The Role of Environment in Galaxy Evolution in the SERVS Survey. I. Density Maps and Cluster Candidates
Creators
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1.
Tufts University
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National Radio Astronomy Observatory
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National Academies of Sciences, Engineering, and Medicine
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University of Hawaii at Manoa
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California Institute of Technology
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University of Sussex
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Leiden University
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Liverpool John Moores University
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University of Portsmouth
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International Centre for Radio Astronomy Research
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Centre of Excellence for All-Sky Astrophysics
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University of Copenhagen
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Instituto de Astrofísica de Canarias
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University of La Laguna
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University of the Western Cape
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Istituto di Radioastronomia di Bologna
Abstract
We use photometric redshifts derived from new u-band through 4.5 μm Spitzer IRAC photometry in the 4.8 deg² of the XMM-LSS field to construct surface density maps in the redshift range of 0.1–1.5. Our density maps show evidence for large-scale structure in the form of filaments spanning several tens of megaparsecs. Using these maps, we identify 339 overdensities that our simulated light-cone analysis suggests are likely associated with dark matter halos with masses, M_(halo), log(M_(halo)/M_⊙) > 13.7. From this list of overdensities we recover 43 of 70 known X-ray-detected and spectroscopically confirmed clusters. The missing X-ray clusters are largely at lower redshifts and lower masses than our target log(M_(halo)/M_⊙) > 13.7. The bulk of the overdensities are compact, but a quarter show extended morphologies that include likely projection effects, clusters embedded in apparent filaments, and at least one potential cluster merger (at z ~ 1.28). The strongest overdensity in our highest-redshift slice (at z ~ 1.5) shows a compact red galaxy core, potentially implying a massive evolved cluster.
Additional Information
© 2020. The American Astronomical Society. Received 2019 June 19; revised 2019 November 8; accepted 2019 November 18; published 2020 February 5. The authors acknowledge useful discussions with Rachel Bezanson, Frank van den Bosch, and Eric Gawiser that helped guide our analysis. The authors especially thank Ryan Cybulski for providing his Voronoi Tesselation idl code, which N.K. translated into python and has used for this project. B.D. acknowledges financial support from the National Science Foundation, grant No. 1716907.Attached Files
Published - Krefting_2020_ApJ_889_185.pdf
Accepted Version - 1912.02238.pdf
Files
1912.02238.pdf
Additional details
Identifiers
- Eprint ID
- 101167
- Resolver ID
- CaltechAUTHORS:20200206-125057334
Related works
- Describes
- https://arxiv.org/abs/1912.02238 (URL)
Funding
- NSF
- AST-1716907
Dates
- Created
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2020-02-07Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field