Signatures of a spinning supermassive black hole binary on the mas-scale jet of the quasar S5 1928+738 based on 25 yr of VLBI data

Author:

Kun E12345ORCID,Britzen S6,Frey S457ORCID,Gabányi K É4589,Gergely L Á101112

Affiliation:

1. Theoretical Physics IV, Faculty for Physics & Astronomy, Ruhr University Bochum , D-44780 Bochum , Germany

2. Faculty for Physics & Astronomy, Astronomical Institute, Ruhr University Bochum , D-44780 Bochum , Germany

3. Ruhr Astroparticle and Plasma Physics Center, Ruhr-Universität Bochum , D-44780 Bochum , Germany

4. Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Sciences , Konkoly Thege Miklós út 15-17, H-1121 Budapest , Hungary

5. CSFK, MTA Centre of Excellence , Konkoly Thege Miklós út 15-17, H-1121 Budapest , Hungary

6. Max-Planck-Institute für Radioastronomie , Auf dem Hügel 69, D-53121 Bonn , Germany

7. Institute of Physics and Astronomy, ELTE Eötvös Loránd University , Pázmány Péter sétány 1/A, H-1117 Budapest , Hungary

8. Department of Astronomy, Institute of Physics and Astronomy, ELTE Eötvös Loránd University , Pázmány Péter sétány 1/A, H-1117 Budapest , Hungary

9. HUN-REN–ELTE Extragalactic Astrophysics Research Group , Pázmány Péter sétány 1/A, H-1117 Budapest , Hungary

10. Department of Experimental Physics, University of Szeged , Dóm tér 9, H-6720 Szeged , Hungary

11. Department of Theoretical Physics, University of Szeged , Tisza Lajos krt. 84-86, H-6720 Szeged , Hungary

12. Department of Theoretical Physics, HUN-REN Wigner Research Centre for Physics , Konkoly-Thege Miklós út 29-33, H-1121 Budapest , Hungary

Abstract

ABSTRACT In a previous work, we have identified the spin of the dominant black hole of a binary from its jet properties. Analysing Very Long Baseline Array (VLBA) observations of the quasar S5 1928+738, taken at 15-GHz during 43 epochs between 1995.96 and 2013.06, we showed that the inclination angle variation of the inner (<2 mas) jet symmetry axis naturally decomposes into a periodic and a monotonic contribution. The former emerges due to the Keplerian orbital evolution, while the latter is interpreted as the signature of the spin-orbit precession of the jet emitting black hole. In this paper, we revisit the analysis of the quasar S5 1928+738 by including new 15-GHz VLBA observations extending over 29 additional epochs, between 2013.34 and 2020.89. The extended data set confirms our previous findings which are further supported by the flux density variation of the jet. By applying an enhanced jet precession model that can handle arbitrary spin orientations κ with respect to the orbital angular momentum of a binary supermassive black hole system, we estimate the binary mass ratio as ν = 0.21 ± 0.04 for κ = 0 (i.e. when the spin direction is perpendicular to the orbital plane) and as ν = 0.32 ± 0.07 for κ = π/2 (i.e. when the spin lies in the orbital plane). We estimate more precisely the spin precession velocity, halving its uncertainty from $(-0.05\pm 0.02)$ to $(-0.04\pm 0.01)^{\circ }\, \mathrm{yr}^{-1}$.

Funder

Alexander von Humboldt Foundation

DFG

National Science Foundation

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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