X-RAY SPECTRAL PROPERTIES OF THE CLUSTER ABELL-2029

We have analyzed ASCA and ROSAT PSPC spectra and images of the galaxy cluster Abell 2029. The ASCA spectra of the cluster indicate that the gas temperature declines with radius. The PSPC image shows that the cl uster is very regular and smooth. Also, there is no significant eviden ce for any irregularities in the temperature distribution in the clust er, as would be produced by a subcluster merger. These results suggest that A2029 is a relaxed cluster and that the gas is in hydrostatic eq uilibrium. We use the assumption of equilibrium to determine the gravi tational mass of the cluster as a function of radius. At a radius of 1 6' (1.92 h(50)(-1) Mpc; H-0 = 50 h(50) km s(-1) Mpc(-1)), the gravitat ional mass is M-tot = (9.42 +/- 4.22) x 10(14) h(50)(-1) M., while the mass of gas is M-gas = (2.52 +/- 0.77) x 10(14) h(50)(-5/2) M.. The g as fraction is found to increase with radius; within a spherical radiu s of 16', the fraction is M-gas/M-tot = (0.26 +/- 0.14) h(50)(-3/2). T he iron abundance in the gas is found to be 0.40 +/- 0.04 solar. There is no significant evidence for any variation in the abundance with po sition in the cluster. The global X-ray spectra, central X-ray spectra , and ROSAT surface brightness all require a cooling flow at the clust er center. The global X-ray spectrum implies that the total cooling ra te is 363(-96)(+79) h(50)(-2) M. yr(-1). The global X-ray spectra are consistent with the Galactic value for the soft X-ray absorption towar d the cluster. White et al. and Alien & Fabian have suggested that the re is significant excess absorption associated with the cooling flow i n the cluster. The ROSAT PSPC spectra of the central regions of the cl uster are inconsistent with a large value of foreground excess absorpt ion. The upper limit on excess foreground absorption is 7.3 x 10(19) c m(-2). However, the spectra do not rule out a significant amount of in trinsic absorbing gas located within the cooling flow region.