Table 1: Results of fitting the 4U 1705-44 spectra in the energy band 0.3-200 keV.
Parameter Value
$N_{\rm H}$ $\rm (\times 10^{22}\;cm^{-2})$ $1.9 \pm 0.1$
$k T_{\rm bb}$ (keV) $0.56 \pm 0.01$
$N_{\rm bb}$ (keV) $(2.23 \pm 0.11)\times 10^{-2}$
$k T_{\rm W}$ (keV) $\rm 1.13 ^{+0.05}_{-0.02}$
$k T_{\rm e}$ (keV) $2.72 \pm 0.09$
$\tau$ $11.0 \pm 0.6$
$N_{\rm c}$ $0.35 \pm 0.02$
$E_{\rm Fe}$ (keV) $\rm 6.7^{+0.2}_{-0.5}$
$R_{\rm in}$ ( R$_{\rm g}$) $\rm 8.1^{+4.2}_{-2.1}$
Incl (deg) $\rm 28^{+20}_{-8}$
$I_{\rm Fe}$ (ph cm-2 s-1) $(4.7^{+2.0}_{-0.6}) \times 10^{-3}$
Fe Eq. W. (eV) 109
$\Gamma$ $\rm 2.9^{+0.2}_{-0.3}$
Np $\rm0.7 ^{+0.4}_{-0.2}$
$F_{\rm tot ab}$ 5.81
$F_{\rm tot}$ 16.7
$\chi^2_{\rm red}$/d.o.f. 1.183 /524
Note- The model consists of blackbody, Comptonization comptt, and power-law components, and a diskline emission line, all subject to interstellar absorption. Uncertainties are at the 90% confidence level for a single parameter. The total flux is in the 0.1-100 keV energy range and in units of $\times 10^{-9}$ ergs cm-2s-1.

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