CaltechAUTHORS
  A Caltech Library Service

Broadband X-ray Spectral Analysis of the Double-Nucleus Luminous Infrared Galaxy Mrk 463

Yamada, Satoshi and Ueda, Yoshihiro and Oda, Saeko and Tanimoto, Atsushi and Imanishi, Masatoshi and Terashima, Yuichi and Ricci, Claudio (2018) Broadband X-ray Spectral Analysis of the Double-Nucleus Luminous Infrared Galaxy Mrk 463. Astrophysical Journal, 858 (2). Art. No. 106. ISSN 1538-4357. http://resolver.caltech.edu/CaltechAUTHORS:20180402-090755050

[img] PDF - Submitted Version
See Usage Policy.

1789Kb

Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:20180402-090755050

Abstract

We present a broadband (0.4–70 keV) X-ray spectral analysis of the luminous infrared galaxy (LIRG) system Mrk 463 observed with Nuclear Spectroscopic Telescope Array (NuSTAR), Chandra, and XMM-Newton, which contains double active galactic nuclei (AGNs; Mrk 463E and Mrk 463W) with a separation of ~3.8 kpc. Detecting their transmitted hard X-ray >10 keV continua with NuSTAR, we confirm that Mrk 463E and Mrk 463W have AGNs with intrinsic luminosities of (1.6–2.2) × 10^(43) and (0.5–0.6) × 10^(43) erg s^(−1) (2–10 keV) obscured by hydrogen column densities of 8 × 10^(23) and 3 × 10^(23) cm^(−2), respectively. Both nuclei show strong reflection components from cold matter. The luminosity ratio between X-ray (2–10 keV) and [O IV] 25.89 μm of Mrk 463E is ~5 times smaller than those of normal Seyfert galaxies, suggesting that the intrinsic SED is X-ray weak relative to the UV luminosity. In fact, the bolometric AGN luminosity of Mrk 463E estimated from L'-band (3.8 μm), [O IV] 25.89 μm, and [Ne V] 14.32 μm lines indicate a large bolometric-to-X-ray luminosity ratio, κ_(2–10 keV) ≈ 110–410, and a high Eddington ratio, λ_(Edd) ~ 0.4–0.8. We suggest that the merger triggered a rapid growth of the black hole in Mrk 463E, which is not yet deeply "buried" by circumnuclear dust. By contrast, the L'-band luminosity of Mrk 463W is unusually small relative to the X-ray luminosity, suggesting that the Eddington ratio is low (<10^(−3)) and it might be still in an early phase of merger-driven AGN activity.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aabacbDOIArticle
http://arxiv.org/abs/1803.11223PublisherDiscussion Paper
ORCID:
AuthorORCID
Ueda, Yoshihiro0000-0001-7821-6715
Tanimoto, Atsushi0000-0002-0114-5581
Imanishi, Masatoshi0000-0001-6186-8792
Terashima, Yuichi0000-0003-1780-5481
Ricci, Claudio0000-0001-5231-2645
Additional Information:© 2018 The American Astronomical Society. Received 2018 January 23; revised 2018 March 19; accepted 2018 March 27; published 2018 May 11. Part of this work was financially supported by the Grant-in-Aid for Scientific Research 17K05384 (Y.U.), 15K05030 (M.I.), 15H02070, 16K05296 (Y.T.), and for JSPS Fellows for young researchers (A.T.). C.R. acknowledges financial support from the China-CONICYT fellowship, FONDECYT 1141218, and Basal-CATA PFB-06/2007. Support for this work was provided by the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory and funded by the National Aeronautics and Space Administration. This research also made use of data obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, and with Chandra, supported by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA.
Group:NuSTAR
Subject Keywords:black hole physics – galaxies: active – galaxies: individual (Mrk 463) – infrared: galaxies – X-rays: galaxies
Record Number:CaltechAUTHORS:20180402-090755050
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20180402-090755050
Official Citation:Satoshi Yamada et al 2018 ApJ 858 106
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:85555
Collection:CaltechAUTHORS
Deposited By: Joy Painter
Deposited On:02 Apr 2018 16:15
Last Modified:18 May 2018 18:06

Repository Staff Only: item control page