Показать сокращенную информацию
dc.contributor.author | Perrott Y. | |
dc.contributor.author | Olamaie M. | |
dc.contributor.author | Rumsey C. | |
dc.contributor.author | Brown M. | |
dc.contributor.author | Feroz F. | |
dc.contributor.author | Grainge K. | |
dc.contributor.author | Hobson M. | |
dc.contributor.author | Lasenby A. | |
dc.contributor.author | MacTavish C. | |
dc.contributor.author | Pooley G. | |
dc.contributor.author | Saunders R. | |
dc.contributor.author | Schammel M. | |
dc.contributor.author | Scott P. | |
dc.contributor.author | Shimwell T. | |
dc.contributor.author | Titterington D. | |
dc.contributor.author | Waldram E. | |
dc.contributor.author | Aghanim N. | |
dc.contributor.author | Arnaud M. | |
dc.contributor.author | Ashdown M. | |
dc.contributor.author | Aussel H. | |
dc.contributor.author | Barrena R. | |
dc.contributor.author | Bikmaev I. | |
dc.contributor.author | Böhringer H. | |
dc.contributor.author | Burenin R. | |
dc.contributor.author | Carvalho P. | |
dc.contributor.author | Chon G. | |
dc.contributor.author | Comis B. | |
dc.contributor.author | Dahle H. | |
dc.contributor.author | Democles J. | |
dc.contributor.author | Douspis M. | |
dc.contributor.author | Harrison D. | |
dc.contributor.author | Hempel A. | |
dc.contributor.author | Hurier G. | |
dc.contributor.author | Khamitov I. | |
dc.contributor.author | Kneissl R. | |
dc.contributor.author | MacÍas-Pérez J. | |
dc.contributor.author | Melin J. | |
dc.contributor.author | Pointecouteau E. | |
dc.contributor.author | Pratt G. | |
dc.contributor.author | Rubiño-Martín J. | |
dc.contributor.author | Stolyarov V. | |
dc.contributor.author | Sutton D. | |
dc.date.accessioned | 2018-09-18T20:01:50Z | |
dc.date.available | 2018-09-18T20:01:50Z | |
dc.date.issued | 2015 | |
dc.identifier.issn | 0004-6361 | |
dc.identifier.uri | https://dspace.kpfu.ru/xmlui/handle/net/135887 | |
dc.description.abstract | © 2015 ESO. We present observations and analysis of a sample of 123 galaxy clusters from the 2013 Planck catalogue of Sunyaev-Zel'dovich sources with the Arcminute Microkelvin Imager (AMI), a ground-based radio interferometer. AMI provides an independent measurement with higher angular resolution, 3 arcmin compared to the Planck beams of 5-10 arcmin. The AMI observations thus provide validation of the cluster detections, improved positional estimates, and a consistency check on the fitted size (θ<inf>s</inf>) and flux (Y<inf>tot</inf>) parameters in the generalised Navarro, Frenk and White (GNFW) model. We detect 99 of the clusters. We use the AMI positional estimates to check the positional estimates and error-bars produced by the Planck algorithms PowellSnakes and MMF3. We find that Y<inf>tot</inf> values as measured by AMI are biased downwards with respect to the Planck constraints, especially for high Planck-S/N clusters. We perform simulations to show that this can be explained by deviation from the universal pressure profile shape used to model the clusters. We show that AMI data can constrain the α and β parameters describing the shape of the profile in the GNFW model for individual clusters provided careful attention is paid to the degeneracies between parameters, but one requires information on a wider range of angular scales than are present in AMI data alone to correctly constrain all parameters simultaneously. | |
dc.relation.ispartofseries | Astronomy and Astrophysics | |
dc.subject | Cosmic background radiation | |
dc.subject | Cosmology: observations | |
dc.subject | Galaxies: clusters: general | |
dc.subject | Galaxies: clusters: intracluster medium | |
dc.subject | X-rays: galaxies: clusters | |
dc.title | Comparison of Sunyaev-Zel'dovich measurements from Planck and from the Arcminute Microkelvin Imager for 99 galaxy clusters | |
dc.type | Article | |
dc.relation.ispartofseries-volume | 580 | |
dc.collection | Публикации сотрудников КФУ | |
dc.source.id | SCOPUS00046361-2015-580-SID84938946603 |