Table 4
Star-forming clumps: low- and high-z samples.
| Sample | SFR tracer | Av correction | Object | Scale | z | Instrument | Reference |
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) |
|
|
|||||||
| Planesas+97 | Hα | Hα/Hβ ratio | Circumnuclear star-forming rings, HII regions | 30–80 pc | <0.005 | narrow band, NOT | (a) |
| Bastian+06 | Hβ | Hγ/Hβ ratio | Antennae, HII regions | ~ 100 pc | 0.00569 | VLT-VIMOS | (b) |
| Liu+13 | Paα | Averaged(1), Hα/Paα ratio | Nearby spiral galaxies, HII regions | ~ 20 pc | <0.003 | HST-NICMOS | (c) |
| Arribas+14 | Hα | Hα/Hβ ratio | Low-z U/LIRGs, HII regions | 200–400 pc | <0.018 | VLT-VIMOS, INTEGRAL | (d) |
| Genzel+11 | Hα | SED fitting(2) | High-z galaxies, giant HII regions | 1.5–1.8 kpc | 2.2–2.4 | AO VLT-SINFONI | (e) |
| AG+12 | Hα | Averaged(3), Hα/Hβ ratio | SMG, integrated measurements | ~ 5 kpc | 2.0–2.7 | NIFS, VLT-SINFONI | (f) |
| Swinbank+12 | Hα | SED fitting(2) | High-z disks, HII regions and integrated measurements | 0.9–1.0 kpc | 0.8–2.2 | AO VLT-SINFONI | (g) |
| Zanella+15 | Hβ | SED fitting(4) | HII region | <0.5 kpc | 1.987 | HST-WFC3 | (h) |
Notes. Scale shown in Col. (5) corresponds to the typical physical resolution of the observations. (1) Average extinction correction of AV = 2.2 mag based on measurements from Calzetti et al. (2007). (2) Luminosities are corrected from extinction using stellar E(B−V) values from SED fitting. The extinction of the stars is then re-scaled to the extinction of the gas using the standard recipe AHα = 7.4 E(B−V), where E(B−V)stars = 0.44 E(B−V)gas from Calzetti et al. (2000). (3) Average extinction of AV = 2.9 mag from Takata et al. (2006). (4) Luminosities are corrected from extinction using stellar E(B−V) values from SED fitting. The extinction of the stars is then re-scaled to the extinction of the gas using the recipe E(B−V)stars = 0.83 E(B−V)gas from Kashino et al. (2013).
Reference. (a) Planesas et al. (1997); (b) Bastian et al. (2006); (c) Liu et al. (2013); (d) Arribas et al. (2014); (e) Genzel et al. (2011); (f) Alaghband-Zadeh et al. (2012); (g) Swinbank et al. (2012); (h) Zanella et al. (2015).
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