| DOI | Resolve DOI: https://doi.org/10.1088/0004-637X/765/2/117 |
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| Author | Search for: Erfanianfar, G.; Search for: Finoguenov, A.; Search for: Tanaka, M.; Search for: Lerchster, M.; Search for: Nandra, K.; Search for: Laird, E.; Search for: Connelly, J. L.; Search for: Bielby, R.; Search for: Mirkazemi, M.; Search for: Faber, S. M.; Search for: Kocevski, D.; Search for: Cooper, M.; Search for: Newman, J. A.; Search for: Jeltema, T.; Search for: Coil, A. L.; Search for: Brimioulle, F.; Search for: Davis, M.; Search for: McCracken, H. J.; Search for: Willmer, C.; Search for: Gerke, B.; Search for: Cappelluti, N.; Search for: Gwyn, S.1 |
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| Affiliation | - National Research Council of Canada. National Science Infrastructure
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| Format | Text, Article |
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| Abstract | We present the results of a search for extended X-ray sources and their corresponding galaxy groups from 800 ks Chandra coverage of the All-wavelength Extended Groth Strip International Survey (AEGIS). This yields one of the largest X-ray-selected galaxy group catalogs from a blind survey to date. The red-sequence technique and spectroscopic redshifts allow us to identify 100% of reliable sources, leading to a catalog of 52 galaxy groups. These groups span the redshift range z ∼ 0.066-1.544 and virial mass range M200 ∼ 1.34 × 10¹³-1.33 × 10¹⁴4. For the 49 extended sources that lie within DEEP2 and DEEP3 Galaxy Redshift Survey coverage, we identify spectroscopic counterparts and determine velocity dispersions. We select member galaxies by applying different cuts along the line of sight or in projected spatial coordinates. A constant cut along the line of sight can cause a large scatter in scaling relations in low-mass or high-mass systems depending on the size of the cut. A velocity-dispersion-based virial radius can cause a larger overestimation of velocity dispersion in comparison to an X-ray-based virial radius for low-mass systems. There is no significant difference between these two radial cuts for more massive systems. Independent of radial cut, an overestimation of velocity dispersion can be created in the case of the existence of significant substructure and compactness in X-ray emission, which mostly occur in low-mass systems. We also present a comparison between X-ray galaxy groups and optical galaxy groups detected using the Voronoi-Delaunay method for DEEP2 data in this field. © 2013. The American Astronomical Society. All rights reserved. |
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| Publication date | 2013-02-26 |
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| In | |
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| Language | English |
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| Peer reviewed | Yes |
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| NPARC number | 21271778 |
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| Export citation | Export as RIS |
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| Report a correction | Report a correction (opens in a new tab) |
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| Record identifier | 953cb7ce-64dc-4097-88c5-ae8b7c33d53f |
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| Record created | 2014-04-17 |
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| Record modified | 2020-04-22 |
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