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| Autores principales: | , , , , , , , |
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| Formato: | Preprint |
| Publicado: |
2025
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| Acceso en línea: | https://arxiv.org/abs/2504.06170 |
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| _version_ | 1866910906683752448 |
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| author | Maity, A. K. Dewangan, L. K. Jadhav, O. R. Sharma, Saurabh Yadav, Ram Kesh Fukui, Y. Sano, H. Inoue, T. |
| author_facet | Maity, A. K. Dewangan, L. K. Jadhav, O. R. Sharma, Saurabh Yadav, Ram Kesh Fukui, Y. Sano, H. Inoue, T. |
| contents | We present a multi-wavelength study of an extended area hosting the bubble N59-North to explore the physical processes driving massive star formation (MSF). The Spitzer 8 $μ$m image reveals an elongated/filamentary infrared-dark cloud (length $\sim$28 pc) associated with N59-North, which contains several protostars and seven ATLASGAL dust clumps at the same distance. The existence of this filament is confirmed through $^{13}$CO and NH$_3$ molecular line data in a velocity range of [95, 106] km s$^{-1}$. All dust clumps satisfy Kauffmann & Pillai's condition for MSF. Using Spitzer 8 $μ$m image, a new embedded hub-filament system candidate (C-HFS) is investigated toward the ATLASGAL clump, located near the filament's central region. MeerKAT 1.3 GHz continuum emission, detected for the first time toward C-HFS, reveals an ultracompact HII region driven by a B2-type star, suggesting an early stage of HFS with minimal feedback from the young massive star. The comparison of the position-velocity (PV) and position-position-velocity (PPV) diagrams with existing theoretical models suggests that rotation, central collapse, and end-dominated collapse are not responsible for the observed gas motion in the filament. The PPV diagram indicates the expansion of N59-North by revealing blue- and red-shifted gas velocities at the edge of the bubble. Based on comparisons with magnetohydrodynamic simulations, this study suggests that cloud-cloud collision (CCC) led to the formation of the filament, likely giving it a conical structure with gas converging toward its central region, where C-HFS is located. Overall, the study supports multi-scale filamentary mass accretion for MSF, likely triggered by CCC. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_06170 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Investigating Embedded Structures and Gas Kinematics in the IRDC Hosting Bubble N59-North Maity, A. K. Dewangan, L. K. Jadhav, O. R. Sharma, Saurabh Yadav, Ram Kesh Fukui, Y. Sano, H. Inoue, T. Astrophysics of Galaxies We present a multi-wavelength study of an extended area hosting the bubble N59-North to explore the physical processes driving massive star formation (MSF). The Spitzer 8 $μ$m image reveals an elongated/filamentary infrared-dark cloud (length $\sim$28 pc) associated with N59-North, which contains several protostars and seven ATLASGAL dust clumps at the same distance. The existence of this filament is confirmed through $^{13}$CO and NH$_3$ molecular line data in a velocity range of [95, 106] km s$^{-1}$. All dust clumps satisfy Kauffmann & Pillai's condition for MSF. Using Spitzer 8 $μ$m image, a new embedded hub-filament system candidate (C-HFS) is investigated toward the ATLASGAL clump, located near the filament's central region. MeerKAT 1.3 GHz continuum emission, detected for the first time toward C-HFS, reveals an ultracompact HII region driven by a B2-type star, suggesting an early stage of HFS with minimal feedback from the young massive star. The comparison of the position-velocity (PV) and position-position-velocity (PPV) diagrams with existing theoretical models suggests that rotation, central collapse, and end-dominated collapse are not responsible for the observed gas motion in the filament. The PPV diagram indicates the expansion of N59-North by revealing blue- and red-shifted gas velocities at the edge of the bubble. Based on comparisons with magnetohydrodynamic simulations, this study suggests that cloud-cloud collision (CCC) led to the formation of the filament, likely giving it a conical structure with gas converging toward its central region, where C-HFS is located. Overall, the study supports multi-scale filamentary mass accretion for MSF, likely triggered by CCC. |
| title | Investigating Embedded Structures and Gas Kinematics in the IRDC Hosting Bubble N59-North |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2504.06170 |