Unveiling the hot molecular core in the ultracompact H II region with extended emission G12.21-0.10
Abstract We present a multiwavelength study of the cometary H II region G12.21-0.10 using the VLA and OVRO. Both radio continuum (0.3, 0.7, 2 and 3.6 cm) and spectral lines of H41α, 13CS(2−1) & (1−0), and NH3(2,2) & (4,4) observations are included. We find two 3 mm continuum peaks toward G12.21-0.10; one of them is spatially coincident with the UC H II region, while the other coincides spatially with a molecular clump. We also find that the 0.7, 2 and 3.6 cm continuum and H41α line are only detected toward the UC H II region, while the 13CS, and NH3 are spatially associated with the molecular clump. Based on the morphology, kinetic temperature (≈86 K), volumetric density (≈1.5×106 cm−3) and linear size (≈0.22 pc) of the molecular clump, we suggest this source is consistent with a hot molecular core.
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Universidad Nacional Autónoma de México, Instituto de Astronomía
2018
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oai:scielo:S0185-110120180001000092019-08-05Unveiling the hot molecular core in the ultracompact H II region with extended emission G12.21-0.10Fuente,E. de laTrinidad,M. A.Porras,A.Rodríguez-Rico,C.Araya,E. D.Kurtz,S.Hofner,P.Nigoche-Netro,A. ISM: clouds ISM: molecules molecular processes radio continuum: ISM radio lines: ISM stars: formation Abstract We present a multiwavelength study of the cometary H II region G12.21-0.10 using the VLA and OVRO. Both radio continuum (0.3, 0.7, 2 and 3.6 cm) and spectral lines of H41α, 13CS(2−1) & (1−0), and NH3(2,2) & (4,4) observations are included. We find two 3 mm continuum peaks toward G12.21-0.10; one of them is spatially coincident with the UC H II region, while the other coincides spatially with a molecular clump. We also find that the 0.7, 2 and 3.6 cm continuum and H41α line are only detected toward the UC H II region, while the 13CS, and NH3 are spatially associated with the molecular clump. Based on the morphology, kinetic temperature (≈86 K), volumetric density (≈1.5×106 cm−3) and linear size (≈0.22 pc) of the molecular clump, we suggest this source is consistent with a hot molecular core.info:eu-repo/semantics/openAccessUniversidad Nacional Autónoma de México, Instituto de AstronomíaRevista mexicana de astronomía y astrofísica v.54 n.1 20182018-01-01info:eu-repo/semantics/articletext/htmlhttp://www.scielo.org.mx/scielo.php?script=sci_arttext&pid=S0185-11012018000100009en |
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| author |
Fuente,E. de la Trinidad,M. A. Porras,A. Rodríguez-Rico,C. Araya,E. D. Kurtz,S. Hofner,P. Nigoche-Netro,A. |
| spellingShingle |
Fuente,E. de la Trinidad,M. A. Porras,A. Rodríguez-Rico,C. Araya,E. D. Kurtz,S. Hofner,P. Nigoche-Netro,A. Unveiling the hot molecular core in the ultracompact H II region with extended emission G12.21-0.10 |
| author_facet |
Fuente,E. de la Trinidad,M. A. Porras,A. Rodríguez-Rico,C. Araya,E. D. Kurtz,S. Hofner,P. Nigoche-Netro,A. |
| author_sort |
Fuente,E. de la |
| title |
Unveiling the hot molecular core in the ultracompact H II region with extended emission G12.21-0.10 |
| title_short |
Unveiling the hot molecular core in the ultracompact H II region with extended emission G12.21-0.10 |
| title_full |
Unveiling the hot molecular core in the ultracompact H II region with extended emission G12.21-0.10 |
| title_fullStr |
Unveiling the hot molecular core in the ultracompact H II region with extended emission G12.21-0.10 |
| title_full_unstemmed |
Unveiling the hot molecular core in the ultracompact H II region with extended emission G12.21-0.10 |
| title_sort |
unveiling the hot molecular core in the ultracompact h ii region with extended emission g12.21-0.10 |
| description |
Abstract We present a multiwavelength study of the cometary H II region G12.21-0.10 using the VLA and OVRO. Both radio continuum (0.3, 0.7, 2 and 3.6 cm) and spectral lines of H41α, 13CS(2−1) & (1−0), and NH3(2,2) & (4,4) observations are included. We find two 3 mm continuum peaks toward G12.21-0.10; one of them is spatially coincident with the UC H II region, while the other coincides spatially with a molecular clump. We also find that the 0.7, 2 and 3.6 cm continuum and H41α line are only detected toward the UC H II region, while the 13CS, and NH3 are spatially associated with the molecular clump. Based on the morphology, kinetic temperature (≈86 K), volumetric density (≈1.5×106 cm−3) and linear size (≈0.22 pc) of the molecular clump, we suggest this source is consistent with a hot molecular core. |
| publisher |
Universidad Nacional Autónoma de México, Instituto de Astronomía |
| publishDate |
2018 |
| url |
http://www.scielo.org.mx/scielo.php?script=sci_arttext&pid=S0185-11012018000100009 |
| work_keys_str_mv |
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1756220880985260032 |