Other
Scientific paper
Dec 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998phdt.........1d&link_type=abstract
Thesis (PHD). CORNELL UNIVERSITY , Source DAI-B 59/06, p. 2802, Dec 1998, 279 pages.
Other
6
Galaxy Clusters, Peculiar Velocities
Scientific paper
We have compiled Tully-Fisher (TF) measurements for 522 late-type galaxies in the fields of 52 rich Abell clusters distributed throughout the sky between ~50 and 200h-1 Mpc. Galaxy fluxes and rotational velocity widths are determined from I band photometry and optical rotation curves, with the latter data supplemented by H scI profiles. The data are applied to the construction of an I band TF template, resulting in a relation with a kinematical zero-point accurate to 0.02 magnitudes. Individual cluster TF relations are referred to the template to compute cluster peculiar motions. The line-of-sight dispersion in the peculiar motions is 341 ± 43 km s-1. The reflex motion of our Local Group of galaxies is measured with respect to the reference frame defined by our cluster sample and the distant portion of the Giovanelli et al. (1998a) cluster set. We find the Local Group motion in this frame to be 564 ± 113 km s-1 in the direction (l,b)=(267o,26o) ± 11o when peculiar velocities are weighted according to their errors. After optimizing the dipole calculation to sample equal volumes fairly, the vector is 499 ± 217 km s-1 towards (256o,45o)±36o. Both solutions agree, at the 1/sigma level or better, with the best estimates for the Local Group motion in the CMB frame. In other words, the cluster sample as a whole moves slowly in the CMB reference frame; the bulk flow of the cluster frame is at most ~200 km s-1. In contrast to recent claims, our results suggest that the bulk of the local peculiar motion stems from relatively nearby mass inhomogeneities. Finally, we apply the combined sample of our peculiar velocities and the 24 peculiar velocities from Giovanelli et al. (1998a) to a test of the putative Hubble bubble recently claimed by Zehavi and coworkers. In contrast to their findings, our data supports a relatively quiescent Hubble flow beyond ~30h-1 Mpc.
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