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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/22436
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CONICET Digital (CONICET) |
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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 Técnicas2025-09-29T10:26:24Zoai: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:34982025-09-29 10:26:24.337CONICET 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) |
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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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1844614265551454208 |
score |
13.070432 |