Table 1
Data used in this study.
| Cluster | RA | Dec | z | Instrument | Filters | Seeing | G14 | M15 |
|
|
||||||||
| XDCScmJ032903 | 03 29 02.81 | +02 56 25.18 | 0.4122 | CFHT/Megacam | r + (v,i) | 0.73′′ | Y | Y |
| MACSJ0454.1-0300 | 04 54 10.92 | –03 01 07.14 | 0.5377 | CFHT/Megacam | r + (v,z) | 0.76′′ | Y | Y |
| ABELL0851 | 09 42 56.64 | +46 59 21.91 | 0.4069 | CFHT/Megacam | i + (v,z) | 0.80′′ | Y | Y |
| LCDCS0829 | 13 47 31.99 | –11 45 42.01 | 0.4510 | CFHT/Megacam | r + (v,i) | 0.83′′ | Y | Y |
| MS1621.5+2640 | 16 23 35.50 | +26 34 13.00 | 0.4260 | CFHT/Megacam | r + (v,i) | 0.65′′ | Y | N |
| OC02J1701+6412 | 17 01 22.60 | +64 14 09.00 | 0.4530 | CFHT/Megacam | r + (i,v) | 0.73′′ | N | N |
| NEP0200 | 17 57 19.39 | +66 31 31.00 | 0.6909 | CFHT/Megacam | i + (v,r) | 0.97′′ | N | N |
| RXJ2328.8+1453 | 23 28 49.90 | +14 53 12.01 | 0.4970 | CFHT/Megacam | r + (v,i) | 0.70′′ | Y | N |
| CLJ0152.7-1357 | 01 52 40.99 | –13 57 45.00 | 0.8310 | Subaru/Suprime-Cam | r + (v,z) | 0.70′′ | Y | Y |
| MACSJ0717.5+3745 | 07 17 33.79 | +37 45 20.01 | 0.5458 | Subaru/Suprime-Cam | r + (v,z) | 0.69′′ | N | N |
| BMW-HRIJ122657 | 12 26 58.00 | +33 32 54.09 | 0.8900 | Subaru/Suprime-Cam | r + (i,z) | 0.80′′ | Y | Y |
| MACSJ1423.8+2404 | 14 23 48.29 | +24 04 46.99 | 0.5450 | Subaru/Suprime-Cam | i + (v,r) | 0.88′′ | Y | Y |
| MACSJ1621.4+3810 | 16 21 23.99 | +38 10 01.99 | 0.4650 | Subaru/Suprime-Cam | i + (v,r) | 0.62′′ | N | Y |
| RXJ1716.4+6708 | 17 16 49.60 | +67 08 30.01 | 0.8130 | Subaru/Suprime-Cam | r + (v,z) | 0.63′′ | Y/N | N |
| CXOSEXSIJ205617* | 20 56 17.16 | –04 41 55.10 | 0.6002 | Subaru/Suprime-Cam | r + (v,i) | 0.61′′ | Y | N |
| MS2053.7-0449* | 20 56 22.37 | –04 37 43.42 | 0.5830 | Subaru/Suprime-Cam | r + (v,i) | 0.61′′ | Y | N |
Notes. The different columns correspond to #1: cluster ID; #2: right ascension; #3: declination; #4: redshift; #5: telescope/camera; #6: filters, we give first the band on which we perform shape measurements and in parentheses the two other bands used for the color−color cut; and #7: seeing for the band on which we perform shape measurements. Columns #8 (G14) and #9 (M15) show whether the cluster was studied in Guennou et al. (2014) or Martinet et al. (2015b). In the first case, we know if it presents substructures based on X-ray images, and in most cases, on optical galaxy spectroscopy as well. For RX_J1716.4+6708, we have spectroscopy but no XMM image. In the second, we have photo-zs in the inner part, and in most cases, an optical galaxy luminosity function for the cluster. Hereafter, we use abridged names.
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