Another look at the BL Lacertae flux and spectral variability - Observations by GASP-WEBT, XMM-Newton, and Swift in 2008–2009

C. M. Raiteri; M. Villata; L. Bruschini; A. Capetti; O. M. Kurtanidze; V. M. Larionov; P. Romano; S. Vercellone; I. Agudo; H. D. Aller; M. F. Aller; A. A. Arkharov; U. Bach; A. Berdyugin; D. A. Blinov; M. Böttcher; C. S. Buemi; P. Calcidese; D. Carosati; R. Casas; W.-P. Chen; J. Coloma; C. Diltz; A. Di Paola; M. Dolci; N. V. Efimova; E. Forné; J. L. Gómez; M. A. Gurwell; A. Hakola; T. Hovatta; H. Y. Hsiao; B. Jordan; S. G. Jorstad; E. Koptelova; S. O. Kurtanidze; A. Lähteenmäki; E. G. Larionova; P. Leto; E. Lindfors; R. Ligustri; A. P. Marscher; D. A. Morozova; M. G. Nikolashvili; K. Nilsson; J. A. Ros; P. Roustazadeh; A. C. Sadun; A. Sillanpää; J. Sainio; L. O. Takalo; M. Tornikoski; C. Trigilio; I. S. Troitsky; G. Umana

doi:10.1051/0004-6361/201015191

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Volume 524 (December 2010)

A&A, 524 (2010) A43

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Fig. 3

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Optical flux densities (R band, top panel), after correction for Galactic extinction and host galaxy contamination, compared to radio flux densities at different frequencies. Blue circles represent GASP data; red diamonds indicate data from the VLA/VLBA PCD. The vertical green line corresponds to the XMM-Newton pointing of May 16–17; the yellow strip highlights the period of Swift observations, from 2008 August 20 to October 2.

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