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ERRATUM: "MULTI-WAVELENGTH OBSERVATIONS OF THE FLARING GAMMA-RAY BLAZAR 3C 66A IN 2008 OCTOBER" (2011, ApJ, 726, 43)

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Published 2011 March 24 © 2011. The American Astronomical Society. All rights reserved.
, , Citation A. A. Abdo et al 2011 ApJ 731 77 DOI 10.1088/0004-637X/731/1/77

This is a correction for 2011 ApJ 726 43

0004-637X/731/1/77

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Due to an error at the publisher, Figure 8 was accidentally duplicated as Figure 7 in the published article. The correct Figure 7 is now provided and its caption is included for completeness. IOP publishing sincerely regrets this error.

Figure 7.

Figure 7. SSC models for redshifts z= 0.444, 0.3, 0.2, and 0.1 from top to bottom. The Fermi-LAT and VERITAS data points follow the same convention used in the paper to distinguish between flare (red) and dark run (blue) data points. In each panel, the EBL-absorbed model is shown as a solid red line and the de-absorbed model as a dashed red line. De-absorbed VERITAS flare points are shown as open squares. In all cases, the optical depth values from Franceschini et al. (2008) are used. The best agreement between the model and the data is achieved when the source is located at z = 0.2–0.3. For lower redshifts, the model spectrum is systematically too hard, while at z = 0.444, the model spectrum is too soft.

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10.1088/0004-637X/731/1/77