Optical Spectral Variability of the Very-High-Energy Gamma-Ray Blazar 1ES 1011+496

Details Optical Spectral Variability of the Very-High-Energy Gamma-Ray Blazar 1ES 1011+496 Optical Spectral Variability of the Very-High-Energy Gamma-Ray Blazar 1ES 1011+496

2010-10-27

arxiv.org/abs/1010.5676v1

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

Accepted for publication in ApJ. 16 pages, including 7 figures

Scientific paper

We present results of five years of optical (UBVRI) observations of the very-high-energy gamma-ray blazar 1ES 1011+496 at the MDM Observatory. We calibrated UBVRI magnitudes of five comparison stars in the field of the object. Most of our observations were done during moderately faint states of 1ES 1011+496 with R > 15.0. The light curves exhibit moderate, closely correlated variability in all optical wavebands on time scales of a few days. A cross-correlation analysis between optical bands does not show significant evidence for time lags. We find a positive correlation (Pearson's r = 0.57; probability of non-correlation P(>r) ~ 4e-8) between the R-band magnitude and the B - R color index, indicating a bluer-when-brighter trend. Snap-shot optical spectral energy distributions (SEDs) exhibit a peak within the optical regime, typically between the V and B bands. We find a strong (r = 0.78; probability of non-correlation P (>r) ~ 1e-15) positive correlation between the peak flux and the peak frequency, best fit by a relation $\nu F_{\nu}^{\rm pk} \propto \nu_{\rm pk}^k$ with k = 2.05 +/- 0.17. Such a correlation is consistent with the optical (synchrotron) variability of 1ES 1011+496 being primarily driven by changes in the magnetic field.

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