The optical-UV emissivity of quasars: dependence on black hole mass and radio loudness

Abstract

We analyzed a large sample of radio-loud and radio-quiet quasar spectra at redshift 1.0 ≤ z ≤ 1.2 to compare the inferred underlying quasar continuum slopes (after removal of the host galaxy contribution) with accretion disk models. The latter predict redder (decreasing) α₃₀₀₀ continuum slopes (Lν ∝  ν^α at 3000 Å) with increasing black hole mass, bluer α₃₀₀₀ with increasing luminosity at 3000 Å, and bluer α₃₀₀₀ with increasing spin of the black hole, when all other parameters are held fixed. We find no clear evidence for any of these predictions in the data. In particular, we find the following. (i) α₃₀₀₀ shows no significant dependence on black hole mass or luminosity. Dedicated Monte Carlo tests suggest that the substantial observational uncertainties in the black hole virial masses can effectively erase any intrinsic dependence of α₃₀₀₀ on black hole mass, in line with some previous studies. (ii) The mean slope α₃₀₀₀ of radio-loud sources, thought to be produced by rapidly spinning black holes, is comparable to, or even redder than, that of radio-quiet quasars. Indeed, although quasars appear to become more radio loud with decreasing luminosity, we still do not detect any significant dependence of α₃₀₀₀ on radio loudness. The predicted mean α₃₀₀₀ slopes tend to be bluer than in the data. Disk models with high inclinations and dust extinction tend to produce redder slopes closer to empirical estimates. Our mean α₃₀₀₀ values are close to the ones independently inferred at z < 0.5, suggesting weak evolution with redshift, at least for moderately luminous quasars.

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Identifiers

ORCID for Diego Altamirano: orcid.org/0000-0002-3422-0074

ORCID for Poshak Gandhi: orcid.org/0000-0003-3105-2615

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