All Tables

Table 1: Number of data pairs, after applying stability criteria to the PMT anode currents and to the trigger rates. Single Pointing (SP), Doubling Pointing (DP), and Single Pointing with Veto (SPV) are explained in the text. The fraction of the data set with a cosmic ray trigger rate below 15 Hz, which we ascribe to seasonal increases in atmospheric extinction, is also listed.
Table 2: Number of events before and after cuts, for the Mrk 421 data sets. $N_\sigma$ is calculated after correcting for the $\sim$ $80\%$ data acquisition efficiency.
Table 3: Multiwavelength fluxes from Mrk 421 coincident with CELESTE data. The epoch numbers (1) through (5) are referred to in the text and figures. (a) ASM counts per second (see ASM in references). RXTE PCA 2-10 keV fluxes are in (b) $10^{-10}~{\rm erg~cm^{-2}~s^{-1}}$ , 3-20 keV (Krawczynski et al. 2001), and in (c) counts per second (B $\l$ azejowski et al. 2005). (d) CAT fluxes are in $10^{-12}~{\rm photons~cm^{-2}~s^{-1}},~E>250~{\rm GeV}$ (Piron et al. 2001a,b). (e) HEGRA fluxes are in $10^{-12}~{\rm photons~cm^{-2}~s^{-1}},~E>1000~{\rm GeV}$ (Krawczynski et al. 2001 for the 2000 data, Aharonian et al. 2003 for 2001). (f) VERITAS fluxes above 300 GeV are in gamma/min, where the Crab gave 2.40 (2.93) gamma/min for 02/03 (03/04) (Holder et al. 2001; B $\l$ azejowski et al. 2005). (g) CELESTE fluxes are in $10^{-9}~{\rm photons~cm^{-2}~s^{-1}},~E>100~{\rm GeV}$ .
Table 4: Number of events before and after cuts for the Mrk 501 data sets. $N_\sigma$ is calculated after correcting for the $\sim$ $80\%$ data acquisition efficiency.
Table 5: Number of events before and after cuts for the 1ES 1426+428 data sets. $N_\sigma$ is calculated after correcting for the $\sim$ 80% data acquisition efficiency.