| Title: |
Early Planet Formation in Embedded Disks (eDisk): XVI. Asymmetric dust disk driving a multicomponent molecular outflow in the young Class 0 protostar GSS30 IRS3. |
| Authors: |
Santamaría-Miranda, Alejandro, de Gregorio-Monsalvo, Itziar, Ohashi, Nagayoshi, Tobin, John J., Sai, Jinshi, Jørgensen, Jes K., Aso, Yusuke, Daniel Lin, Zhe-Yu, Flores, Christian, Kido, Miyu, Koch, Patrick M., Kwon, Woojin, Lee, Chang Won, Li, Zhi-Yun, Looney, Leslie W., Plunkett, Adele L., Takakuwa, Shigehisa, R van't Hoff, Merel L., Williams, Jonathan P., Yen, Hsi-Wei |
| Source: |
Astronomy & Astrophysics / Astronomie et Astrophysique; 9/26/2024, Vol. 690, p1-23, 23p |
| Subject Terms: |
CIRCUMSTELLAR matter, LOW mass stars, STELLAR winds, STELLAR mass, ORIGIN of planets, PROTOSTARS |
| Abstract: |
We present the results of the observations made within the ALMA Large Program called Early Planet Formation in Embedded disks of the Class 0 protostar GSS30 IRS3. Our observations included the 1.3 mm continuum with a resolution of 0″.05 (7.8 au) and several molecular species, including 12CO, 13CO, C18O, H2CO, and c-C3H2. The dust continuum analysis unveiled a disk-shaped structure with a major axis of ~200 au. We observed an asymmetry in the minor axis of the continuum emission suggesting that the emission is optically thick and the disk is flared. On the other hand, we identified two prominent bumps along the major axis located at distances of 26 and 50 au from the central protostar. The origin of the bumps remains uncertain and might be an embedded substructure within the disk or the temperature distribution and not the surface density because the continuum emission is optically thick. The 12CO emission reveals a molecular outflow consisting of three distinct components: a collimated component, an intermediate-velocity component exhibiting an hourglass shape, and a wider angle low-velocity component. We associate these components with the coexistence of a jet and a disk wind. The C18O emission traces both a circumstellar disk in Keplerian rotation and the infall of the rotating envelope. We measured a stellar dynamical mass of 0.35 ±0.09 M⊙. [ABSTRACT FROM AUTHOR] |
|
Copyright of Astronomy & Astrophysics / Astronomie et Astrophysique is the property of EDP Sciences and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.) |
| Database: |
Complementary Index |
