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    A Catalog of X-Ray Point Sources in the Abell 133 Region

    Access Status
    Fulltext not available
    Authors
    Shin, J.
    Plotkin, Richard
    Woo, J.
    Gallo, E.
    Mulchaey, J.
    Date
    2018
    Type
    Journal Article
    
    Metadata
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    Citation
    Shin, J. and Plotkin, R. and Woo, J. and Gallo, E. and Mulchaey, J. 2018. A Catalog of X-Ray Point Sources in the Abell 133 Region. Astrophysical Journal Supplement Series. 238: 23.
    Source Title
    Astrophysical Journal Supplement Series
    DOI
    10.3847/1538-4365/aadcb0
    ISSN
    0067-0049
    School
    Curtin Institute of Radio Astronomy (Physics)
    URI
    http://hdl.handle.net/20.500.11937/73004
    Collection
    • Curtin Research Publications
    Abstract

    © 2018. The American Astronomical Society. All rights reserved.. As an evolutionary phase of galaxies, active galactic nuclei (AGNs) over a large range of redshifts have been utilized for understanding cosmic evolution. In particular, the population and evolution of AGNs have been investigated through the study of the cosmic X-ray background in various fields. As one of the deep fields observed by Chandra, with a total of 2.8 Ms exposures, Abell 133 is a special region for investigating AGNs, providing a testbed for probing the environmental effects on AGN triggers, since cluster environments can be different from field environments. The achieved flux limits of data at the 50% completeness levels of 6.95 ×10-16, 1.43 ×10-16, and 1.57 ×10-15 erg s-1 cm-2 are 0.5-8, 0.5-2, and 2-8 keV. Using the wavdetect and no-source binomial probability (i.e., p < 0.007), we analyze the combined Chandra image, detecting 1617 (in 0.5-8 keV), 1324 (in 0.5-2 keV), and 1028 (in 2-8 keV) X-ray point sources in the Abell 133 region. Here, we present the X-ray point source catalog with the source fluxes, which can be combined with multiwavelength data for future works. We find that the number count distribution of the X-ray point sources is well reproduced with a broken power-law model, while the best-fit model parameters are sensitive to the fitting range of the number count distribution. Finally, we find an excess of number density (a decrease of AGN fraction) at the central region of the cluster, which reflects the effect of dense environments on AGN triggers, a finding similar to those of other studies of galaxy clusters.

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