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Table 4:

X-ray luminosities in the 0.3-0.7 keV band of various X-ray emitting components in gas-poor galaxies.

Name 		$L_{{\rm X,~unres}} $ $ L_{{\rm X,~sss}} $ $ L_{{\rm X,~gas}} $ LX/LK $ (L_{X}/L_{K})_{{\rm corr}} $ Age
  ( $ {\rm erg \ s^{-1}} $) ( ${\rm erg \ s^{-1}}) $ ( $ {\rm erg \ s^{-1}} $) ( ${\rm erg \ s}^{-1} \ L_{K,\odot}^{-1} $) ( ${\rm erg \ s}^{-1} \ L_{K,\odot}^{-1} $) (Gyr)
  (1) (2) (3) (4) (5) (6)
M 31 bulge $ 1.1 \times 10^{38} $ $ 3.5 \times 10^{37} $ $ 7.9 \times 10^{37} $ $ (1.8 \pm 0.2) \times 10^{27} $ $ (2.2 \pm 0.2) \times 10^{27} $ 6-10a
M 32 $ 6.4 \times 10^{35} $ $ 9.0 \times 10^{35} $ - $ (1.8 \pm 0.2) \times 10^{27} $ $ (2.4 \pm 0.2) \times 10^{27} $ 4-10b
M 105 $ 6.4 \times 10^{37} $ $ 1.9 \times 10^{37} $ - $ (2.0 \pm 0.2) \times 10^{27} $ $ (2.0 \pm 0.2) \times 10^{27} $ 8-15c
NGC 3377 $ 6.7 \times 10^{37} $ $ 1.1 \times 10^{37} $ - $ (3.9 \pm 0.6) \times 10^{27} $ $ (2.4 \pm 0.6) \times 10^{27} $ 4.1d
NGC 3585 $ 6.2 \times 10^{38} $ - - $ (4.1 \pm 0.3) \times 10^{27} $ $ (2.6 \pm 0.3) \times 10^{27} $ 3.1d
NGC 4278 $ 5.5 \times 10^{38} $ $ 3.4 \times 10^{37} $ $ 4.1 \times 10^{38} $ $ (3.2 \pm 0.2) \times 10^{27} $ $ (3.2 \pm 0.2) \times 10^{27} $ 10.7d
Sagittarius $ 3.5 \times 10^{32} $ $ 7.3 \times 10^{32} $ - $ (1.2 \pm 0.4) \times 10^{27} $ $ (1.7 \pm 0.4) \times 10^{27} $ 6.5-9.5e
Milky Way - - - $ (3.4 \pm 1.0) \times 10^{27} $ - -

Notes. (1) Luminosity of unresolved X-ray emission. (2) Luminosity of resolved supersoft sources. (3) Luminosity of ionized gas. (4) Observed X-ray to K-band ratio. (5) X-ray to K-band ratio transformed to the same point source detection sensitivity of $ 2 \times 10^{36} \ {\rm erg \ s^{-1}} $. The errors in Cols. (4) and (5) correspond to statistical uncertainties in X-ray count rates. (6) Age of the stellar population. References for ages: (a) Olsen et al. (2006), (b) Coelho et al. (2009), (c) Gregg et al. (2004), (d) Terlevich & Forbes (2002), (e) Bellazzini et al. (2006).


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