Candidate young stellar objects in the S-cluster: Kinematic
analysis of a subpopulation of the low-mass G objects close to
Sgr A

J 2024

Candidate young stellar objects in the S-cluster: Kinematic analysis of a subpopulation of the low-mass G objects close to Sgr A

PEISSKER, F., Michal ZAJAČEK, M. MELAMED, B. ALI, M. SINGHAL et. al.

Basic information

Original name

Candidate young stellar objects in the S-cluster: Kinematic analysis of a subpopulation of the low-mass G objects close to Sgr A

Authors

PEISSKER, F., Michal ZAJAČEK (703 Slovakia, belonging to the institution), M. MELAMED, B. ALI, M. SINGHAL, T. DASSEL, A. ECKART and V. KARAS

Edition

Astronomy and Astrophysics, EDP Sciences, 2024, 0004-6361

Other information

Language

English

Type of outcome

Článek v odborném periodiku

Field of Study

10308 Astronomy

Country of publisher

France

Confidentiality degree

není předmětem státního či obchodního tajemství

References:

URL URL

Impact factor

Impact factor: 6.500 in 2022

Organization unit

Faculty of Science

DOI

http://dx.doi.org/10.1051/0004-6361/202449729

UT WoS

001247650500010

Keywords in English

stars: black holes; stars: formation; Galaxy: center; galaxies: star formation

Abstract

V originále

Context. The observation of several L-band emission sources in the S cluster has led to a rich discussion of their nature. However, a definitive answer to the classification of the dusty objects requires an explanation for the detection of compact Doppler-shifted Br gamma emission. The ionized hydrogen in combination with the observation of mid-infrared L-band continuum emission suggests that most of these sources are embedded in a dusty envelope. These embedded sources are part of the S-cluster, and their relationship to the S-stars is still under debate. To date, the question of the origin of these two populations has been vague, although all explanations favor migration processes for the individual cluster members. Aims. This work revisits the S-cluster and its dusty members orbiting the supermassive black hole Sgr A* on bound Keplerian orbits from a kinematic perspective. The aim is to explore the Keplerian parameters for patterns that might imply a nonrandom distribution of the sample. Additionally, various analytical aspects are considered to address the nature of the dusty sources. Methods. Based on the photometric analysis, we estimated the individual H - K and K - L colors for the source sample and compared the results to known cluster members. The classification revealed a noticeable contrast between the S-stars and the dusty sources. To fit the flux-density distribution, we utilized the radiative transfer code HYPERION and implemented a young stellar object Class I model. We obtained the position angle from the Keplerian fit results; additionally, we analyzed the distribution of the inclinations and the longitudes of the ascending node. Results. The colors of the dusty sources suggest a stellar nature consistent with the spectral energy distribution in the near and mid-infrared domains. Furthermore, the evaporation timescales of dusty and gaseous clumps in the vicinity of Sgr A* are much shorter (<< 2 yr) than the epochs covered by the observations (approximate to 15 yr). In addition to the strong evidence for the stellar classification of the D-sources, we also find a clear disk-like pattern following the arrangements of S-stars proposed in the literature. Furthermore, we find a global intrinsic inclination for all dusty sources of 60 +/- 20 degrees, implying a common formation process. Conclusions. The pattern of the dusty sources manifested in the distribution of the position angles, inclinations, and longitudes of the ascending node strongly suggests two different scenarios: the main-sequence stars and the dusty stellar S-cluster sources share a common formation history or migrated with a similar formation channel in the vicinity of Sgr A*. Alternatively, the gravitational influence of Sgr A* in combination with a massive perturber, such as a putative intermediate mass black hole in the IRS 13 cluster, forces the dusty objects and S-stars to follow a particular orbital arrangement.

Links

GM24-10599M, research and development project

Name: Hvězdy v galaktických jádrech: vzájemný vztah s masivními černými dírami

Investor: Czech Science Foundation, Stars in galactic nuclei: interrelation with massive black holes

Citovat

PEISSKER, F., Michal ZAJAČEK, M. MELAMED, B. ALI, M. SINGHAL, T. DASSEL, A. ECKART and V. KARAS. Candidate young stellar objects in the S-cluster: Kinematic analysis of a subpopulation of the low-mass G objects close to Sgr A. Astronomy and Astrophysics. EDP Sciences, 2024, vol. 686, June 2024, p. 1-32. ISSN 0004-6361. Available from: https://dx.doi.org/10.1051/0004-6361/202449729.

@article{2417426,
   author = {Peissker, F. and Zajaček, Michal and Melamed, M. and Ali, B. and Singhal, M. and Dassel, T. and Eckart, A. and Karas, V.},
   article_number = {June 2024},
   doi = {http://dx.doi.org/10.1051/0004-6361/202449729},
   keywords = {stars: black holes; stars: formation; Galaxy: center; galaxies: star formation},
   language = {eng},
   issn = {0004-6361},
   journal = {Astronomy and Astrophysics},
   title = {Candidate young stellar objects in the S-cluster: Kinematic analysis of a subpopulation of the low-mass G objects close to Sgr A},
   url = {https://www.aanda.org/articles/aa/full_html/2024/06/aa49729-24/aa49729-24.html},
   volume = {686},
   year = {2024}
}

TY  - JOUR
ID  - 2417426
AU  - Peissker, F. - Zajaček, Michal - Melamed, M. - Ali, B. - Singhal, M. - Dassel, T. - Eckart, A. - Karas, V.
PY  - 2024
TI  - Candidate young stellar objects in the S-cluster: Kinematic analysis of a subpopulation of the low-mass G objects close to Sgr A
JF  - Astronomy and Astrophysics
VL  - 686
IS  - June 2024
SP  - 1-32
EP  - 1-32
PB  - EDP Sciences
SN  - 00046361
KW  - stars: black holes
KW  - stars: formation
KW  - Galaxy: center
KW  - galaxies: star formation
UR  - https://www.aanda.org/articles/aa/full_html/2024/06/aa49729-24/aa49729-24.html
N2  - Context. The observation of several L-band emission sources in the S cluster has led to a rich discussion of their nature. However, a definitive answer to the classification of the dusty objects requires an explanation for the detection of compact Doppler-shifted Br gamma emission. The ionized hydrogen in combination with the observation of mid-infrared L-band continuum emission suggests that most of these sources are embedded in a dusty envelope. These embedded sources are part of the S-cluster, and their relationship to the S-stars is still under debate. To date, the question of the origin of these two populations has been vague, although all explanations favor migration processes for the individual cluster members. Aims. This work revisits the S-cluster and its dusty members orbiting the supermassive black hole Sgr A* on bound Keplerian orbits from a kinematic perspective. The aim is to explore the Keplerian parameters for patterns that might imply a nonrandom distribution of the sample. Additionally, various analytical aspects are considered to address the nature of the dusty sources. Methods. Based on the photometric analysis, we estimated the individual H - K and K - L colors for the source sample and compared the results to known cluster members. The classification revealed a noticeable contrast between the S-stars and the dusty sources. To fit the flux-density distribution, we utilized the radiative transfer code HYPERION and implemented a young stellar object Class I model. We obtained the position angle from the Keplerian fit results; additionally, we analyzed the distribution of the inclinations and the longitudes of the ascending node. Results. The colors of the dusty sources suggest a stellar nature consistent with the spectral energy distribution in the near and mid-infrared domains. Furthermore, the evaporation timescales of dusty and gaseous clumps in the vicinity of Sgr A* are much shorter (<< 2 yr) than the epochs covered by the observations (approximate to 15 yr). In addition to the strong evidence for the stellar classification of the D-sources, we also find a clear disk-like pattern following the arrangements of S-stars proposed in the literature. Furthermore, we find a global intrinsic inclination for all dusty sources of 60 +/- 20 degrees, implying a common formation process. Conclusions. The pattern of the dusty sources manifested in the distribution of the position angles, inclinations, and longitudes of the ascending node strongly suggests two different scenarios: the main-sequence stars and the dusty stellar S-cluster sources share a common formation history or migrated with a similar formation channel in the vicinity of Sgr A*. Alternatively, the gravitational influence of Sgr A* in combination with a massive perturber, such as a putative intermediate mass black hole in the IRS 13 cluster, forces the dusty objects and S-stars to follow a particular orbital arrangement.
ER  -

PEISSKER, F., Michal ZAJAČEK, M. MELAMED, B. ALI, M. SINGHAL, T. DASSEL, A. ECKART and V. KARAS. Candidate young stellar objects in the S-cluster: Kinematic analysis of a subpopulation of the low-mass G objects close to Sgr A. \textit{Astronomy and Astrophysics}. EDP Sciences, 2024, vol.~686, June 2024, p.~1-32. ISSN~0004-6361. Available from: https://dx.doi.org/10.1051/0004-6361/202449729.

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