A1 Refereed original research article in a scientific journal
On the need of an ultramassive black hole in OJ 287
Authors: Valtonen MJ, Zola S, Gopakumar A, Lahteenmaki A, Tornikoski M, Dey L, Gupta AC, Pursimo T, Knudstrup E, Gomez JL, Hudec R, Jelinek M, Strobl J, Berdyugin AV, Ciprini S, Reichart DE, Kouprianov VV, Matsumoto K, Drozdz M, Mugrauer M, Sadun A, Zejmo M, Sillanpaa A, Lehto HJ, Nilsson K, Imazawa R, Uemura M, Davidson JW
Publisher: OXFORD UNIV PRESS
Publication year: 2023
Journal: Monthly Notices of the Royal Astronomical Society
Journal name in source: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Journal acronym: MON NOT R ASTRON SOC
Volume: 525
Issue: 1
First page : 1153
Last page: 1157
Number of pages: 5
ISSN: 0035-8711
DOI: https://doi.org/10.1093/mnras/stad2249
Web address : https://doi.org/10.1093/mnras/stad2249
Self-archived copy’s web address: https://research.utu.fi/converis/portal/detail/Publication/181193340
The highly variable blazar OJ 287 is commonly discussed as an example of a binary black hole system. The 130 yr long optical light curve is well explained by a model where the central body is a massive black hole of 18.35 $\times$ 10(9) solar mass that supports a thin accretion disc. The secondary black hole of 0.15 x 10(9) solar mass impacts the disc twice during its 12 yr orbit, and causes observable flares. Recently, it has been argued that an accretion disc with a typical Active Galactic Nuclei (AGN) accretion rate and above mentioned central body mass should be at least six magnitudes brighter than OJ 287's host galaxy and would therefore be observationally excluded. Based on the observations of OJ 287's radio jet, detailed in Marscher and Jorstad (2011), and up-to-date accretion disc models of Azadi et al. (2022), we show that the V-band magnitude of the accretion disc is unlikely to exceed the host galaxy brightness by more than one magnitude, and could well be fainter than the host. This is because accretion power is necessary to launch the jet as well as to create electromagnetic radiation, distributed across many wavelengths, and not concentrated especially on the optical V-band. Further, we note that the claimed V-band concentration of accretion power leads to serious problems while interpreting observations of other AGN. Therefore, we infer that the mass of the primary black hole and its accretion rate do not need to be smaller than what is determined in the standard model for OJ 287.
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