Table 2
Derived upper limits for the [O ii] luminosities and corresponding SFR.
| BR1202-0725 | |||||
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|
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| Object |
|
SFR1 (this work) |
|
SFR2 (this work) | SFR3 (literature) |
| [× 1042 erg/s] | [M⊙ yr-1] | [× 1042 erg/s] | [M⊙ yr-1] | [M⊙ yr-1] | |
|
|
|||||
| SMG | ≤ 1.8 | ≤ 26 | ≤ 0.7 | ≤ 10 | (1) |
| Lyα1 ([C ii]) | ≤ 2.5 | ≤ 34 | ≤ 1.0 | ≤ 14 | (2) |
| Lyα1 (Lyα) | ≤ 3.4 | ≤ 48 | ≤ 0.7 | ≤ 9 | (2) |
| Lyα2 | ≤ 2.5 | ≤ 35 | ≤ 1.2 | ≤ 16 | (3) |
|
|
|||||
| J1000+0234 | |||||
|
|
|||||
| SMG (Lyα) | ≤ 5.8 | ≤ 82 | ≤ 2.8 | ≤ 39 | (4) |
| SMG (12CO(4−3)) | ≤ 7.9 | ≤ 111 | ≤ 2.3 | ≤ 32 | (4) |
Notes. (1) [a] 2000 (FIR); [b] 2600 (FIR, SED model); [b] 6800 ± 1000 ([C ii]); [b] 4000 (radio, SED model). (2) [c] 15−54 (UV); [d] ≈ 13 (UV); [e] ≤ 36 (FIR, SED model); [e] 19 ([C ii]). (3) [e] 170 (FIR, SED model); [e] 70 ([C ii]). (4) [f] 1000-4000 (FIR, SED model); [f] 3700 ± 700 (radio); [f] 2900 ± 100 (3.6 μm band).
calculated using the [Oii] emission line less affected by sky emission lines and assuming a line ratio of [Oii]3729/3726 = 1;
in parenthesis the emission line or spectrum continuum used to calculate the SFR. All works use a Salpeter IMF with solar abundances.
Reference. [a] Salomé et al. (2012); [b] Carniani et al. (2013); [c] Fontana et al. (1998); [d] Ohyama et al. (2004); [e] Carilli et al. (2013); [f] Capak et al. (2008).
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