The nature of accreting black holes in nearby galaxy nuclei

We have found compact X-ray sources in the center of 21 (54%) of 39 nearby face-on spiral and elliptical galaxies with available ROSAT HRI data. ROSAT X-ray luminosities (0.2-2.4 keV) of these compact X-ray sources are simila r to 10(37)-10(40) ergs s(-1) (with a mean of 3 x 10(39) ergs s(-1)). The m ean displacement between the location of the compact)(-ray source and the o ptical photometric center of the galaxy is similar to 390 pc. The fact that compact nuclear sources were found in nearly all (five of six) galaxies wi th previous evidence for a black hole or an active galactic nucleus (AGN) i ndicates that at least some of the X-ray sources are accreting supermassive black holes. ASCA spectra of six of the 21 galaxies show the presence of a hard component with relatively steep (Gamma approximate to 2.5) spectral s lope. A multicolor disk blackbody model fits the data from the spiral galax ies well, suggesting that the X-ray object in these galaxies may be similar to a black hole candidate in its soft thigh) state. ASCA data from the ell iptical galaxies indicate that hot (kT approximate to 0.7 keV) gas dominate s the emission. The fact that (for both spiral and elliptical galaxies) the spectral slope is steeper than in normal type 1 AGNs and that relatively low absorbing col umns (N-H approximate to 10(21) cm(-2)) were found to the power-law compone nt indicates that these objects are somehow geometrically and/or physically different from AGNs in normal active galaxies. The X-ray sources in the sp iral and elliptical galaxies may be black hole X-ray binaries, low-luminosi ty AGNs, or possibly young X-ray luminous supernovae. Assuming the sources in the spiral galaxies are accreting black holes in their soft state, we es timate black hole masses similar to 10(2)-10(4) M..