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Intermediate- mass black holes in AGN discs - II. Model predictions and observational constraints

McKernan, B. and Ford, K. E. S. and Kocsis, B. and Lyra, W. and Winter, L. M. (2014) Intermediate- mass black holes in AGN discs - II. Model predictions and observational constraints. Monthly Notices of the Royal Astronomical Society, 441 (1). pp. 900-909. ISSN 0035-8711.

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If intermediate mass black holes (IMBHs) grow efficiently in gas disks around supermassive black holes, their host active galactic nucleus (AGN) disks should exhibit myriad observational signatures. Gap-opening IMBHs in AGN disks can exhibit spectral features and variability analagous to gapped protoplanetary disks. A gap-opening IMBH in the innermost disk imprints ripples and oscillations on the broad Fe Kα line which may be detectable with future X-ray missions. A non-gap-opening IMBH will accrete and produce a soft X-ray excess relative to continuum emission. An IMBH on a retrograde orbit in an AGN disk will not open a gap and will generate soft X-rays from a bow-shock 'headwind'. Accreting IMBH in a large cavity can generate ULX-like X-ray luminosities and LINER-like optical line ratios from local ionized gas. We propose that many LINERs house a weakly accreting MBH binary in a large central disk cavity and will be luminous sources of gravitational waves (GW). IMBHs in galactic nuclei may also be detected via intermittent observational signatures including: UV/X-ray flares due to tidal disruption events, asymmetric X-ray intensity distributions as revealed by AGN transits, quasi-periodic oscillations and underluminous Type Ia supernovae. GW emitted during IMBH inspiral and collisions may be detected with eLISA and LIGO, particularly from LINERs. We summarize observational signatures and compare to current data where possible or suggest future observations.

Item Type:Article
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URLURL TypeDescription DOIArticle
McKernan, B.0000-0002-9726-0508
Kocsis, B.0000-0002-4865-7517
Lyra, W.0000-0002-3768-7542
Additional Information:© 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 March 17. Received 2014 January 28; in original form 2012 September 24. We thank the referee for a report that helped us condense and focus this paper. We acknowledge very useful discussions with Tahir Yaqoob, Stephan Rosswog, Zoltan Haiman, Ari Laor, Hagai Perets, Kayhan Gültekin and Mordecai Mac Low. BM and KESF acknowledge support from NASA-APRA08-0117 and NSF PAARE AST-1153335. BK was supported in part by the W.M. Keck Foundation Fund of the Institute for Advanced Study and NASA grant NNX11AF29G. WL acknowledges support by the National Science Foundation under grant no. AST10-09802. This work was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute.
Funding AgencyGrant Number
W. M. Keck Foundation Fund of the Institute for Advanced StudyUNSPECIFIED
NASA Sagan Fellowship ProgramUNSPECIFIED
NASA Exoplanet Science InstituteUNSPECIFIED
Subject Keywords:accretion accretion discs; planets and satellites: formation; planet-disc interactions; protoplanetary discs; galaxies: active; galaxies: Seyfert
Issue or Number:1
Record Number:CaltechAUTHORS:20140620-081340662
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:46382
Deposited By: Tony Diaz
Deposited On:20 Jun 2014 18:09
Last Modified:09 Mar 2020 13:19

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