Table 2.
Spectral parameters obtained for the best fit of Fermi-LAT data for each source from the energy range between 100 MeV and 500 GeV using four different spectral models: PL, BPL, LP and PLSEC.
| Source | Model | Energy | Spectral parameters | Integral flux | TS | Ratio- | Fvar |
|---|---|---|---|---|---|---|---|
| [GeV] | 10−8[cm−2 s−1] | test | [%] | ||||
| PKS 0447−439 | Broken power law | 0.1 … 500 | Γ1 = 1.839 ± 0.009 | (7.62 ± 0.13) | 29305.1 | 7.3σ | (47.91 ± 1.16) |
| Γ2 = 2.825 ± 0.171 | |||||||
| Eb = 42.84 ± 1.78 | |||||||
| PG 1553+113 | Log parabola | 0.1 … 500 | Γα = 1.587 ± 0.013 | (5.59 ± 0.15) | 34701.6 | 11.01σ | (22.87 ± 1.14) |
| Γβ = 0.045 ± 0.005 | |||||||
| Eb = 1.49 ± 0.95 | |||||||
| PKS 2155−304 | PLSuperExpCutOff | 0.1 … 500 | Γ1 = 1.749 ± 0.154 | (12.82 ± 0.22) | 59800.5 | 9.63σ | (36.62 ± 1.07) |
| Γ2 = 0.620 ± 0.154 | |||||||
| Ec = 110.57 ± 37.9 | |||||||
| PKS 0426−380 | Log parabola | 0.1 … 500 | Γα = 1.742 ± 0.025 | (24.05 ± 0.31) | 92892.5 | 21.19σ | (62.39 ± 0.01) |
| Γβ = 0.020 ± 0.004 | |||||||
| Eb = 0.76 ± 0.03 | |||||||
| PKS 0301−243 | Log parabola | 0.1 … 500 | Γα = 1.622 ± 0.043 | (3.23 ± 0.11) | 9639.4 | 5.94σ | (82.28 ± 1.90) |
| Γβ = 0.039 ± 0.006 | |||||||
| Eb = 0.11 ± 0.02 | |||||||
| PKS 0537−441 | PLSuperExpCutOff | 0.1 … 500 | Γ1 = 1.662 ± 0.026 | (19.38 ± 0.20) | 63570.9 | 16.78σ | (85.13 ± 0.08) |
| Γ2 = 0.267 ± 0.009 | |||||||
| Ec = 0.24 ± 0.06 | |||||||
Notes. The second-to-last column gives the significance, obtained by comparing the likelihood values for each models against those for the PL model using Log likelihood ratio test. The last column summarizes the fractional variability amplitude Fvar calculated form monthly light curves (Vaughan et al. 2003; Edelson et al. 2002). Error bars correspond to 1σ error; only statistical errors are shown.
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