Primary black hole spin in oj 287 AS determined by the general relativity centenary flare

Valtonen, M.; Zola, S.; Ciprini, S.; Gopakumar, A.; Matsumoto, K.; Sadakane, K.; Kidger, M.; Gazeas, K.; Nilsson, K.; Berdyugin, A.; Piirola, V.; Jermak, H.; Baliyan, K.; Alicavus, F.; Boyd, D.; Campas Torrent, M.; Campos, F.; Carrillo Gomez, J.; Caton, D.; Chavushyan, V.; Dalessio, J.; Debski, B.; Dimitrov, D.; Drozdz, M.; Er, Hüseyin; Erdem, A.; Escartin Perez, A.; Ramazani, V.; Filippenko, A.; Ganesh, S.; Garcia, F.; Gomez Pinilla, F.; Gopinathan, M.; Haislip, J.; Hudec, R.; Hurst, G.; Ivarsen, K.; Jelinek, M.; Joshi, A.; Kagitani, M.; Kaur, N.; Keel, W.; Lacluyze, A.; Lee, B.; Lindfors, E.; Lozano De Haro, J.; Moore, J.; Mugrauer, M.; Naves Nogues, R.; Neely, A.; Nelson, R.; Ogloza, W.; Okano, S.; Pandey, J.; Perri, M.; Pihajoki, P.; Poyner, G.; Provencal, J.; Pursimo, T.; Raj, A.; Reichart, D.; Reinthal, R.; Sadegi, S.; Sakanoi, T.; Salto Gonzalez, J.; Sameer, Sameer; Schweyer, T.; Siwak, M.; Soldan Alfaro, F.; Sonbas, E.; Steele, I.; Stocke, J.; Strobl, J.; Takalo, L.; Tomov, T.; Tremosa Espasa, L.; Valdes, J.; Valero Perez, J.; Verrecchia, F.; Webb, J.; Yoneda, M.; Zejmo, M.; Zheng, W.; Telting, J.; Saario, J.; Reynolds, T.; Kvammen, A.; Gafton, E.; Karjalainen, R.; Harmanen, J.; Blay, P.

doi:10.3847/2041-8205/819/2/l37

Primary black hole spin in oj 287 AS determined by the general relativity centenary flare

Valtonen M. J., Zola S., Ciprini S., Gopakumar A., Matsumoto K., Sadakane K., ...Daha Fazla

Astrophysical Journal Letters, cilt.819, 2016 (SCI-Expanded, Scopus)

Yayın Türü: Makale / Tam Makale
Cilt numarası: 819
Basım Tarihi: 2016
Doi Numarası: 10.3847/2041-8205/819/2/l37
Dergi Adı: Astrophysical Journal Letters
Derginin Tarandığı İndeksler: Science Citation Index Expanded (SCI-EXPANDED), Scopus
Anahtar Kelimeler: black hole physics, quasars: general, quasars: individual (OJ 287), quasars: supermassive black holes
Atatürk Üniversitesi Adresli: Hayır

Özet

OJ 287 is a quasi-periodic quasar with roughly 12 year optical cycles. It displays prominent outbursts that are predictable in a binary black hole model. The model predicted a major optical outburst in 2015 December. We found that the outburst did occur within the expected time range, peaking on 2015 December 5 at magnitude 12.9 in the optical R-band. Based on Swift/XRT satellite measurements and optical polarization data, we find that it included a major thermal component. Its timing provides an accurate estimate for the spin of the primary black hole, chi = 0.313 +/- 0.01. The present outburst also confirms the established general relativistic properties of the system such as the loss of orbital energy to gravitational radiation at the 2% accuracy level, and it opens up the possibility of testing the black hole no-hair theorem with 10% accuracy during the present decade.