| Full text | |
| Author(s): Show less - |
Surcis, G.
;
Vlemmings, W. H. T.
;
Goddi, C.
;
Torrelles, J. M.
;
Gomez, J. F.
;
Rodriguez-Kamenetzky, A.
;
Carrasco-Gonzalez, C.
;
Curiel, S.
;
Kim, S. -W
;
Kim, J. -S
;
van Langevelde, H. J.
Total Authors: 11
|
| Document type: | Journal article |
| Source: | Astronomy & Astrophysics; v. 673, p. 32-pg., 2023-04-24. |
| Abstract | |
Context. Several radio sources have been detected in the high-mass star-forming region W75N(B), with the massive young stellar objects VLA1 and VLA2 shown to be of particular interest among them. These objects are thought to be at di fferent evolutionary stages: VLA1 is in the early stage of photoionization and driving a thermal radio jet, while VLA2 is a thermal, collimated ionized wind surrounded by a dusty disk or envelope. In both sources, 22 GHz H2O masers have been detected in the past. Those around VLA1 show a persistent linear distribution along the thermal radio jet, while those around VLA2 have traced the evolution from a non-collimated to a collimated outflow over a period of similar to 20 yr. The magnetic field inferred from the H2O masers has shown an orientation rotation following the direction of the major-axis of the shell around VLA2, whereas it is immutable around VLA1. Aims. By monitoring the polarized emission of the 22 GHz H2O masers around both VLA1 and VLA2 over a period of six years, we aim to determine whether the H2O maser distributions show any variation over time and whether the magnetic field behaves accordingly. Methods. The European VLBI Network was used in full polarization and phase-reference mode in order to determine the absolute positions of the 22 GHz H2O masers with a beam size of similar to 1 mas and to determine the orientation and the strength of the magnetic field. We observed four epochs separated by two years from 2014 to 2020. Results. We detected polarized emission from the H2O masers around both VLA1 and VLA2 in all the epochs. By comparing the H2O masers detected in the four epochs, we find that the masers around VLA1 are tracing a nondissociative shock originating from the expansion of the thermal radio jet, while the masers around VLA2 are tracing an asymmetric expansion of the gas that is halted in the northeast where the gas likely encounters a very dense medium. We also found that the magnetic field inferred from the H2O masers in each epoch can be considered as a portion of a quasi-static magnetic field estimated in that location rather than in that time. This allowed us to study the morphology of the magnetic field around both VLA1 and VLA2 locally across a larger area by considering the vectors estimated in all the epochs as a whole. We find that the magnetic field in VLA1 is located along the jet axis, bending toward the north and south at the northeasterly and southwesterly ends of the jet, respectively, reconnecting with the large-scale magnetic field. The magnetic field in VLA2 is perpendicular to the expansion directions until it encounters the denser matter in the northeast, where the magnetic field is parallel to the expansion direction and agrees with the large-scale magnetic field. We also measured the magnetic field strength along the line of sight in three of the four epochs, with resulting values of -764mG < B-||(VLA1) < -676mG and -355mG < B-||(VLA2) < -2426 mG. (AU) | |
| FAPESP's process: | 21/01183-8 - Astrophysical jets at the highest-angular resolution with very long baseline interferometry |
| Grantee: | Ciriaco Goddi |
| Support Opportunities: | Research Grants - Young Investigators Grants |