tokens: in Table 1 . In each case, the log-likelihood ratio with respect to a power-law hypothesis, TS, is also given. The maximum energy displayed for each spectrum (see also panel (b) in Figure 1 and Table 3 ) corresponds to the highest energy of photons attributed to CTA 102 at more than 95% confidence level (CL), as evaluated using gtsrcprob . Figure 2. Spectra for dates, where near-simultaneous data by all three observatories are available. The MJDs are indicated. The gray spectrum is the MJD 57670 spectrum for comparison. Table 1 Fermi -LAT Detailed Results of CTA 102 Used for Each Spectrum Shown in Figure 2 Note. The columns give the center of the daily binned time interval in which the spectrum is extracted in MJD, the integrated flux density, the photon index, the curvature index, and the Log-likelihood ratio between the two spectral hypothesis (Log parabola with respect to power law). 2.2. X-Ray Analysis The Neil Gehrels Swift Gamma-Ray Burst Mission (hereafter Swift , Gehrels et al. 2004 ) is a multiwavelength space instrument, which monitors sources in the optical, ultraviolet, and X-ray energy bands. X-ray observations of CTA 102 were possible thanks to the X-ray Telescope (XRT, Burrows et al. 2005 ) onboard. It monitored CTA 102 since 2005 in 144 pointing observations taken in the energy range of 0.3–10 keV. For the goal of this paper, data collected between MJD 57668 and MJD 57821, which correspond to the ObsIDs of 00033509084-00033509120 have been analyzed and are presented in the light curve (Figure 1 (c)). X-ray data analysis was performed using version 6.20 of the HEASOFT package. 7 7 http://heasarc.gsfc.nasa.gov/docs/software/lheasoft The data were recalibrated using the standard procedure xrtpipeline . Spectral fitting was carried out using XSPEC v.12.8.2 (Arnaud 1996 ). Data were binned in order to have at least 30 counts per bin and were fitted using a power-law model, Equation ( 1 ), with the Galactic absorption value of cm −2 (Kalberla et al. 2005 ) set as a frozen parameter. Furthermore, it was tested whether the spectrum can be better descibed with a broken power-law model. According to reduced values, a simple power law is preferred for all X-ray spectra of CTA 102. The observations presented in the SEDs (Figure 2 ) are summarized in Table 2 . While there is some variability in the spectral index, this is mostly minor and most of the X-ray variability comes from a change in the normalization. Table 2 Swift -XRT Observations of CTA 102 Used for the Spectra Shown in Figure 2 Note. The columns give the MJD, the observation ID, the duration of the observation, as well as the spectral parameters, i.e., normalization and Index . The normalization energy is keV. 2.3. Optical/UV Analysis In the optical and ultraviolet regime, CTA 102 was monitored with the UVOT instrument on board Swift . The monitoring was performed in the bands UVW 2 (188 nm), UVM 2 (217 nm), UVW 1 (251 nm), U (345 nm), B (439 nm), and V (544 nm), with the
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