The Bolometric Luminosity Correction of Radio-Quiet and Radio-Loud Quasars at 1

Abstract

To understand the impact of active galactic nuclei (AGN) on their host galaxies and large scale environment it is crucial to determine their total radiative power across all wavelengths (i.e., bolometric luminosity). In this contribution we describe how quasar accretion disk spectral energy distribution (SED) templates, parameterized by the black hole (BH) mass, Eddington ratio, and spin can be used to estimate their total radiated luminosity. To estimate the bolometric luminosity of AGN, we integrate the accretion disk SEDs from 1 µm to 10 keV. Our approach self-consistently covers any gaps in observations and does not include reprocessed emission from the torus. The accretion disk SED, and consequently the bolometric correction inferred from it, strongly depend on the BH mass, the Eddington ratio, and spin. In particular, the bolometric correction in the visible bands (5000 Å and 3000 Å) strongly depends on BH mass, and at X-ray strongly depends on the Eddington ratio. At wavelengths closer to the peak of the accretion disk SED the dependence becomes weaker. Additionally, maximally-rotating (spin = 1) quasars require a higher bolometric correction than their non-rotating (spin = 0) counterparts at all wavelengths. The SEDs and the bolometric correction presented in this work can determine the radiative power of any sample of radio-quiet to radio-loud Type 1 AGN with observations in the range from 1 µm to 10 keV provided the observations are corrected for extinction.

Powerful Radio-loud Quasars Are Triggered by Galaxy Mergers in the Cosmic Bright Ages

“…The 3CR bolometric luminosities were determined from quasar PSF magnitudes obtained during our Galfit decompositions described further in Section 3.2 and given in Table 2. Bolometric correction factors were obtained from Azadi et al (2022) for radio-loud quasars at 1 < z < 2, after redshifting the F140W filter to the appropriate rest-frame value for each source. The black hole masses and bolometric luminosities are taken from the reference papers for the control samples; the values are given in Table 3.…”