Table 2.
Illustration of the photometric data set used in this work.
| Name | u/U | B/g | V | r/R | i/I | z/Z | Y/J1 | J | Ks | [3.6] μm | [4.5] μm | [5.8] μm | [8.0] μm |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| SPTCL-0205 | 26.2 (b) | 26.7 (b) | 25.6 (b) | 25.9 (b) | 25.4 (b) | 24.2 (b) | 24.2 (h) | 23.9 (h) | 24.0 (h) | 23.7 (j) | 23.2 (j) | − | − |
| SPTCL-0546 | 25.3 (b) | 26.1 (b) | 25.3 (b) | 25.6 (b) | 25.0 (b) | 23.8 (b) | 24.1 (h) | 23.9 (h) | 23.9 (h) | 24.0 (j) | 23.8 (j) | − | − |
| SPTCL-2106 | 26.0 (b) | 26.3 (b) | 25.9 (b) | 25.8 (b) | 25.3 (b) | 24.6 (b) | 24.4 (h) | 24.1 (h) | 23.6 (g) | 23.7 (j) | 23.0 (j) | − | − |
| SpARCS-0219 | 25.8 (b) | 26.0 (b) | 25.3 (b) | 25.5 (b) | 25.2 (b) | 24.1 (b) | 24.4 (h) | 24.3 (h) | 24.0 (h) | 24.0 (j) | 23.8 (j) | 21.4 (j) | 21.4 (j) |
| SpARCS-0335 | 26.3 (b) | 26.4 (b) | 25.9 (b) | 26.3 (b) | 25.5 (b) | 24.6 (b) | 25.2 (g) | 24.3 (h) | 23.7 (h) | 24.4 (j) | 24.3 (j) | 21.6 (j) | 21.6 (j) |
| SpARCS-0035 | 25.9 (b) | 26.4 (b) | 25.8 (b) | 26.0 (b) | 25.5 (b) | 25.5 (d) | 24.2 (h) | 24.9 (g) | 24.2 (g) | 24.6 (j) | 24.5 (j) | 22.8 (j) | 22.6 (j) |
| SpARCS-1034 | − | 26.0 (c) | − | 26.1 (c) | 25.5 (c) | 25.4 (e) | 25.1 (e) | 24.5 (i) | 24.0 (i) | 22.7 (j) | 22.4 (j) | 19.9 (j) | 19.7 (j) |
| SpARCS-1051 | 26.3 (a) | 26.1 (c) | − | 26.1 (c) | 25.6 (c) | 25.4 (e) | 25.0 (e) | 24.5 (i) | 24.1 (i) | 22.6 (j) | 22.5 (j) | 19.7 (j) | 19.6 (j) |
| SpARCS-1616 | 25.9 (a) | 26.2 (c) | − | 26.1 (c) | 25.7 (c) | 25.6 (e) | 24.7 (e) | 24.2 (i) | 23.8 (i) | 22.7 (j) | 22.6 (j) | 21.2 (j) | 21.3 (j) |
| SpARCS-1634 | 25.9 (a) | 26.4 (c) | − | 26.2 (c) | 25.8 (c) | 25.0 (f) | − | 24.2 (i) | 23.8 (i) | 23.0 (j) | 22.8 (j) | 21.3 (j) | 21.3 (j) |
| SpARCS-1638 | 26.1 (a) | 26.4 (c) | − | 26.2 (c) | 25.6 (c) | 25.3 (f) | 24.2 (c) | 24.1 (i) | 23.6 (i) | 22.8 (j) | 22.5 (j) | 21.3 (j) | 21.4 (j) |
| COSMOS/UltraVISTA | 26.8 (a) | 26.9 (c) | 26.4 (c) | 26.4 (c) | 26.0 (c) | 25.2 (c) | 24.5 (k) | 24.3 (k) | 23.8 (k) | 23.9 (j) | 23.6 (j) | 21.7 (j) | 21.7 (j) |
Notes. The reported depths 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 extinction, and so are indicative of the galaxy population we study. The instruments and filters used for the different clusters are indicated. For IRAC we measure fluxes in apertures with a diameter of 3″ and convert them back to 2″ by using the detection band, convolved to both PSF sizes, as described in Sect. 3.1. For reference, we list the median 5-σ depths of 13 stacks in the DR1 COSMOS/UltraVISTA catalogues (these are measured in 
apertures Muzzin et al. 2013a). That subset of filters of the full COSMOS/UltraVISTA data set is used to provide a statistical background correction in this work, and thus to provide a verification of our fiducial method to measure the cluster SMF (cf. Sect. 3.5).
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