integrated flux as a free parameter[^12] is used. $$\frac{dN}{dE}=\frac{N(\Gamma +1)E^{\Gamma}}{E^{\Gamma +1}_{\text{max}}-E^{\Gamma +1}_{\text{min}}}$$ where $\Gamma$ is the photon index, $E_{\text{min}}=100\,\text{MeV}$, $E_{\text{max}}=300\,\text{GeV}$, and N is the integral flux between $E_{\text{min}}$ and $E_{\text{max}}$.

We analysed the source in the period MJD 57225–57232, modelling its spectrum with a simple power-law. The likelihood fit obtained a Test Statistic of $TS= 111$. The resulting power law index of the fitted model is $\Gamma=1.81 \pm 0.14$. The spectral index of the investigated period is within the error bars of the one reported in 3FGL. In Figure \[vhe\_sed\], we show the flux values in six logarithmically spaced bins from 100MeV to 300GeV. Upper-limits are shown when the detection significances are lower than $3\,\sigma$.

X-rays {#xray3}
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The results of our X-ray analysis are shown in Figure \[fig\_lc\] with the details available in Table \[tab\_xray\]. The X-ray flux peaks three nights before the VHE gamma-ray peak. The X-ray spectrum is usually soft (Photon index, $\Gamma_X \geq 2.4$). The constant flux hypothesis is rejected with $>10\,\sigma$ level of confidence. However, only a hint of brighter-harder trend with $2\,\sigma$ level of confidence is present in our data sample. The trend between X-ray spectral index and flux ($F_{0.3-10\,\text{keV}}$) can be described by 