Table 3
Values for the data points of the galaxy SMF shown in Fig. 5.
| log (M⋆) | Cluster z ~ 1 | Number | Field 0.85 < z < 1.20 | Φ [10-5 dex-1 Mpc-3] | ||
| [M⊙] | Total | Quiescent | Star-forming | Total | Quiescent | Star-forming |
|
|
||||||
| 10.10 |
|
|
|
308.6 ± 5.1 | 78.9 ± 2.6 | 229.7 ± 4.4 |
| 10.30 |
|
|
|
260.8 ± 4.7 | 91.3 ± 2.8 | 169.5 ± 3.8 |
| 10.50 |
|
|
|
217.4 ± 4.3 | 91.7 ± 2.8 | 125.7 ± 3.3 |
| 10.70 |
|
|
|
183.0 ± 3.9 | 94.9 ± 2.8 | 88.1 ± 2.7 |
| 10.90 |
|
|
|
112.9 ± 3.1 | 72.7 ± 2.5 | 40.2 ± 1.8 |
| 11.10 |
|
|
|
52.1 ± 2.1 | 40.5 ± 1.8 | 11.7 ± 1.0 |
| 11.30 |
|
|
|
17.6 ± 1.2 | 15.3 ± 1.1 | 2.3 ± 0.4 |
| 11.50 |
|
|
[0] | 3.8 ± 0.6 | 3.4 ± 0.5 | 0.4 ± 0.2 |
Notes.These are the raw, membership-corrected, numbers of galaxies for the clusters. To obtain the units shown in the figures for the clusters, these values need to be multiplied by 5, since the binsize is 0.2 dex in stellar mass. Numbers in brackets show the total number of spectroscopic cluster members in each bin. Note that the spectroscopic completeness is highest in the high-mass bins. Errors represent 1σ uncertainties estimated from Monte-Carlo simulations for the cluster data, and Poissonian errors for the field data.
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