Erratum: Updating quasar bolometric luminosity corrections

By J. Runnoe, M. Brotherton, Zhaohui Shang. 2012

217 citations recorded by the source corpus.

Bolometric corrections are used in quasar studies to quantify total energy output based on a measurement of a monochromatic luminosity. First, we enumerate and discuss the practical difficulties of determining such corrections, then we present bolometric luminosities between 1 μm and 8 keV rest frame and corrections derived from the detailed spectral energy distributions of 63 bright quasars of low to moderate redshift (z = 0.03–1.4). Exploring several mathematical fittings, we provide practical bolometric corrections of the forms Liso = ζλ Lλ and log (Liso) = A + Blog (λLλ )f orλ = 1450, 3000 and 5100 A, where Liso is the bolometric luminosity calculated under the assumption of isotropy. The significant scatter in the 5100 A bolometric correction can be reduced by adding a first-order correction using the optical slope, αλ,opt. We recommend an adjustment to the bolometric correction to account for viewing angle and the anisotropic emission expected from accretion discs. For optical/UV monochromatic luminosities, radio-loud and radio-quiet bolometric corrections are consistent within 95 per cent confidence intervals, so we do not make separate radio-loud and radio-quiet corrections. In addition, we provide several bolometric corrections to the 2–10 keV X-ray luminosity, which are shown to have very large scatter. Separate radio-loud and radio-quiet corrections are warranted by the X-ray data.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/425678cd8ccf393735377f4bfa012b14e9b0ba6a

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Citations in the corpus

• An ALMA [C ii] Survey of 27 Quasars at z > 5.94 (2018, methodology): “8BH min bol 38 1 We derive the bolometric luminosity from the observed flux density at 1450Å, following the conversion derived by Runnoe et al. (2012) and recomputed in Venemans et al. (2016): l = + l - - ( Å) ( )L Llog erg s 4.553 0.911 log 1450 erg s .”
• Science with the space-based interferometer eLISA. III: probing the expansion of the universe using gravitational wave standard sirens (2016, methodology): “For standard quasars, a (linear) bolometric correction of 3-to-10 applies to single filter bands ranging from 145nm to 510nm [70].”
• THE DISCOVERY OF THE FIRST “CHANGING LOOK” QUASAR: NEW INSIGHTS INTO THE PHYSICS AND PHENOMENOLOGY OF ACTIVE GALACTIC NUCLEI (2014, methodology): “We estimate the bolometric AGN luminosity (Lbol) to be 8.8×10 44 erg s−1, using λL5100 (see Richards et al. 2006, for a discussion of the reliability of various bolometric luminosities) and a conversion factor of 8.1 to convert from monochromatic to bolometric luminosity (Runnoe et al. 2012).”
• Evolution of broad-line emission from active galactic nuclei (2013, background): “Over the entire 2–10 keV luminosity range of 1042– 1045 erg s−1 covered by the Stern & Laor sample, Lbol ≈ 45L2−10 keV within ±5% (Runnoe et al. 2012), while the mean value of the ratio LbHα/LX decreases by more than a factor of 2 between type 1.0 and 1.8 sources.”
• STAR FORMATION AND GAS KINEMATICS OF QUASAR HOST GALAXIES AT z ∼ 6: NEW INSIGHTS FROM ALMA (2013, methodology): “We calculate the 1 μm to 8 keV quasar bolometric luminosities for the four sources using an isotropic bolometric correction of Lbol = 4.2L1450 (Runnoe et al. 2012a, 2012b), where L1450 is the rest-frame 1450 Å luminosity calculated from the 1450 Å magnitudes in the discovery papers (Fan et al.…”
• Now You See It, Now You Don't: The Disappearing Central Engine of the Quasar J1011+5442 (2015, methodology): “In the bright state, we apply the 5100 Å bolometric correction with a nonzero intercept from table 1 of Runnoe et al. (2012) to the monochromatic optical luminosity λLλ(5100 Å) = (6.3±0.1)×1043 erg s−1 to calculate a bolometric luminosity of Lbol = (6.8±0.1)×10 44 erg s−1.”
• Black Hole Growth to z = 2 - I: Improved Virial Methods for Measuring M_BH and L/L_Edd (2012, methodology): “However, the best-fit trends of Runnoe et al. (2012) predict fbol ( 3000Å ) ≃ 5.3 for sources withL3000≃ 1045, consistent with the commonly used value of 5.15.”
• A diversity of dusty AGN tori - Data release for the VLTI/MIDI AGN Large Program and first results for 23 galaxies (2013, methodology): “This is the model 7 We assume Lbol ≈ 1.5LUV, from Elvis et al. (1994) and Runnoe et al. (2012), with the assumption of a flat powerlaw spectrum in the optical (e.g. Kishimoto et al., 2008).”
• The dust covering factor in active galactic nuclei (2016, background): “However, the correction factors adopted by different authors differ significantly (e.g. Shen et al. 2011; Trakhtenbrot & Netzer 2012; Runnoe et al. 2012; Krawczyk et al. 2013).”
• Universal bolometric corrections for active galactic nuclei over seven luminosity decades (2020, methodology): “Runnoe et al. (2012a) sampled the optical band giving the bolometric corrections at three different wavelengths (1450 Å, 3500 Å and 4000 Å), while IR bolometric corrections were provided in Runnoe et al. (2012b).”