Instituto Nazionale Of Astrofisica Instituto Of Astrofisica E Planetologia Spaziali

Rome, Italy

Instituto Nazionale Of Astrofisica Instituto Of Astrofisica E Planetologia Spaziali

Rome, Italy
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Gruppioni C.,Instituto Nazionale Of Astrofisica Osservatorio Astronomico Of Bologna | Berta S.,Max Planck Institute for Extraterrestrial Physics | Spinoglio L.,Instituto Nazionale Of Astrofisica Instituto Of Astrofisica E Planetologia Spaziali | Pereira-Santaella M.,CSIC - National Institute of Aerospace Technology | And 9 more authors.
Monthly Notices of the Royal Astronomical Society | Year: 2016

We present new estimates of AGN accretion and star formation (SF) luminosity in galaxies obtained for the local 12 μm sample of Seyfert galaxies (12MGS), by performing a detailed broad-band spectral energy distribution (SED) decomposition including the emission of stars, dust heated by SF and a possible AGN dusty torus. Thanks to the availability of data from the X-rays to the sub-millimetre, we constrain and test the contribution of the stellar, AGN and SF components to the SEDs. The availability of Spitzer-InfraRed Spectrograph (IRS) low-resolution mid-infrared (mid-IR) spectra is crucial to constrain the dusty torus component at its peak wavelengths. The results of SED fitting are also tested against the available information in other bands: the reconstructed AGN bolometric luminosity is compared to those derived from X-rays and from the high excitation IR lines tracing AGN activity like [Ne v] and [O iv]. The IR luminosity due to SF and the intrinsic AGN bolometric luminosity are shown to be strongly related to the IR line luminosity. Variations of these relations with different AGN fractions are investigated, showing that the relation dispersions are mainly due to different AGN relative contribution within the galaxy. Extrapolating these local relations between line and SF or AGN luminosities to higher redshifts, by means of recent Herschel galaxy evolution results, we then obtain mid-and far-IR line luminosity functions useful to estimate how many star-forming galaxies and AGN we expect to detect in the different lines at different redshifts and luminosities with future IR facilities (e.g. JWST, SPICA). © 2016 The Authors.

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