of $\approx6$ than the one observed by the Whipple collaboration during a flare on 1995 December 20. The spectrum is softer than the Crab Nebula spectrum and also softer than the flare spectrum observed by the Whipple collaboration.

Long-term VHE Light Curve
-------------------------

In Fig. \[fig:lccom\] we show a light curve including all reported VHE $\gamma$-ray measurements and upper limits for 1ES2344+514. These data have been normalized to an integral Crab flux $F(E>350\,\mathrm{GeV})$; the fluxes given in the literature were extrapolated, if necessary, using the spectral index found in this paper (in the following, “Crab units” refer to this energy threshold). Except for the 1995 December 20 flare and the MAGIC data, all these measurements are on the sensitivity level of the respective instruments. Therefore, none of the latter data points exceeds a significance of $4.3\sigma$. All reported observations with significances below $2.0\sigma$ ($\approx$95% probability) were converted to $99\%$ upper flux limits.

In 1995/1996, Whipple discovered 1ES2344+514 at a flux level of $(0.11\pm0.05)$ Crab units at $E>350$ GeV, except for the 1995 December flare, when $(0.63\pm0.15)$ Crab units were obtained [@Catanese]. Follow-up observations by Whipple and HEGRA in 1996-1998 yielded upper limits of $0.08$ and $0.12$ Crab units, respectively. In 