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The identification of dust heating mechanisms in nearby galaxies using Herschel 160/250 and 250/350μm surface brightness ratios

Bendo, G. J. and Baes, M. and Bianchi, S. and Boquien, M. and Boselli, A. and Cooray, A. and Cortese, L. and De Looze, I. and di Serego Alighieri, S. and Fritz, J. and Gentile, G. and Hughes, T. M. and Lu, N. and Pappalardo, C. and Smith, M. W. L. and Spinoglio, L. and Viaene, S. and Vlahakis, C. (2015) The identification of dust heating mechanisms in nearby galaxies using Herschel 160/250 and 250/350μm surface brightness ratios. Monthly Notices of the Royal Astronomical Society, 448 (1). pp. 135-167. ISSN 0035-8711.

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We examined variations in the 160/250 and 250/350 μm surface brightness ratios within 24 nearby (<30 Mpc) face-on spiral galaxies observed with the Herschel Space Observatory to identify the heating mechanisms for dust emitting at these wavelengths. The analysis consisted of both qualitative and quantitative comparisons of the 160/250 and 250/350 μm ratios to Hα and 24 μm emission, which trace the light from star-forming regions, and 3.6 μm emission, which traces the light from the older stellar populations of the galaxies. We find broad variations in the heating mechanisms for the dust. In one subset of galaxies, we found evidence that emission at ≤160 μm (and in rare cases potentially at ≤350 μm) originates from dust heated by star-forming regions. In another subset, we found that the emission at ≥250 μm (and sometimes at ≥160 μm) originates from dust heated by the older stellar population. In the rest of the sample, either the results are indeterminate or both of these stellar populations may contribute equally to the global dust heating. The observed variations in dust heating mechanisms do not necessarily match what has been predicted by dust emission and radiative transfer models, which could lead to overestimated dust temperatures, underestimated dust masses, false detections of variability in dust emissivity, and inaccurate star formation rate measurements.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper Information
Bianchi, S.0000-0002-4622-4240
Boquien, M.0000-0003-0946-6176
Cooray, A.0000-0002-3892-0190
Cortese, L.0000-0002-7422-9823
di Serego Alighieri, S.0000-0001-8769-2692
Lu, N.0000-0002-8948-1044
Pappalardo, C.0000-0003-2606-6019
Smith, M. W. L.0000-0002-3532-6970
Vlahakis, C.0000-0003-3745-4228
Additional Information:© 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 September 4. Received 2014 September 3; in original form 2014 July 25. First published online February 2, 2015. We thank the reviewer for the helpful comments on this paper. GJB is funded by the STFC. IDL is a postdoctoral researcher of the FWO-Vlaanderen (Belgium). The Herschel spacecraft was designed, built, tested, and launched under a contract to ESA managed by the Herschel/Planck Project team by an industrial consortium under the overall responsibility of the prime contractor Thales Alenia Space (Cannes), and including Astrium (Friedrichshafen) responsible for the payload module and for system testing at spacecraft level, Thales Alenia Space (Turin) responsible for the service module, and Astrium (Toulouse) responsible for the telescope, with in excess of a hundred subcontractors. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, 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). HIPE is a joint development (are joint developments) by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Science and Technology Facilities Council (STFC)UNSPECIFIED
Canadian Space Agency (CSA)UNSPECIFIED
National Astronomical Observatories, Chinese Academy of Sciences (NAOC)UNSPECIFIED
Commissariat à l’Energie Atomique (CEA)UNSPECIFIED
Centre National d'Études Spatiales (CNES)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
United Kingdom Space Agency (UKSA)UNSPECIFIED
Subject Keywords:galaxies: ISM galaxies: spiral infrared: galaxies
Issue or Number:1
Record Number:CaltechAUTHORS:20150406-073106027
Persistent URL:
Official Citation:G. J. Bendo, M. Baes, S. Bianchi, M. Boquien, A. Boselli, A. Cooray, L. Cortese, I. De Looze, S. di Serego Alighieri, J. Fritz, G. Gentile, T. M. Hughes, N. Lu, C. Pappalardo, M. W. L. Smith, L. Spinoglio, S. Viaene, and C. Vlahakis The identification of dust heating mechanisms in nearby galaxies using Herschel 160/250 and 250/350 μm surface brightness ratios MNRAS (March 21, 2015) Vol. 448 135-167 doi:10.1093/mnras/stu1841 First published online February 2, 2015
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:56362
Deposited By: Ruth Sustaita
Deposited On:06 Apr 2015 20:13
Last Modified:09 Mar 2020 13:18

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