Boselli, A. and Ciesla, L. and Cortese, L. and Buat, V. and Boquien, M. and Bendo, G. J. and Boissier, S. and Eales, S. and Gavazzi, G. and Hughes, T. M. and Pohlen, M. and Smith, M. W. L. and Baes, M. and Bianchi, S. and Clements, D. L. and Cooray, A. and Davies, J. and Gear, W. and Madden, S. and Magrini, L. and Panuzzo, P. and Remy, A. and Spinoglio, L. and Zibetti, S. (2012) Far-infrared colours of nearby late-type galaxies in the Herschel Reference Survey. Astronomy and Astrophysics, 540 . Art. No. A54. ISSN 0004-6361 http://resolver.caltech.edu/CaltechAUTHORS:20120529-073728982
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We study the far infrared (60–500 μm) colours of late-type galaxies in the Herschel Reference Survey, a K-band selected, volume limited sample of nearby galaxies. The far infrared colours are correlated with each other, with tighter correlations for the indices that are closer in wavelength. We also compare the different colour indices to various tracers of the physical properties of the target galaxies, such as the surface brightness of the ionising and non-ionising stellar radiation, the dust attenuation and the metallicity. The emission properties of the cold dust dominating the far infrared spectral domain are regulated by the properties of the interstellar radiation field. Consistent with that observed in nearby, resolved galaxies, our analysis shows that the ionising and the non-ionising stellar radiation, including that emitted by the most evolved, cold stars, both contribute to the heating of the cold dust component. This work also shows that metallicity is another key parameter characterising the cold dust emission of normal, late-type galaxies. A single modified black body with a grain emissivity index β = 1.5 better fits the observed SPIRE flux density ratios S250/S350 vs. S350/S500 than β = 2, although values of β ≃ 2 are possible in metal rich, high surface brightness galaxies. Values of β ≲ 1.5 better represent metal poor, lowsurface brightness objects. This observational evidence provides strong constraints for dust emission models of normal, late type galaxies.
|Additional Information:||© 2012 ESO. Received: 7 December 2011. Accepted: 10 January 2012. Published online 26 March 2012. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. We thank the referee, D. Dale, for precious comments which helped improving the quality of the manuscript. 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, UCL-MSSL, UKATC, Univ. Sussex (UK); 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). 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. The research leading to these results has received funding from the European Community’s Seventh Framework Programme (/FP7/2007- 2013/) under grant agreement No. 229517. 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 and of the GOLDMine database (http://goldmine.mib.infn.it/).|
|Subject Keywords:||infrared: galaxies; galaxies: spiral; galaxies: ISM|
|Official Citation:||Far-infrared colours of nearby late-type galaxies in the Herschel Reference Survey A54 A. Boselli et al. Published online: 26 March 2012 DOI: http://dx.doi.org/10.1051/0004-6361/201118602|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Ruth Sustaita|
|Deposited On:||29 May 2012 17:41|
|Last Modified:||26 Dec 2012 15:15|
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