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Table A.2

Summary of stacked properties when stacking as a function of stellar mass.

Redshift range Stellar mass range f160 μm [mJy] log LUV log LIR N

0.02 ≤ z ≤ 0.50 9.60 ≤ log (M/M) ≤ 9.80 1.39±0.16 9.64 9.90±0.10 184
0.02 ≤ z ≤ 0.50 9.80 ≤ log (M/M) ≤ 10.00 2.18±0.23 9.69 10.12±0.09 170
0.02 ≤ z ≤ 0.50 10.00 ≤ log (M/M) ≤ 10.20 2.55±0.23 9.67 10.19±0.07 111
0.50 ≤ z ≤ 1.00 9.80 ≤ log (M/M) ≤ 10.00 0.42±0.04 9.78 10.13±0.10 2896
0.50 ≤ z ≤ 1.00 10.00 ≤ log (M/M) ≤ 10.20 0.83±0.05 9.83 10.46±0.05 2246
0.50 ≤ z ≤ 1.00 10.20 ≤ log (M/M) ≤ 10.40 1.30±0.06 9.82 10.64±0.04 1499
0.50 ≤ z ≤ 1.00 10.40 ≤ log (M/M) ≤ 10.60 1.85±0.09 9.79 10.79±0.05 865
0.50 ≤ z ≤ 1.00 10.60 ≤ log (M/M) ≤ 10.80 2.38±0.11 9.77 10.98±0.04 576
1.00 ≤ z ≤ 1.50 10.00 ≤ log (M/M) ≤ 10.20 0.70±0.04 9.95 10.81±0.05 2877
1.00 ≤ z ≤ 1.50 10.20 ≤ log (M/M) ≤ 10.40 0.90±0.05 9.97 10.90±0.04 2101
1.00 ≤ z ≤ 1.50 10.40 ≤ log (M/M) ≤ 10.60 1.41±0.06 9.93 11.10±0.03 1541
1.00 ≤ z ≤ 1.50 10.60 ≤ log (M/M) ≤ 10.80 1.64±0.10 9.87 11.15±0.05 1152
1.00 ≤ z ≤ 1.50 10.80 ≤ log (M/M) ≤ 11.00 1.71±0.10 9.83 11.18±0.05 869
1.50 ≤ z ≤ 2.00 10.00 ≤ log (M/M) ≤ 10.20 0.62±0.05 10.04 11.11±0.06 2688
1.50 ≤ z ≤ 2.00 10.20 ≤ log (M/M) ≤ 10.40 0.85±0.06 9.98 11.25±0.06 1682
1.50 ≤ z ≤ 2.00 10.40 ≤ log (M/M) ≤ 10.60 1.13±0.08 9.93 11.37±0.06 1158
1.50 ≤ z ≤ 2.00 10.60 ≤ log (M/M) ≤ 10.80 1.33±0.10 9.89 11.46±0.06 851
1.50 ≤ z ≤ 2.00 10.80 ≤ log (M/M) ≤ 11.00 1.08±0.12 9.83 11.35±0.09 656
2.00 ≤ z ≤ 2.50 10.20 ≤ log (M/M) ≤ 10.40 0.40±0.05 10.27 11.26±0.12 2083
2.00 ≤ z ≤ 2.50 10.40 ≤ log (M/M) ≤ 10.60 0.70±0.07 10.21 11.50±0.09 1514
2.00 ≤ z ≤ 2.50 10.60 ≤ log (M/M) ≤ 10.80 0.90±0.08 10.06 11.60±0.07 984
2.00 ≤ z ≤ 2.50 10.80 ≤ log (M/M) ≤ 11.00 1.32±0.12 9.976 11.76±0.07 616
2.00 ≤ z ≤ 2.50 11.00 ≤ log (M/M) ≤ 11.20 1.30±0.15 9.90 11.76±0.09 389
2.50 ≤ z ≤ 3.00 10.60 ≤ log (M/M) ≤ 10.80 0.69±0.10 10.38 11.75±0.12 645
2.50 ≤ z ≤ 3.00 10.80 ≤ log (M/M) ≤ 11.00 1.05±0.13 10.16 11.93±0.11 418
2.50 ≤ z ≤ 3.00 11.00 ≤ log (M/M) ≤ 11.20 0.90±0.17 10.04 11.87±0.16 197

Notes. The uncertainties in the rest-frame UV luminosity are related to the normalization of the templates to the observed photometry; they are typically lower than 0.05 dex. The uncertainties in the total IR luminosities are obtained as the difference in the total IR luminosity when considering f160 μm ± Δf160 μm. N indicates the number of galaxies in each bin.

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