Super-Eddington Accretion in the WISE-selected Extremely Luminous Infrared Galaxy W2246-0526
Journal article, 2018

We use optical and near-infrared spectroscopy to observe rest-UV emission lines and estimate the black hole mass of WISEA J224607.56-052634.9 (W2246-0526) at z = 4.601, the most luminous hot, dust-obscured galaxy yet discovered by WISE. From the broad component of the Mg ii 2799 Å emission line, we measure a black hole mass of log(M BH/M ) = 9.6 ± 0.4. The broad C iv 1549 Å line is asymmetric and significantly blueshifted. The derived M BH from the blueshift-corrected broad C iv line width agrees with the Mg ii result. From direct measurement using a well-sampled SED, the bolometric luminosity is 3.6 -1014 L . The corresponding Eddington ratio for W2246-0526 is λ Edd = L AGN/L Edd = 2.8. This high Eddington ratio may reach the level where the luminosity is saturating due to photon trapping in the accretion flow and may be insensitive to the mass accretion rate. In this case, the M BH growth rate in W2246-0526 would exceed the apparent accretion rate derived from the observed luminosity.

quasars: emission lines

quasars: supermassive black holes

infrared: galaxies

galaxies: individual (WISEA J224607.56-052634.9)

galaxies: active

galaxies: nuclei

Author

Chao Wei Tsai

University of California

Peter Eisenhardt

Jet Propulsion Laboratory, California Institute of Technology

Hyunsung D. Jun

Korea Institute for Advanced Study

Jingwen Wu

Chinese Academy of Sciences

Roberto Assef

Universidad Diego Portales

A. Blain

University Of Leicester

T. Diaz-Santos

Universidad Diego Portales

Suzy Jones

Chalmers, Space, Earth and Environment, Astronomy and Plasmaphysics

D. Stern

Jet Propulsion Laboratory, California Institute of Technology

Edward Wright

University of California

Sherry C.C. Yeh

W. M. Keck Observatory

Astrophysical Journal

0004-637X (ISSN) 1538-4357 (eISSN)

Vol. 868 1 15

Subject Categories

Meteorology and Atmospheric Sciences

Astronomy, Astrophysics and Cosmology

Atom and Molecular Physics and Optics

DOI

10.3847/1538-4357/aae698

More information

Latest update

12/7/2018