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Date and Time of the Query: 2018-10-22 T20:58:08 PDT
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For refcode 1992ApJ...398..441S:
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Copyright by American Astronomical Society. Reproduced by permission
1992ApJ...398..441S A STUDY OF THE VELOCITY FIELD IN THE LOCAL SUPERCLUSTER BASED ON A NEW PECULIAR-VELOCITY SAMPLE KAZUHIRO SHIMASAKU AND SADANORI OKAMURA Department of Astronomy, Faculty of Science, University of Tokyo, Bunkyo- ku, Tokyo 113, Japan Received 1991 November 11; accepted 1992 April 24 ABSTRACT We study the velocity field in the Local Supercluster (LS) on the basis of a newly compiled data set of peculiar velocities of 306 spiral galaxies as well as two well-known samples by Aaronson et al. (194 spirals) and by Faber et al. (400 ellipticals). Our sample is the largest one of spiral galaxies available at present with distance estimates as good as those for the sample of Aaronson et al. Galaxy distances in our sample are determined in this study using the Tully-Fisher relation. We apply to our sample and Aaronson et al.'s sample a slightly simplified version of the standard Great Attractor (GA) model and determine the model parameters by the identical procedures. These parameters are compared with those obtained by Faber & Burstein from the sample of Faber et al. using the standard GA model. We find a broad agreement in the model parameters. However, the direction of the GA is different by at most 26^deg^ among the three samples. The difference is significant in terms of the Local Anomaly, which is the perturbation in the nearby velocity field introduced in the standard GA model in order to explain the discrepancy between the observed and the predicted velocities of the Local Group (LG) with respect to the cosmic microwave background (CMB). The direction of the GA obtained from our sample is different from the direction of the LG motion with respect to the CMB by only 13^deg^ while the difference amounts to 37^deg^ and 38^deg^ for the samples of Aaronson et al. and Faber et al., respectively. Thus, the observed and the predicted motions of the LG agree reasonably well in our sample, unlike the other samples. This suggests that it is not necessary to invoke the Local Anomaly. Since the velocity field obtained from the three samples are consistent in the common region, the difference of the GA parameters is probably due to the difference of the sampling regions. This indicates that the standard GA model is too simple to delineate the detailed local peculiar velocity field and to discuss whether the Local Anomaly exists or not. Subject headings: galaxies: mustering - galaxies: distances and redshifts
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