| Canadian
Cluster Comparison Project |
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| "A survey that is good for the masses" |
|
| Members
of the CCCP team |
The Canadian Cluster Comparison
Project (CCCP) is a study of a large sample of X-ray selected clusters
with the aim of examining the relationship between baryonic tracers of
cluster mass and to probe the cluster-to-cluster variation in the
thermal properties of the hot intracluster medium (ICM). Previous work
has been based on inhomogeneous data sets and small samples. The final
CCCP sample will be of order 60 massive X-ray selected clusters of
galaxies for which we obtained deep imaging from the
Canada-France-Hawaii Telescope (CFHT). The imaging data are used to
determine the cluster mass directly using weak gravitational lensing.
Comparison with existing X-ray and SZ data, as well as the optical
properties allows us to calibrate the various mass-tracer relations,
which is important for planned large cluster abundance studies. In
addition detailed comparison with simulations and X-ray observations
will enable us to study the physical origins of these relations and
their scatter, thus improving our knowledge of cluster formation. |
| CCCP
sample of clusters |
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| Image Gallery |
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| Members
of the CCCP team |
|
| Henk
Hoekstra |
University
of Victoria |
| Arif
Babul |
University
of Victoria |
| Michael
Balogh |
University
of Waterloo |
| Ian
McCarthy |
University
of Victoria |
| Don
Horner |
University
of Massachussetts |
| Jonathan
Sievers |
CITA,
University of Toronto |
| CCCP
sample of galaxy clusters |
| As CCCP is an ongoing project,
the sample of galaxy clusters that is studied changes over
time. Also, the sample is not clearly defined, although the
clusters in the MegaCam sample we selected to have ASCA temperatures
>5 keV. The CFH12k sample is based on a search through the CFHT
archive at CADC. Roughly half of these clusters are part of
the Canadian Network for Observational Cosmology (CNOC) sample, whereas
the other half were observed by various people. Clusters for which B
and R band data were available were selected, although some of the
low-z clusters lack color information, but were included to extend the
redshift range of the sample. The clusters (exept MS1231) have ASCA
temperatures measured, and many have been observed with new generation
X-ray telescopes such as Chandra and XMM. Some of the clusters are also
being observed using the Cosmic Background Imager (CBI) to obtain a
measure of the SZ decrement. |
| Clusters
observed with CFH12k |
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| name |
redshift |
B |
R |
CBI | |
| Abell
267 |
0.23 |
v |
v |
||
| Abell
370 |
0.375 |
v |
v |
||
| Abell
399 |
0.0718 |
v |
|||
| Abell
478 |
0.0881 |
v |
|||
| Abell
1689 |
0.1832 |
v |
v |
v |
|
| Abell
1763 |
0.223 |
v |
v |
||
| Abell
2218 |
0.1756 |
v |
v |
||
| Abell
2219 |
0.2256 |
v |
v |
||
| Abell
2390 |
0.2280 |
v |
v |
||
| MS0016+16 |
0.5465 |
v |
v |
||
| MS0906+11 |
0.1704 |
v |
v |
||
| MS1224+20 |
0.3255 |
v |
v |
||
| MS1231+15 |
0.2353 |
v |
v |
||
| MS1358+62 |
0.3290 |
v |
v |
||
| MS1455+22 |
0.2568 |
v |
v |
||
| MS1512+36 |
0.3727 |
v |
v |
||
| MS1621+26 |
0.4275 |
v |
v |
||
| CL0024+16 |
0.39 |
v |
v |
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| Clusters
(to be) observed with MegaCam |
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| name |
redshift | g' |
r' |
CBI | |
| Abell
115 |
0.20 |
2004B | |||
| Abell
223 |
0.21 |
2004B | |||
| Abell
520 |
0.20 |
2004B | |||
| Abell
521 |
0.25 |
2004B | |||
| Abell
586 |
0.17 |
2004B | |||
| Abell
611 |
0.29 |
2004B | |||
| Abell
697 |
0.28 |
2004B | |||
| Abell
851 |
0.41 |
2004B | |||
| Abell
854 |
0.21 |
2004B | |||
| Abell
1246 |
0.19 |
2004B | |||
| Abell 1835 |
|||||
| Abell 2163 |
v |
||||
| Abell
2259 |
0.16 |
2004B | |||
| Abell
2261 |
0.22 |
2004B | |||
| Abell
2537 |
0.30 |
2004B | |||
| MS0440+02 |
0.19 |
2004B | |||
| MS0451-03 |
0.54 |
2004B | |||
| MS1008-12 |
0.30 |
2004B | |||
| CL0910+41 |
0.44 |
2004B | |||
| CL1938+54 |
0.26 |
2004B | |||
| MACS
J0717.5+3745 |
0.55 |
2004B | |||
| RX J1347.5-1145 |
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| Image
gallery |
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