The bolometric and UV attenuation in normal spiral galaxies of the Herschel Reference Survey⋆

S. Viaene (1) , M. Baes (1) , G. Bendo (2) , M. Boquien (3, 4) , A. Boselli (5) , L. Ciesla (6) , L. Cortese (7) , I. de Looze (8, 1, 3) , S. Eales (9) , J. Fritz (1) , O. Ł. Karczewski (6) , S. Madden (6) , M. W. L. Smith (9) , L. Spinoglio (10)

1 Sterrenkundig Observatorium
2 University of Manchester [Manchester]
3 CAM - University of Cambridge [UK]
4 Universidad de Antofagasta
5 LAM - Laboratoire d'Astrophysique de Marseille
6 AIM (UMR7158 / UMR_E_9005 / UM_112) - Astrophysique Interprétation Modélisation
7 UWA - The University of Western Australia
8 UCL - University College of London [London]
9 Cardiff University
10 IAPS - Istituto di Astrofisica e Planetologia Spaziali - INAF

The dust in nearby galaxies absorbs a fraction of the UV-optical-near-infrared radiation produced by stars. This energy is consequently re-emitted in the infrared. We investigate the portion of the stellar radiation absorbed by spiral galaxies from the Herschel Reference Survey (HRS) by modelling their UV-to-submillimetre spectral energy distributions. Our models provide an attenuated and intrinsic spectral energy distribution (SED), from which we find that on average 32% of all starlight is absorbed by dust. We define the UV heating fraction as the percentage of dust luminosity that comes from absorbed UV photons and find this to be 56%, on average. This percentage varies with morphological type, with later types having significantly higher UV heating fractions. We find a strong correlation between the UV heating fraction and specific star formation rate and provide a power-law fit. Our models allow us to revisit the IRX – AFUV relations, and derive these quantities directly within a self-consistent framework. We calibrate this relation for different bins of NUV − r colour and provide simple relations to relate these parameters. We investigated the robustness of our method and conclude that the derived parameters are reliable within the uncertainties that are inherent to the adopted SED model. This calls for a deeper investigation of how well extinction and attenuation can be determined through panchromatic SED modelling.

Mots clés: galaxies: ISM; Galaxy: fundamental parameters; extinction; infrared: ISM; dust

Domaines: Astrophysique [astro-ph]

S. Viaene, M. Baes, G. Bendo, M. Boquien, A. Boselli, et al.. The bolometric and UV attenuation in normal spiral galaxies of the Herschel Reference Survey⋆. Astronomy and Astrophysics - A&A, 2016, 586, pp.A13. ⟨10.1051/0004-6361/201527586⟩. ⟨cea-01430174⟩