Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant

Autores
Gomez, H. L.; Dune, L.; Ivison, R. J.; Reynoso, Estela Marta; Thompson, M.; Sibthorpe, B.; Eales, S. A.; Delaney, T. M.; Maddox, S.; Isaak, K.
Año de publicación
2009
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Whether or not supernovae contribute significantly to the overall dust budget is a controversial subject. Submillimetre (sub-mm) observations, sensitive to cold dust, have shown an excess at 450 and 850 µm in young remnants Cassiopeia A (Cas A) and Kepler. Some of the submm emission from Cas A has been shown to be contaminated by unrelated material along the line of sight. In this paper, we explore the emission from material towards Kepler using sub-mm continuum imaging and spectroscopic observations of atomic and molecular gas, via H I,12CO(J = 2–1) and 13CO(J = 2–1). We detect weak CO emission (peak T ∗A = 0.2–1 K, 1–2 km s−1 full width at half-maximum) from diffuse, optically thin gas at the locations of some of the sub-mm clumps. The contribution to the sub-mm emission from foreground molecular and atomic clouds is negligible. The revised dust mass for Kepler’s remnant is 0.1–1.2 M⊙, about half of the quoted values in the original study by Morgan et al., but still sufficient to explain the origin of dust at high redshifts.
Fil: Gomez, H. L.. University Of New South Wales; Australia
Fil: Dune, L.. The University Of Nottingham; Reino Unido
Fil: Ivison, R. J.. University of Edinburgh; Reino Unido
Fil: Reynoso, Estela Marta. 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: Thompson, M.. University Of Hertfordshire; Reino Unido
Fil: Sibthorpe, B.. Royal Observatory Edinburgh; Reino Unido
Fil: Eales, S. A.. University Of New South Wales; Australia
Fil: Delaney, T. M.. Massachusetts Institute of Technology; Estados Unidos
Fil: Maddox, S.. The University Of Nottingham; Reino Unido
Fil: Isaak, K.. University Of New South Wales; Australia
Materia
SUPERNOVA: KEPLER
ISM: SUBMILLIMETRE DUST
RADIO LINES: ISM
GALAXIES: ABUNDANCES
SUBMILLIMETRE
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:11336/20708
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/20708
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnantGomez, H. L.Dune, L.Ivison, R. J.Reynoso, Estela MartaThompson, M.Sibthorpe, B.Eales, S. A.Delaney, T. M.Maddox, S.Isaak, K.SUPERNOVA: KEPLERISM: SUBMILLIMETRE DUSTRADIO LINES: ISMGALAXIES: ABUNDANCESSUBMILLIMETREhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Whether or not supernovae contribute significantly to the overall dust budget is a controversial subject. Submillimetre (sub-mm) observations, sensitive to cold dust, have shown an excess at 450 and 850 µm in young remnants Cassiopeia A (Cas A) and Kepler. Some of the submm emission from Cas A has been shown to be contaminated by unrelated material along the line of sight. In this paper, we explore the emission from material towards Kepler using sub-mm continuum imaging and spectroscopic observations of atomic and molecular gas, via H I,12CO(J = 2–1) and 13CO(J = 2–1). We detect weak CO emission (peak T ∗A = 0.2–1 K, 1–2 km s−1 full width at half-maximum) from diffuse, optically thin gas at the locations of some of the sub-mm clumps. The contribution to the sub-mm emission from foreground molecular and atomic clouds is negligible. The revised dust mass for Kepler’s remnant is 0.1–1.2 M⊙, about half of the quoted values in the original study by Morgan et al., but still sufficient to explain the origin of dust at high redshifts.Fil: Gomez, H. L.. University Of New South Wales; AustraliaFil: Dune, L.. The University Of Nottingham; Reino UnidoFil: Ivison, R. J.. University of Edinburgh; Reino UnidoFil: Reynoso, Estela Marta. 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: Thompson, M.. University Of Hertfordshire; Reino UnidoFil: Sibthorpe, B.. Royal Observatory Edinburgh; Reino UnidoFil: Eales, S. A.. University Of New South Wales; AustraliaFil: Delaney, T. M.. Massachusetts Institute of Technology; Estados UnidosFil: Maddox, S.. The University Of Nottingham; Reino UnidoFil: Isaak, K.. University Of New South Wales; AustraliaWiley Blackwell Publishing, Inc2009-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/20708Gomez, H. L.; Dune, L.; Ivison, R. J.; Reynoso, Estela Marta; Thompson, M.; et al.; Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 397; 3; 12-2009; 1621-16320035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2009.15061.xinfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-lookup/doi/10.1111/j.1365-2966.2009.15061.xinfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/0905.2564info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T12:01:02Zoai:ri.conicet.gov.ar:11336/20708instacron: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:34982025-10-22 12:01:03.179CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant
title Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant
spellingShingle Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant
Gomez, H. L.
SUPERNOVA: KEPLER
ISM: SUBMILLIMETRE DUST
RADIO LINES: ISM
GALAXIES: ABUNDANCES
SUBMILLIMETRE
title_short Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant
title_full Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant
title_fullStr Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant
title_full_unstemmed Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant
title_sort Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant
dc.creator.none.fl_str_mv Gomez, H. L.
Dune, L.
Ivison, R. J.
Reynoso, Estela Marta
Thompson, M.
Sibthorpe, B.
Eales, S. A.
Delaney, T. M.
Maddox, S.
Isaak, K.
author Gomez, H. L.
author_facet Gomez, H. L.
Dune, L.
Ivison, R. J.
Reynoso, Estela Marta
Thompson, M.
Sibthorpe, B.
Eales, S. A.
Delaney, T. M.
Maddox, S.
Isaak, K.
author_role author
author2 Dune, L.
Ivison, R. J.
Reynoso, Estela Marta
Thompson, M.
Sibthorpe, B.
Eales, S. A.
Delaney, T. M.
Maddox, S.
Isaak, K.
author2_role author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv SUPERNOVA: KEPLER
ISM: SUBMILLIMETRE DUST
RADIO LINES: ISM
GALAXIES: ABUNDANCES
SUBMILLIMETRE
topic SUPERNOVA: KEPLER
ISM: SUBMILLIMETRE DUST
RADIO LINES: ISM
GALAXIES: ABUNDANCES
SUBMILLIMETRE
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Whether or not supernovae contribute significantly to the overall dust budget is a controversial subject. Submillimetre (sub-mm) observations, sensitive to cold dust, have shown an excess at 450 and 850 µm in young remnants Cassiopeia A (Cas A) and Kepler. Some of the submm emission from Cas A has been shown to be contaminated by unrelated material along the line of sight. In this paper, we explore the emission from material towards Kepler using sub-mm continuum imaging and spectroscopic observations of atomic and molecular gas, via H I,12CO(J = 2–1) and 13CO(J = 2–1). We detect weak CO emission (peak T ∗A = 0.2–1 K, 1–2 km s−1 full width at half-maximum) from diffuse, optically thin gas at the locations of some of the sub-mm clumps. The contribution to the sub-mm emission from foreground molecular and atomic clouds is negligible. The revised dust mass for Kepler’s remnant is 0.1–1.2 M⊙, about half of the quoted values in the original study by Morgan et al., but still sufficient to explain the origin of dust at high redshifts.
Fil: Gomez, H. L.. University Of New South Wales; Australia
Fil: Dune, L.. The University Of Nottingham; Reino Unido
Fil: Ivison, R. J.. University of Edinburgh; Reino Unido
Fil: Reynoso, Estela Marta. 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: Thompson, M.. University Of Hertfordshire; Reino Unido
Fil: Sibthorpe, B.. Royal Observatory Edinburgh; Reino Unido
Fil: Eales, S. A.. University Of New South Wales; Australia
Fil: Delaney, T. M.. Massachusetts Institute of Technology; Estados Unidos
Fil: Maddox, S.. The University Of Nottingham; Reino Unido
Fil: Isaak, K.. University Of New South Wales; Australia
description Whether or not supernovae contribute significantly to the overall dust budget is a controversial subject. Submillimetre (sub-mm) observations, sensitive to cold dust, have shown an excess at 450 and 850 µm in young remnants Cassiopeia A (Cas A) and Kepler. Some of the submm emission from Cas A has been shown to be contaminated by unrelated material along the line of sight. In this paper, we explore the emission from material towards Kepler using sub-mm continuum imaging and spectroscopic observations of atomic and molecular gas, via H I,12CO(J = 2–1) and 13CO(J = 2–1). We detect weak CO emission (peak T ∗A = 0.2–1 K, 1–2 km s−1 full width at half-maximum) from diffuse, optically thin gas at the locations of some of the sub-mm clumps. The contribution to the sub-mm emission from foreground molecular and atomic clouds is negligible. The revised dust mass for Kepler’s remnant is 0.1–1.2 M⊙, about half of the quoted values in the original study by Morgan et al., but still sufficient to explain the origin of dust at high redshifts.
publishDate 2009
dc.date.none.fl_str_mv 2009-12
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/11336/20708
Gomez, H. L.; Dune, L.; Ivison, R. J.; Reynoso, Estela Marta; Thompson, M.; et al.; Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 397; 3; 12-2009; 1621-1632
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/20708
identifier_str_mv Gomez, H. L.; Dune, L.; Ivison, R. J.; Reynoso, Estela Marta; Thompson, M.; et al.; Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 397; 3; 12-2009; 1621-1632
0035-8711
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2009.15061.x
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-lookup/doi/10.1111/j.1365-2966.2009.15061.x
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/0905.2564
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 Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
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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score 12.982451

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