SIMBAD references

J.-U. Ness and S. Starrfield, Arizona State University; J. J. Drake, Smithsonian Astrophysical Observatory; M. F. Bode, Liverpool John Moores University; T. J. O'Brien and R. J. Davis, University of Manchester; J. Osborne, K. L. Page, A. Beardmore, and M. Goad, University of Leicester; G. Schwarz, West Chester University; J. Krautter, University of Heidelberg; A. Evans, Keele University; S. P. S. Eyres, University of Central Lancashire; R. Gonzalez, XMM Science Operations Centre; and R. D. Gehrz and C. E. Woodward, University of Minnesota, report that RS Oph has been observed three times with Chandra on Sept. 4 (day 203.6 after outburst, 39600 s), 7 (day 206.28, 39800 s), and 8 (day 207.92, 17900 s), as well as with XMM-Newton on Sept. 6 (day 205.25, 55300 s). All x-ray spectra revealed only emission lines from highly ionized species and no continuum. The emission lines are from the blast wave generated by the explosion, and the H-like and He-like lines of neon and oxygen were detected as well as N VII, Mg XI, Fe XVII, and Fe XVIII. The widths of the emission lines indicate velocities of 800-1000 km/s, similar to those in June 2006 (reported on CBET 559). The observed flux integrated over 0.35-2 keV was 2.2 x 10**(-12) erg/cm**2/s in the summed Chandra observation and (1.3-1.6) x 10**(-12) erg/cm**2/s in the XMM observation (which is lower due to chip gaps), and is thus a factor of four lower than in June 2006. Compared to the June observation, all emission lines are weaker, but the lines formed at lower temperatures are stronger than lines formed at higher temperatures, which indicates a decrease in kinetic temperature of the shell. The x-ray light curves show no variability, as expected, now that the supersoft continuum emission from the white dwarf has disappeared.