Table 4: Best fit models to the 0.3-7 keV ACIS-I and ACIS-S spectra of r2-3 and r2-4a. Numbers in parentheses represent 90% confidence uncertainties on the last digit.
Observation $\alpha_{r2-3}$ $L_{\rm r2-3}$b $\chi^2$/d.o.f. $\alpha_{\rm r2-4}$ $L_{\rm r2-4}$b $\chi^2$/d.o.f.
c1 2.1(2) 3.3 11/18 1.7(2) 2.4 13/14
c3 $\dots$ $\dots$ $\dots$ 1.4(3) 3.9 16/10
c5 1.9(3) 2.5 16/12 1.5(3) 4.1 20/12
c7 2.1(4) 2.2 6/9 1.8(3) 2.5 6/11
c9 1.7(3) 3.4 15/15 1.5(4) 3.4 12/6
c12 1.7(2) 3.0 20/11 2.3(4) 0.9 6/7
c14 1.7(2) 4.0 11/11 1.5(2) 3.0 10/12
c15 1.6(2) 4.5 11/16 1.8(2) 3.0 12/11
c17 $\dots$ $\dots$ $\dots$ 1.6(2) 2.0 11/10
c22 2.2(9) 2.0 4/3 1.9(5) 1.8 3/6
c23 2.6(7) 0.7 1/3 1.6(2) 4.0 4/11
c28 1.8(3) 3.8 8/10 2.2(6) 1.9 10/6
c29 1.5(3) 4.4 6/9 1.4(2) 3.5 11/11
c31 2.1(3) 3.0 11/9 1.3(2) 3.7 13/9
c34 1.9(3) 2.3 6/7 2.3(4) 2.0 8.5/10
c35 2.0(4) 2.7 3/7 1.7(3) 3.5 5/7
a An absorbed power law model was used, with line-of-sight absorption
$N_{\rm H} = 1.0 \times 10^{21}$ atom cm-2 and spectral index $\alpha$.
b 0.3-10 keV luminosity/1037 erg s-1.

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