UV variability of IRAS 13224-3809, a rapidly X-ray variable far-infrared luminous galaxy

Details UV variability of IRAS 13224-3809, a rapidly X-ray variable far-infrared luminous galaxy UV variability of IRAS 13224-3809, a rapidly X-ray variable far-infrared luminous galaxy

Mar 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...283l...9m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 283, no. 2, p. L9-L12

Astronomy and Astrophysics

Astronomy

9

Emission Spectra, Far Ultraviolet Radiation, Luminosity, Lyman Alpha Radiation, Seyfert Galaxies, Spaceborne Astronomy, Spectrum Analysis, Ultraviolet Astronomy, X Ray Sources, H Alpha Line, H Beta Line, Iue, Radio Spectra, Red Shift, Spectral Energy Distribution

Scientific paper

We have detected strong Ly-alpha line variability in IRAS 13224-3809, a very luminous IRAS galaxy known to be a strong and rapidly variable soft X-ray emitter. While a relatively broad Ly-alpha component (full width at half maximum (FWHM) approximately 500 km/s) remains essentially constant along three IUE observations performed between January and May 1993, the initially strong narrow core component vanishes completely becoming a strong absorption. IRAS 13224-3809 has a deficit of UV emission when compared to Seyfert 1 galaxies. The UV-X-ray energy distribution suggests that the UV bump frequently found in these galaxies might be present at higher energies, well within the ROSAT band (0.1-2.4 keV). The strong far infrared emission, the X-ray and Ly-alpha profile variability, the absence of broad Balmer lines components and the high H-alpha/H-beta ratios could be explained assuming the presence of a nucleus that has become 'active' after a recent merging episode, being surrounded by large amounts of gas and dust which would obscure selectively different emitting regions.

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