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Title: Disk–Jet Connection in Active Supermassive Black Holes in the Standard Accretion Disk Regime

We study the disk–jet connection in supermassive black holes by investigating the properties of their optical and radio emissions utilizing the SDSS DR7 and the NVSS catalogs. Our sample contains 7017 radio-loud quasars with detection both at 1.4 GHz and SDSS optical spectra. Using this radio-loud quasar sample, we investigate the correlation among the jet power ($${P}_{\mathrm{jet}}$$), the bolometric disk luminosity ($${L}_{\mathrm{disk}}$$), and the black hole mass ($${M}_{\mathrm{BH}}$$) in the standard accretion disk regime. We find that the jet powers correlate with the bolometric disk luminosities as $$\mathrm{log}{P}_{\mathrm{jet}}=(0.96\pm 0.012)\mathrm{log}{L}_{\mathrm{disk}}+(0.79\pm 0.55)$$. This suggests the jet production efficiency of $${\eta }_{\mathrm{jet}}\simeq {1.1}_{-0.76}^{+2.6}\,\times {10}^{-2}$$ assuming the disk radiative efficiency of 0.1, implying low black hole spin parameters and/or low magnetic flux for radio-loud quasars. But it can be also due to the dependence of this efficiency on the geometrical thickness of the accretion flow, which is expected to be small for quasars accreting at the disk Eddington ratios $$0.01\lesssim \lambda \lesssim 0.3$$. This low jet production efficiency does not significantly increase even if we set the disk radiative efficiency to be 0.3. We also investigate the fundamental plane in our samples among $${P}_{\mathrm{jet}}$$, $${L}_{\mathrm{disk}}$$, and $${M}_{\mathrm{BH}}$$. In conclusion, we could not find a statistically significant fundamental plane for radio-loud quasars in the standard accretion regime.
Authors:
ORCiD logo [1] ;  [1] ; ORCiD logo [2] ;  [3] ;  [4]
  1. Institute of Space and Astronautical Science JAXA, Kanagawa (Japan)
  2. Hiroshima Univ., Hiroshima (Japan)
  3. Nicolaus Copernicus Astronomical Center, Warsaw (Poland)
  4. SLAC National Accelerator Lab., Stanford Univ., Menlo Park, CA (United States)
Publication Date:
Report Number(s):
SLAC-PUB-17169
Journal ID: ISSN 1538-4357; TRN: US1703135
Grant/Contract Number:
AC02-76SF00515
Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal (Online)
Additional Journal Information:
Journal Name: The Astrophysical Journal (Online); Journal Volume: 840; Journal Issue: 1; Journal ID: ISSN 1538-4357
Publisher:
Institute of Physics (IOP)
Research Org:
SLAC National Accelerator Lab., Menlo Park, CA (United States)
Sponsoring Org:
USDOE
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; accretion; accretion disks; black hole physics; galaxies: active; galaxies: jets; quasars: supermassive black holes
OSTI Identifier:
1406497

Inoue, Yoshiyuki, Doi, Akihiro, Tanaka, Yasuyuki T., Sikora, Marek, and Madejski, Grzegorz M.. Disk–Jet Connection in Active Supermassive Black Holes in the Standard Accretion Disk Regime. United States: N. p., Web. doi:10.3847/1538-4357/aa6b57.
Inoue, Yoshiyuki, Doi, Akihiro, Tanaka, Yasuyuki T., Sikora, Marek, & Madejski, Grzegorz M.. Disk–Jet Connection in Active Supermassive Black Holes in the Standard Accretion Disk Regime. United States. doi:10.3847/1538-4357/aa6b57.
Inoue, Yoshiyuki, Doi, Akihiro, Tanaka, Yasuyuki T., Sikora, Marek, and Madejski, Grzegorz M.. 2017. "Disk–Jet Connection in Active Supermassive Black Holes in the Standard Accretion Disk Regime". United States. doi:10.3847/1538-4357/aa6b57. https://www.osti.gov/servlets/purl/1406497.
@article{osti_1406497,
title = {Disk–Jet Connection in Active Supermassive Black Holes in the Standard Accretion Disk Regime},
author = {Inoue, Yoshiyuki and Doi, Akihiro and Tanaka, Yasuyuki T. and Sikora, Marek and Madejski, Grzegorz M.},
abstractNote = {We study the disk–jet connection in supermassive black holes by investigating the properties of their optical and radio emissions utilizing the SDSS DR7 and the NVSS catalogs. Our sample contains 7017 radio-loud quasars with detection both at 1.4 GHz and SDSS optical spectra. Using this radio-loud quasar sample, we investigate the correlation among the jet power (${P}_{\mathrm{jet}}$), the bolometric disk luminosity (${L}_{\mathrm{disk}}$), and the black hole mass (${M}_{\mathrm{BH}}$) in the standard accretion disk regime. We find that the jet powers correlate with the bolometric disk luminosities as $\mathrm{log}{P}_{\mathrm{jet}}=(0.96\pm 0.012)\mathrm{log}{L}_{\mathrm{disk}}+(0.79\pm 0.55)$. This suggests the jet production efficiency of ${\eta }_{\mathrm{jet}}\simeq {1.1}_{-0.76}^{+2.6}\,\times {10}^{-2}$ assuming the disk radiative efficiency of 0.1, implying low black hole spin parameters and/or low magnetic flux for radio-loud quasars. But it can be also due to the dependence of this efficiency on the geometrical thickness of the accretion flow, which is expected to be small for quasars accreting at the disk Eddington ratios $0.01\lesssim \lambda \lesssim 0.3$. This low jet production efficiency does not significantly increase even if we set the disk radiative efficiency to be 0.3. We also investigate the fundamental plane in our samples among ${P}_{\mathrm{jet}}$, ${L}_{\mathrm{disk}}$, and ${M}_{\mathrm{BH}}$. In conclusion, we could not find a statistically significant fundamental plane for radio-loud quasars in the standard accretion regime.},
doi = {10.3847/1538-4357/aa6b57},
journal = {The Astrophysical Journal (Online)},
number = 1,
volume = 840,
place = {United States},
year = {2017},
month = {5}
}