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| Autores principales: | , , , , , , , |
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| Formato: | Preprint |
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2026
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| Acceso en línea: | https://arxiv.org/abs/2603.16425 |
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| author | Jadhav, O. R. Dewangan, L. K. Zinchenko, I. I. Pillai, Thushara G. S. Sanhueza, Patricio Maity, A. K. Yadav, Ram K. Sharma, Saurabh |
| author_facet | Jadhav, O. R. Dewangan, L. K. Zinchenko, I. I. Pillai, Thushara G. S. Sanhueza, Patricio Maity, A. K. Yadav, Ram K. Sharma, Saurabh |
| contents | We present the SOFIA/HAWC+ 214 $μ$m polarimetric observations toward the infrared dark cloud G351.77-0.53 (hereafter G351), complemented by existing multi-wavelength data sets. Infrared excess from the embedded sources indicate ongoing star formation activity in the cloud. The G351 cloud hosts two prominent star-forming clumps, i.e., c1 and c2. The plane-of-the-sky magnetic field lines from Planck observations are predominantly oriented perpendicular to the filament's major axis. Magnetic field orientations from SOFIA/HAWC+ 214 $μ$m observations reveal distinct hourglass-shaped field configuration toward c1, while the field lines remain perpendicular to the rest of the filament. Using the Davis-Chandrasekhar-Fermi method, we estimate a mean plane-of-the-sky magnetic field strength of $\sim$147 $\pm$ 60 $μ$G in the G351 filament, with values reaching $\sim$0.8 mG toward c1. The mass-to-flux ratio analysis indicates that the filament is magnetically transcritical, where the gravitational and magnetic field energies are comparable. The hourglass-shaped magnetic field observed toward c1 could result from magnetically regulated gravitational collapse, the alignment of converging sub-filaments with the magnetic field, or a combination of both processes. The energy budget analysis further indicates that magnetic fields play an important role in governing the cloud's gas dynamics, followed by contributions from turbulence and gravity. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2603_16425 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Unveiling an Hourglass-Shaped Magnetic Field toward IRDC G351.77-0.53 Jadhav, O. R. Dewangan, L. K. Zinchenko, I. I. Pillai, Thushara G. S. Sanhueza, Patricio Maity, A. K. Yadav, Ram K. Sharma, Saurabh Astrophysics of Galaxies We present the SOFIA/HAWC+ 214 $μ$m polarimetric observations toward the infrared dark cloud G351.77-0.53 (hereafter G351), complemented by existing multi-wavelength data sets. Infrared excess from the embedded sources indicate ongoing star formation activity in the cloud. The G351 cloud hosts two prominent star-forming clumps, i.e., c1 and c2. The plane-of-the-sky magnetic field lines from Planck observations are predominantly oriented perpendicular to the filament's major axis. Magnetic field orientations from SOFIA/HAWC+ 214 $μ$m observations reveal distinct hourglass-shaped field configuration toward c1, while the field lines remain perpendicular to the rest of the filament. Using the Davis-Chandrasekhar-Fermi method, we estimate a mean plane-of-the-sky magnetic field strength of $\sim$147 $\pm$ 60 $μ$G in the G351 filament, with values reaching $\sim$0.8 mG toward c1. The mass-to-flux ratio analysis indicates that the filament is magnetically transcritical, where the gravitational and magnetic field energies are comparable. The hourglass-shaped magnetic field observed toward c1 could result from magnetically regulated gravitational collapse, the alignment of converging sub-filaments with the magnetic field, or a combination of both processes. The energy budget analysis further indicates that magnetic fields play an important role in governing the cloud's gas dynamics, followed by contributions from turbulence and gravity. |
| title | Unveiling an Hourglass-Shaped Magnetic Field toward IRDC G351.77-0.53 |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2603.16425 |