The variety of extreme blazars in the AstroSat view

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Table 4.

Source power-law indices of the SED in the optical/UV-to-X-ray part, α_ox, and the HE γ-ray part, α_γ, as well as the time ranges and collected data sets for the modelling.

Source	Spectrum	α_ox	α_γ	Time range	Main data
1ES 0120+340	S1	0.38 ± 0.06	0.65 ± 0.25	2015/01–2021/01	A1+A2, L1

RGB J0710+591	S1	0.40 ± 0.07	0.55 ± 0.14	2008/09–2009/08	UVOT09, XRT09, L1, VERITAS09
	S2	0.15 ± 0.10	0.33 ± 0.11	2013/01–2016/12	UVOT13, XRT13, NuSTAR13, L2
	S3	0.23 ± 0.09	0.24 ± 0.12	2017/01–2021/01	UVIT(A1), A1, L3

1ES 1101–232	S1	0.31 ± 0.04	0.31 ± 0.19	2015/01–2019/01	A1, L2

1ES 1741+196	S1	0.04 ± 0.05	0.16 ± 0.15	2010/01–2011/01	UVOT10, XRT10, L1, MAGIC10
	S2	0.26 ± 0.05	0.14 ± 0.08	2017/01–2021/01	A1+A2, L2
	S3	0.23 ± 0.07	0.14 ± 0.08	2017/01–2021/01	UVIT(A3), A3, L2

1ES 2322–409	S1	−0.21 ± 0.07	0.21 ± 0.05	2019/01–2021/01	A1, L1

Notes. The definitions of the AstroSat and Fermi-LAT spectra are provided in Tables 2 and 3, respectively, while the additional archival data sets can be found in Fig. 3. The SED index α is defined as νF_ν ∝ ν^α and related to the photon index Γ_p by α = 2 − Γ_p.

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