J/A+A/580/A95 Planck/AMI Sunyaev-Zel'dovich measurements (Perrott+, 2015)
Comparison of Sunyaev-Zel'dovich measurements from Planck and from the
Arcminute Microkelvin Imager for 99 galaxy clusters.
Perrott Y.C., Olamaie M., Rumsey C., Brown M.L., Feroz F., Grainge K.J.B.,
Hobson M.P., Lasenby A.N., MacTavish C.J., Pooley G.G., Saunders R.D.E.,
Schammel M.P., Scott P.F., Shimwell T.W., Titterington D.J., Waldram E.M.,
Aghanim N., Arnaud M., Ashdown M., Aussel H., Barrena R., Bikmaev I.,
Boehringer H., Burenin R., Carvalho P., Chon G., Comis B., Dahle H.,
Democles J., Douspis M., Harrison D., Hempel A., Hurier G., Khamitov I.,
Kneissl R., Macias-Perez J.F., Melin J.-B., Pointecouteau E., Pratt G.W.,
Rubino-Martin J.A., Stolyarov V., Sutton D.
<Astron. Astrophys., 580, A95-95 (2015)>
=2015A&A...580A..95P 2015A&A...580A..95P (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Redshifts
Keywords: cosmology: observations - galaxies: clusters: general -
galaxies: clusters: intracluster medium -
cosmic background radiation - X-rays: galaxies: clusters
Abstract:
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, 3arcmin compared to the Planck beams of
5-10arcmin. The AMI observations thus provide validation of the
cluster detections, improved positional estimates, and a consistency
check on the fitted size (θs) and flux (Ytot) 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 Ytot 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.
Description:
Clusters are observed using a single pointing centre on the SA, which
has a primary beam of size ∼20-arcmin FWHM, to noise levels of
≤120Jy/beam. To cover the same area with the LA, which has a primary
beam of size ∼6-arcmin FWHM, the cluster field is observed as a
61-point hexagonal raster. The noise level of the raster is
100uJy/beam in the central 19 pointings, and slightly higher in the
outer regions.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 338 229 Summary of results for all clusters between
20°≤DE<87° with Planck S/N>5
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See also:
VIII/91 : Planck Catalog of Compact Sources Release 1 (Planck, 2013)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [PSZ1]
6- 18 A13 --- PSZ1 Cluster name, GLLL.ll+BB.bb
20- 24 F5.2 --- S/N Planck signal-to-noise ratio
26- 28 I3 --- Det Planck detection flags (1)
30- 31 A2 --- Cat Category (2)
33- 38 F6.2 --- Dln(Z) ? Bayesian evidence difference
40- 92 A53 --- ONames Aliase(s) (3)
94-100 A7 --- AMI References to previously published AMI
analyses (4)
102-108 F7.5 --- z ? Redshift from the Planck 2013 SZ catalogue
109-338 A230 --- Notes Notes (5)
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Note (1): Pipelines detecting the cluster (e.g. 110 indicates that the cluster
was detected by MMF3, MMF1 but not PwS).
Note (2): Detection/rejection reasons as follows:
LZ = rejected because low redshift
R = rejected by automated point-source criteria
SE = rejected manually for difficult source environment
Y = clear detection
M = moderate detection
N = non-detection
NN = clear non-detection
Note (3): Some aliases for previously-known clusters are given from:
Zwicky (1937ApJ....86..217Z 1937ApJ....86..217Z, and references therein),
Abell (1958ApJS....3..211A 1958ApJS....3..211A), Zwicky et al. (1961, Catalogue of galaxies and
of clusters of galaxies, Vol. I), Gower et al. (1967MmRAS..71...49G 1967MmRAS..71...49G),
Albert et al. (1977ApJ...211..309A 1977ApJ...211..309A), Fetisova (1981SvA....25..647F 1981SvA....25..647F),
Pravdo & Marshall (1984ApJ...281..570P 1984ApJ...281..570P), Appenzeller et al. (1998,
Cat. J/ApJS/117/319), Voges et al. (1999, Cat. IX/10), Ebeling et al.
(2001ApJ...553..668E 2001ApJ...553..668E), Ebeling et al. (2002, Cat. J/ApJ/580/774),
Wen et al. (2009, Cat. J/ApJS/183/197), Piffaretti et al. (2011,
Cat. J/A+A/534/A109, and references therein), Mehrtens et al. (2012,
Cat. J/MNRAS/423/1024), Wen et al. (2012, Cat. J/ApJS/199/34),
Planck Collaboration VIII (2011, Cat. J/A+A/536/A8).
Note (4): Reference numbers refer to previously published AMI analyses
as follows:
1 = Barker et al. (2006MNRAS.369L...1A 2006MNRAS.369L...1A)
2 = Hurley-Walker et al. (2011MNRAS.414L..75H 2011MNRAS.414L..75H)
3 = Zwart et al. (2011MNRAS.418.2754Z 2011MNRAS.418.2754Z)
4 = Hurley-Walker et al. (2012MNRAS.419.2921A 2012MNRAS.419.2921A)
5 = Rodriguez-Gonzalvez et al. (2012MNRAS.425..162R 2012MNRAS.425..162R)
6 = AP2013, Planck and AMI Collaborations, 2013A&A...550A.128P 2013A&A...550A.128P
7 = Shimwell et al. (2013MNRAS.433.2920A 2013MNRAS.433.2920A)
Note (5): For non-detections, predicted S/N ratios in the naturally-weighted
(σNW) and uv-tapered (σtap) maps are also given based on the
Planck mean posterior parameter values.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 03-Nov-2015