Table 5.
Properties of efficiently star-forming, high-redshift radio galaxies.
| SFR | MH2 | fgas | SFE | tdepl | Size | log(Σgas) | log(ΣSFR) | ||
|---|---|---|---|---|---|---|---|---|---|
| (M⊙ yr−1) | (1010 M⊙) | (%) | (Gyr−1) | (Myr) | (kpc) | log(M⊙ pc−2) | log(M⊙ yr−1 kpc−2) | ||
| PKS 0529-549 |  |
3.9 ± 1.0(b) | 12 ± 7 | 26 ± 8 | 38 ± 12 | 4(c) | 2.9 ± 0.1 | 1.3 ± 0.1 | |
| 4C 41.17 |  |
5.4 ± 0.6(e) | 18 ± 2 |  |
 |
4.3(f) | 2.97 ± 0.05 |  |
|
| MRC 0152-209 |  |
2.2 ± 0.2(g) | 3.7 ± 0.3 |  |
12 ± 2 | 1.5(h) | 3.49 ± 0.04 |  |
Notes. Star formation rates are derived from the LIR (8–1000 μm) using the formula provided in Kennicutt (1998a) assuming continuous bursts of age 10–100 Myr, and converted to the Kroupa (2001) IMF. Molecular gas masses are estimated from either [C I] or CO emission as described in Sect. 5.1. The quoted uncertainties refer to measurement errors. The definitions of fgas, SFE, and tdepl can be found in Sect. 4. Σgas is calculated as MH2/(πR2), where R refers to the radius of the star-forming region. ΣSFR is calculated as SFR/(πR2). These numbers refer to the star formation within the host galaxies only, and do not include the H2 gas mass in the extended halo.
References. (a) Falkendal et al. 2019; (b) this work; (c) Lelli et al. 2018; (d) Drouart et al. 2016; (e) De Breuck et al. 2005; (f) Miley et al. 1992; (g) Emonts et al. 2015a; (h) Emonts et al. 2015b.
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