure, reflecting the removal of angular momentum from the system. In IRS2, the jet is very collimated and shows a chain of knots, suggesting episodic accretion events. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2407_17249 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Early Planet Formation in Embedded Disks (eDisk). XI. A high-resolution view toward the BHR 71 Class 0 protostellar wide binary Gavino, Sacha Jørgensen, Jes K. Sharma, Rajeeb Yang, Yao-Lun Li, Zhi-Yun Tobin, John J. Ohashi, Nagayoshi Takakuwa, Shigehisa Plunkett, Adele Kwon, Woojin de Gregorio-Monsalvo, Itziar Lin, Zhe-Yu Daniel Santamaría-Miranda, Alejandro Aso, Yusuke Sai, Jinshi Aikawa, Yuri Tomida, Kengo Koch, Patrick M. Lee, Jeong-Eun Lee, Chang Won Lai, Shih-Ping Looney, Leslie W. Narayanan, Suchitra Phuong, Nguyen Thi Thieme, Travis J. Hoff, Merel L. R. van 't Willians, Jonathan P. Yen, Hsi-Wei Earth and Planetary Astrophysics Solar and Stellar Astrophysics We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of the binary Class 0 protostellar system BHR 71 IRS1 and IRS2 as part of the Early Planet Formation in Embedded Disks (eDisk) ALMA Large Program. We describe the $^{12}$CO ($J$=2--1), $^{13}$CO ($J$=2--1), C$^{18}$O ($J$=2--1), H$_2$CO ($J=3_{2,1}$--$2_{2,0}$), and SiO ($J$=5--4) molecular lines along with the 1.3 mm continuum at high spatial resolution ($\sim$0.08" or $\sim$5 au). Dust continuum emission is detected toward BHR 71 IRS1 and IRS2, with a central compact component and extended continuum emission. The compact components are smooth and show no sign of substructures such as spirals, rings or gaps. However, there is a brightness asymmetry along the minor axis of the presumed disk in IRS1, possibly indicative of an inclined geometrically and optically thick disk-like component. Using a position-velocity diagram analysis of the C$^{18}$O line, clear Keplerian motions were not detected toward either source. If Keplerian rotationally-supported disks are present, they are likely deeply embedded in their envelope. However, we can set upper limits of the central protostellar mass of 0.46 M$_\odot$ and 0.26 M$_\odot$ for BHR 71 IRS1 and BHR 71 IRS2, respectively. Outflows traced by $^{12}$CO and SiO are detected in both sources. The outflows can be divided into two components, a wide-angle outflow and a jet. In IRS1, the jet exhibits a double helical structure, reflecting the removal of angular momentum from the system. In IRS2, the jet is very collimated and shows a chain of knots, suggesting episodic accretion events. |
| title | Early Planet Formation in Embedded Disks (eDisk). XI. A high-resolution view toward the BHR 71 Class 0 protostellar wide binary |
| topic | Earth and Planetary Astrophysics Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2407.17249 |