2018A&A...619A..93B


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.12CET06:43:52

2018A&A...619A..93B - Astronomy and Astrophysics, volume 619A, 93-93 (2018/11-1)

Hard X-ray properties of NuSTAR blazars.

BHATTA G., MOHORIAN M. and BILINSKY I.

Abstract (from CDS):


Context. Investigation of the hard X-ray emission properties of blazars is key to the understanding of the central engine of the sources and associated jet process. In particular, simultaneous spectral and timing analyses of the intraday hard X-ray observations provide us a means to peer into the compact innermost blazar regions that are not accessible to our current instruments.
Aims. The primary objective of the work is to associate the observed hard X-ray variability properties in blazars with their flux and spectral states, thereby, based on the correlation among these states, extract the details about the emission regions and processes occurring near the central engine.
Methods. We carried out timing, spectral, and cross-correlation analysis of 31 NuSTAR observations of 13 blazars. We investigated the spectral shapes of the sources using single power-law, broken power-law, and log-parabola models. We also studied the co-relation between the soft and hard emission using z-transformed discrete correlation function. In addition, we attempted to constrain the smallest emission regions using minimum variability timescales derived from the light curves.
Results. We found that, for most of the sources, the hard X-ray emission can be well represented by the log-parabola model and that the spectral slopes for different blazar subclasses are consistent with the so-called blazar sequence. We also report the steepest spectra (Γ∼3) in the BL Lacertae PKS 2155-304 and the hardest spectra (Γ∼1.4) in the flat-spectrum radio quasar PKS 2149-306. In addition, we noted a close connection between the flux and spectral slope within the source subclass in the sense that high flux and/or flux states tend to be harder in spectra. In BL Lacertae objects, assuming particle acceleration by diffusive shocks and synchrotron cooling as the dominant processes governing the observed flux variability, we constrain the magnetic field of the emission region to be a few Gauss; whereas in flat-spectrum radio quasars, using external Compton models, we estimate the energy of the lower end of the injected electrons to be a few Lorentz factors.

Abstract Copyright: © ESO 2018

Journal keyword(s): accretion - accretion disks - radiation mechanisms: non-thermal - galaxies: active - BL Lacertae objects: general

Simbad objects: 14

goto Full paper

goto View the reference in ADS

Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 6C 001403+811827 QSO 00 17 08.4748554 +81 35 08.136591   17.60 16.52 15.95   ~ 354 1
2 QSO J0225+1846 QSO 02 25 04.6672463736 +18 46 48.759971912   20.0 20.0 19.09   ~ 70 1
3 QSO B0229+200 BLL 02 32 48.6154943841 +20 17 17.493345304   18.0 18.00     ~ 246 3
4 8C 0716+714 BLL 07 21 53.4484901266 +71 20 36.362058601   15.5 14.17 14.27   ~ 1105 1
5 4C 71.07 QSO 08 41 24.36526906 +70 53 42.1730054     16.5 16.8   ~ 682 1
6 Mrk 421 BLL 11 04 27.3139210166 +38 12 31.798324828   13.50 12.90 8.31   ~ 2334 1
7 3C 273 BLL 12 29 06.6996828061 +02 03 08.598846466   13.05 14.830 14.11   ~ 5252 1
8 3C 279 QSO 12 56 11.1664521013 -05 47 21.531840471   18.01 17.75 15.87   ~ 2643 2
9 7C 1441+2514 QSO 14 43 56.89219806 +25 01 44.4907918   19.5   19.7   ~ 90 1
10 4C 39.49 BLL 16 53 52.21668494 +39 45 36.6089458 14.09 14.15 13.29 8.26   ~ 1879 2
11 QSO B1959+650 BLL 19 59 59.8525497024 +65 08 54.651170114     12.8 11.21   ~ 486 2
12 QSO B2149-306 QSO 21 51 55.52398143 -30 27 53.6979987   17.95 18.0 17.48   ~ 214 1
13 QSO B2155-304 BLL 21 58 52.0651817803 -30 13 32.120657891   13.36 13.09 12.62   ~ 1521 1
14 NAME BL Lac BLL 22 02 43.2913773726 +42 16 39.978417860   15.66 14.72     ~ 1977 1

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2018A&A...619A..93B and select 'bookmark this link' or equivalent in the popup menu


2019.12.12-06:43:52

© Université de Strasbourg/CNRS

    • Contact