A Caltech Library Service

Quantifying the Heating Sources for Mid-infrared Dust Emissions in Galaxies: The Case of M 81

Lu, N. and Bendo, G. J. and Boselli, A. and Baes, M. and Wu, H. and Madden, S. C. and De Looze, I. and Rémy-Ruyer, A. and Boquien, M. and Wilson, C. D. and Galametz, M. and Lam, M. I. and Cooray, A. and Spinoglio, L. and Zhao, Y. (2014) Quantifying the Heating Sources for Mid-infrared Dust Emissions in Galaxies: The Case of M 81. Astrophysical Journal, 797 (2). Art. No. 129. ISSN 0004-637X.

[img] PDF - Published Version
See Usage Policy.

PDF - Submitted Version
See Usage Policy.


Use this Persistent URL to link to this item:


With the newly available photometric images at 250 and 500 μm from the Herschel Space Observatory, we study quantitative correlations over a sub-kiloparsec scale among three distinct emission components in the interstellar medium of the nearby spiral galaxy M 81 (NGC 3031): (1) I8 or I24, the surface brightness of the mid-infrared emission observed in the Spitzer Space Telescope 8 or 24 μm band, with I8 and I24 being dominated by the emissions from polycyclic aromatic hydrocarbons (PAHs) and very small grains (VSGs) of dust, respectively; (2) I500, that of the cold dust continuum emission in the Herschel Space Observatory 500 μm band, dominated by the emission from large dust grains heated by evolved stars; and (3) IHα, a nominal surface brightness of the Hα line emission, from gas ionized by newly formed massive stars. The results from our correlation study, free from any assumption on or modeling of dust emissivity law or dust temperatures, present solid evidence for significant heating of PAHs and VSGs by evolved stars. In the case of M 81, about 67% (48%) of the 8 μm (24 μm ) emission derives its heating from evolved stars, with the remainder attributed to radiation heating associated with ionizing stars.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Lu, N.0000-0002-8948-1044
Boquien, M.0000-0003-0946-6176
Wilson, C. D.0000-0001-5817-0991
Galametz, M.0000-0002-0283-8689
Cooray, A.0000-0002-3892-0190
Additional Information:We thank the anonymous referee for a number of useful comments that improved the presentation and clarity of this paper. 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. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, OAMP (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech/JPL, IPAC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA). Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
Funding AgencyGrant Number
Canadian Space Agency (CSA)UNSPECIFIED
National Astronomical Observatories, Chinese Academy of Sciences (NAOC)UNSPECIFIED
Commissariat à l’Energie Atomique (CEA)UNSPECIFIED
Agenzia Spaziale Italiana (ASI)UNSPECIFIED
Ministerio de Ciencia e Innovación (MCINN)UNSPECIFIED
Stockholm ObservatoryUNSPECIFIED
Science and Technology Facilities Council (STFC)UNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Subject Keywords:galaxies: individual: M81, galaxies: ISM, galaxies: star formation, infrared: galaxies, infrared: ISM, ISM: lines and bands
Issue or Number:2
Record Number:CaltechAUTHORS:20141103-100247552
Persistent URL:
Official Citation:Quantifying the Heating Sources for Mid-infrared Dust Emissions in Galaxies: The Case of M 81 N. Lu et al. 2014 ApJ 797 129
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:51167
Deposited By: Ruth Sustaita
Deposited On:03 Nov 2014 20:43
Last Modified:09 Mar 2020 13:19

Repository Staff Only: item control page