Astronomy:PKS 1302-102

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Coordinates: Sky map 13h 05m 33.01498s, −10° 33′ 19.4266″

PKS 1302-102
Observation data (Epoch J2000.0)
ConstellationVirgo[1]
Right ascension 13h 05m 33.01498s[2]
Declination−10° 33′ 19.4266″[2]
Redshift0.2784[1]
Distance3.5×10^9 ly (1.1 Gpc)[1]
TypeFSRS, FSRQ, FSQ, QSO, E4[2][1]
Apparent magnitude (V)14.9[1]
Other designations
PG 1302-102, PG 1302-103, ICRF J130533.0-103319, PKS 1302-102, PKS 1302-103, PKS J1305-1033, PKS B1302-102, QSO J1305-1033, QSO B1302-1017[2]
See also: Quasar,List of quasars]]

PKS 1302-102 is a quasar in the Virgo constellation, located at a distance of approximately 1.1 Gpc (around 3.5 billion light-years).[1] It has an apparent magnitude of about 14.9 mag in the V band with a redshift of 0.2784.[1] The quasar is hosted by a bright elliptical galaxy,[3] with two neighboring companions at distances of 3 kpc and 6 kpc. The light curve of PKS 1302-102 appears to be sinusoidal with an amplitude of 0.14 mag and a period of 1,884 ± 88 days, which suggests evidence of a supermassive black hole binary.[4]

Possible black hole binary

PKS 1302-102 was selected from the Catalina Real-Time Transient Survey as one of 20 quasars with apparent periodic variations in the light curve. Of these quasars, PKS 1302-102 appeared to be the best candidate in terms of sinusoidal behavior and other selection criteria, such as data coverage of more than 1.5 cycles in the measured period.[4] One plausible interpretation of the apparent periodic behavior is the possibility of two supermassive black holes (SMBH) orbiting each other with a separation of approximately 0.1 pc in the final stages of a 3.3 billion year old galaxy merger. If this turns out to be the case, it would make PKS 1302-102 an important object of study to various areas of research, including gravitational wave studies and the unsolved final parsec problem in a merger of black holes.

Other explanations, of lesser likelihood, to the observed sinusoidal periodicity include a hot spot on the inner part of the black hole's accretion disk and the possibility of a warped accretion disk which partially eclipses in the orbit around a single SMBH.[4] However, it also remains possible that the periodic behavior in PKS 1302-102 is indeed just a random occurrence in the light curve of an ordinary quasar, as spurious nearly-periodic variations can occur over limited time periods as part of stochastic quasar variability.[5] Further observations of the quasar could either promote true periodicity or rule out a binary interpretation, especially if the measured light curve randomly diverges from the sinusoidal model.[5]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 "PG 1302-102". NED. http://ned.ipac.caltech.edu/cgi-bin/objsearch?objname=PG+1302-102+&extend=no&hconst=73&omegam=0.27&omegav=0.73&corr_z=1&out_csys=Equatorial&out_equinox=J2000.0&obj_sort=RA+or+Longitude&of=pre_text&zv_breaker=30000.0&list_limit=5&img_stamp=YES. Retrieved 2015-01-11. 
  2. ↑ 2.0 2.1 2.2 2.3 "ICRF J130533.0-103319". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=ICRF+J130533.0-103319. 
  3. ↑ Disney, M. J.; Boyce, P. J.; Blades, J. C.; Boksenberg, A.; Crane, P.; Deharveng, J. M.; Macchetto, F.; Mackay, C. D. et al. (1995-07-13). "Interacting elliptical galaxies as hosts of intermediate-redshift quasars" (in en). Nature 376 (6536): 150–153. doi:10.1038/376150a0. Bibcode: 1995Natur.376..150D. 
  4. ↑ 4.0 4.1 4.2 Graham, Matthew J.; Djorgovski, S. G.; Stern, Daniel; Glikman, Eilat; Drake, Andrew J.; Mahabal, Ashish A.; Donalek, Ciro; Larson, Steve et al. (2015-02-01). "A possible close supermassive black-hole binary in a quasar with optical periodicity". Nature 518 (7537): 74–76. doi:10.1038/nature14143. ISSN 0028-0836. PMID 25561176. Bibcode: 2015Natur.518...74G. 
  5. ↑ 5.0 5.1 Vaughan, S.; Uttley, P.; Markowitz, A. G.; Huppenkothen, D.; Middleton, M. J.; Alston, W. N.; Scargle, J. D.; Farr, W. M. (2016-09-01). "False periodicities in quasar time-domain surveys". Monthly Notices of the Royal Astronomical Society 461 (3): 3145–3152. doi:10.1093/mnras/stw1412. ISSN 0035-8711. Bibcode: 2016MNRAS.461.3145V. 

Further reading



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