Studies of scaling relations in groups and clusters of galaxies have shown that the X-ray properties of groups deviate the most from the self-similar prediction. This is because groups are more affected by non-gravitational processes due to their shallower potential well, a behaviour which makes groups an ideal class of systems for the study of the impact of feedback. From the observational point of view, the study of the X-ray properties of groups, especially at high redshifts is hindered by their lower surface brightness compared to their more massive counterparts. We present the result from the Chandra Deep Group Survey, a survey dedicated to find high redshift groups in the deepest observations available in the Chandra archive. We found 26 groups and 36 clusters with available redshifts, with largest redshift being 1.3. We have used this sample to investigate the evolution of cool cores in these two classes of systems using cooling time divided by the age of the cluster as a parameter to describe the cooling state. We have found that groups and clusters have similar evolution in their cool core properties. Both classes of systems have a wide spread in the cool core parameter at low redshifts, which then narrows at high redshifts showing a lack of strong cool core systems.
|Advisor:||Smith, Graham P.|
|School:||University of Birmingham (United Kingdom)|
|Department:||School of Physics and Astronomy|
|Source:||DAI-B 78/09(E), Dissertation Abstracts International|
|Keywords:||Chandra groups evolution, Chandra survey, Galaxy clusters, Galaxy groups, High energy astronomy, X-ray astronomy|
Copyright in each Dissertation and Thesis is retained by the author. All Rights Reserved
The supplemental file or files you are about to download were provided to ProQuest by the author as part of a
dissertation or thesis. The supplemental files are provided "AS IS" without warranty. ProQuest is not responsible for the
content, format or impact on the supplemental file(s) on our system. in some cases, the file type may be unknown or
may be a .exe file. We recommend caution as you open such files.
Copyright of the original materials contained in the supplemental file is retained by the author and your access to the
supplemental files is subject to the ProQuest Terms and Conditions of use.
Depending on the size of the file(s) you are downloading, the system may take some time to download them. Please be