Optical identification of the ASCA Large Sky Survey

We present results of optical identification of the X-ray sources detected in the ASCA Large Sky Survey. Optical spectroscopic observations were done for 34 X-ray sources that were detected with the SIS in the 2-7 keV band ab ove 3.5 sigma. The flux limit corresponds to similar to 1 x 10(-13) ergs cm (-2) s(-1) in the 2-10 keV band. The sources are identified with 30 active galactic nuclei (AGNs), two clusters of galaxies, and one Galactic star. On ly one source is still unidentified. All of the X-ray sources that have a hard X-ray spectrum with an apparent p hoton index of smaller than 1 in the 0.7-10 keV band are identified with na rrow-line or weak-broad-line AGNs at redshifts smaller than 0.5. This fact supports the idea that absorbed X-ray spectra of narrow-line and weak-broad line AGNs make the cosmic X-ray background (CXB) spectrum harder in the har d X-ray band than that of a broad-line AGN, which is the main contributor i n the soft X-ray band. Assuming their intrinsic spectra are same as a broad -line AGN (a power-law model with a photon index of 1.7), their X-ray spect ra are fitted with hydrogen column densities of log N-H(cm(-2)) = 22-23 at the object's redshift. On the other hand, X-ray spectra of the other AGNs a re consistent with that of a nearby type 1 Seyfert galaxy. In the sample, f our high-redshift luminous broad-line AGNs show a hard X-ray spectrum with an apparent photon index of 1.3 +/- 0.3. The hardness may be explained by t he reflection component of a type 1 Seyfert galaxy. The hard X-ray spectra may also be explained by absorption with log N-H(cm(-2)) = 22-23 at the obj ect's redshift, if we assume an intrinsic photon index of 1.7. The origin o f the hardness is not clear yet. Based on the log N-log S relations of each population, contributions to the CXB in the 2-10 keV band are estimated to be 9% for less-absorbed AGNs (lo g N-H(cm(-2)) < 22) including the four high-redshift broad-line AGNs with a hard X-ray spectrum, 4% for absorbed AGNs (22 < log N-H(cm(-2)) < 23, with out the four hard broad-line AGNs), and 1% for clusters of galaxies in the flux range from 3 x 10(-11) ergs cm(-2) s(-1) to 2 x 10(-13) ergs cm(-2) s( -1). If the four hard broad-line AGNs are included in the absorbed AGNs, th e contribution of the absorbed AGNs to the CXB is estimated to be 6%. In optical spectra, there is no high-redshift luminous cousin of a narrow-l ine AGN in our sample. The redshift distribution of the absorbed AGNs is li mited below z = 0.5 excluding the four hard broad-line AGNs, in contrast to the existence of 15 less-absorbed AGNs above z = 0.5. The redshift distrib ution of the absorbed AGNs suggests a deficiency of AGNs with column densit ies of log N-H(cm(-2))= 22-2-3 in the redshift range 0.5-2, or in the X-ray luminosity range larger than 10(44) ergs s(-1), or both. If the large colu mn densities of the four hard broad-line AGNs are real, they could compleme nt the deficiency of X-ray absorbed luminous high-redshift AGNs.