Monitoring dusty sources in the vicinity of Sagittarius A*

0536734 - ASÚ 2021 RIV FR eng J - Journal Article
Peissker, F. - Hosseini, E. - Zajaček, M. - Eckart, A. - Saalfeld, R. - Valencia-S, M. - Parsa, M. - Karas, Vladimír
Monitoring dusty sources in the vicinity of Sagittarius A*.
Astronomy & Astrophysics. Roč. 634, February (2020), č. článku A35. ISSN 0004-6361. E-ISSN 1432-0746
R&D Projects: GA ČR(CZ) GC19-01137J
Institutional support: RVO:67985815
Keywords : stars * black holes * abundances
OECD category: Astronomy (including astrophysics,space science)
Impact factor: 5.803, year: 2020
Method of publishing: Limited access
https://doi.org/10.1051/0004-6361/201935953

Using SINFONI, we are able to determine the spectroscopic properties of the dusty infrared sources. Furthermore, we can extract spatial and velocity information of these objects. We are able to identify X7, X7.1, X8, G1, DSO/G2, D2, D23, D3, D3.1, D5, and D9 in the Doppler-shifted line maps of the SINFONI H + K data. From our K- and L '-band NACO data, we derive the related magnitudes of the brightest sources located west of Sgr A*. The spectroscopic analysis indicates that the investigated objects could be dust-embedded pre-main-sequence stars. The Doppler-shifted [FeIII] line can be spectroscopically identified in several sources that are located between 17:45:40.05 and 17:45:42.00 in Dec However, the sources with a DEC less than 17:45:40.05 show no [FeIII] emission. Therefore, these two groups show different spectroscopic features that could be explained by the interaction with a non-spherical outflow that originates at the position of Sgr A*. Following this, the hot bubble around Sgr A* consists out of isolated sources with [FeIII] line emission that can partially account for the previously detected [FeIII] distribution on larger scales.
Permanent Link: http://hdl.handle.net/11104/0314457