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
- Institución
- Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
- OAI Identificador
- paperaa:paper_00046361_v480_n2_p439_Paron
Ver los metadatos del registro completo
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paperaa:paper_00046361_v480_n2_p439_Paron |
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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 |
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