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Table 2:

Best-fit parameters for the X-ray spectra of 1ES 1210-646 from the observations described in this paper.
Model XRT #1 XRT #2 XRT #3 JEM-X+IBIS
parameter (0.3-9 keV) (0.3-9 keV) (0.3-9 keV) (3-100 keV)
powerlaw (+Fe line):        
$\chi^2$/d.o.f. 207.3/182 69.8/51 188.6/147 --
$N_{\rm H}$ ($\times$1021 cm-2) 5.2 $\pm$ 0.4 $\rm 5.0^{+0.8}_{-0.7}$ 5.1 $\pm$ 0.5 --
$\Gamma$ 1.80 $\pm$ 0.07 $\rm 1.63^{+0.15}_{-0.14}$ 1.45 $\pm$ 0.08 --
Normalisation* $\rm 11.5^{+0.9}_{-1.0}$ $\rm0.47^{+0.09}_{-0.07}$ 33 $\pm$ 3 --
E (keV) $\rm 6.71^{+0.05}_{-0.03}$ -- -- --
$\sigma $ (keV) $\rm0.16^{+0.05}_{-0.04}$ -- -- --
I ($\times$10-4 ph cm-2 s-1) $\rm 5.8^{+1.3}_{-1.2}$ -- --  
bremsstrahlung (+Fe line):        
$\chi^2$/d.o.f. 221.7/182 72.3/51 186.3/147 --
$N_{\rm H}$ ($\times$1021 cm-2) 4.3 $\pm$ 0.3 $\rm 4.3^{+0.7}_{-0.6}$ 4.7 $\pm$ 0.4 --
$kT_{\rm br}$ (keV) $\rm 7.3^{+1.4}_{-1.1}$ $\rm 12^{+9}_{-4}$ $\rm 22^{+11}_{-6}$ --
Normalisation* $\rm 12.1^{+0.6}_{-0.5}$ 0.56 $\pm$ 0.04 48 $\pm$ 2 --
E (keV) 6.72 $\pm$ 0.04 -- -- --
$\sigma $ (keV) $\rm0.17^{+0.06}_{-0.04}$ -- -- --
I ($\times$10-4 ph cm-2 s-1) $\rm 6.2^{+1.2}_{-1.3}$ -- --  
BB+powerlaw:        
$\chi^2$/d.o.f. -- -- -- 99.7/86
$N_{\rm H}$ ($\times$1021 cm-2) -- -- -- [5.0]
$kT_{\rm BB}$ (keV) -- -- -- $\rm 1.54^{+0.06}_{-0.08}$
$R_{\rm BB}$ $^{\dagger}$ (km) -- -- -- $\rm 5.9^{+1.5}_{-1.9}$
$\Gamma$ -- -- -- 2.1 $\pm$ 0.7
N* $_{\rm pow}$ -- -- -- $\rm 2.9^{+46.7}_{-2.8}$
$C_{\rm calib}$ -- -- -- $\rm 2.0^{+3.5}_{-1.7}$
bremsstrahlung+powerlaw:        
$\chi^2$/d.o.f. -- -- -- 120.4/86
$N_{\rm H}$ ($\times$1021 cm-2) -- -- -- [5.0]
$kT_{\rm br}$ (keV) -- -- -- $\rm 8.7^{+2.7}_{-1.7}$
N*$_{\rm br}$ -- -- -- $\rm 72^{+10}_{-25}$
$\Gamma$ -- -- -- $\rm 1.5^{+0.7}_{-4.3}$
N* $_{\rm pow}$ -- -- -- $\rm 1.7^{+32.1}_{-1.7}$
$C_{\rm calib}$ -- -- -- $\rm0.13^{+0.10}_{-0.06}$
X-ray luminosity$\ddagger$:        
0.5-2 keV 0.2 0.1 0.7 --
2-10 keV 0.4 0.2 1.9 2.0
20-100 keV -- -- -- 0.1

Notes. The above luminosities, corrected for interstellar Galactic absorption, are computed assuming a distance d = 2.8 kpc (Masetti et al. 2009) and are expressed in units of 1035 erg s-1. In the cases in which the X-ray data could not completely cover the X-ray interval of interest for the luminosity determination, an extrapolation of the best-fit model is applied. (*)  In units of 10-3. $^{(\dagger)}$  Computed assuming a distance d = 2.8 kpc to the source. $^{(\ddagger)}$  Computed using the powerlaw model for the XRT spectra and the BB+powerlaw model for the JEM-X+IBIS spectrum.


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