X-ray and multiwavelength view of NGC 4278 - A LINER-Seyfert connection?

G. Younes; D. Porquet; B. Sabra; N. Grosso; J. N. Reeves; M. G. Allen

doi:10.1051/0004-6361/201014371

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Volume 517 (July 2010)

A&A, 517 (2010) A33

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Table 2:

Best fit parameters of a *mekal* plus an absorbed power-law model for the *Chandra* data and an absorbed power-law model for the *XMM-Newton* spectra.
Obs. ID	Nh^a	$\Gamma$	Pl norm.	kT^a	EM^ab	Flux^c	Corr. flux^c	Pl^d
	10²⁰ cm^-2		10^-4 Photons keV^-1 cm^-2 s^-1	keV	10⁶² cm^-3	10^-13 erg s^-1	10^-13 erg s^-1	%
4741	<6.78	2.13 [2.00-2.28]	4.28 [3.92-4.71]	0.62 [0.58-0.66]	2.64 [2.27-2.99]	18.1 [17.1-18.8]	18.5 [18.2-20.1]	94
7077		2.26 [2.16-2.39]	1.82 [1.68-1.99]			7.8 [7.5-7.9]	8.21 [8.0-9.0]	83
7078		2.34 [2.22-2.47]	4.21 [3.90-4.61]			16.0 [14.9-16.2]	16.5 [16.1-18.5]	93
7079		2.38 [2.28-2.50]	3.76 [3.54-4.07]			14.1 [13.3-14.3]	15.05 [14.7-16.4]	90
7080		2.02 [1.84-2.20]	1.10 [0.96-1.26]			5.9 [5.5-6.1]	6.0 [5.7-6.8]	80
7081		2.12 [2.00-2.25]	1.25 [1.14-1.29]			6.2 [5.9-6.4]	6.4 [6.2-7.1]	81
Reduced $\chi^{2} = 0.93$ for 310 d.o.f.
0205010101	3.82 [3.05-4.59]	2.05 [2.03-2.07]	8.07 [7.90-8.24]			33.8 [32.8-33.2]	34.5 [34.2-34.8]	100
Reduced $\chi^{2} = 1.01$ for 487 d.o.f.

Notes. ^(a) Parameter linked for the different Chandra observations; ^(b) the emission measure (EM) of the mekal model, $EM=\int$ $n_{\rm e}$ $n_{\rm H}$ dV; ^(c) fluxes in the 0.5-8 keV energy range; ^(d) the power-law component fraction to the total corrected flux.

Source LaTeX | All tables | In the text

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