The structure of the IRAS05168+3634 star-forming region

Nikoghosyan, E. H.; Azatyan, N. M.; Andreasyan, D.; Baghdasaryan, D. S.

doi:10.1007/s10509-021-04023-4

Cited by 3 publications

(4 citation statements)

References 35 publications

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“…The second one is a physically connected pair of ultra compact H II (UCHII) regions, G45.07+0.13 and G45.12+0.13, associated with IRAS 19110+1045 and IRAS 19111+1048 sources, respectively. For both regions, detailed studies of both the ISM and the stars were carried out in Azatyan (2019), Azatyan et al (2022), Nikoghosyan et al (2021).…”

Section: Description Of Star-forming Regionsmentioning

confidence: 99%

“…According to Sakai et al (2012) the trigonometric parallax of IRAS 05168+3634 is 0.532 ± 0.053 mas, which corresponds to a distance of 1.88 +0.21 −0.17 kpc. Based on the Gaia EDR3 database, in Nikoghosyan et al (2021) it was shown that all IRAS sub-regions belong to the same molecular cloud, which is located at a distance of ∼ 1.9 kpc.…”

Section: Iras 05168+3634 Regionmentioning

confidence: 99%

“…Based on the FIR Herschel database it was shown that the ISM has an inhomogeneous structure, forming relativity dense clumps around the IRAS sources, which are interconnected by a filament structure (Nikoghosyan et al, 2021). In general, in the sub-regions T d varies from 11 to 24 K, and N(H 2 ) -from 1.0 to 4.0 × 10 23 cm −2 .…”

Section: Iras 05168+3634 Regionmentioning

confidence: 99%

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Properties of interstellar matter and stellar population in two star-forming regions

Nikoghosyan

2022

ComBAO

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This study aims to compare the properties of interstellar medium in two star-forming regions with different stellar content, with and without high-mass YSOs. The first region is an extended molecular cloud surrounding five IRAS sources: 05168+3634, 05184+3635, 05177+3636, 05162+3639, and IRAS 05156+3643. The second one is a physically connected pair of ultra compact HII regions, G45.07+0.13 & G45.12+0.13, associated with IRAS 19110+1045 and IRAS 19111+1048 sources, respectively. Using these two star formation regions as an example, one can see the relationship between the initial parameters of the parent molecular cloud (hydrogen column density, dust temperature), the process of star formation itself (external triggering shock or independent condensations), and the parameters of the stellar content. High-mass YSOs were obtained only in the G45.07+0.13 & G45.12+0.13 regions, in which, apparently, the initial density of the parent molecular cloud was higher and the star formation process was initiated by an external triggering shock. In addition, in the IRAS 05168+3634 region, there is a relationship between the density of the interstellar medium and the activity of the star formation process. In those subregions, where the mass and density of the initial, parent molecular cloud is greater, the process of star formation is likely to be more active and have a longer duration. In addition, in these sub-groups, on average, the mass of stars is larger.

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Section: Description Of Star-forming Regionsmentioning

confidence: 99%

Section: Iras 05168+3634 Regionmentioning

confidence: 99%

Section: Iras 05168+3634 Regionmentioning

confidence: 99%

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Properties of interstellar matter and stellar population in two star-forming regions

Nikoghosyan

2022

ComBAO

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“…For all regions a detailed study was conducted, which includes the following topics: 1) determination of the parameters of ISM, namely the distribution of N(H 2 ) hydrogen column density and T d dust temperature; 2) the search for young stellar clusters; 3) identification of the clusters' members using their infrared properties; 4) investigation of the structural properties of the young stellar clusters; 5) determination of the age and age spread of the clusters' members; 6) construction of the Luminosity Functions and Mass Functions for the clusters. This thesis is based on the papers Azatyan (2019), Azatyan & Nikoghosyan (2018), Azatyan et al (2016Azatyan et al ( , 2020Azatyan et al ( , 2022, Nikoghosyan & Azatyan (2014), Nikoghosyan et al (2020Nikoghosyan et al ( , 2021.…”

Section: Introductionmentioning

confidence: 99%

Search and study of young infrared stellar clusters

Azatyan

2022

ComBAO

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The “bricks” of the Galactic disc are giant molecular clouds, which are birthplaces of stellar population. Therefore, there is a genetic connection between young stellar objects (YSOs) and their surrounding Interstellar Medium (ISM). The thesis is devoted to a search for young stellar clusters in the vicinity of IRAS sources and a detailed study of three selected star-forming regions: IRAS 05137+3919, 05168+3634, and 19110+1045, which includes determining the parameters of the ISM based on far-infrared data, the identification and classification of YSOs using color-color and color-magnitude diagrams, the modeling of stellar parameters, and the construction and interpretation of the luminosity functions. It is likely that the three young stellar clusters were formed under different scenarios. The age spread of the IRAS05137+3919 and IRAS05168+3634 regions is much larger, and, therefore, we concluded that the stellar population is formed as a result of independent condensations. The age spread of the IRAS clusters’ members in the third region, which is a pair of ultra-compact HII regions (UCHIIs), namely G45.12+0.13 and G45.07+0.13, is small. The small age spread suggests that the clusters may originate from a single triggering event. Moreover, high-mass YSOs were obtained only in the G45.07+0.13 and G45.12+0.13 UCHII regions where the ISM initial density was higher and the star formation proceeded relatively quickly.

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Search and study of young infrared stellar clusters

Azatyan

2024

Astrophys Space Sci

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The structure of the IRAS05168+3634 star-forming region

Cited by 3 publications

References 35 publications

Properties of interstellar matter and stellar population in two star-forming regions

Properties of interstellar matter and stellar population in two star-forming regions

Search and study of young infrared stellar clusters

Search and study of young infrared stellar clusters

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