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Table 1:

The list of early-type galaxies and galaxy bulges studied in this paper.

Name 		Distance $N_{\rm H}$ Morphological LK $ T_{{\rm obs}} $ $ T_{{\rm filt}} $ $L_{{\rm lim}}$ R1 R2
  (Mpc) (cm-2) type ( ${L_{K,\odot}}) $ (ks) (ks) ( $ {\rm erg \ s^{-1}} $) ( $\hbox{$^{\prime\prime}$ }$) ( $\hbox{$^{\prime\prime}$ }$)
  (1) (2) (3) (4) (5) (6) (7) (8) (9)
M 31 bulge 0.78a $ 6.7 \times 10^{20} $ SA(s)b $ 3.7 \times 10^{10} $ 180.1 143.7 $ 2 \times 10^{35} $ 300 720
M 32 0.805b $ 6.3 \times 10^{20} $ cE2 $ 8.5 \times 10^{8} $ 178.8 172.2 $ 1 \times 10^{34} $ 25 90
M 60 16.8c $ 2.2 \times 10^{20} $ E2 $ 2.2 \times 10^{11} $ 109.3 90.5 $ 9 \times 10^{36} $ 50 125
M 84 18.4c $ 2.6 \times 10^{20} $ E1 $ 1.6 \times 10^{11} $ 117.0 113.8 $ 9 \times 10^{36} $ 50 100
M 105 9.8d $ 2.8 \times 10^{20} $ E1 $ 4.1 \times 10^{10} $ 341.4 314.0 $ 1 \times 10^{36} $ 30 90
NGC 1291 8.9e $ 2.1 \times 10^{20} $ (R)SB(s)0/a $ 6.3 \times 10^{10} $ 76.7 51.2 $ 5 \times 10^{36} $ 60 130
NGC 3377 11.2c $ 2.9 \times 10^{20} $ E5-6 $ 2.0 \times 10^{10} $ 40.2 34.0 $ 2 \times 10^{37} $ - 79
NGC 3585 20.0c $ 5.6 \times 10^{20} $ E7/S0 $ 1.5 \times 10^{11} $ 95.9 89.1 $ 2 \times 10^{37} $ 50 180
NGC 4278 16.1c $ 1.8 \times 10^{20} $ E1-2 $ 5.5 \times 10^{10} $ 467.7 443.0 $ 2 \times 10^{36} $ 50 110
NGC 4365 20.4c $ 1.6 \times 10^{20} $ E3 $ 1.1 \times 10^{11} $ 198.3 181.4 $ 8 \times 10^{36} $ 30 80
NGC 4636 14.7c $ 1.8 \times 10^{20} $ E/S0_1 $ 8.1 \times 10^{10} $ 212.5 202.1 $ 5 \times 10^{36} $ 30 102
NGC 4697 11.8c $ 2.1 \times 10^{20} $ E6 $ 5.1 \times 10^{10} $ 195.6 162.0 $ 4 \times 10^{36} $ 30 95
NGC 5128 3.7f $ 8.6 \times 10^{20} $ S0 pec $ 5.8 \times 10^{10} $ 569.1 568.9 $ 1 \times 10^{36} $ 65 240
Sagittarius 0.0248g $ 1.2 \times 10^{21} $ dSph(t) $ 8.9 \times 10^{5} $ 30.1 29.7 $ 1 \times 10^{32} $ - 55

Notes. (1) References for distances: (a) Macri (1983); Stanek & Garnavich (1998) - (b) Mateo (1998) - (c) Tonry et al. (2001) - (d) Jensen et al. (2003) - (e) de Vaucouleurs (1975) - (f) Ferrarese et al. (2007) - (g) Kunder & Chaboyer (2009)(2) Galactic absorption column density (Dickey & Lockman 1990). (3) Taken from NED (http://nedwww.ipac.caltech.edu/). (4) K-band luminosity of galaxies. (5), (6) Exposure times before and after data filtering, (7) Point source detection sensitivity in the 0.5-8 keV energy range (8), (9) The radii used for the inner and outer regions in obtaining the spectra presented in Fig. 2. The orientation and shape of the regions were taken from K-band measurements (http://irsa.ipac.caltech.edu/applications/2MASS/).


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