ASCA OBSERVATIONS OF TYPE-2 SEYFERT-GALAXIES .1. DATA-ANALYSIS RESULTS

We present ASCA spatial, temporal, and spectral data for a sample of 2 6 observations of 25 type 2 active galactic nuclei (AGNs), composed of 17 Seyfert 2 galaxies and eight narrow emission line galaxies (NELGs) . Twenty-four of the 25 sources were detected. The ASCA images are gen erally consistent with emission from point sources at energies above s imilar to 3 keV. We use archival ROSAT data to examine each field at h igh spatial resolution and to check for the presence of sources that w ould contaminate the ASCA data. Of the five sources bright enough for 128 s temporal analysis, three are variable at >99% confidence, with c haracteristics consistent with those observed in Seyfert 1 galaxies. A nalysis on a timescale of 5760 s reveals six sources variable at >99% confidence, and comparison with previous X-ray results shows most of t he sample to be variable in hard X-ray flux on timescales of years. Si mple continuum models are fitted to the sample spectra to characterize the variety of spectral forms and hence to determine the fundamental nature of the X-ray spectrum of each source. No single spectral model provides an adequate fit to all the sample sources. Thirty-six percent of the sample cannot be adequately fitted by any of our test models ( all rejected at >95% confidence). Approximately half of the sample hav e an iron K alpha line with an equivalent width consistent with an ori gin in the line-of-sight absorber; the remaining lines must be produce d in material out of the line of sight. Absorbing columns up to 10(24) atoms cm(-2) are detected, and even larger columns are inferred for s ome sources. The mean underlying hard X-ray power-law index is Gamma s imilar to 2. Many X-ray emission lines were detected at high levels of confidence. The iron K-shell regime is dominated by emission from ''n eutral'' material. Many data sets also show evidence for complexity in the iron K alpha profile, which may be interpreted as evidence for br oad-line profiles, including flux both redward and blueward of the lin e peak, and/or for the existence of hydrogen-like and helium-like iron K lines. Hydrogen-like and helium-like lines are detected from Fe, Ne , Si, S, and Ar in addition to Mg Lines. While almost half of the samp le have an estimated starburst contribution of >30% in the 0.5-4.5 keV bandpass, the soft X-ray emission lines are not solely associated wit h a strong starburst component.