The Spectral Energy Distributions of the Fermi Blazars and Connection Among Low-Energy Peaked Bl Lacertae, High-Energy Peaked Bl Lacertae, and Flat Spectrum Radio Quasars

Li, H. Z.; Xie, Gaogang; Yi, Ting-Feng; Chen, L. E.; Hong, Dunpin

doi:10.1088/0004-637x/709/2/1407

Cited by 14 publications

(25 citation statements)

References 29 publications

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“…Chen et al, 2013;Fan et al, 2012;Li et al, 2010;Lyu et al, 2014;Xie et al, 2003). This suggests that FSRQs and LBLs have a similar property, but HBLs have a distinct property.…”

Section: Discussionmentioning

confidence: 97%

“…Moreover, some authors found that HBLs do not follow the blazars sequence (e.g. Chen et al, 2013;Fan et al, 2012;Giommi et al, 2005;Li et al, 2010;Padovani et al, 2003;Padovani, 2007) .…”

Section: Discussionmentioning

confidence: 99%

“…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 relationship between of BL Lacs objects and FSRQs has been discussed by a number of authors (e.g., Comastri et al, 1997;Fossati et al, 1998;Ghisellini et al, 1998Ghisellini et al, , 2009Li et al, 2010;Sambruna et al, 1996;Xie et al, 2001Xie et al, , 2003Xie et al, , 2004Xie et al, , 2006Xie et al, , 2007Xie et al, , 2008Zheng et al, 2007), who assembled the SED of many radio, X-ray, and γ-ray selected blazars. Fossati et al (1998) studied the SEDs of a combined blazar sample, and found that the SEDs properties of these subclasses present a remarkable continuity and a systematic trend as a function of source luminosity, which suggests that the parameter describing the blazar continua is likely to be the source luminosity.…”

Section: Introductionmentioning

confidence: 99%

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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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“…Chen et al, 2013;Fan et al, 2012;Li et al, 2010;Lyu et al, 2014;Xie et al, 2003). This suggests that FSRQs and LBLs have a similar property, but HBLs have a distinct property.…”

Section: Discussionmentioning

confidence: 97%

“…Moreover, some authors found that HBLs do not follow the blazars sequence (e.g. Chen et al, 2013;Fan et al, 2012;Giommi et al, 2005;Li et al, 2010;Padovani et al, 2003;Padovani, 2007) .…”

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

The broadband spectral energy distributions of SDSS blazars

Chen

Jiang

et al. 2015

Res. Astron. Astrophys.

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“…The present study allows us to check, for the first time, whether the difference persists even when the two blazar subclasses are subjected to the condition of TeV detection. From Table 1, our sample consists of seven HBLs [with the lower hump of the spectral energy distribution (SED) peaking above 10 15 Hz] and 15 other blazars which can be together termed LBLs (see Abdo et al 2010b; Li et al 2010) including J1218−0119 which is a flat‐spectrum core‐dominated quasar. The estimated INOV DCs are 38 per cent for HBLs (26 nights’ data) and 63 per cent for LBLs (90 nights’ data) (Table 3).…”

Section: Discussionmentioning

confidence: 99%

Rapid optical variability of TeV blazars

Gopal-Krishna

Goyal

Joshi

et al. 2011

Monthly Notices of the Royal Astronomical Society

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In this first systematic attempt to characterise the intranight optical variability (INOV) of TeV detected blazars, we have monitored a well defined set of 9 TeV blazars on total 26 nights during 2004-2010. In this R (or V)-band monitoring programme only one blazar was monitored per night for a minimum duration of 4 hours. Using the CCD, an INOV detection threshold of ~ 1-2 % was achieved in the densely sampled DLCs. We have further expanded the sample by including another 13 TeV blazars from literature. This enlarged sample of 22 TeV blazars, monitored on a total of 116 nights (including 55 nights newly reported here), has enabled us to arrive at the first estimate of the INOV duty cycle of TeV detected blazars. Applying the C-test, the INOV DC is found to be 59 %, which decreases to 47 % if only INOV fractional amplitudes above 3 % are considered. These observations also permit, for the first time, a comparison of the INOV characteristics of the two major subclasses of TeV detected BL Lacs, namely LBLs and HBLs, for which we find the INOV DCs to be ~ 63 % and ~ 38 %, respectively. This demonstrates that the INOV differential between LBLs and HBLs persists even when only their TeV detected subsets are considered. Despite dense sampling, the intranight light curves of the 22 TeV blazars have not revealed even a single feature on time scale substantially shorter than 1 hour, even though the inner jets of TeV blazars are believed to have exceptionally large bulk Lorentz factors (and correspondingly stronger time compression). An intriguing feature, clearly detected in the light curve of the HBL J1555+1111, is a 4 per cent `dip' on a 1 hour timescale. This unique feature could have arisen from absorption in a dusty gas cloud, occulting a superluminally moving optical knot in the parsec scale jet of this relatively luminous BL Lacs object.Comment: 39 pages, 3 figures, accepted for publication in MNRA

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The evolutionary sequence of Fermi blazars

Cha

Zhang

et al. 2013

Astrophys Space Sci

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The Spectral Energy Distributions of the Fermi Blazars and Connection Among Low-Energy Peaked Bl Lacertae, High-Energy Peaked Bl Lacertae, and Flat Spectrum Radio Quasars

Cited by 14 publications

References 29 publications

The broadband spectral energy distributions of SDSS blazars

The broadband spectral energy distributions of SDSS blazars

Rapid optical variability of TeV blazars

The evolutionary sequence of Fermi blazars

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