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2018RAA....18..120L - Research in Astron. and astroph., 18, 120-120 (2018/October-0)

Spectral energy distributions for TeV blazars.

LIN C. and FAN J.-H.

Abstract (from CDS):

In this work, we collected a sample of 69 TeV blazars from TeVCat, obtained their multi-wavelength observations, and fitted their spectral energy distributions by using a second degree polynomial function. The structure parameters of synchrotron bumps for 68 blazars and those of inverse-Compton bumps for 56 blazars were derived. Then, we conducted statistical analysis on the parameters (curvature, peak frequency, peak luminosity, bolometric luminosity and X/γ-ray spectral indexes). From our analysis and discussions, we can conclude the following: (1) There is a clear positive correlation between the synchrotron peak frequency, $logν_p^s$, and the inverse-Compton peak frequency, $logν_p^IC$, and between the synchrotron peak luminosity, $logν_p^sL^s{vp}$, and the inverse-Compton peak luminosity, $logν_p^IC L^ICp}$ . (2) The correlation between the peak frequency and the curvature of synchrotron bump is clearly different from that of the inverse-Compton bump, which further indicates that there are different emission mechanisms between them. (3) There is a correlation between $logν_p^IC$ and γ-ray spectral index, αγ, for the TeV blazars: $logν_p^IC = -(4.59 ±0.30)α_γ + (32.67 ±0.59)$, which is consistent with previous work. (4) An "L-shape" relation is found between $logν_p^s$ and $α_X$ for both TeV blazars and Fermi blazars. A significant correlation between $logν_p^s$ and X-ray photon index ($α_X$) is found for the TeV blazars with high synchrotron peak frequency: $logν_p^s = -(3.20 ±0.34)α_X + (24.33 ±0.79)$, while the correlation is positive for low synchrotron peaked TeV sources. (5) In the $α_X - α_γ$diagram, there is also an "L-shape." The anti-correlation is consistent with results available in the literature, and we also find a positive correlation between them. (6) Inverse-Compton dominant sources have luminous bolometric luminosities.