ROSAT and ASCA Observations of the Seyfert Galaxy 1H0419-577, Identified with LB 1727

Details ROSAT and ASCA Observations of the Seyfert Galaxy 1H0419-577, Identified with LB 1727 ROSAT and ASCA Observations of the Seyfert Galaxy 1H0419-577, Identified with LB 1727

May 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998nasa.reptu....t&link_type=abstract

Technical Report, NASA/CR-1998-208595; NAS 1.26:208595

Computer Science

Seyfert Galaxies, Rosat Mission, X Rays, Active Galaxies, Galactic Nuclei, Targets, Spectra, K Lines, Line Of Sight, Continuums

Scientific paper

We discuss the properties of the Seyfert 1.5 galaxy LB 1727 based upon the analysis of two ASCA observations, a two-month Rosat monitoring campaign, and optical data. The target is identified with the HEAO-A1 source 1H0419-577, so it has been observed by ASCA and ROSAT in order to obtain better X-ray variability and spectra data. Only modest (20%) variability is observed within or between ASCA and BeppoSAX observations in the approximately 2 - 10 keV band. However, the soft X-ray flux increased by a factor of 3 over a period of 2 months, while it was monitored daily by the ROSAT HRI instrument. The hard X-ray continuum can be parameterized as a power-law of slope Gamma approximately 1.5 - 1.6 across 9.7 - 11 keV in the rest-frame. We also report the first detection of an iron K(alpha) line in this source, consistent with emission from neutral material. The X-ray spectrum steepens sharply below 0.7 keV yielding a power-law of slope Gamma approximately 3.2. There is no evidence for absorption by neutral material, instrinsic to the nucleus. If the nucleus is unattenuated, then the break energy between the soft-excess and hard component is 0.7+/-0.08 keV. An ionized absorber may produce some tum-up in the spectrum at low energies, but a steepening of the underlying continuum is also required to explain the simultaneous ASCA and HRI data. We cannot rule out the possibility that a significant column of ionized material exists in the line-of-sight, if that is true, then the continuum break-energy can only be constrained to lie within the approximately 0.1 - -0.7 keV band.

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