The Red-Sequence Cluster Survey. I. The Survey and Cluster Catalogs for Patches RCS 0926+37 and RCS 1327+29

By M. Gladders, H. Yee. 2004

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The Red-Sequence Cluster Survey (RCS) is a ~100 deg2, two-filter imaging survey in the RC and z′ filters, designed primarily to locate and characterize galaxy clusters to redshifts as high as z = 1.4. This paper provides a detailed description of the survey strategy and execution, including a thorough discussion of the photometric and astrometric calibration of the survey data. The data are shown to be calibrated to a typical photometric uncertainty of 0.03-0.05 mag, with total astrometric uncertainties less than 0.″25 for most objects. We also provide a detailed discussion of the adaptation of a previously described cluster search algorithm (the cluster red-sequence method) to the vagaries of real survey data, with particular attention to techniques for accounting for subtle variations in survey depths caused by changes in seeing and sky brightness and transparency. A first catalog of RCS clusters is also presented, for the survey patches RCS 0926+37 and RCS 1327+29. These catalogs, representing about 10% of the total survey and comprising a total of 429 candidate clusters and groups, contain a total of 67 cluster candidates at a photometric redshift of 0.9 < z < 1.4, down to the chosen significance threshold of 3.29 σ.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/baa6163361975117c4ae7e7e28d4590b6455b9ae

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Citations in the corpus

On the efficiency and reliability of cluster mass estimates based on member galaxies (2006, methodology): “…clusters (Dalton et al. 1992; Lumsden et al. 1992; Lopes et al. 2004), and much more sophisticated algorithms than Abell’s (1958) have been applied for extracting the 2-dimensional signal produced by a galaxy overdensity (e.g. Ramella et al. 2001; Gladders & Yee 2005, and references therein).”
ANCIENT LIGHT FROM YOUNG COSMIC CITIES: PHYSICAL AND OBSERVATIONAL SIGNATURES OF GALAXY PROTO-CLUSTERS (2013, background): “…massive clusters are found atz< 1 (e.g., Ebeling et al. 2001; Olsen et al. 2007; Foley et al. 2011; Menanteau et al. 2012), at 1< z< 1.5 (e.g., Gladders & Yee 2005; Goto et al. 2008; Wilson et al. 2009; Fassbender et al. 2011a) andz & 1.5 (e.g., Henry et al. 2010; Tanaka et al. 2010; Santos…”
GALAXY CLUSTERS IDENTIFIED FROM THE SDSS DR6 AND THEIR PROPERTIES (2009, methodology): “To reduce projection effect, several methods have been developed to search for clusters in multicolor photometric data and have been successfully used to the Red-Sequence Cluster Survey (Gladders & Yee 2000, 2005) and the SDSS (Goto et al. 2002a; Miller et al. 2005; Koester et al. 2007a).”
THE GEMINI CLUSTER ASTROPHYSICS SPECTROSCOPIC SURVEY (GCLASS): THE ROLE OF ENVIRONMENT AND SELF-REGULATION IN GALAXY EVOLUTION AT z ∼ 1 (2011, methodology): “The SpARCS cluster detection algorithm is a slightly modified version of the Gladders & Yee (2000, 2005) algorithm and is discussed in Muzzin et al. (2008).”
GRAVITATIONAL LENS MODELS BASED ON SUBMILLIMETER ARRAY IMAGING OF HERSCHEL-SELECTED STRONGLY LENSED SUB-MILLIMETER GALAXIES AT z > 1.5 (2013, background): “However, it should be noted that there are two nearby clusters detected in the Red-Sequence Cluster (RSC) survey (RCS J132427+2845.2 at z = 0.997±0.017 and RCS J132419+2844.7 at z = 0.802± 0.018 Gladders & Yee 2005).”
Measurement of Galaxy Cluster Sizes, Radial Profiles, and Luminosity Functions from SDSS Photometric Data (2004, methodology): “As galaxy surveys increase in area, it becomes feasible to measure the background counts directly from the general field, as done by Gladders & Yee (2005).”
THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. V. IMPROVING THE DARK-ENERGY CONSTRAINTS ABOVE z > 1 AND BUILDING AN EARLY-TYPE-HOSTED SUPERNOVA SAMPLE (2011, methodology): “…on HST. Clusters were selected from the IRAC Shallow Cluster Survey (Eisenhardt et al. 2008), the Red-Sequence Cluster Surveys (RCS and RCS-2, Gladders & Yee 2005; Gilbank et al. 2010), the XMM Cluster Survey (Sahlén et al. 2009), the Palomar Distant Cluster Survey (Postman et al. 1996),…”
The GALEX Ultraviolet Atlas of Nearby Galaxies (2006, background): “A similar behavior is seen when optical or optical-NIR colors are used, both locally and at high redshift (Gladders & Yee 2005).”
The X-Ray Luminosity-Mass Relation for Local Clusters of Galaxies (2006, background): “…are currently known, the number will grow considerably in the next five years, as a result of improved search techniques using multi-band optical (Gladders & Yee 2005) combined with infrared (Stanford et al. 2005) or X-ray (Rosati et al. 1998; Romer et al. 2000; Mullis et al. 2005) imaging.”
Virial Masses and the Baryon Fraction in Galaxies (2005, methodology): “The Red-Sequence Cluster Survey (RCS) is a galaxy cluster survey designed to provide a large sample of optically selected clusters of galaxies in a large volume (see Gladders & Yee (2005) for a detailed discussion of the survey).”
A GMBCG GALAXY CLUSTER CATALOG OF 55,424 RICH CLUSTERS FROM SDSS DR7 (2010, methodology): “…constraints from optically selected galaxy clusters have been carried out recently by Gladders et al. (2007) based on the RCS cluster catalog (Gladders & Yee 2005a), by Rozo et al. (2007b,a, 2010), based on the maxBCG catalog (Koester et al. 2007a,b) and by Wen et al. (2010) based on a…”
EVOLUTION OF GALAXIES AND THEIR ENVIRONMENTS AT z = 0.1–3 IN COSMOS (2013, unknown): “…line-of-sight discrimination is usually accomplished using: 1) color selection (e.g. using broadband colors to select red sequence galaxies, Gladders & Yee 2005); 2) spectroscopic redshifts (in COSMOS e.g., Kovač et al. 2010; Peng et al. 2010) and 3) photometric redshifts derived from…”
The XMM Cluster Survey:Optical analysis methodology and the first data release (2011, methodology): “…composite red-sequence of 73 clusters at z ∼ 0.1 detected by the SDSS-C4 survey (Miller et al. 2005), which is then evolved with redshift using the Bruzual & Charlot (2003) population synthesis models assuming a single-burst Salpeter IMF with a formation redshift of zf = 2.5 (Gladders & Yee 2005).”
A MaxBCG Catalog of 13,823 Galaxy Clusters from the Sloan Digital Sky Survey (2007, background): “This tight clustering of galaxies in color, magnitude, and space allows significant improvements in cluster finding (Ostrander et al. 1998; Gladders & Yee 2000; Bahcall et al. 2003; Gladders & Yee 2005).”
THE PRISM MULTI-OBJECT SURVEY (PRIMUS). I. SURVEY OVERVIEW AND CHARACTERISTICS (2010, background): “…redshifts are commonly used to fill this gap and have become popular because they are much easier to acquire and therefore can be done for much larger data sets (e.g., Budavari et al. 2003; Mobasher et al. 2004; Padmanabhan et al. 2005; Gladders & Yee 2005; Pelló et al. 2009; Adami et al. 2010).”
The realm of the galaxy protoclusters (2016, methodology): “The pioneering work on the Red Sequence Cluster Survey (RCS) by Gladders & Yee (2000, 2005), and its successor, RCS-2 (Gilbank et al., 2011), showed that large samples of clusters can be efficiently selected out to z ≈ 1 by making use of standard optical filters combined with the z-band to pinpoint…”
STELLAR MASSES FROM THE CANDELS SURVEY: THE GOODS-SOUTH AND UDS FIELDS (2014, methodology): “…et al. The Astrophysical Journal, 801:97 (17pp), 2015 March 10 Santini et al. with IMACS as part of the Arizona CDFS Environment Survey (Cooper et al. 2012c) and as part of the spectroscopic followup of the Red-Sequence Cluster Survey (RCS; Gladders & Yee 2005, zRCS; R. Yan et al., in preparation).”
A WEAK LENSING STUDY OF X-RAY GROUPS IN THE COSMOS SURVEY: FORM AND EVOLUTION OF THE MASS–LUMINOSITY RELATION (2009, methodology): “At present, there are five popular methods for detecting groups and clusters of galaxies: a) optical detection via the red-sequence (e.g. Gladders & Yee 2005; Koester et al. 2007), b) detection via the Sunyaev-Zeldovich (SZ) effect which measures the distortion of the CMB spectrum due to the hot…”