The optical-gamma correlation in BL Lacertae
1 INAF, Osservatorio Astrofisico di Torino
2 Dip. di Fisica, Università degli Studi di Perugia, Perugia
3 INAF, Istituto di Radioastronomia, Bologna
4 Astron. Inst., St.-Petersburg State Univ., Russia
5 Pulkovo Observatory, St.-Petersburg, Russia
6 Isaac Newton Institute of Chile, St.-Petersburg Branch
7 Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA
8 Maidanak Observatory of the Ulugh Beg Astronomical Institute, Uzbekistan
9 Steward Observatory, University of Arizona, Tucson, AZ, USA
10 Instituto de Astrofisica de Canarias (IAC), La Laguna, Tenerife, Spain
11 Departamento de Astrofisica, Universidad de La Laguna, La Laguna, Tenerife, Spain
Published online: 9 December 2013
We present multifrequency light curves of BL Lacertae from February 2008 to October 2012. Lowenergy data (optical and millimetre) were acquired in the framework of a GASP-WEBT project. High-energy data (ultraviolet, X-ray, and γ-ray) come from observations of the Swift, RXTE, and Fermi satellites. After a period of moderate activity, in May 2011 the source suddenly started to flare at γ and optical-UV frequencies. Activity at millimetre wavelengths and X rays began 3-4 months later. This behaviour offered a good opportunity to study the correlation among flux variability in different bands, in particular between the best-sampled optical and γ-ray light curves. However, even in this fortuitous case, we can only define a general correlation with likely no time lag, but with a lag uncertainty of ±1 day. Indeed, the data reveal a complex relationship between the γ and optical fluxes, which cannot be unveiled because of the small gaps in the sampling of this extremely variable source.
© Owned by the authors, published by EDP Sciences, 2013
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