2018A&A...615A.123Q


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.01CET21:39:19

2018A&A...615A.123Q - Astronomy and Astrophysics, volume 615A, 123-123 (2018/7-1)

Model simulation of jet precession in quasar PG 1302-102.

QIAN S.J., BRITZEN S., WITZEL A., KRICHBAUM T.P. and KUN E.

Abstract (from CDS):


Context. The study of periodic (or quasi-periodic) variabilities in optical and radio bands and quasi-periodic radio-jet swings are important to further our understanding of the physical processes in blazars. Among these the correlation between the periodic or quasi-periodic phenomena in radio and optical bands is particularly significant, because it can provide unique information about the relativistic jets and central engines in the nuclei of blazars.
Aims. We aim to investigate the possibility that the radio jet swing on parsec scales observed in PG 1302-102 (z = 0.278) is a quasi-periodic phenomenon and study its correlation with the periodic optical variability claimed in a recently published work, seeking evidence for a binary black hole system.
Methods. The precessing jet-nozzle model proposed in our previous works was applied to simulate the kinematics of the superluminal components. It is shown that the inner-jet kinematic features can well be explained in terms of the precessing nozzle model.
Results. Based on the model simulation (model fitting) of the inner kinematics for its six superluminal components, a precession period of ∼5.1583±0.5yr is derived for the radio jet swing and the kinematics of all the six components are consistently interpreted. The similarity between the radio jet precession period and the optical period found in its optical light curve may be physically significant. Both periodic behaviors in radio and optical bands could be explained in terms of the orbital motion of a black hole binary, if the orbital plane makes large inclinations to the sky plane: the orbital motion of the primary hole produces the periodic jet swing and the orbital motion of the secondary hole produces the periodic optical variability as suggested in the literature. Thus the total mass and the mass ratio of the binary are estimated.
Conclusions. Based on this analysis, we show that PG 1302-102 might have a supermassive black hole binary existing in its nucleus and it is starting to enter its inspiral phase of merging. Gravitational radiation would start to dominate the energy-momentum loss for its orbital shrinkage.

Abstract Copyright: © ESO 2018

Journal keyword(s): galaxies: jets - galaxies: nuclei - quasars: individual: 1302-102 - quasars: supermassive black holes

CDS comments: Knots CN not in SIMBAD.

Simbad objects: 14

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Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 UGC 1841 Sy1 02 23 11.41124 +42 59 31.3840   15.71 14.81     ~ 533 2
2 4C 50.11 QSO 03 59 29.74726473 +50 57 50.1615765           ~ 401 1
3 QSO B0420-0127 QSO 04 23 15.80072776 -01 20 33.0654034   17.50 17.00 16.28   ~ 1084 3
4 QSO B0605-0834 BLL 06 07 59.69923743 -08 34 49.9781718     18.5 17.70   ~ 407 1
5 QSO J0854+2006 BLL 08 54 48.8749311881 +20 06 30.642936668   15.91 15.43 15.56   ~ 2060 1
6 3C 273 BLL 12 29 06.6996828061 +02 03 08.598846466   13.05 14.830 14.11   ~ 5404 1
7 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6351 3
8 3C 279 Bla 12 56 11.1664521013 -05 47 21.531840471   18.01 17.75 15.87   ~ 2752 2
9 ICRF J130533.0-103319 Sy1 13 05 33.0149111397 -10 33 19.430590671   15.18 15.23 14.46   ~ 512 1
10 7C 1308+3236 BLL 13 10 28.66387 +32 20 43.7831   15.61 15.24 17.91   ~ 760 1
11 3C 345 QSO 16 42 58.8100340220 +39 48 36.999540578   16.81 16.59 16.84   ~ 1574 2
12 NAME BL Lac BLL 22 02 43.2913773726 +42 16 39.978417860   15.66 14.72     ~ 2037 1
13 3C 454.3 Bla 22 53 57.74798 +16 08 53.5611   16.57 16.10 15.22   ~ 2556 2
14 GrW 150914 GWE ~ ~           ~ 416 1

    Equat.    Gal    SGal    Ecl

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