A Search for QPOs in the Blazar OJ287: Preliminary Results from the 2015/2016 Observing Campaign
Journal
Date Issued
2016
Author(s)
Zola, S.
•
Valtonen, M.
•
Bhatta, G.
•
Goyal, A.
•
Debski, B.
•
Baran, A.
•
Krzesinski, J.
•
Siwak, M.
•
Ciprini, S.
•
Gopakumar, A.
•
Jermak, H.
•
Nilsson, K.
•
Reichart, D.
•
Matsumoto, K.
•
Sadakane, K.
•
Gazeas, K.
•
Kidger, M.
•
Piirola, V.
•
Alicavus, F.
•
Baliyan, K.
•
Berdyugin, A.
•
Boyd, D.
•
Campas Torrent, M.
•
Campos, F.
•
Carrillo Gómez, J.
•
Caton, D.
•
Chavushyan, V.
•
Dalessio, J.
•
Dimitrov, D.
•
Drozdz, M.
•
Er, H.
•
Erdem, A.
•
Escartin Pérez, A.
•
Fallah Ramazani, V.
•
Filippenko, A.
•
Garcia, F.
•
Gómez Pinilla, F.
•
Gopinathan, M.
•
Haislip, J.
•
Harmanen, 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.
•
•
Pihajoki, P.
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Poyner, G.
•
Provencal, J.
•
Pursimo, T.
•
Raj, A.
•
Reinthal, R.
•
Sadegi, S.
•
Sakanoi, T.
•
Sameer
•
Salto González, J. -L.
•
Schweyer, T.
•
Soldán Alfaro, F.
•
Karaman, N.
•
Sonbas, E.
•
Steele, I.
•
Stocke, J.
•
Strobl, J.
•
Takalo, L.
•
Tomov, T.
•
Tremosa Espasa, L.
•
Valdes, J.
•
Valero Pérez, J.
•
•
Webb, J.
•
Yoneda, M.
•
Zejmo, M.
•
Zheng, W.
•
Telting, J.
•
Saario, J.
•
Reynolds, T.
•
Kvammen, A.
•
Gafton, E.
•
Karjalainen, R.
•
Blay, P.
Abstract
We analyse the light curve in the R band of the blazar OJ287, gathered during the 2015/2016 observing season. We did a search for quasi-periodic oscillations (QPOs) using several methods over a wide range of timescales. No statistically significant periods were found in the high-frequency domain both in the ground-based data and in Kepler observations. In the longer-period domain, the Lomb–Scargle periodogram revealed several peaks above the 99% significance level. The longest one—about 95 days—corresponds to the innermost stable circular orbit (ISCO) period of the more massive black hole. The 43-day period could be an alias, or it can be attributed to accretion in the form of a two-armed spiral wave.
Volume
4
Issue
4
Start page
41
Issn Identifier
2075-4434
Ads BibCode
2016Galax...4...41Z
Rights
open.access
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