Absence of the predicted 2022 October outburst of OJ 287 and implications for binary SMBH scenarios. Issue 1 (23rd February 2023)

• Record Type: Journal Article
• Authors: Komossa, S; Grupe, D; Kraus, A; Gurwell, M A; Haiman, Z; Liu, F K; Tchekhovskoy, A; Gallo, L C; Berton, M; Blandford, R; Gómez, J L; Gonzalez, A G
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 522:Issue 1(2023)
• Page Start: L84
• Page End: L88
• Publication Date: 2023-02-23
• Subjects: galaxies: active -- galaxies: jets -- galaxies: nuclei -- quasars: individual: OJ 287 -- quasars: supermassive black holes; Astronomy -- Research -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnrasl/slad016
• Languages: English
• ISSNs: 1745-3933

Abstract

ABSTRACT: The project MOMO (Multiwavelength Observations and Modelling of OJ 287) was set up to test predictions of binary supermassive black hole (SMBH) scenarios and to understand disc–jet physics of the blazar OJ 287. After a correction, the precessing binary (PB) SMBH model predicted the next main outburst of OJ 287 in 2022 October, making the outburst well observable and the model testable. We have densely covered this period in our ongoing multifrequency radio, optical, ultraviolet (UV), and X-ray monitoring. The predicted outburst was not detected. Instead, OJ 287 was at low optical–UV emission levels, declining further into November. The predicted thermal bremsstrahlung spectrum was not observed either, at any epoch. Further, applying scaling relations, we estimate an SMBH mass of OJ 287 of 10 8 M⊙ . The latest in a sequence of deep low states that recur every 1–2 yr is used to determine an upper limit on the Eddington ratio and on the accretion-disc luminosity. This limit is at least a factor of 10 lower than required by the PB model with its massive primary SMBH of >10 10 M⊙ . All these results favour alternative binary SMBH models of OJ 287 that require neither strong orbital precession nor a very large mass of the primary SMBH.