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P. I. Choi (Univ. of California, Santa Cruz), A. H. Gonzalez (Harvard-Smithsonian Center for Astrophysics)
We present preliminary results from our program to observe the integrated HI profiles for a sample of 52 galaxy clusters at 0.12 < z < 0.26. Our initial observations of a subset of 12 systems, demonstrate the feasibility of measuring both HI and total cluster masses with the Gregorian receiver at Arecibo. The initial sample, selected to contain systems with existing X-ray data, can be used to test the robustness of virial HI masses. Further, we aim to use the derived HI masses in conjunction with published optical and X-ray data to better constrain the relationship between cluster environment, the HI reservoir, and star formation rate.
This poster represents a first look at evolution in the global HI content at intermediate redshift, as HI observations of clusters in this redshift range were not possible prior to the Gregorian upgrade at Arecibo. For this study we utilize the L-wide receiver in conjunction with the Category B 1120-1265 MHz bandpass filter, which permits us to probe out to z=0.26. To measure the clusters out to an Abell radius (1.5h-1 Mpc, or 16\prime-10\prime in this redshift range), observations were performed in spectral-line, drift-scan mode.
The author(s) of this abstract have provided an email address for comments about the abstract: pchoi@ucolick.org