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(fwd) V4743 Sgr, from Sumner Starrfield Date: Sun, 03 Aug 2003 19:48:42 -0700 (MST) From: Sumner Starrfield <sumner.starrfield@asu.edu> Subject: V4743 Sgr: Dear Dr. Kato The following paper was accepted by ApJ Letters and we have put it in astro-ph. It does not include any of the optical observations - that will be in another paper. The VSNET observers may be interested in the light curve: ------------------------------------------------------------------------------ \\ Paper: astro-ph/0308017 From: Jan-Uwe Ness <jness@hs.uni-hamburg.de> Date: Fri, 1 Aug 2003 16:08:54 GMT (164kb) Title: A Chandra LETGS observation of V4743 Sagittarius: A Super Soft X-ray Source and a Violently Variable Light Curve Authors: J.-U. Ness, S. Starrfield, V. Burwitz, P. Hauschildt, R. Wichmann, J.J. Drake, R.M. Wagner, H.E. Bond, J. Krautter, M. Orio, M. Hernanz, R.D. Gehrz, C.E. Woodward, Y. Butt, K. Mukai, and S. Balman Comments: 5 pages, 5 figures, accepted by ApJL \\ V4743 Sgr (Nova Sgr 2002 No. 3) was discovered on 20 September 2002. We obtained a 5ks ACIS-S spectrum in November 2002 and found that the nova was faint in X-rays. We then obtained a 25ks CHANDRA LETGS observation on 19 March 2003. By this time, it had evolved into the Super Soft X-ray phase exhibiting a continuous spectrum with deep absorption features. The light curve from the observation showed large amplitude oscillations with a period of 1325s (22min) followed by a decline in total count rate after ~13ks of observations. The count rate dropped from ~40cts/s to practically zero within ~6ks and stayed low for the rest of the observation (~6ks). The spectral hardness ratio changed from maxima to minima in correlation with the oscillations, and then became significantly softer during the decay. Strong H-like and He-like lines of oxygen, nitrogen, and carbon were found in absorption during the bright phase, indicating temperatures between 1-2MK, but they were shifted in wavelength corresponding to a Doppler velocity of -2400km/s. The spectrum obtained after the decline in count rate showed emission lines of CVI, NVI, and NVII suggesting that we were seeing expanding gas ejected during the outburst, probably originating from CNO-cycled material. An XMM-Newton ToO observation, obtained on 4 April 2003 and a later LETGS observation from 18 July 2003 also showed oscillations, but with smaller amplitudes. \\ ( http://arXiv.org/abs/astro-ph/0308017 , 164kb)
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