Table 6
Properties of emission-line galaxies detected with the tuneable filter.
| Host | G1 | G2 | G3 | |
|
|
||||
| RA (J2000) | 09:07:38.5 | 09:07:38.9 | 09:07:39.4 | 09:07:42.9 |
| Dec (J2000) | +14:01:08.46 | +14:01:09.12 | +14:01:27.83 | +14:00:15.40 |
| Redshift | 0.28256a | 0.2828a | 0.283b |
c
|
| Projected | 7.3 | 28.7 | 107.8 | 584.5 |
| distance (kpc)d | ||||
| MB (mag) | −19.4 ± 0.1 | −17.1 ± 0.1 | −18.7 ± 0.1 | −21.5 ± 0.1 |
| MKs (mag) | −19.5 ± 0.2 | −17.9 ± 0.2 | −19.1 ± 0.2 | −22.4 ± 0.2 |
| AV (mag) | <0.04 | ~0.6 | ~0 | ~0.6 |
| log M⋆(M⊙) | 8.95 ± 0.04 |
|
8.8 ± 0.1 |
|
| Age (Myr) | 350 ± 30 |
|
|
|
| SFR (M⊙ yr-1) | 0.4 ± 0.1 |
|
|
|
| χ2/ n.o.f. e | 24.7 / 20 | 3.1 / 4 | 14.8 / 8 | 18.0 / 9 |
Notes. The SEDs were fitted with Le Phare by assuming a Calzetti dust-attenuation law and a Chabrier IMF. For details, see Sect. 4.2.2.
The SED blueward of the Balmer break is poorly sampled, resulting in a not
well-constrained photo-z of
(99% c.l.). The only strong emission line falling in that redshift interval is
Hα at z = 0.283. The
reported galaxy properties were obtained for that redshift.
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