Issue |
A&A
Volume 388, Number 2, June III 2002
|
|
---|---|---|
Page(s) | 732 - 740 | |
Section | Numerical methods and codes | |
DOI | https://doi.org/10.1051/0004-6361:20020538 | |
Published online | 31 May 2002 |
Cluster detection from surface-brightness fluctuations in SDSS data
Max-Planck-Institut für Astrophysik, PO Box 1317, 85741 Garching, Germany
Corresponding author: M. Bartelmann, nsb@npa-garching.npg.de
Received:
9
November
2001
Accepted:
4
April
2002
Galaxy clusters can be detected as surface brightness enhancements
in smoothed optical surveys. This method does not require
individual galaxies to be identifiable, and enables clusters to be
detected out to surprisingly high redshifts, as recently
demonstrated by the Las Campanas Distant Cluster Survey
(LCDCS). Here, we investigate redshift limits for cluster detection
in the Sloan Digital Sky Survey (SDSS). Calibrating assumptions
about the surface brightness profile, the mass-to-light ratio, and
the spectral energy distribution of galaxy clusters using available
observational data, we show that it should be possible to detect
galaxy groups out to redshifts of ~0.5, and massive galaxy
clusters out to redshifts of ~1.2 in summed SDSS
data. Redshift estimates can be derived from the SDSS magnitudes of
brightest cluster members out to redshifts near unity. Over the
area of sky it covers, SDSS should find
of the clusters
detectable by the Planck satellite through the thermal
Sunyaev-Zel'dovich effect. The few Planck clusters not
detected in SDSS will almost all be at
.
Key words: methods: data analysis / techniques: image processing / surveys / galaxies: clusters: general / cosmology: observations
© ESO, 2002
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