FERMI-LAT-SCIENTIFIC PLOTS
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Light curve of PG 1553+113 during the 2012 observation campaign. Upper panel: nightly light curve in VHE γ-rays observed with the MAGIC telescopes for E>150 GeV. For comparison the flux during the low state of the source in 2007 and the high state in 2008 measured by MAGIC (Aleksi ́c et al. 2012a) are shown by the dotted and dashed lines, respectively. Middle panel: Fermi -LAT light curve computed with a 10-day binning for energies between 0.1 to 100 GeV; the dashed gray lines show a zero order polynomial fit and the mean flux of the source from 2FGL catalog (Nolan et al. 2012). Lower panel: flux in the X-ray band in one night bins observed by Swift-XRT from 2 to 10 keV is represented in gray squares. For comparison previous measurements from 2010 and 2011 with Swift-XRT are plotted as dashed lines. The vertical lines denote the flare intervals observed in the VHE band and X-rays. No hints of flare are observed in the HE band.
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Light curve of PG 1553+113 during the 2012 observation campaign. Upper panel: nightly light curve in VHE γ-rays observed with the MAGIC telescopes for E>150 GeV. For comparison the flux during the low state of the source in 2007 and the high state in 2008 measured by MAGIC (Aleksi ́c et al. 2012a) are shown by the dotted and dashed lines, respectively. Middle panel: Fermi -LAT light curve computed with a 10-day binning for energies between 0.1 to 100 GeV; the dashed gray lines show a zero order polynomial fit and the mean flux of the source from 2FGL catalog (Nolan et al. 2012). Lower panel: flux in the X-ray band in one night bins observed by Swift-XRT from 2 to 10 keV is represented in gray squares. For comparison previous measurements from 2010 and 2011 with Swift-XRT are plotted as dashed lines. The vertical lines denote the flare intervals observed in the VHE band and X-rays. No hints of flare are observed in the HE band.