Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...433..577p&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 433, no. 2, p. 577-582
Astronomy and Astrophysics
Astrophysics
4
Cooling Flows (Astrophysics), Emission Spectra, Galactic Clusters, Intergalactic Media, Line Spectra, Lyman Alpha Radiation, Oxygen, Ultraviolet Spectra, Visible Spectrum, X Ray Absorption, Carbon, Computerized Simulation, Hubble Space Telescope, Iue, Neon, Nitrogen, Red Shift, Rosat Mission, Silicon, Sulfur
Scientific paper
Recently Miyaji et al. (1993) detected excess soft X-ray absorption in the Broad Band X Ray Telescope (BBXRT) spectrum of the cluster A2256. The absorption was due to the K-edge of oxygen; from the observed edge energy and the redshift of the cluster, Miyaji et al. argued that the primary absorber was oxygen in an ionization state between O(+2) and O(+4) at a temperature in the range 0.5-5 x 105 K. Such gas should produce strong UV and optical line emission. We predict the strongest UV and optical line fluxes for this X-ray absorbing gas. The strongest UV lines include Lyman-alpha, C III lambda-1909, C IV lambda-1549, O IV lambda-1401, O V lambda-1218, O VI lambda-1034, Si III lambda-1207, and Si IV lambda-1397 lines. These lines should be detectable with the International Ultraviolet Explorer, the Hubble Space Telescope, or the Hopkins Ultraviolet Telescope. In the optical the lines are weaker, but the (O II) lambda lambda-3726, 3729, (O III) lambda lambda-4959, 5007, (N II) lambda lambda-6567, 6584, (Ne III) lambda lambda-3918, 3969, (S II) lambda-6720, and (S III) lambda-9320 lines should be detected with moderate exposures if the warm absorber is near the lower limit of the allowed temperature range, T less than or approximately equal to 1.5 x 105 K. In this limit the H-alpha and (S III) lambda-3720 lines will require longer exposure times, but should be detectable as well.
Pistinner Shlomi
Sarazin Craig L.
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