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The dynamics and structure of rich clusters of galaxies. I - Velocity data
An extensive spectroscopic study of 10 rich southern X-ray clusters ofgalaxies is presented. Between 40 and 200 redshifts have been obtainedin the field of each of the clusters, which cover a wide range ofmorphological types and richnesses. Applying rigorous statisticalanalyses to the total data base of 1000 precise radial velocitiesprovides the necessary information to undertake a thorough dynamicalinvestigation of these individual clusters and of cluster systems ingeneral.
| The HEAO A-1 all-sky survey of fast X-ray transients
Ten fast X-ray transient sources were discovered in the first completepass of the sky by the HEAO A-1 Sky Survey Experiment, including 7relatively faint sources and 3 bright ones. The survey technique andeach of the transients are described. Four of the transients areidentified with active coronal sources; the remaining ones areunidentified. The statistical properties of the total sample of 10sources are discussed, including event rates, distribution on the sky,and the number-flux distribution.
| Sense of rotation in 109 spirals, and the leading arms in the interacting galaxies NGC 3786 and NGC 5426
From analysis of 132 spiral galaxies, designed to determine the sense ofwinding of the arms, 107 are reliably found to have trailing arms, buttwo others, NGC 3786 (paired with the spiral NGC 3788) and NGC 5426(paired with NGC 5427), have leading arms. The sample of galaxies havinga well-established sense of spiral rotation now totals 190; the arms areleading in only four of these, all objects interacting dynamically withcompanion galaxies. A mechanism that might have induced such leadingspiral patterns is suggested and discussed.
| Southern Galaxy Catalogue.
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| A catalog of morphological types in 55 rich clusters of galaxies
Data are presented from a study of 55 rich clusters of galaxies. Thedata include positions, morphological types, estimated total magnitudes,bulge sizes, and ellipticities for about 6000 galaxies, as determinedfrom high scale photographic plates. Data reduction procedures aredescribed, and a brief analysis of cluster richness, which indicatesthat Abell richness classes are only rough indicators of total clustermembership, is included.
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