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Colección SciELO Chile

MOMO. VI. Multifrequency Radio Variability of the Blazar OJ 287 from 2015 to 2022, Absence of Predicted 2021 Pecursor-flare Activity, and a New Binary Interpretation of the 2016/2017 Outburst

Indexado

WoS	WOS:000937575100001
Scopus	SCOPUS_ID:85149130600

DOI

10.3847/1538-4357/ACAF71

Año

2023

Tipo

artículo de investigación

Citas Totales

Autores Afiliación Chile

Instituciones Chile

% Participación
Internacional

Autores
Afiliación Extranjera

Instituciones
Extranjeras

Abstract

Based on our dedicated Swift monitoring program, MOMO, OJ 287 is one of the best-monitored blazars in the X-ray-UV-optical regime. Here, we report results from our accompanying, dense, multifrequency (1.4-44 GHz) radio monitoring of OJ 287 between 2015 and 2022 covering a broad range of activity states. Fermi γ-ray observations were added. We characterize the radio flux and spectral variability in detail, including discrete correlation function and other variability analyses, and discuss its connection with the multiwavelength emission. Deep fades of the radio and optical-UV fluxes are found to occur every 1-2 yr. Further, it is shown that a precursor flare of thermal bremsstrahlung predicted by one of the binary supermassive black hole (SMBH) models of OJ 287 was absent. We then focus on the nature of the extraordinary, nonthermal, 2016/2017 outburst that we initially discovered with Swift. We interpret it as the latest of the famous optical double-peaked outbursts of OJ 287, favoring binary scenarios that do not require a highly precessing secondary SMBH.

Revista

Revista	ISSN
Astrophysical Journal	0004-637X

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Disciplinas de Investigación

WOS
Astronomy & Astrophysics

Scopus
Sin Disciplinas

SciELO
Sin Disciplinas

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Publicaciones WoS (Ediciones: ISSHP, ISTP, AHCI, SSCI, SCI), Scopus, SciELO Chile.

Colaboración Institucional

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Autores - Afiliación

Ord.	Autor	Género	Institución - País
1	Komossa, S.	Mujer	Max Planck Institute for Radio Astronomy - Alemania Max Planck Inst Radioastron - Alemania
2	Wiesemeyer, H.	Hombre	Max Planck Institute for Radio Astronomy - Alemania Max Planck Inst Radioastron - Alemania
3	Grupe, Dirk	Hombre	Northern Kentucky University - Estados Unidos Northern Kentucky Univ - Estados Unidos
4	Gonzalez, A. G.	-	Saint Mary's University - Canadá St Marys Univ - Canadá
5	Gurwell, Mark	Hombre	Harvard-Smithsonian Center for Astrophysics - Estados Unidos Harvard & Smithsonian - Estados Unidos
6	Gallo, L. C.	-	Saint Mary's University - Canadá St Marys Univ - Canadá
7	Liu, F. K.	-	Peking University - China Peking Univ - China
8	Myserlis, I.	Hombre	Max Planck Institute for Radio Astronomy - Alemania Institut de Radioastronomie Milliḿetrique - España Max Planck Inst Radioastron - Alemania Inst Radioastronomie Millimetr - España
9	Krichbaum, Thomas P.	Hombre	Max Planck Institute for Radio Astronomy - Alemania Max Planck Inst Radioastron - Alemania
10	Laine, S.	Hombre	Infrared Processing & Analysis Center - Estados Unidos IPAC - Estados Unidos
11	Bach, Uwe	-	Max Planck Institute for Radio Astronomy - Alemania Max Planck Inst Radioastron - Alemania
12	Gómez, J. L.	-	Instituto de Astrofísica de Andalucía - CSIC - España CSIC - España
13	Parker, M. L.	-	Institute of Astronomy - Reino Unido UNIV CAMBRIDGE - Reino Unido
14	Yao, Su	-	Max Planck Institute for Radio Astronomy - Alemania Max Planck Inst Radioastron - Alemania
15	Berton, M.	Hombre	European Southern Observatory Santiago - Chile Observatorio Europeo Austral - Chile

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Financiamiento

Fuente
National Aeronautics and Space Administration
Smithsonian Institution
Academia Sinica
Jet Propulsion Laboratory, California Institute of Technology
IPAC
Max-Planck-Institut fur Radioastronomie
Smithsonian Institution and the Academia Sinica

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Agradecimientos

Agradecimiento
It is our great pleasure to thank the Swift team for carrying out the observations of OJ 287 that we proposed, and for very useful discussions regarding the observational set-up and related questions throughout the years. We would like to thank Alan Roy for useful comments on the manuscript. This work is partly based on data obtained with the 100 m telescope of the Max-Planck-Institut für Radioastronomie at Effelsberg. The Submillimeter Array near the summit of Maunakea is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (SSDC), Italy. This work has made use of Fermi-LAT data supplied by Kocevski et al. () at https://fermi.gsfc.nasa.gov/ssc/data/access/lat/LightCurveRepository/ . This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.
It is our great pleasure to thank the Swift team for carrying out the observations of OJ 287 that we proposed, and for very useful discussions regarding the observational set-up and related questions throughout the years. We would like to thank Alan Roy for useful comments on the manuscript. This work is partly based on data obtained with the 100 m telescope of the Max-Planck-Institut für Radioastronomie at Effelsberg. The Submillimeter Array near the summit of Maunakea is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (SSDC), Italy. This work has made use of Fermi-LAT data supplied by Kocevski et al. () at https://fermi.gsfc.nasa.gov/ssc/data/access/lat/LightCurveRepository/ . This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.
It is our great pleasure to thank the Swift team for carrying out the observations of OJ 287 that we proposed, and for very useful discussions regarding the observational set-up and related questions throughout the years. We would like to thank Alan Roy for useful comments on the manuscript. This work is partly based on data obtained with the 100 m telescope of the Max-Planck-Institut fuer Radioastronomie at Effelsberg. The Submillimeter Array near the summit of Maunakea is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (SSDC), Italy. This work has made use of Fermi-LAT data supplied by Kocevski et al. (2021) at https://fermi.gsfc.nasa.gov/ssc/data/access/lat/LightCurveRepository/. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.