The neutral gas environment of the young supernova remnant SN 1006 (G327.6+14.6)

Autores
Dubner, Gloria Mabel; Giacani, Elsa Beatriz; Goss, W. M.; Green, A. J.; Nyman, L. Å.
Año de publicación
2002
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Using the Australia Telescope Compact Array, we have carried out a survey of the H i emission in the direction of the bilateral supernova remnant (SNR) SN 1006 (G327.6+14.6). The angular resolution of the data is 4.07×3.00, and the rms noise ∼39 mJy/beam (∼0.3 K). To recover structures at low spatial frequencies, single dish data have been added to the interferometric images. We have also studied the 12CO emission in the transitions J = 1–0 and J = 2–1, looking for very compact clumps of molecular gas as possible sites for the acceleration of electrons and nuclei to TeV energies associated with the γ-ray source detected on the NE limb of SN 1006. These molecular gas observations produced only marginal detections. From the present observations we conclude that the distribution of the surrounding neutral gas had no strong influence in shaping this SNR with a bilateral appearance. Intrinsic factors may have contributed to the present morphology. The remnant of SN 1006 appears to be evolving in a smooth environment with an atomic volume density n0 ∼ 0.3 cm−3. The existence of an H i concentration projected on the center of SN 1006 suggests an upper limit of ∼−20 km s−1 on the systemic velocity of the SNR. This limit is compatible with a distance to the SNR of about 1.7 kpc, in good agreement with previous estimates. An extended H i cloud with volume density ∼0.5 cm−3 is detected towards the NW border of SN 1006. This concentration may be responsible for the formation of the bright Balmer filaments observed in SN 1006. The absorbing column density towards SN 1006 has been estimated to be N h ∼ 6.8 × 1020 cm−2, in good agreement with previous suggestions based on X-ray results.
Fil: Dubner, Gloria Mabel. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Giacani, Elsa Beatriz. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Goss, W. M.. National Radio Astronomy Observatory; Estados Unidos
Fil: Green, A. J.. University of Sydney; Australia
Fil: Nyman, L. Å.. European Southern Observatory; Chile. Chalmers University Of Technology; Suecia
Materia
ISM: INDIVIDUAL OBJECTS: SN 1006-G327.6+14.6
ISM:SUPERNOVA REMNANTS
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/22436
Acceder
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network_name_str CONICET Digital (CONICET)
spelling The neutral gas environment of the young supernova remnant SN 1006 (G327.6+14.6)Dubner, Gloria MabelGiacani, Elsa BeatrizGoss, W. M.Green, A. J.Nyman, L. Å.ISM: INDIVIDUAL OBJECTS: SN 1006-G327.6+14.6ISM:SUPERNOVA REMNANTShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Using the Australia Telescope Compact Array, we have carried out a survey of the H i emission in the direction of the bilateral supernova remnant (SNR) SN 1006 (G327.6+14.6). The angular resolution of the data is 4.07×3.00, and the rms noise ∼39 mJy/beam (∼0.3 K). To recover structures at low spatial frequencies, single dish data have been added to the interferometric images. We have also studied the 12CO emission in the transitions J = 1–0 and J = 2–1, looking for very compact clumps of molecular gas as possible sites for the acceleration of electrons and nuclei to TeV energies associated with the γ-ray source detected on the NE limb of SN 1006. These molecular gas observations produced only marginal detections. From the present observations we conclude that the distribution of the surrounding neutral gas had no strong influence in shaping this SNR with a bilateral appearance. Intrinsic factors may have contributed to the present morphology. The remnant of SN 1006 appears to be evolving in a smooth environment with an atomic volume density n0 ∼ 0.3 cm−3. The existence of an H i concentration projected on the center of SN 1006 suggests an upper limit of ∼−20 km s−1 on the systemic velocity of the SNR. This limit is compatible with a distance to the SNR of about 1.7 kpc, in good agreement with previous estimates. An extended H i cloud with volume density ∼0.5 cm−3 is detected towards the NW border of SN 1006. This concentration may be responsible for the formation of the bright Balmer filaments observed in SN 1006. The absorbing column density towards SN 1006 has been estimated to be N h ∼ 6.8 × 1020 cm−2, in good agreement with previous suggestions based on X-ray results.Fil: Dubner, Gloria Mabel. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Giacani, Elsa Beatriz. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Goss, W. M.. National Radio Astronomy Observatory; Estados UnidosFil: Green, A. J.. University of Sydney; AustraliaFil: Nyman, L. Å.. European Southern Observatory; Chile. Chalmers University Of Technology; SueciaEDP Sciences2002-06info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/22436Dubner, Gloria Mabel; Giacani, Elsa Beatriz; Goss, W. M.; Green, A. J.; Nyman, L. Å.; The neutral gas environment of the young supernova remnant SN 1006 (G327.6+14.6); EDP Sciences; Astronomy and Astrophysics; 387; 3; 6-2002; 1047-10560004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20020365info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2002/21/aa2223/aa2223.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T15:23:32Zoai:ri.conicet.gov.ar:11336/22436instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-10-15 15:23:32.55CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The neutral gas environment of the young supernova remnant SN 1006 (G327.6+14.6)
title The neutral gas environment of the young supernova remnant SN 1006 (G327.6+14.6)
spellingShingle The neutral gas environment of the young supernova remnant SN 1006 (G327.6+14.6)
Dubner, Gloria Mabel
ISM: INDIVIDUAL OBJECTS: SN 1006-G327.6+14.6
ISM:SUPERNOVA REMNANTS
title_short The neutral gas environment of the young supernova remnant SN 1006 (G327.6+14.6)
title_full The neutral gas environment of the young supernova remnant SN 1006 (G327.6+14.6)
title_fullStr The neutral gas environment of the young supernova remnant SN 1006 (G327.6+14.6)
title_full_unstemmed The neutral gas environment of the young supernova remnant SN 1006 (G327.6+14.6)
title_sort The neutral gas environment of the young supernova remnant SN 1006 (G327.6+14.6)
dc.creator.none.fl_str_mv Dubner, Gloria Mabel
Giacani, Elsa Beatriz
Goss, W. M.
Green, A. J.
Nyman, L. Å.
author Dubner, Gloria Mabel
author_facet Dubner, Gloria Mabel
Giacani, Elsa Beatriz
Goss, W. M.
Green, A. J.
Nyman, L. Å.
author_role author
author2 Giacani, Elsa Beatriz
Goss, W. M.
Green, A. J.
Nyman, L. Å.
author2_role author
author
author
author
dc.subject.none.fl_str_mv ISM: INDIVIDUAL OBJECTS: SN 1006-G327.6+14.6
ISM:SUPERNOVA REMNANTS
topic ISM: INDIVIDUAL OBJECTS: SN 1006-G327.6+14.6
ISM:SUPERNOVA REMNANTS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Using the Australia Telescope Compact Array, we have carried out a survey of the H i emission in the direction of the bilateral supernova remnant (SNR) SN 1006 (G327.6+14.6). The angular resolution of the data is 4.07×3.00, and the rms noise ∼39 mJy/beam (∼0.3 K). To recover structures at low spatial frequencies, single dish data have been added to the interferometric images. We have also studied the 12CO emission in the transitions J = 1–0 and J = 2–1, looking for very compact clumps of molecular gas as possible sites for the acceleration of electrons and nuclei to TeV energies associated with the γ-ray source detected on the NE limb of SN 1006. These molecular gas observations produced only marginal detections. From the present observations we conclude that the distribution of the surrounding neutral gas had no strong influence in shaping this SNR with a bilateral appearance. Intrinsic factors may have contributed to the present morphology. The remnant of SN 1006 appears to be evolving in a smooth environment with an atomic volume density n0 ∼ 0.3 cm−3. The existence of an H i concentration projected on the center of SN 1006 suggests an upper limit of ∼−20 km s−1 on the systemic velocity of the SNR. This limit is compatible with a distance to the SNR of about 1.7 kpc, in good agreement with previous estimates. An extended H i cloud with volume density ∼0.5 cm−3 is detected towards the NW border of SN 1006. This concentration may be responsible for the formation of the bright Balmer filaments observed in SN 1006. The absorbing column density towards SN 1006 has been estimated to be N h ∼ 6.8 × 1020 cm−2, in good agreement with previous suggestions based on X-ray results.
Fil: Dubner, Gloria Mabel. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Giacani, Elsa Beatriz. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Goss, W. M.. National Radio Astronomy Observatory; Estados Unidos
Fil: Green, A. J.. University of Sydney; Australia
Fil: Nyman, L. Å.. European Southern Observatory; Chile. Chalmers University Of Technology; Suecia
description Using the Australia Telescope Compact Array, we have carried out a survey of the H i emission in the direction of the bilateral supernova remnant (SNR) SN 1006 (G327.6+14.6). The angular resolution of the data is 4.07×3.00, and the rms noise ∼39 mJy/beam (∼0.3 K). To recover structures at low spatial frequencies, single dish data have been added to the interferometric images. We have also studied the 12CO emission in the transitions J = 1–0 and J = 2–1, looking for very compact clumps of molecular gas as possible sites for the acceleration of electrons and nuclei to TeV energies associated with the γ-ray source detected on the NE limb of SN 1006. These molecular gas observations produced only marginal detections. From the present observations we conclude that the distribution of the surrounding neutral gas had no strong influence in shaping this SNR with a bilateral appearance. Intrinsic factors may have contributed to the present morphology. The remnant of SN 1006 appears to be evolving in a smooth environment with an atomic volume density n0 ∼ 0.3 cm−3. The existence of an H i concentration projected on the center of SN 1006 suggests an upper limit of ∼−20 km s−1 on the systemic velocity of the SNR. This limit is compatible with a distance to the SNR of about 1.7 kpc, in good agreement with previous estimates. An extended H i cloud with volume density ∼0.5 cm−3 is detected towards the NW border of SN 1006. This concentration may be responsible for the formation of the bright Balmer filaments observed in SN 1006. The absorbing column density towards SN 1006 has been estimated to be N h ∼ 6.8 × 1020 cm−2, in good agreement with previous suggestions based on X-ray results.
publishDate 2002
dc.date.none.fl_str_mv 2002-06
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/11336/22436
Dubner, Gloria Mabel; Giacani, Elsa Beatriz; Goss, W. M.; Green, A. J.; Nyman, L. Å.; The neutral gas environment of the young supernova remnant SN 1006 (G327.6+14.6); EDP Sciences; Astronomy and Astrophysics; 387; 3; 6-2002; 1047-1056
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/22436
identifier_str_mv Dubner, Gloria Mabel; Giacani, Elsa Beatriz; Goss, W. M.; Green, A. J.; Nyman, L. Å.; The neutral gas environment of the young supernova remnant SN 1006 (G327.6+14.6); EDP Sciences; Astronomy and Astrophysics; 387; 3; 6-2002; 1047-1056
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20020365
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2002/21/aa2223/aa2223.html
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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