Sunyaev-Zel'dovich observations of a statistically complete sample of galaxy clusters with OCRA-p

We present 30-GHz Sunyaev-Zel'dovich (SZ) observations of a statistically complete sample of galaxy clusters with the One Centimetre Receiver Array-prototype (OCRA-p). The clusters are the 18 most X-ray luminous clusters at z > 0.2 in the ROSAT Brightest Cluster Sample. We correct for contam...

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Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society 2011-12, Vol.418 (3), p.1441-1451
Main Authors: Lancaster, Katy, Birkinshaw, Mark, Gawroński, Marcin P., Battye, Richard, Browne, Ian, Davis, Richard, Giles, Paul, Feiler, Roman, Kus, Andrzej, Lew, Bartosz, Lowe, Stuart, Maughan, Ben, Alareedh, Abdulaziz, Pazderska, Bogna, Pazderski, Eugeniusz, Peel, Mike, Roukema, Boudewijn F., Wilkinson, Peter
Format: Article
Language:English
Subjects:
Astronomy
cosmology: observations
Earth, ocean, space
Exact sciences and technology
galaxies: clusters: general
methods: observational
Radio astronomy
Radio telescopes
Stars & galaxies
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Summary:We present 30-GHz Sunyaev-Zel'dovich (SZ) observations of a statistically complete sample of galaxy clusters with the One Centimetre Receiver Array-prototype (OCRA-p). The clusters are the 18 most X-ray luminous clusters at z > 0.2 in the ROSAT Brightest Cluster Sample. We correct for contaminant radio sources via supplementary observations with the Green Bank Telescope, also at 30 GHz, and remove a cluster that is contaminated by an unresolved X-ray source. All 17 remaining clusters have central SZ effects with Comptonization parameter y 0 exceeding 1.9 × 10−4, and 13 are detected at significance ≥3σ. We use our data to examine scalings between y 0 and X-ray temperature, X-ray luminosity and the X-ray mass proxy Y X, and find good agreement with predictions from self-similar models of cluster formation, with an intrinsic scatter in y 0 of about 25 per cent. We also comment on the success of the observations in the face of the contaminant source population, and the implications for upcoming cm-wave surveys.
ISSN:0035-8711
1365-2966
DOI:10.1111/j.1365-2966.2011.19241.x