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

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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 sub-mm emission from Cas A has...

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Autores principales:	Gomez, H.L., Dunne, L., Ivison, R.J., Reynoso, E.M., Thompson, M.A., Sibthorpe, B., Eales, S.A., Delaney, T.M., Maddox, S., Isaak, K.
Formato:	JOUR
Materias:	Galaxies: abundances ISM: submillimetre dust Radio lines: ISM Submillimetre Supernovae: Kepler
Acceso en línea:	http://hdl.handle.net/20.500.12110/paper_00358711_v397_n3_p1621_Gomez
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	todo:paper_00358711_v397_n3_p1621_Gomez
record_format	dspace
spelling	todo:paper_00358711_v397_n3_p1621_Gomez2023-10-03T14:46:55Z Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant Gomez, H.L. Dunne, L. Ivison, R.J. Reynoso, E.M. Thompson, M.A. Sibthorpe, B. Eales, S.A. Delaney, T.M. Maddox, S. Isaak, K. Galaxies: abundances ISM: submillimetre dust Radio lines: ISM Submillimetre Supernovae: Kepler 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 sub-mm 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. © 2009 RAS. Fil:Reynoso, E.M. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_00358711_v397_n3_p1621_Gomez
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	Galaxies: abundances ISM: submillimetre dust Radio lines: ISM Submillimetre Supernovae: Kepler
spellingShingle	Galaxies: abundances ISM: submillimetre dust Radio lines: ISM Submillimetre Supernovae: Kepler Gomez, H.L. Dunne, L. Ivison, R.J. Reynoso, E.M. Thompson, M.A. Sibthorpe, B. Eales, S.A. Delaney, T.M. Maddox, S. Isaak, K. Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant
topic_facet	Galaxies: abundances ISM: submillimetre dust Radio lines: ISM Submillimetre Supernovae: Kepler
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 sub-mm 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. © 2009 RAS.
format	JOUR
author	Gomez, H.L. Dunne, L. Ivison, R.J. Reynoso, E.M. Thompson, M.A. Sibthorpe, B. Eales, S.A. Delaney, T.M. Maddox, S. Isaak, K.
author_facet	Gomez, H.L. Dunne, L. Ivison, R.J. Reynoso, E.M. Thompson, M.A. Sibthorpe, B. Eales, S.A. Delaney, T.M. Maddox, S. Isaak, K.
author_sort	Gomez, H.L.
title	Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant
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
url	http://hdl.handle.net/20.500.12110/paper_00358711_v397_n3_p1621_Gomez
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Accounting for the foreground contribution to the dust emission towards Kepler's supernova remnant

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