Table 2: Best-fit parameters for the diffuse emissiona.
Parameters Head Tail
vpshock
$kT_{\rm e}$ [keV] 0.39 (0.38-0.40) 0.35 (0.34-0.39)
$n_{\rm e}t_{\rm p}$ [1012 cm-3 s] (>14.6) 9.0 (>2.0)
$[{\rm O/H}]$b 0.36 (0.30-0.47) 0.47 (0.36-0.64)
$[{\rm Ne/H}]$b 0.82 (0.74-0.96) 0.79 (0.63-1.0)
$[{\rm Fe/H}]$b 0.09 (0.07-0.11) 0.11 (0.09-0.15)
E.M. [1058 cm-3]c 4.4 (3.8-4.8) 2.8 (2.1-3.5)
$N_{\rm H}^{{\rm LMC}}$ [ $10^{21}~{\rm cm}^{-2}$]d 5.6 (4.7-6.4) 1.8 (1.0-3.1)
Flux [ $10^{-13}~{\rm erg~cm}^{-2}~{\rm s}^{-1}$]e 3.2 3.6
Power-lawf
Flux [ $10^{-14}~{\rm erg~cm}^{-2}~{\rm s}^{-1}$]e 4.6 (3.6-5.6) -
a Parentheses indicate single parameter 90% confidence regions. b Abundance ratio relative to the solar value (Anders & Grevesse 1989). c $E.M. = n_{\rm e}^2V$, where $n_{\rm e}$ and V are the electron density and the volume, respectively. d Calculated using the photometric absorption cross-sections by Balucinska-Church & McCammon (1992) with the LMC abundances (Russell & Dopita 1992). e In the 0.5-10.0 keV band. f $\Gamma$ is fixed to the best-fit value for Source 1 (1.57).

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