Hard X-ray properties of blazars

By D. Donato, G. Ghisellini, G. Tagliaferri, G. Fossati. 2001

219 citations recorded by the source corpus.

We have considered all blazars observed in the X{ray band and for which the slope of the X{ray spectrum is available. We have collected 421 spectra of 268 blazars, including 12 archival unpublished ASCA spectra of 7 blazars whose analysis is presented here. The X{ray spectra of blazars show trends as a function of their power, conrming that the blazar overall energy distribution can be parameterized on the basis of one parameter only, i.e. the bolometric luminosity. This is conrmed by the relatively new hard (2{10 keV) X{ray data. Our results conrm the idea that in low power objects the X{ray emission mechanism is the synchrotron process, dominating both the soft and the hard X{ray emissions. Low energy peaked BL Lac objects are intermediate, often showing harder spectra in the hard X{ray band, suggesting that the synchrotron process dominates in the soft band, with the inverse Compton process dominating at high energies. The most powerful objects have X{ray spectra that are flat both in the soft and in the hard band, consistent with a dominating inverse Compton component.

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Citations in the corpus

TeV BL Lac objects at the dawn of the Fermi era (2009, background): “It is widely accepted that the SEDs of blazars follow a sequence with the luminosity (Fossati et al. 1998; Donato et al. 2001): the powerful sources are characterized by SEDs with synchrotron and IC peaks E-mail: fabrizio.tavecchio@brera.inaf.it in the submm/IR and MeV bands, respectively, while…”
The transition between BL Lac objects and flat spectrum radio quasars (2010, background): “In other words: if the BLL sources in the 1LAC catalog with unknown redshift will turn out to be atz∼<0.5–1, then they will fit in the phenomenological blazar sequence [i.e. they would beBL Lacs of low and moderate luminosity, with the majority having a flat γ–ray slope (i.e.αγ <1–1.2); Fossati et a”
Canonical high power blazars (2009, background): “We can ask if our “canonical” jet can reproduce the phenomenological blazar sequence as proposed by Fossati et al. (1998)(see also Donato et al. 2001 and Ghisellini et al. 1998).”
The Fermi blazar sequence (2017, background): “Donato et al. (2001) later considered the slope of the X–ray emission for the same objects, that was added to the average SEDs.”
THE SPECTRAL ENERGY DISTRIBUTIONS OF FERMI BLAZARS (2016, methodology): “For spectral indexes, we adopt αR = 0 for radio band (Donato et al. 2001, Abdo et al. 2010a), while for optical band, α = 0.5 for BLs and α = 1 for the rest of the sources as similar to what have been done by Donato et al. (2001): 〈αX〉 = 1.30 for BLs, 〈αX〉 = 0.78 for FSRQs, and 〈αX〉 = 1.05 for BCUs.”
Are Quasar Jets Dominated by Poynting Flux? (2005, background): “Spectra below the break are hard, with a power-law index of the energy flux, F−αν , in the range 0.3 ≤ α ≤ 0.8 (Reeves & Turner 2000; Donato et al. 2001; Giommi et al. 2002).”
Spectral energy distributions of a large sample of BL Lacertae objects (2005, methodology): “To calculate the luminosities, redshift data was collected from VCV2000, Stocke et al. (1991), Laurent-Muehleisen et al. (1999), Donato et al. (2001) and SIMBAD database3.”
Astrophysical and cosmological information from large-scale submillimetre surveys of extragalactic sources (2007, methodology): “To allow for the corresponding steepening of radio spectra, we have adopted the spectral shape given by Donato et al. (2001) and Costamante & Ghisellini (2002), including their (controversial, see Antón & Browne 2005 and Nieppola et al. 2006) anti-correlation between break frequency and radio…”