Chandra HETG Observations of the Magnetic Cataclysmic Variable V1223 Sagittarii

K. Mukai (1) - T. Kallman (1) - E. Schlegel (2) - A. Bruch (3) - G. Handler (4) - J. Kemp (5)

(1) Code 662, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA
(2) Harvard Smithonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
(3) Laboratório Nacional de Astrofísica, CP 21, BR-37500-000 Itajubá - MG, Brazil
(4) South African Astronomical Observatory, PO Box 9, Observatory 7935, South Africa
(5) Joint Astronomy Centre, University Park, 500 North A'ohoku Place, Hilo, HI 96720, USA

Abstract:

V1223 Sgr is among the brightest magnetic cataclysmic variables in the 1-10 keV band, with a 3.36 hr orbital period and a 745.6 s spin period. Here we report selected results from our Chandra HETG observations, performed on 2000 April 30/May 1. We detected K-alpha lines of many atomic species in the phase-averaged HETG spectrum. We find that the Fe L lines are substantially weaker than would be expected in a collisionally excited plasma. The ratios of helium-like triplets indicate a high density. We also find evidence of an ionized absorber. We suggest the accretion flow just before it reached the shock is the likely location for both the absorber and the low energy emitter.