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Table 3:

Results of spectral fits of unresolved emission.

Name 		$kT_{\rm MKL}$ $\Gamma$ $L_{\rm MKL}$ $ L_{\rm PL} $ $ L_{\rm LMXB} $ $ L_{\rm MKL}/L_{\rm PL}$ $L_{\rm MKL}/(L_{\rm PL}-L_{\rm LMXB})$ $ \chi^2 $/d.o.f
  (keV)   ( $ {\rm erg \ s^{-1}} $) ( $ {\rm erg \ s^{-1}} $) ( $ {\rm erg \ s^{-1}} $)      
  (1) (2) (3) (4) (5) (6) (7) (8)
M 31 bulge $ 0.32 \pm 0.01 $ $ 1.82 \pm 0.04 $ $ 1.8 \times 10^{38} $ $ 2.5 \times 10^{38} $ - 0.72 0.72 473/223
M 32 $ 0.60 \pm 0.13 $ $ 1.65 \pm 0.15 $ $ 1.1 \times 10^{36} $ $ 5.3 \times 10^{36} $ - 0.21 0.21 76/70
M 60 $ 0.80 \pm 0.01 $ $ 1.70 \pm 0.11 $ $ 6.2 \times 10^{40} $ $ 1.5 \times 10^{40} $ $ 2.0 \times 10^{39} $ 4.13 4.77 1015/100
M 84 $ 0.65 \pm 0.01 $ $ 1.45 \pm 0.12 $ $ 3.0 \times 10^{40} $ $ 1.1 \times 10^{40} $ $ 1.5 \times 10^{39} $ 2.73 3.16 385/122
M 105 $ 0.64 \pm 0.05 $ $ 2.26 \pm 0.19 $ $ 4.7 \times 10^{37} $ $ 1.8 \times 10^{38} $ $ 3.8 \times 10^{37} $ 0.26 0.33 74/73
NGC 1291 $ 0.31 \pm 0.03 $ $ 2.64 \pm 0.23 $ $ 6.3 \times 10^{38} $ $ 9.9 \times 10^{38} $ $ 3.2 \times 10^{38} $ 0.64 0.94 83/67
NGC 3377 0.4 $ 2.15 \pm 0.47 $ ${<} 1.8 \times 10^{37} $ $ 3.0 \times 10^{38} $ $ 3.3 \times 10^{38} $ <0.06 - 45/34
NGC 3585 0.4 $ 2.75 \pm 0.61 $ ${<} 8.0 \times 10^{38} $ $ 2.5 \times 10^{39} $ $ 3.0 \times 10^{39} $ <0.32 - 46/39
NGC 4278 $ 0.47 \pm 0.06 $ $ 2.34 \pm 0.31 $ $ 5.1 \times 10^{38} $ $ 1.1 \times 10^{39} $ $ 1.1 \times 10^{38} $ 0.46 0.52 151/132
NGC 4365 $ 0.49 \pm 0.04 $ $ 1.67 \pm 0.17 $ $ 2.4 \times 10^{39} $ $ 2.8 \times 10^{39} $ $ 9.0 \times 10^{38} $ 0.86 1.26 128/98
NGC 4636 $ 0.59 \pm 0.01 $ $ 2.64 \pm 0.05 $ $ 1.1 \times 10^{41} $ $ 1.3 \times 10^{40} $ $ 4.1 \times 10^{38} $ 8.46 8.74 1122/199
NGC 4697 $ 0.33 \pm 0.03 $ $ 2.54 \pm 0.54 $ $ 7.3 \times 10^{38} $ $ 4.7 \times 10^{38} $ $ 2.1 \times 10^{38} $ 1.55 2.81 78/66
NGC 5128 $ 0.62 \pm 0.01 $ $ -0.76 \pm 0.01$ $ 2.1 \times 10^{39} $ $ 3.0 \times 10^{40} $ $ 5.1 \times 10^{37} $ 0.07 0.07 3547/435
Sagittarius 0.4 $ 2.44 \pm 0.51 $ ${<} 1.2 \times 10^{33}$ $ 2.5 \times 10^{33} $ - < 0.48 < 0.48 18/20

Notes. (1) Temperature of the thermal emission. (2) Photon index of the power-law. (3), (4) Luminosities of the thermal and power-law components in the 0.5-8 keV energy range. (5) The combined luminosity of unresolved low-mass X-ray binaries brighter than $10^{35} \ {\rm erg \ s^{-1}}$ (but fainter than the sensitivity limit for the given galaxy) estimated from the K-band luminosity of the studied region and the average LMXB X-ray luminosity function of Gilfanov (2004). (6) The observed luminosity ratio of the soft thermal component to the power-law. (7) Same as (6) but corrected for contribution of unresolved LMXBs. For NGC 3377 and NGC 3585, the predicted LMXB luminosity exceeds the observed luminosity of the power-law component, presumably because of a scatter in X/K ratios for LMXBs, therefore no LMXB-corrected luminosity ratio is computed. (8) Goodness of fit.


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