186          93       $\phantom{<}2.0$E-10     4.2E-11     +7.0E-11   -7.0E-11
       310          155      $\phantom{<}7.0$E-11     1.4E-11     +3.8E-11   -2.4E-11
       516          259      $\phantom{<}1.8$E-11     3.2E-12     +6.4E-12   -6.4E-12
       861          431      $\phantom{<}2.4$E-12     8.6E-13     +8.4E-13   -8.4E-13
      1437          720      $\phantom{<}2.7$E-13     2.2E-13     +9.4E-14   -7.1E-13
      2397         1201      $\phantom{<}1.2$E-13     6.8E-14     +4.1E-14   -1.6E-13
      3999         2003      $\phantom{<}3.5$E-14     3.2E-14     +1.2E-14   -1.3E-13
      6670         3341           $<8.4$E-15                                
  ------------- ----------- ---------------------- ------------- ---------- ----------

  : Differential flux of 1ES2344+514 along with statistical and systematical errors.[]{data-label="tab:spd"}

![Differential photon spectrum for 1ES2344+514 as measured with MAGIC (solid curve). The gray band represents systematic errors coming from varying the $\gamma$ efficiency in the determination of the spectrum. The Crab nebula spectrum as measured with MAGIC is also shown (gray dotted curve; small gray numbers indicate the fraction of Crab nebula flux for the 1ES2344+514 flux points) and the Whipple flare spectrum (dashed curve) as reported by @Schroedter.[]{data-label="fig:spectrum"}](f4.eps){width="\linewidth"}

![image](f5.eps){width="\linewidth"}

Discussion
==========

We observed a highly significant VHE $\gamma$-ray emission from the blazar 1ES2344+514. The flux exhibited no significant variations on a timescale of days, with one night showing a higher flux level (by a factor of 2) as compared to the surrounding nights; such a variation is statistically expected to occur with a 34.4% probability in 21 observation nights. The observed flux was lower by a factor 