A molecular shell with star formation toward the supernova remnant G349.7 + 0.2

A field of about 38′ × 38′ around the supernova remnant (SNR) G349.7 + 0.2 has been surveyed in the CO J = 1-0 transition with the 12 m telescope of the NRAO, using the on-the-fly technique. The resolution of the observations is 54″. We have found that this remnant is interacting with a small CO clo...

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Detalles Bibliográficos
Publicado:	2001
Materias:	ISM: Clouds ISM: Individual (G349.7 + 0.2) ISM: Molecules Stars: Formation Supernova remnants
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046256_v121_n1_p347_Reynoso http://hdl.handle.net/20.500.12110/paper_00046256_v121_n1_p347_Reynoso
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paper:paper_00046256_v121_n1_p347_Reynoso
record_format	dspace
spelling	paper:paper_00046256_v121_n1_p347_Reynoso2023-06-08T14:27:12Z A molecular shell with star formation toward the supernova remnant G349.7 + 0.2 ISM: Clouds ISM: Individual (G349.7 + 0.2) ISM: Molecules Stars: Formation Supernova remnants A field of about 38′ × 38′ around the supernova remnant (SNR) G349.7 + 0.2 has been surveyed in the CO J = 1-0 transition with the 12 m telescope of the NRAO, using the on-the-fly technique. The resolution of the observations is 54″. We have found that this remnant is interacting with a small CO cloud, which, in turn, is part of a much larger molecular complex, which we call the "large CO shell." The large CO shell has a diameter of about 100 pc, an H 2 mass of 9.3 × 10 5 M ⊙ , and a density of 35 cm -3 . We investigate the origin of this structure and suggest as a suitable hypothesis that an old supernova explosion occurred about 4 × 10 6 yr ago. Analyzing the interaction between G349.7 + 0.2 and the large CO shell, it is possible to determine that the shock front currently driven into the molecular gas is a nondissociative shock (C-type), in agreement with the presence of OH 1720 MHz masers. The positional and kinematic coincidence of one of the CO clouds that constitute the large CO shell, an IRAS pointlike source, and an ultracompact H II region indicates the presence of a recently formed star. We suggest that the formation of this star was triggered during the expansion of the large CO shell and suggest the possibility that the same expansion also created the progenitor star of G349.7 + 0.2. The large CO shell would then be one of the few observational examples of supernova-induced star formation. 2001 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046256_v121_n1_p347_Reynoso http://hdl.handle.net/20.500.12110/paper_00046256_v121_n1_p347_Reynoso
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	ISM: Clouds ISM: Individual (G349.7 + 0.2) ISM: Molecules Stars: Formation Supernova remnants
spellingShingle	ISM: Clouds ISM: Individual (G349.7 + 0.2) ISM: Molecules Stars: Formation Supernova remnants A molecular shell with star formation toward the supernova remnant G349.7 + 0.2
topic_facet	ISM: Clouds ISM: Individual (G349.7 + 0.2) ISM: Molecules Stars: Formation Supernova remnants
description	A field of about 38′ × 38′ around the supernova remnant (SNR) G349.7 + 0.2 has been surveyed in the CO J = 1-0 transition with the 12 m telescope of the NRAO, using the on-the-fly technique. The resolution of the observations is 54″. We have found that this remnant is interacting with a small CO cloud, which, in turn, is part of a much larger molecular complex, which we call the "large CO shell." The large CO shell has a diameter of about 100 pc, an H 2 mass of 9.3 × 10 5 M ⊙ , and a density of 35 cm -3 . We investigate the origin of this structure and suggest as a suitable hypothesis that an old supernova explosion occurred about 4 × 10 6 yr ago. Analyzing the interaction between G349.7 + 0.2 and the large CO shell, it is possible to determine that the shock front currently driven into the molecular gas is a nondissociative shock (C-type), in agreement with the presence of OH 1720 MHz masers. The positional and kinematic coincidence of one of the CO clouds that constitute the large CO shell, an IRAS pointlike source, and an ultracompact H II region indicates the presence of a recently formed star. We suggest that the formation of this star was triggered during the expansion of the large CO shell and suggest the possibility that the same expansion also created the progenitor star of G349.7 + 0.2. The large CO shell would then be one of the few observational examples of supernova-induced star formation.
title	A molecular shell with star formation toward the supernova remnant G349.7 + 0.2
title_short	A molecular shell with star formation toward the supernova remnant G349.7 + 0.2
title_full	A molecular shell with star formation toward the supernova remnant G349.7 + 0.2
title_fullStr	A molecular shell with star formation toward the supernova remnant G349.7 + 0.2
title_full_unstemmed	A molecular shell with star formation toward the supernova remnant G349.7 + 0.2
title_sort	molecular shell with star formation toward the supernova remnant g349.7 + 0.2
publishDate	2001
url	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046256_v121_n1_p347_Reynoso http://hdl.handle.net/20.500.12110/paper_00046256_v121_n1_p347_Reynoso
_version_	1768545952489013248

A molecular shell with star formation toward the supernova remnant G349.7 + 0.2

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