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Searching for stellar population in the molecular cloud GRSMC 045.49+00.04

Published online by Cambridge University Press:  25 September 2024

Naira Azatyan Open the ORCID record for Naira Azatyan [Opens in a new window] ,
Elena Nikoghosyan Open the ORCID record for Elena Nikoghosyan [Opens in a new window] ,
Anahit Samsonyan Open the ORCID record for Anahit Samsonyan [Opens in a new window] ,
Davide Elia ,
Lex Kaper ,
Ararat Yeghikyan ,
Derenik Andreasyan  and
Daniel Baghdasaryan
Naira Azatyan*
Affiliation:
Byurakan Astrophysical Observatory, Aragatsotn Province, Byurakan, Armenia
Elena Nikoghosyan
Affiliation:
Byurakan Astrophysical Observatory, Aragatsotn Province, Byurakan, Armenia
Anahit Samsonyan
Affiliation:
Byurakan Astrophysical Observatory, Aragatsotn Province, Byurakan, Armenia
Davide Elia
Affiliation:
NAF – Istituto di Astrofisica e Planetologia Spaziali, Roma, Italy
Lex Kaper
Affiliation:
Anton Pannekoek Institute, University of Amsterdam, Amsterdam, The Netherlands
Ararat Yeghikyan
Affiliation:
Byurakan Astrophysical Observatory, Aragatsotn Province, Byurakan, Armenia
Derenik Andreasyan
Affiliation:
Byurakan Astrophysical Observatory, Aragatsotn Province, Byurakan, Armenia
Daniel Baghdasaryan
Affiliation:
Byurakan Astrophysical Observatory, Aragatsotn Province, Byurakan, Armenia
*
Corresponding author: Naira Azatyan; Email: [email protected].
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Abstract

Understanding the characteristics of young stellar populations is essential for deriving insights into star formation processes within parent molecular clouds and the influence of massive stars on these processes. This study primarily aims to investigate the young stellar objects (YSOs) within the molecular cloud G 045.49+00.04, including three ultra-compact HII (UC HII) regions: G 45.48+0.13 (IRAS 19117+1107), G 45.45+0.06 (IRAS 19120+1103), and G 45.47+0.05. We used near-, mid-, and far-infrared photometric data along with radiation transfer models and the modified blackbody fitting to identify and study the YSOs and the interstellar medium (ISM). In total, we identified 1482 YSOs in a 12 arcmin radius covering GRSMC 045.49+00.04, with a mass range from 1.5 M${}_{\odot}$ to 22 M${}_{\odot}$. Of these, 315 objects form relatively dense clusters in the UC HII regions, close to the IRAS 19120+1103 and 19117+1107 sources. In each UC HII region, several high-mass stars have been identified, which in all likelihood are responsible for the ionization. The YSOs with 21.8 M${}_{\odot}$ and 13.7 ± 0.4 M${}_{\odot}$ are associated with IRAS 19120+1103 and 19117+1107, respectively. The non-cluster YSOs (1168) are uniformly distributed on the field. The distribution of YSOs from both samples on the colour-magnitude diagram and by the evolutionary ages is different. About 75% of objects in the IRAS clusters are concentrated around the Zero Age Main Sequence and have a well-defined peak at an age of Log(Age[years]) $\approx$ 6.75, with a narrow spread. The non-cluster objects have two concentrations located to the right and left of the 0.1 Myr isochrone and two well-defined peaks at Log(Age) $\approx$ 6.25 and 5.25. The fraction of the near-infrared excess stars, as well as the mass function confirm that the evolutionary age of the cluster is about 1 Myr. The K luminosity functions’ α slopes for the IRAS clusters and non-cluster objects are 0.32 ± 0.04 and 0.72 ± 0.13, respectively. The steeper α slope is suggesting that the non-cluster objects are less evolved, which is well consistent with the evolutionary age. Similar results – including evolutionary age, narrow age spread, and the less evolved nature of non-cluster objects – were also observed for the YSOs in the neighbouring G 45.14+00.14. The both regions (G 045.49+00.04 and G 45.14+00.14) are located and distinguished by their brightness and density at the edge of the bubble around the highly variable X-ray binary GRS 1915+105, which includes a black hole and a K-giant companion. Based on the above, we can assume that the process of star formation in the young IRAS clusters was triggered by the GRS 1915+105-initiated shock front inside the ISM massive condensation, through the process of ‘collecting and collapse’. Most non-cluster objects probably belong to a later generation. Their formation could be triggered by the recurrent activity of GRS 1915+105 and/or through the edge collapse scenario and mass accumulation through the gas flows along the ISM filaments.

Keywords

Stars: formationstars: pre-main sequence(ISM:) HII regionsISM: bubbles
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 41 , 2024 , e055
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© The Author(s), 2024. Published by Cambridge University Press on behalf of Astronomical Society of Australia

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