Bent-double radio sources as tracers of clusters of galaxies

Details Bent-double radio sources as tracers of clusters of galaxies Bent-double radio sources as tracers of clusters of galaxies

Jun 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000phdt........13b&link_type=abstract

Thesis (PhD). COLUMBIA UNIVERSITY, Source DAI-B 60/12, p. 6149, Jun 2000, 142 pages.

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An imaging and spectroscopic study of 384 bent-double radio sources selected from the VLA FIRST survey is presented. In most models, the bending of these sources' lobes is a result of interaction with a dense intra-cluster medium (ICM) in which the host galaxies are embedded. Therefore, these types of radio objects should act as tracers of clusters of galaxies. We find that ~60% of the bent doubles are located in cluster environments with Abell richness class 0 or greater. The remaining 40% are found in groups (some of them poor). We discuss possible scenarios that could produce bent doubles in these surroundings. Several radio and optical properties of the bent doubles and their environments are examined for possible correlations. The results are consistent with similar studies done for radio sources found in Abell clusters. Several moderate-to-high-z bent double sources are studied in detail, and spectro-copy confirms them to be associated with rich clusters. These clusters represent the most distant clusters known that are associated with wide-angle-tail (WAT) radio sources. The WAT morphology is the most common one in our sample; these sources are high-power FR Is with large linear extents and opening angles and are usually found to be associated with cD galaxies in the cores of clusters. In Chapter 1, we review other cluster searches and discuss different radio source morphologies. The sample selection techniques and radio properties of the 384 bent doubles are presented in Chapter 2. The following three chapters are arranged in order of redshift: a complete, mostly low-redshift sample of bent doubles is studied in Chapter 3, a moderate-to-high redshift sample is presented in Chapter 4, and a high-redshift object is examined in Chapter 5. We conclude (Chapter 6) with a summary of our results and prospects for the future.

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