Table 1.
Overview of the 11 GOGREEN clusters studied here.
| Name | RA |
Dec |
Redshift (a) | λ10.2, R < 1000 kpc(b) | IQ (c) | Ks, lim(d) | M⋆, lim(e) |
|---|---|---|---|---|---|---|---|
| [″] | [magAB] | [M⊙] | |||||
| SPTCL-0205 | 02:05:48.19 | −58:28:49.0 | 1.320[106/31] | 41.1 ± 7.7 | 0.75 | 23.25 | 9.90 |
| SPTCL-0546 | 05:46:33.67 | −53:45:40.6 | 1.067[156/70] | 94.1 ± 10.6 | 0.64 | 23.47 | 9.64 |
| SPTCL-2106 | 21:06:04.59 | −58:44:27.9 | 1.132[95/56] | 108.6 ± 11.2 | 0.42 | 23.19 | 9.79 |
| SpARCS-0035 | 00:35:49.68 | −43:12:23.8 | 1.335[326/33] | 45.2 ± 7.9 | 0.39 | 23.81 | 9.70 |
| SpARCS-0219 | 02:19:43.56 | −05:31:29.6 | 1.325[338/12] | 22.2 ± 6.3 | 0.73 | 23.27 | 9.90 |
| SpARCS-0335 | 03:35:03.56 | −29:28:55.8 | 1.368[133/32] | 32.4 ± 7.1 | 0.58 | 22.91 | 10.07 |
| SpARCS-1034 | 10:34:49.47 | +58:18:33.1 | 1.386[84/24] | 20.8 ± 6.2 | 0.58 | 24.22 | 9.55 |
| SpARCS-1051 | 10:51:11.23 | +58:18:02.7 | 1.035[199/48] | 13.5 ± 5.7 | 0.72 | 24.17 | 9.35 |
| SpARCS-1616 | 16:16:41.32 | +55:45:12.4 | 1.156[243/70] | 49.4 ± 8.1 | 0.75 | 23.76 | 9.59 |
| SpARCS-1634 | 16:34:37.00 | +40:21:49.3 | 1.177[191/69] | 35.8 ± 7.2 | 0.65 | 24.01 | 9.50 |
| SpARCS-1638 | 16:38:51.64 | +40:38:42.9 | 1.196[192/68] | 18.7 ± 5.9 | 0.71 | 23.94 | 9.54 |
Notes.
In brackets the number of spectroscopic redshifts overlapping with the region for which we have photometry, and the number of spectroscopic cluster members (here defined as being within 0.02 from the cluster mean redshift, which, depending on the cluster redshift, corresponds to a velocity cut of 2500−3000 km s−1 in the cluster rest-frame), respectively. We note that these cluster members are selected slightly differently from our other papers, where a selection was made in projected phase-space coordinates (cf. Biviano et al., in prep.). This subtle difference is not relevant for the conclusions presented in this paper, and the approach followed here renders the membership selection more intuitive, when combined with photometric information.
Richness, defined as the number of cluster members with M⋆ ≥ 1010.2 M⊙ that are found within a circular aperture with R < 1000 kpc. This parameter is used to scale galaxy counts in the SMF in low-mass bins where not every cluster contributes to the measurement of the SMF due to incompleteness.
Faintest magnitude at which 80% of injected sources are still recovered. More details are given in Sect. 3.4.
Stellar mass limit based on a relatively old stellar population, as described in Sect. 3.4. This is the stellar mass limit we adopt for the quiescent population. For star-forming galaxies, which are brighter for their stellar mass, we expect to probe 0.2 dex below this limit.
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