between zenith angles of 24$^\circ$ and 34$^\circ$ with energies between 10 GeV and 30 TeV. Every event was assigned a parameter called hadronness ($h$), which is a measure for the probability that it is a hadronic (background) event. The final separation was achieved by a cut in $h$. The same cut procedure was applied to the final 1ES2344+514 sample. The arrival directions of the showers in equatorial coordinates were calculated using the DISP method [@Fomin; @Lessard2001; @MAGIC_disp]. The energy of the primary $\gamma$-ray was reconstructed from the image parameters again using the random forest method and taking into account the full instrumental energy resolution.

![Sky map for 1ES2344+514 produced with a DISP analysis: The figure shows the (background-subtracted, see e.g. Rowell 2003) excess events above 300 photoelectrons, corresponding to a $\gamma$-ray energy of $\approx 180$ GeV. The sky map has been smoothed using a two dimensional Gaussian with $\sigma=0.1^\circ$, roughly corresponding to the $\gamma$ PSF of the MAGIC telescope for point sources (indicated by the white circle). The colors encode the number of excess events in units of $10^{-5} \mathrm{sr}^{-1}$. The black cross marks the expected source position.[]{data-label="fig:skymap"}](f1.eps){width="0.75\linewidth"}

![$\theta^2$ plot for the 1ES2344+514 observations. On-source events are given as black 