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MOMO - V. Effelsberg, Swift, and Fermi study of the blazar and supermassive binary black hole candidate OJ 287 in a period of high activity

Ciprini S; Gurwell MA; Gomez JL; Laine S; Bach U; Kraus A; Myserlis I; Krichbaum TP; Gonzalez A; Grupe D; Valtonen MJ; Komossa S; Gallo LC

MOMO - V. Effelsberg, Swift, and Fermi study of the blazar and supermassive binary black hole candidate OJ 287 in a period of high activity

Ciprini S
Gurwell MA
Gomez JL
Laine S
Bach U
Kraus A
Myserlis I
Krichbaum TP
Gonzalez A
Grupe D
Valtonen MJ
Komossa S
Gallo LC
Katso/Avaa
ValtonenEtAl2022MOMOVEffelsbergSwiftAndFermi.pdf (1.634Mb)
Lataukset: 

OXFORD UNIV PRESS
doi:10.1093/mnras/stac792
URI
https://academic.oup.com/mnras/article/513/3/3165/6553855
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Julkaisun pysyvä osoite on:
https://urn.fi/URN:NBN:fi-fe2022081154696
Tiivistelmä
We report results from our ongoing project MOMO (Multiwavelength Observations and Modelling of OJ 287). In this latest publication of a sequence, we combine our Swift UVOT-XRT and Effelsberg radio data (2.6-44 GHz) between 2019 and 2022.04 with public SMA data and gamma-ray data from the Fermi satellite. The observational epoch covers OJ 287 in a high state of activity from radio to X-rays. The epoch also covers two major events predicted by the binary supermassive black hole (SMBH) model of OJ 287. Spectral and timing analyses clearly establish: a new UV-optical minimum state in 2021 December at an epoch where the secondary SMBH is predicted to cross the disc surrounding the primary SMBH; an overall low level of gamma-ray activity in comparison to pre-2017 epochs; the presence of a remarkable, long-lasting UV-optical flare event of intermediate amplitude in 2020-2021; a high level of activity in the radio band with multiple flares; and particularly a bright, ongoing radio flare peaking in 2021 November that may be associated with a gamma-ray flare, the strongest in 6 yr. Several explanations for the UV-optical minimum state are explored, including the possibility that a secondary SMBH launches a temporary jet, but the observations are best explained by variability associated with the main jet.
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