High-resolution CO observations towards the bright eastern knot of the SNR Puppis A

Autores
Paron, S.; Dubner, G.; Reynoso, E.; Rubio, M.
Año de publicación
2008
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Aims.This paper reports molecular observations towards the bright eastern knot (BEK) in the SNR Puppis A, a feature where radio and X-ray studies suggest that the shock front is interacting with a dense molecular clump.Methods.We performed high-resolution millimetric observations towards the BEK of Puppis A using the SEST telescope in the CO -0 and 2-1 lines (beams of 45 and 23, respectively). More extended, lower angular resolution CO -0 observations taken from NANTEN archival data were also analyzed to obtain a complete picture.Results. In the velocity range near 16 km s-1, which is the Puppis A systemic velocity, our study revealed two important properties: (i) no dense molecular gas is detected immediately adjacent to the eastern border of the BEK and (ii) the molecular clump detected very close to the radiocontinuum maximum is probably located in the foreground along the line of sight and has not yet been reached by the SNR shock front. We propose two possible scenarios for explaining the absence of molecular emission eastwards of the BEK border of Puppis A. Either the shock front has completely engulfed and destroyed a molecular clump or the shock front is interacting with part of a larger cloud, and we do not detect CO emission immediately beyond it because the molecules have been dissociated by photodissociation and by reactions with photoionized material due to the radiative precursor. © 2008 ESO.
Fil:Paron, S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
Fil:Dubner, G. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
Fil:Reynoso, E. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
Fuente
Astron. Astrophys. 2008;480(2):439-443
Materia
ISM: clouds
ISM: molecules
ISM: supernova remnants
Data reduction
Radio astronomy
Signal to noise ratio
Space telescopes
ISM: clouds
ISM: molecules
ISM: supernova remnants
Carbon monoxide
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by/2.5/ar
Repositorio
Biblioteca Digital (UBA-FCEN)
Institución
Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
OAI Identificador
paperaa:paper_00046361_v480_n2_p439_Paron

id BDUBAFCEN_d21d850a6e747b95a6598bd0104e8277
oai_identifier_str paperaa:paper_00046361_v480_n2_p439_Paron
network_acronym_str BDUBAFCEN
repository_id_str 1896
network_name_str Biblioteca Digital (UBA-FCEN)
spelling High-resolution CO observations towards the bright eastern knot of the SNR Puppis AParon, S.Dubner, G.Reynoso, E.Rubio, M.ISM: cloudsISM: moleculesISM: supernova remnantsData reductionRadio astronomySignal to noise ratioSpace telescopesISM: cloudsISM: moleculesISM: supernova remnantsCarbon monoxideAims.This paper reports molecular observations towards the bright eastern knot (BEK) in the SNR Puppis A, a feature where radio and X-ray studies suggest that the shock front is interacting with a dense molecular clump.Methods.We performed high-resolution millimetric observations towards the BEK of Puppis A using the SEST telescope in the CO -0 and 2-1 lines (beams of 45 and 23, respectively). More extended, lower angular resolution CO -0 observations taken from NANTEN archival data were also analyzed to obtain a complete picture.Results. In the velocity range near 16 km s-1, which is the Puppis A systemic velocity, our study revealed two important properties: (i) no dense molecular gas is detected immediately adjacent to the eastern border of the BEK and (ii) the molecular clump detected very close to the radiocontinuum maximum is probably located in the foreground along the line of sight and has not yet been reached by the SNR shock front. We propose two possible scenarios for explaining the absence of molecular emission eastwards of the BEK border of Puppis A. Either the shock front has completely engulfed and destroyed a molecular clump or the shock front is interacting with part of a larger cloud, and we do not detect CO emission immediately beyond it because the molecules have been dissociated by photodissociation and by reactions with photoionized material due to the radiative precursor. © 2008 ESO.Fil:Paron, S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.Fil:Dubner, G. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.Fil:Reynoso, E. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.2008info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://hdl.handle.net/20.500.12110/paper_00046361_v480_n2_p439_ParonAstron. Astrophys. 2008;480(2):439-443reponame:Biblioteca Digital (UBA-FCEN)instname:Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturalesinstacron:UBA-FCENenginfo:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/2.5/ar2025-09-29T13:43:00Zpaperaa:paper_00046361_v480_n2_p439_ParonInstitucionalhttps://digital.bl.fcen.uba.ar/Universidad públicaNo correspondehttps://digital.bl.fcen.uba.ar/cgi-bin/oaiserver.cgiana@bl.fcen.uba.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:18962025-09-29 13:43:01.842Biblioteca Digital (UBA-FCEN) - Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturalesfalse
dc.title.none.fl_str_mv High-resolution CO observations towards the bright eastern knot of the SNR Puppis A
title High-resolution CO observations towards the bright eastern knot of the SNR Puppis A
spellingShingle High-resolution CO observations towards the bright eastern knot of the SNR Puppis A
Paron, S.
ISM: clouds
ISM: molecules
ISM: supernova remnants
Data reduction
Radio astronomy
Signal to noise ratio
Space telescopes
ISM: clouds
ISM: molecules
ISM: supernova remnants
Carbon monoxide
title_short High-resolution CO observations towards the bright eastern knot of the SNR Puppis A
title_full High-resolution CO observations towards the bright eastern knot of the SNR Puppis A
title_fullStr High-resolution CO observations towards the bright eastern knot of the SNR Puppis A
title_full_unstemmed High-resolution CO observations towards the bright eastern knot of the SNR Puppis A
title_sort High-resolution CO observations towards the bright eastern knot of the SNR Puppis A
dc.creator.none.fl_str_mv Paron, S.
Dubner, G.
Reynoso, E.
Rubio, M.
author Paron, S.
author_facet Paron, S.
Dubner, G.
Reynoso, E.
Rubio, M.
author_role author
author2 Dubner, G.
Reynoso, E.
Rubio, M.
author2_role author
author
author
dc.subject.none.fl_str_mv ISM: clouds
ISM: molecules
ISM: supernova remnants
Data reduction
Radio astronomy
Signal to noise ratio
Space telescopes
ISM: clouds
ISM: molecules
ISM: supernova remnants
Carbon monoxide
topic ISM: clouds
ISM: molecules
ISM: supernova remnants
Data reduction
Radio astronomy
Signal to noise ratio
Space telescopes
ISM: clouds
ISM: molecules
ISM: supernova remnants
Carbon monoxide
dc.description.none.fl_txt_mv Aims.This paper reports molecular observations towards the bright eastern knot (BEK) in the SNR Puppis A, a feature where radio and X-ray studies suggest that the shock front is interacting with a dense molecular clump.Methods.We performed high-resolution millimetric observations towards the BEK of Puppis A using the SEST telescope in the CO -0 and 2-1 lines (beams of 45 and 23, respectively). More extended, lower angular resolution CO -0 observations taken from NANTEN archival data were also analyzed to obtain a complete picture.Results. In the velocity range near 16 km s-1, which is the Puppis A systemic velocity, our study revealed two important properties: (i) no dense molecular gas is detected immediately adjacent to the eastern border of the BEK and (ii) the molecular clump detected very close to the radiocontinuum maximum is probably located in the foreground along the line of sight and has not yet been reached by the SNR shock front. We propose two possible scenarios for explaining the absence of molecular emission eastwards of the BEK border of Puppis A. Either the shock front has completely engulfed and destroyed a molecular clump or the shock front is interacting with part of a larger cloud, and we do not detect CO emission immediately beyond it because the molecules have been dissociated by photodissociation and by reactions with photoionized material due to the radiative precursor. © 2008 ESO.
Fil:Paron, S. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
Fil:Dubner, G. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
Fil:Reynoso, E. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
description Aims.This paper reports molecular observations towards the bright eastern knot (BEK) in the SNR Puppis A, a feature where radio and X-ray studies suggest that the shock front is interacting with a dense molecular clump.Methods.We performed high-resolution millimetric observations towards the BEK of Puppis A using the SEST telescope in the CO -0 and 2-1 lines (beams of 45 and 23, respectively). More extended, lower angular resolution CO -0 observations taken from NANTEN archival data were also analyzed to obtain a complete picture.Results. In the velocity range near 16 km s-1, which is the Puppis A systemic velocity, our study revealed two important properties: (i) no dense molecular gas is detected immediately adjacent to the eastern border of the BEK and (ii) the molecular clump detected very close to the radiocontinuum maximum is probably located in the foreground along the line of sight and has not yet been reached by the SNR shock front. We propose two possible scenarios for explaining the absence of molecular emission eastwards of the BEK border of Puppis A. Either the shock front has completely engulfed and destroyed a molecular clump or the shock front is interacting with part of a larger cloud, and we do not detect CO emission immediately beyond it because the molecules have been dissociated by photodissociation and by reactions with photoionized material due to the radiative precursor. © 2008 ESO.
publishDate 2008
dc.date.none.fl_str_mv 2008
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/20.500.12110/paper_00046361_v480_n2_p439_Paron
url http://hdl.handle.net/20.500.12110/paper_00046361_v480_n2_p439_Paron
dc.language.none.fl_str_mv eng
language eng
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by/2.5/ar
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by/2.5/ar
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv Astron. Astrophys. 2008;480(2):439-443
reponame:Biblioteca Digital (UBA-FCEN)
instname:Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
instacron:UBA-FCEN
reponame_str Biblioteca Digital (UBA-FCEN)
collection Biblioteca Digital (UBA-FCEN)
instname_str Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
instacron_str UBA-FCEN
institution UBA-FCEN
repository.name.fl_str_mv Biblioteca Digital (UBA-FCEN) - Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
repository.mail.fl_str_mv ana@bl.fcen.uba.ar
_version_ 1844618737348509696
score 13.070432