Table 4.
Luminosity properties of the objects described by Capak et al. (2015).
ID | log(LUV/L⊙) | SFR (M⊙ yr−1) | log (LX/L⊙) | ![]() |
---|---|---|---|---|
HZ1 | 11.21 | 24 | 10.31 | 8.19 |
HZ2 | 11.15 | 25 | 10.26 | 8.20 |
HZ3 | 11.08 | 18 | 10.21 | 8.10 |
HZ4 | 11.28 | 51 | 10.36 | 8.38 |
HZ5a | 11.45 | <3 | 10.82b | <7.59 |
HZ5a | <10.37 | <3 | <9.66 | <7.59 |
HZ6 | 11.47 | 49 | 10.50 | 8.35 |
HZ6a | 11.11 | – | 10.23 | – |
HZ6b | 11.0 | – | 10.15 | – |
HZ6c | 11.81 | – | 10.00 | – |
HZ7 | 11.05 | 21 | 10.19 | 8.11 |
HZ8 | 11.04 | 18 | 10.18 | 8.06 |
HZ8W | 10.57 | 6 | 9.82 | 7.76 |
HZ9 | 10.95 | 67 | 10.11 | 8.46 |
HZ10c | 11.14 | 169 | 10.25 | 8.72 |
HZ10Wc | 10.23 | – | 9.54 | – |
Notes. The expected X-ray luminosities in the observer-frame soft band have been estimated by adopting a bolometric correction to the UV luminosity of 5.2 (Runnoe et al. 2012b).
No [C II] redshift measurement available (Capak et al. 2015), photometric redshift is used.
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