Table 1: TeV blazar data.
Source       z          $\alpha_\gamma$         $F_\gamma$ CT     $\alpha_\gamma^{\rm corr}$        $F_\gamma^{\rm corr}$ $F_{5~{\rm GHz}}$       $F_{\rm x}$   Fx,0 Notes
(1)      (2)         (3)         (4) (5)     (6)         (7)   (8)       (9)   (10)  (11)
Mrk 421    0.031 $2.33 \pm 0.08$ 1.03($\pm$0.03)E-10 M    2.15    7.59E-11 0.730    4.0E-10 4.1E-11 Al+07a
Mrk 501    0.034 $2.28 \pm 0.05$ 1.71($\pm$0.11)E-11 M    2.08    1.32E-11 1.400    4.0E-10 3.0E-11 Al+07b
    $2.45 \pm 0.07$ 3.84($\pm$1.00)E-12 M    2.25    4.73E-12      1.7E-10    
PKS 2344+514    0.044 $2.95 \pm 0.12$ 1.21($\pm$0.10)E-11 M    2.67    1.67E-11 0.231 <7.0E-11 1.7E-11 Al+07c
Mrk 180    0.045 $3.30 \pm 0.70$ 8.46($\pm$3.38)E-12 M    3.01    1.23E-11 0.274 <1.0E-10 5.0E-12 Al+06a
1ES 1959+650    0.047 $2.72 \pm 0.14$ 3.04($\pm$0.35)E-11 M    2.41    4.63E-11 0.253    1.4E-10 1.4E-11 Al+06b
BL Lacertae    0.069 $3.60 \pm 0.50$ 3.28($\pm$0.26)E-12 M    3.12    7.15E-12 2.490        -- 5.8E-13 Al+07d
PKS 2005-489    0.071 $4.00 \pm 0.40$ 3.32($\pm$0.48)E-12 H    3.50    7.47E-12 1.190    4.0E-11 0.9E-11 Ah+05a
                    P+99
RGB J0152+017    0.080 $2.95 \pm 0.36$ 4.43($\pm$1.24)E-12 H    2.38    1.15E-11 0.050    2.7E-12 9.1E-13 Ah+08
                    D+01
PKS 2155-304    0.116 $3.37 \pm 0.07$ 2.89($\pm$0.18)E-11 H    2.51    1.36E-10 0.310    2.7E-11 2.0E-11 Ah+05b
1ES 1426+428    0.129 $3.55 \pm 0.46$ 2.53($\pm$0.43)E-11 W    2.54    1.47E-10 0.038    2.0E-11 1.6E-11 Hor+02
                    S+97
1ES 0229+200    0.139 $2.50 \pm 0.19$ 4.46($\pm$0.71)E-12 H    1.46    3.04E-11 0.046    1.5E-11 8.8E-12 Ah+07c
                    P+96
                    D+05
H 2356-309    0.165 $3.09 \pm 0.24$ 2.55($\pm$0.68)E-12 H    1.84    2.66E-11 0.065    1.0E-11 2.4E-11 Ah+06a
                    W+84
1ES 1218+304    0.182 $3.00 \pm 0.40$ 1.01($\pm$0.26)E-11 M    1.61    1.39E-10 0.056        -- 1.5E-11 Al+06c
1ES 1101-232    0.186 $2.94 \pm 0.20$ 4.35($\pm$0.69)E-12 H    1.46    6.08E-11 0.066    5.1E-11 2.5E-11 Ah+07a
1ES 0347-121    0.188 $3.10 \pm 0.23$ 3.86($\pm$0.73)E-12 H    1.67    5.77E-11 0.008    2.8E-11 6.0E-12 Ah+07b
1ES 1011+496    0.212 $4.00 \pm 0.50$ 6.40($\pm$0.32)E-12 M    2.37    1.43E-09 0.636        --     -- Al+07e
PG 1553+113 >0.25 $4.20 \pm 0.30$ 5.24($\pm$0.87)E-12 M <2.28 >2.18E-10 0.286    5.0E-11 1.4E-11 Al+07f
Column 1: source name.
Column 2: source redshift.
Column 3: observed 0.2-2 TeV photon spectral index, and associated statistical uncertainty. The corresponding systematic uncertainties are typically $\sim $0.1 for HESS and $\sim $0.2 for MAGIC.
Column 4: observed >0.2 TeV flux (in erg cm-2 s-1), and associated statistical uncertainty (from observed spectral normalization only).
Column 5: Cherenkov telescope (CT) or array with which the data in Col. 3 have been collected: symbols stand for H = HESS, M = MAGIC, W = Whipple.
Column 6: corrected 0.2-2 TeV photon spectral index.
Column 7: corrected >0.2 TeV flux.
Column 8: 5 GHz flux density (in Jy): data are from the NED, except for 1ES 0347-121 (Fossati et al. 1998) and H 2356-309 (Costamante & Ghisellini 2002).
Column 9: 2-10 keV flux (in erg cm-2 s-1): the data come from the papers listed in Col. 11 or from references quoted therein; when necessary, fluxes have been converted from RXTE/ASM count rates using the conversion 1 ct/s = 3.33E-10 erg cm-2 s-1.
Column 10: minimum 2-10 keV flux (in erg cm-2 s-1).
Column 11: Reference for VHE ${\gamma}$-ray data, and for the baseline X-ray flux when the latter was not taken from the NED - Al+07a: Albert et al. (2007a); Al+07b: Albert et al. (2007b); Al+07c: Albert et al. (2007c); Al+06a: Albert et al. (2006a); Al+06b: Albert et al. (2006b); Al+07d: Albert et al. (2007d); Ah+05a: Aharonian et al. (2005a); P+99: Perlman et al. (1999); Ah+08: Aharonian et al. (2008); D+01: Donato et al. (2001); Ah+05b: Aharonian et al. (2005b); Hor+02: Horan et al. (2002); S+97: Sambruna et al. (1997); Ah+07c: Aharonian et al. (2007c); P+96: Perlman et al. (1996); D+05: Donato et al. (2005); Ah+06a: Aharonian et al. (2006a); W+84: Wood et al. (1984); Al+06c: Albert et al. (2006c); Ah+07a: Aharonian et al. (2007a); Ah+07b: Aharonian et al. (2007b); Al+07e: Albert et al. (2007e); Al+07f: Albert et al. (2007f).

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