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

Author:

Komossa S1,Grupe D2,Kraus A1,Gonzalez A3,Gallo L C3,Valtonen M J45,Laine S6,Krichbaum T P1,Gurwell M A7,Gómez J L8,Ciprini S910,Myserlis I111ORCID,Bach U1ORCID

Affiliation:

1. Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany

2. Department of Physics, Earth Science, and Space System Engineering, Morehead State University, 235 Martindale Dr, Morehead, KY 40351, USA

3. Department of Astronomy and Physics, Saint Mary’s University, 923 Robie Street, Halifax, NS, B3H 3C 3, Canada

4. Finnish Centre for Astronomy with ESO, University of Turku, FI-20014, Turku, Finland

5. Department of Physics and Astronomy, University of Turku, FI-20014, Turku, Finland

6. IPAC, Mail Code 314-6, Caltech, 1200 E. California Blvd., Pasadena, CA 91125, USA

7. Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA 02138, USA

8. Instituto de Astrofísica de Andalucía-CSIC, Glorieta de la Astronomía s/n, E-18008 Granada, Spain

9. Istituto Nazionale di Fisica Nucleare (INFN) Sezione di Roma Tor Vergata, Via della Ricerca Scientifica 1, I-00133, Roma, Italy

10. ASI Space Science Data Center (SSDC), Via del Politecnico, I-00133, Roma, Italy

11. Institut de Radioastronomie Millimétrique, Avenida Divina Pastora 7, Local 20, E-18012, Granada, Spain

Abstract

ABSTRACT 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.

Funder

NASA

Jet Propulsion Laboratory

California Institute of Technology

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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