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Dissecting the origin of the submillimetre emission in nearby galaxies with Herschel and LABOCA

Galametz, M. and Albrecht, M. and Kennicutt, R. and Aniano, G. and Bertoldi, F. and Calzetti, D. and Croxall, K. V. and Dale, D. and Draine, B. and Engelbracht, C. and Gordon, K. and Hinz, J. and Hunt, L. K. and Kirkpatrick, A. and Murphy, E. J. and Roussel, H. and Skibba, R. A. and Walter, F. and Weiss, A. and Wilson, C. D. (2014) Dissecting the origin of the submillimetre emission in nearby galaxies with Herschel and LABOCA. Monthly Notices of the Royal Astronomical Society, 439 (3). pp. 2542-2570. ISSN 0035-8711. doi:10.1093/mnras/stu113. https://resolver.caltech.edu/CaltechAUTHORS:20140530-103402531

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Abstract

We model the infrared to submillimetre spectral energy distribution of 11 nearby galaxies of the Key Insights on Nearby Galaxies: A Far-Infrared Survey with Herschel sample using Spitzer and Herschel data and compare model extrapolations at 870 μm (using different fitting techniques) with Large APEX BOlometer CAmera (LABOCA) 870 μm observations. We investigate how the differences between predictions and observations vary with model assumptions or environment. At global scales, we find that modified blackbody models using realistic cold emissivity indices (β_c = 2 or 1.5) are able to reproduce the 870 μm observed emission within the uncertainties for most of the sample. Low values (β_c < 1.3) would be required in NGC 0337, NGC 1512 and NGC 7793. At local scales, we observe a systematic 870 μm excess when using β_c = 2.0. The β_c = 1.5 or the Draine & Li (2007) models can reconcile predictions with observations in part of the discs. Some of the remaining ‘excesses’ occur towards the centres and can be partly or fully accounted for by non-dust contributions such as CO(3–2) or, to a lesser extent, free–free or synchrotron emission. In three non-barred galaxies, the remaining excesses rather occur in the disc outskirts. This could be a sign of a flattening of the submm slope (and decrease of the effective emissivity index) with radius in these objects.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1401.3693arXivDiscussion Paper
http://mnras.oxfordjournals.org/content/439/3/2542.abstractPublisherArticle
http://dx.doi.org/10.1093/mnras/stu113DOIArticle
ORCID:
AuthorORCID
Galametz, M.0000-0002-0283-8689
Kennicutt, R.0000-0001-5448-1821
Aniano, G.0000-0001-9015-2654
Bertoldi, F.0000-0002-1707-1775
Calzetti, D.0000-0002-5189-8004
Croxall, K. V.0000-0002-5258-7224
Dale, D.0000-0002-5782-9093
Draine, B.0000-0002-0846-936X
Hunt, L. K.0000-0001-9162-2371
Murphy, E. J.0000-0001-7089-7325
Walter, F.0000-0003-4793-7880
Weiss, A.0000-0003-4678-3939
Wilson, C. D.0000-0001-5817-0991
Additional Information:© 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. First published online: February 17, 2014. Accepted 2014 January 15. Received 2014 January 8; in original form 2013 October 31. We would like to thank the referee for a very constructive report that helped to improve the clarity/robustness of the results. The research of CDW is supported by grants from the Natural Sciences and Engineering Research Council of Canada. PACS has been developed by MPE (Germany); UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy) and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy);IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCLMSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK) and NASA (USA).
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
MPE (Germany)UNSPECIFIED
UVIE (Austria)UNSPECIFIED
KU LeuvenUNSPECIFIED
CSL (Belgium)UNSPECIFIED
IMEC (Belgium)UNSPECIFIED
Commissariat à l’Energie Atomique (CEA)UNSPECIFIED
LAM (France)UNSPECIFIED
Max Planck Institute for Astronomy (MPIA)UNSPECIFIED
INAF-IFSI/OAA/OAP/OAT (Italy)UNSPECIFIED
LENS (Italy)UNSPECIFIED
SISSA (Italy)UNSPECIFIED
IAC (Spain)UNSPECIFIED
Bundesministerium für Verkehr, Innovation und Technologie (BMVIT)UNSPECIFIED
ESA-PRODEX (Belgium)UNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Deutsches Zentrum für Luft- und Raumfahrt (DLR)UNSPECIFIED
Agenzia Spaziale Italiana (ASI)UNSPECIFIED
CICYT/MCYT (Spain)UNSPECIFIED
Canadian Space Agency (CSA)UNSPECIFIED
National Astronomical Observatories, Chinese Academy of Sciences (NAOC)UNSPECIFIED
Istituto Nazionale di Astrofisica (INAF)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Agenzia Spaziale Italiana (ASI)UNSPECIFIED
Ministerio de Ciencia e Innovación (MCINN)UNSPECIFIED
Swedish National Space Board (SNSB)UNSPECIFIED
Science and Technology Facilities Council (STFC)UNSPECIFIED
United Kingdom Space Agency (UKSA)UNSPECIFIED
NASAUNSPECIFIED
Subject Keywords:galaxies: ISM
Issue or Number:3
DOI:10.1093/mnras/stu113
Record Number:CaltechAUTHORS:20140530-103402531
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20140530-103402531
Official Citation:M. Galametz, M. Albrecht, R. Kennicutt, G. Aniano, F. Bertoldi, D. Calzetti, K. V. Croxall, D. Dale, B. Draine, C. Engelbracht, K. Gordon, J. Hinz, L. K. Hunt, A. Kirkpatrick, E. Murphy, H. Roussel, R. A. Skibba, F. Walter, A. Weiss, and C. D. Wilson Dissecting the origin of the submillimetre emission in nearby galaxies with Herschel and LABOCA MNRAS (April 11, 2014) Vol. 439 2542-2570 first published online February 17, 2014 doi:10.1093/mnras/stu113
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:46000
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:30 May 2014 18:14
Last Modified:10 Nov 2021 17:19

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