Progress report, submitted December 5, 2002 by Jacqueline van Gorkom


AG 592:        An HI Survey of Clusters in the Local Universe

  
     The scientific goals of this project are as follows:

     1) To study galaxy evolution as a function of environment
     2) To study the assembly of clusters of galaxies and constrain some
          cosmological parameters


The survey proposal aims at getting complete HI imaging data for 12 clusters
covering a range of redshifts from 0 to 0.2. Combined with deep optical
multi color imaging and spectroscopy, this will give the most
complete information yet on the evolution of galaxies in the local
universe. Each cluster will be mosaiced out to two Abell radii, thus allowing
us to probe simultaneously the low density outer parts and dense cluster 
cores. The clusters are in apparently varying degrees of dynamical 
relaxedness, some contain starburst and some post starburst galaxies, all
have a central X ray source. 


The survey team: Jacqueline van Gorkom, Hector Bravo-Alfaro, K. Dwarakanath,
Puragra Guhathakurta, Bianca Poggianti, David Schiminovich, Monica Valluri,
Marc Verheijen, Eric Wilcots, Ann Zabludoff.




Clusters that have been done as part of the survey:

name        redshift  area covered   velocity range covered     line cube   
                        Mpc x Mpc          km/s                rms mJy/beam
                        (H0=100)

Abell   85    0.055     5.0 x 4.3         3720                    0.24
Abell  496    0.033     3.2 x 2.2         2300                    0.20
Abell  754    0.055     2.0 x 1.5         2500                    0.20
Abell 2192    0.188     5.2 x 5.2         2500                    0.033     

Clusters with similar data, that will be included in the analysis:

Abell 1060    0.011     1.8 x 1.2         3000                    0.4-0.6
Abell 2670    0.076     4.9 x 1.9         4122                    0.16


Current observational status

Data for A85, A754 and A2192 were taken in 2000 (not as survey) and 2001. 
The data have been fully reduced. In this current C array a mosaic is made 
of A496 and missing or bad data on A85 and A754 are filled in and replaced.