The Enhancement and Decrement of the Sunyaev-Zeldovich Effect toward the ROSAT Cluster RX J0658-5557

Details The Enhancement and Decrement of the Sunyaev-Zeldovich Effect toward the ROSAT Cluster RX J0658-5557 The Enhancement and Decrement of the Sunyaev-Zeldovich Effect toward the ROSAT Cluster RX J0658-5557

Mar 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999apj...513...23a&link_type=abstract

The Astrophysical Journal, Volume 513, Issue 1, pp. 23-33.

Astronomy and Astrophysics

Astronomy

21

Cosmology: Cosmic Microwave Background, Cosmology: Observations, Cosmology: Distance Scale, Galaxies: Clusters: Individual (Rx J0658-5557), X-Rays: Galaxies

Scientific paper

We report simultaneous observations of the X-ray cluster RX J0658-5557 at 1.2 and 2 mm made with a double-channel photometer on the Swedish ESO Submillimeter Telescope (SEST) in search of Sunyaev-Zeldovich (SZ) effect. The SZ data were analyzed using the relativistically correct expression for the Comptonization, and we find (2.60+/-0.79)x10^-4 from the detected decrement, which is consistent with that computed using the X-ray (ROSAT and ASCA) observations. The uncertainty includes contributions from statistical uncertainties in the detection, systematics, and calibration. The 1.2 mm channel data alone give rise to a larger Comptonization parameter; this result is discussed in terms of contamination from foreground sources and/or dust in the cluster or from a possible systematic effect. We then make use of a combined analysis of the ROSAT and ASCA X-ray satellite observations to determine an isothermal model for the SZ surface brightness. Since the cluster is asymmetrical and probably in a merging process, models are only approximate. The associated uncertainty can, however, be estimated by exploring a set of alternative models. We then find a factor of 1.3 for the global uncertainty on the Comptonization parameter. Combining the SZ and the X-ray measurements, we determine a value for the Hubble constant. The 2 mm data are consistent with H_0(q_0=1/2)=53^+38_-28 km s^-1 Mpc^-1, where the uncertainty is dominated by the uncertainty in the models of the X-ray plasma halo.

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