Astronomy and Astrophysics – Astrophysics
Scientific paper
1997-11-03
Astronomy and Astrophysics
Astrophysics
5 pages, 2 figures. Accepted for publication in Monthly Notices of the Royal Astronomical Society. Also available from http:
Scientific paper
10.1046/j.1365-8711.1998.01286.x
We present UV spectroscopy of RE1034+396, taken with the Faint Object Spectrograph on the Hubble Space Telescope. With a spectral resolution of ~1-2A FWHM and a typical S/N of ~15 per diode, this is one of the first detailed UV spectra of an object in the narrow-line Seyfert 1 (NLS1) class. The spectrum probes the physics and kinematics of the high-ionization and coronal line gas, and the strength and form of the big blue bump component in the UV. We detect many emission lines, including Lyman alpha, CIV1549, HeII1640, CIII]1909 and MgII2798. We also identify a feature at 2647A (in the rest-frame) with highly-ionized iron [FeXI]2649; a line of the same species ([FeXI]7892) has also been seen in the optical spectrum. The velocity widths of the UV lines are relatively narrow (FWHM<2000 km/s) and similar to those of the optical lines, which suggests that all line emission in REJ1034+396, ie. including that of high- and low-ionization species and the forbidden lines, may be dominated by an intermediate-velocity (FWHM~1000 km/s), intermediate-density (log Ne~7.5 cm-3) region of gas. The slope of the UV continuum (alpha~0.9) is soft (ie. red) relative to quasars and the UV-to-soft X-ray flux ratio is unusually low implying that the big blue bump component is very weak in the UV. The present epoch UV to soft X-ray continuum is consistent with earlier data, demonstrating that this extreme big blue bump component is also very stable, unlike many other NLS1s which show extreme patterns of variability.
Mason Keith O.
Puchnarewicz Elizabeth M.
Siemiginowska Aneta
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