The edge-on spiral galaxy NGC 4565 was observed for ∼ 35 ks with ASCA in the 0.5-10 keV energy band. The X-ray emission was dominated by two bright sources, which could be identified with two point-like X-ray sources seen in the ROSAT HRI image. The observed 0.5-10 keV fluxes of these sources, 1.7 × 10-12 erg s-1 cm-2 and 0.7 × 10-12 erg s-1 cm-2, imply bolometric luminosities of 1.2 × 1040 erg s-1 and 4.6 × 1039 erg s-1, respectively. They exhibit similar spectra, which can be explained by emission from optically thick accretion disks with inner-disk temperature of 1.4-1.6 keV. One of them, coincident in position with the nucleus, shows too low absorption to be the active nucleus seen through the galaxy disk. Their spectra and high luminosities suggest that they are both mass-accreting black-hole binaries. However the black-hole mass required by the Eddington limit is rather high (≥ 50M(Fisheye)), and the observed disk temperature is too high to be compatible with the high black-hole mass. Several attempts have been made to solve these problems.
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