\mathrm{cm}^{-2} \mathrm{s}^{-1}$ ($\chi^2/$dof=4.9/7), was found. Note that the probability for finding such an excess in the 21 observation nights is around $34.4\%$. No significant variability within this observation night, encompassing 1.13 hours of effective observation time, can be claimed.

![VHE ($E>200
\mathrm{GeV}$) light curve (upper panel) and simultaneous optical ($R$-band) light curve for 1ES2344+514. The dashed line in the VHE light curve indicates the average flux level of $(2.38\pm0.30)\times10^{-11} \mathrm{cm}^{-2} \mathrm{s}^{-1}$ ($\chi^2_\mathrm{red}=21.2/20$). Note that the contribution of the host galaxy to the optical brightness is non-negligible and given as 3.7 mJy [@KariO].[]{data-label="fig:lc"}](f3.eps){width="\linewidth"}

The observation time can be split into three observation periods (Table \[tab:lc\]). Together with the VHE $\gamma$-ray light curve, an $R$-band optical light curve is shown. Simultaneous X-ray data are only available from the ASM instrument[^3] [@Levine] on board the [*Rossi X-ray Timing Explorer*]{}, the sensitivity of which, however, would be hardly sufficient to resolve the expected $2-10$ keV flux even during flaring states of 1ES2344+514, like those observed with [*BeppoSAX*]{} [@Giommi].

  ---------------- ----------- ------------------------------------------------- --------------
  Period           Obs. time                $F_{>200\mathrm{GeV}}$                $\chi^2/$ndf
  (MJD)                         ($10^{-11}\,\mathrm{cm}^{-2}\,\mathrm{s}^{-1}$)  
  $53585-53597 $   6.37 h                        $3.02\pm0.50$                      $6.1/6$
  $53610-53642 $   8.06 h                        $1.87\pm0.52$                      $0.4/3$
  $53700-53736 $   8.66 h                        $2.20\pm0.51$                      $12.0/9$
  Combined         23.09 h                       $2.38\pm0.30$                     $21.2/20$
  ---------------- ----------- 