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The star-formation rates of QSOs

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arxiv 2205.11645 v1 pith:4NWI5JYC submitted 2022-05-23 astro-ph.GA

The star-formation rates of QSOs

M. Symeonidis , N. Maddox , M.J. Jarvis , M.J. Michalowski , P. Andreani , D.L. Clements , G. De Zotti , S. Duivenvoorden
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J. Gonzalez-Nuevo E. Ibar R.J. Ivison L. Leeuw M.J. Page R. Shirley M.W.L. Smith M. Vaccari
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classification astro-ph.GA
keywords poweremissioninfraredfar-iropticalredshiftaveragefunction
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We examine the far-IR properties of a sample of 5391 optically selected QSOs in the 0.5<z<2.65 redshift range down to log[nuLnu,2500 (erg/s)]>44.7, using SPIRE data from Herschel-ATLAS. We split the sample in a grid of 74 luminosity-redshift bins and compute the average optical-infrared spectral energy distribution (SED) in each bin. By normalising an intrinsic AGN template to the AGN optical power (at 5100A) we decompose the total infrared emission (L_IR; 8-1000um) into an AGN (L_IR,AGN) and star-forming component (L_IR,SF). We find that the AGN contribution to L_IR increases as a function of AGN power which manifests as a reduction of the `far-IR bump' in the average QSO SEDs. We note that L_IR,SF does not correlate with AGN power; the mean star formation rates (SFRs) of AGN host galaxies are a function of redshift only and they range from ~6 Msun/yr at z~0 to a plateau of <200 Msun/yr at z~2.6. Our results indicate that the accuracy of far-IR emission as a proxy for SFR decreases with increasing AGN luminosity. We show that, at any given redshift, observed trends between infrared luminosity (whether monochromatic or total) and AGN power (in the optical or X-rays) can be explained by a simple model which is the sum of two components: (A) the infrared emission from star-formation, uncorrelated with AGN power and (B) the infrared emission from AGN, directly proportional to AGN power in the optical or X-rays.

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  1. A MIGHTEE robust measurement of the star formation rate-radio correlation

    astro-ph.GA 2026-07 conditional novelty 7.0

    The SFR–1.4 GHz radio correlation is log10(SFR) = 0.790(L′)+1.244(1+z)^0.122−0.033M′ with 0.178 dex scatter, showing significant redshift but weak mass dependence when AGN are treated probabilistically.