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Table 2.

Photometric data set used in this work.

Name Ks, det PSF M⋆, det/M u B g V r Rc i Ic z J Ks
FWHM dex
PSZ2 G044.77-51.30 23.14 0.55″ 9.25 25.4a 26.0e 25.9e 24.8a 26.0e 25.4e 24.9f 23.4g 23.3g
PSZ2 G045.32-38.46 23.19 0.57″ 9.36 25.5a 25.6e 25.3e 25.2e 24.9e 24.9d 23.8g 23.3g
PSZ2 G045.87+57.70 22.66 0.54″ 9.61 25.5b 26.1d 25.9d 25.4d 23.8b 23.0g 22.5g
PSZ2 G046.13+30.72 22.38 0.66″ 9.68 25.2b 25.7d 25.8d 24.7d 24.1d 22.8g 22.3g
PSZ2 G070.89+49.26 22.27 0.64″ 9.75 25.5b 26.2d 25.8d 25.1d 24.0b 23.1g 22.4g
PSZ2 G073.31+67.52 22.44 0.55″ 9.69 25.7b 26.3a 25.4a 25.0b 23.9b 23.2g 22.6g
PSZ2 G094.56+51.03 22.38 0.66″ 9.62 25.3b 26.1a d 25.8d 25.0a d 23.5b 23.0g 22.5g
PSZ2 G099.86+58.45 22.31 0.57″ 9.75 25.6a 26.0a d 25.4a d 24.7c d 23.6a 23.1g 22.4g
PSZ2 G111.61-45.71 22.25 0.72″ 9.68 25.5a 26.5e 25.5a 26.3e 25.5a 26.2e 26.0c d 25.7e 25.0a f 23.5g 22.6g
PSZ2 G144.83+25.11 22.95 0.78″ 9.46 25.0a 25.7e 25.4e 25.5e 25.2e 25.0d 23.3g 23.2g
PLCK G147.30-16.60 22.57 0.52″ 9.68 24.5b 25.8d 25.4d 25.1d 23.6b 23.2g 22.7g
PSZ2 G155.27-68.42 22.36 0.59″ 9.69 24.6b 25.7b 25.3b 24.3b 23.8b 23.3g 22.6g
PSZ2 G180.25+21.03 23.13 0.65″ 9.33 25.6a 25.9e 25.6a 25.7e 25.3a 25.5e 24.8d 25.0d 23.1g 23.3g
PSZ2 G183.90+42.99 22.51 0.64″ 9.58 25.4b 25.9d 25.9d 25.5d 23.9b 23.5g 22.9g
PSZ2 G193.31-46.13 22.45 0.59″ 9.73 24.8b 25.8b 25.1b 24.8b 23.6b 23.1g 22.7g
PSZ2 G201.50-27.31 23.08 0.56″ 9.34 25.7a 26.2e 25.6a 26.0e 25.6a 26.0e 24.7c 25.5e 25.1a d 23.5g 23.4g
PSZ2 G208.61-74.39 21.98 0.69″ 10.00 25.0b 25.8b 25.2b 24.5b 23.8b 23.3g 22.4g
PSZ2 G211.21+38.66 22.94 0.78″ 9.33 25.9a 26.1e 25.2a 26.1e 24.9a 26.1e 24.0c 25.4e 25.1a d 23.0g 23.3g
PSZ2 G212.44+63.19 22.54 0.67″ 9.52 25.4b 26.0d 26.0d 25.5d 23.7b 23.7g 22.7g
PSZ2 G219.89-34.39 22.08 0.74″ 9.96 24.9b 25.7b 25.4b 24.4b 23.7b 22.9g 22.4g
PSZ2 G228.16+75.20 22.82 0.73″ 9.45 26.0a 26.6e 26.2e 26.3e 25.3d 25.4d 23.1g 23.2g

Notes. The reported magnitudes are median 5−σ limits measured on the PSF-homogenised stacked images in circular apertures with a diameter of 2″. The values listed are after correction for Galactic dust, and are therefore indicative of the galaxy population we study. The instruments and filters used for the different clusters are indicated. Whenever there are two observations with multiple instruments, both are used in the analysis, but only the magnitude corresponding to the deepest stack is reported below. CFHT/MegaCam filters used until Jan 2015, i-band after Oct 2007.


CFHT/MegaCam filters used after Feb 2015.


CFHT/MegaCam i-band filter used until June 2007.


Subaru/Suprime-Cam fully-depleted back-illuminated CCDs (installed Jan 2009) with SDSS-like filters.


Subaru/Suprime-Cam MIT/LL CCDs (used until Dec 2008) with Johnson/Bessell-like filters.


Subaru/Suprime-Cam MIT/LL CCDs (used until Dec 2008) with standard z-band filter.



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