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Table 2

List of parameters corresponding to the BL Lac objects in our sample obtained with the approach of Sbarufatti et al. (2006, 2009; see text).

Object R E(B − V)Gal α E W min Redshift Log(νpeak)
mag. (mag.) (Å) (Hz)

1FGL J0051.4−6242 17.3 0.016 −1.0 ± 0.1 0.3 >0.30 15.06
1FGL J0054.9−2455* 17.1 0.016 −1.3 ± 0.3 1.2 >0.12 15.10
1FGL J0131.2+6121 18.2 0.922 −1.5 ± 0.4 1.3 >0.08 15.85
1FGL J0137.8+5814 17.5 0.528 −0.7 ± 0.2 0.7 >0.12 14.98
1FGL J0223.0−1118 17.4 0.021 −1.3 ± 0.4 1.6 >0.20 14.84
1FGL J0506.9−5435 16.1 0.030 −1.2 ± 0.2 0.7 >0.40 15.61
1FGL J0604.2−4817 17.4 0.050 −0.9 ± 0.2 1.0 >0.37 15.20
1FGL J0648.8+1516 16.2 0.144 −1.0 ± 0.2 0.9 >0.13 15.52
1FGL J0841.4−3558 17.2 0.495 −0.9 ± 0.3 1.8 >0.15 15.01
1FGL J0848.6+0504 18.3 0.067 −1.2 ± 0.4 1.9 >0.57 16.14
1FGL J1304.3−4352* 15.4 0.133 −1.0 ± 0.2 0.5 >0.19 15.02
1FGL J1307.6−4259 15.1 0.106 −1.3 ± 0.2 0.4 >0.10 15.10
1FGL J1353.6−6640 17.1 0.553 −0.9 ± 0.3 0.3 >0.15 15.11
1FGL J1419.7+7731 17.6 0.035 −1.6 ± 0.3 1.1 >0.27 15.39
1FGL J1553.5−3116* 15.5 0.174 −1.1 ± 0.2 0.3 >0.28 14.42
1FGL J1643.5−0646* 16.7 0.491 +0.1 ± 0.4 2.6 >0.12 14.88
1FGL J1823.5−3454 15.2a 0.129 −1.1 ± 0.2 0.4 >0.17 15.50
1FGL J1841.9+3220 17.0 0.088 −1.0 ± 0.2 0.8 >0.20 15.38
1FGL J1926.8+6153* 16.6 0.058 −0.9 ± 0.2 0.4 >0.16 15.29
1FGL J1933.3+0723 15.3 0.295 −1.2 ± 0.2 0.4 >0.20 14.64
1FGL J1942.7+1033 17.0 0.390 −0.1 ± 0.2 0.2 >0.20 14.75
1FGL J2042.2+2427* 14.0 0.140 ** 1.9 ** 15.32
1FGL J2146.6−1345* 17.5 0.042 −1.1 ± 0.2 0.5 >0.28 14.92
1FGL J2323.0−4919 17.1 0.012 −1.1 ± 0.2 0.4 >0.27 15.04
1FGL J2329.2+3755* 17.0 0.182 −1.3 ± 0.2 0.6 >0.20 15.15

Notes. R-band magnitudes were obtained from the USNO-A2.0 catalog, while the values of E(B − V)Gal are from Schlegel et al. (1998).

(a)

Obtained from the photometry on the acquisition image of the spectrum presented in this work (see text).

(*)

Present in the BL Lac spectroscopic sample of Shaw et al. (2013).

(**)

The optical emission of the source is dominated by the host galaxy; thus, in this case it was not possible to fit the spectrum with a power law according to the method of Sbarufatti et al. (2006).

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