Redshifts and Arp-like Configurations in the Local Group

Abstract

It is shown that each of the geometrically defined "lines" (subgroups) of galaxies in the Local Group of galaxies (considered by Iwanowska) contains members of various redshifts. In each line, however, we can distinguish members of quasi-dis­ crete "quantized" redshift states. The so-called "possible" members of LG are real members of LG, according to the criterion developed in present paper. The redshift state of our Galaxy is represented by k = -1. I. Velocity Dispersion sn-t in the Local Group 1. All Galaxies in lwanowska Lines We consider all galaxies classified by Iwanowska (1989) as members of Arp­ like lines contained in the Local Group (LG). The mean residual velocity of all galaxies listed by Iwanowska is v=60±84{sn_1), n=37, (s~v) (1) It is evident that the dispersion sLG,n-1 (all velocities are given in km s-1) is higher than the mean velocity itself. Here, n is the total number of galaxies forming all the lwanowska's line configurations (resembling Arp configurations). Let the velocity dispersion sn_1 be denoted simply as s. The Local Group dispersions is comparable with the dispersion of the Virgo ellipticals (E+SO) inves­ tigated, among others, by Sulentic (1977), although the Local Group and Virgo Cluster are not comparable with respect to number of members. Hence the follow­ ing question arises: Is the high value of dispersion sLG a subclustering effect (caused by the existence of galaxy subgroups)? Furthermore, will it be possible to reduce this high value of sLG by dividing it into subgroups? For this purpose, we consider a division of the Local Group into its two most natural parts: the M31 galaxy system and the system our Galaxy. Afterwards, we will also investigate the subgroups distinguished by Iwanowska. To ensure the