THE SPECTRAL INDEX PROPERTIES OF<i>FERMI</i>BLAZARS

Jiang, Fan; Yang, Jiang-He; Yuan, Yu-Hai; Wang, J.; Gao, Ying

doi:10.1088/0004-637x/761/2/125

Cited by 40 publications

(48 citation statements)

References 59 publications

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“…The results are consistent with the reported results of Xie et al (2003), who found that HBLs and LBLs locate in different regions in the α ox − α xγ plane, but LBLs and FSRQs occupy the same region in α ox − α xγ plane. In addition, our results also agree with that reported by Fan et al (2012) and Lyu et al (2014).…”

Section: Diagram Of α Rx Versus α Rosupporting

confidence: 93%

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The broadband spectral energy distributions of SDSS blazars

Chen

Jiang

et al. 2015

Res. Astron. Astrophys.

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We compiled the radio, optical, and X-ray data of blazars from the Sloan Digital Sky Survey (SDSS) database, and presented the distribution of luminosities and broad band spectral indices. The distribution of luminosities shows that the averaged luminosity of flat-spectral radio quasars (FSRQs) is larger than that of BL Lacs objects. On the other hand, the broad band spectral energy distribution reveals that FSRQs and low energy peaked BL Lac objects (LBLs) objects have similar spectral properties, but high energy peaked BL Lac objects (HBLs) have a distinct spectral property. This may be due to that different subclasses of blazars have different intrinsic environments and are at different cooling levels. Even so, a unified scheme also is revealed from the color-color diagram, which hints that there are similar physical processes operating in all objects under a range of intrinsic physical conditions or beaming parameter.

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Section: Diagram Of α Rx Versus α Rosupporting

confidence: 93%

“…Some literatures show that HBLs have different properties from FSRQs, but LBLs are similar to FSRQs (e.g. Chen et al, 2013;Fan et al, 2012;Li et al, 2010;Lyu et al, 2014). However, Li et al (2010) and Chen et al (2013) also found that their whole sample suggest the unified scheme of blazars.…”

Section: Introductionmentioning

confidence: 97%

The broadband spectral energy distributions of SDSS blazars

Chen

Jiang

et al. 2015

Res. Astron. Astrophys.

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“…From our SED modeling results (Figure 1), it can be seen that the GeV data at low energies can be fitted well. And the average spectral index between the X-ray and the γ-ray of our calculated radiation spectrums α ′ Xγ = 1.12 is similar to the average observed value of the high peaked frequency BL Lacs αXγ = 1.02 (Fan et al 2012). Which implies the estimated value of γmin is reasonable.…”

Section: The Physical Properties Of Jetsupporting

confidence: 82%

“…However, the observed spectral index between the X-ray and the γ-ray and the GeV data at low energies could place constraints on γmin in some degree (Tavecchio et al 2000;Yan et al 2014). According to the average observed spectral index between the X-ray and the γ-ray of the high peaked frequency BL Lacs αXγ=1.02 (Fan et al 2012) and the GeV data at low energies, we do a preliminary modeling to the SED for each object. Based on the preliminary modeling result, the γmin = 10 are adopted in our fitting.…”

Section: Fitting Strategymentioning

confidence: 99%

The physical properties ofFermiTeV BL Lac objects’ jets

Ding¹,

Zhang²,

Xiong³

et al. 2016

Mon. Not. R. Astron. Soc.

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We investigate the physical properties of Fermi TeV BL Lac objects jets by modeling the quasi-simultaneous spectral energy distribution of 29 Fermi TeV BL Lacs in the frame of a one-zone leptonic synchrotron self-Compton model. Our main results are the following: (i) There is a negative correlation between B and δ in our sample, which suggests that B and δ are dependent on each other mainly in Thomson regime. (ii) There are negative correlations between ν sy and r, the ν IC and r, which is a signature of the energy-dependence statistical acceleration or the stochastic acceleration. There is a significant correlation between r and s, which suggests that the curvature of the electron energy distribution is attributed to the energydependence statistical acceleration mechanism. (iii) By assuming one proton per relativistic electron, we estimate the jet power and radiative power. A size relation P e ∼ P p > P r P B is found in our sample. The P e > P B suggests that the jets are particle dominated, and the P e ∼ P p means that the mean energy of relativistic electrons approaches m p /m e . There are not significant correlations between P jet and black hole mass in high or low state with a subsample of 18 sources, which suggests that the jet power weakly depends on the black hole mass. (iv) There is a correlation between the changes in the flux density at 1 TeV and the changes in the γ peak , which suggests the change/evolution of electron energy distribution may be mainly responsible for the flux variation.

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“…Due to a strong boosting effect, blazars normally produce fully nonthermal, strongly polarized radiation across the electro-magnetic spectrum from radio to γ-rays, are extremely luminous, and can exhibit a superluminal motion effect, among other features (e.g., Brindle et al 1986;Begelman & Sikora 1987;Ulrich et al 1997;Jorstad et al 2001;Fan et al 2012Fan et al , 2015Fan et al , 2016Fan et al , 2017. There are two most evident peaks in the multi-wavelength spectral energy distribution (SED) of blazars where, in the leptonic model, the lower energy peak is believed to be dominated by synchrotron radiation while the radiation at the higher energy peak could be due to the inverse Compton scattering (e.g., Böttcher 2007).…”

Section: Introductionmentioning

confidence: 99%

Constraints on the Location of γ-Ray Sample of Blazars with Radio Core-shift Measurements

Yan

et al. 2018

ApJ

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We model simultaneous or quasi-simultaneous multi-band spectral energy distributions (SEDs) for a sample of 25 blazars that have radio core-shift measurements, where a one-zone leptonic model and Markov chain Monte Carlo technique are adopted. In the SED fitting for 23 low-synchrotron-peaked (LSP) blazars, the seed photons from the broad-line (BLR) and molecular torus are considered respectively in the external Compton process. We find that the SED fitting with the seed photons from the torus are better than those utilizing BLR photons, which suggest that the γ-ray emitting region may be located outside the BLR. Assuming the magnetic field strength in the γ-ray emitting region as constrained from the SED fitting follows the magnetic field distribution as derived from the radio core-shift measurements (i.e.,1 , where R is the distance from the central engine and B 1 pc is the magnetic field strength at 1 pc), we further calculate the location of the γ-ray emitting region, g R , for these blazars. We find that~ǵ  R R R 2 10 10 4 S B L R (R S is the Schwarzschild radius and R BLR is the BLR size), where R BLR is estimated from the broad-line luminosities using the empirical correlations obtained using the reverberation mapping methods.

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THE SPECTRAL INDEX PROPERTIES OFFERMIBLAZARS

Cited by 40 publications

References 59 publications

The broadband spectral energy distributions of SDSS blazars

The broadband spectral energy distributions of SDSS blazars

The physical properties ofFermiTeV BL Lac objects’ jets

Constraints on the Location of γ-Ray Sample of Blazars with Radio Core-shift Measurements

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