Table 1.
IR line fluxes for our sample of star-forming galaxies.
Name | RA (J2000) | Dec. (J2000) | z | Type | [S IV]10.5 μm | Hu-α | [Ne II]12.8 μm | [Ne III]15.6 μm | [O III]52 μm | [N III]57 μm | [O III]88 μm | [N II]122 μm | Refs. |
---|---|---|---|---|---|---|---|---|---|---|---|---|---|
(hh:mm:ss) | (dd:mm:ss) | ||||||||||||
Haro 11 | 00:36:52.45 | −33:33:16.77 | 0.020598 | Dwarf | 49.4 ± 1.1 | 1.6 ± 0.5 | 32.7 ± 0.9 | 112 ± 5 | – | 28.3 ± 0.8 | 172 ± 3 | 3.5 ± 0.3 | 1 |
IRAS00397-1312 | 00:42:15.50 | −12:56:03.0 | 0.261717 | ULIRG | 0.27 ± 0.07 | – | 3.78 ± 0.04 | 2.1 ± 0.2 | 3.0 ± 0.4 | – | – | – | 2, 3 |
NGC 253 | 00:47:33.07 | −25:17:19.0 | 0.000811 | SB | – | – | 2830 ± 60 | 200 ± 10 | – | 400 ± 100 | 330 ± 50 | 410 ± 40 | 4 |
HS0052+2536 | 00:54:56.36 | +25:53:08.0 | 0.045385 | Dwarf | 1.4 ± 0.3 | – | 0.9 ± 0.1 | 1.5 ± 0.5 | – | – | 7.1 ± 0.4 | – | 1 |
UM311 | 01:15:34.40 | −00:51:46.1 | 0.005586 | Dwarf | 3.7 ± 0.3 | – | 4 ± 1 | 10.3 ± 0.5 | – | – | 51 ± 3 | – | 1 |
NGC 625 | 01:35:05.16 | −41:26:08.8 | 0.001321 | Dwarf | 57.2 ± 0.7 | 2.4 ± 0.2 | 16.6 ± 0.5 | 75 ± 3 | – | – | 245 ± 3 | – | 1 |
NGC 891 | 02:22:32.85 | +42:20:52.7 | 0.001761 | SB | – | 0.7 ± 0.3 | 39.4 ± 0.4 | 4.5 ± 0.2 | – | – | – | 19.4 ± 0.8 | 5, 6 |
NGC 1140 | 02:54:33.53 | −10:01:42.1 | 0.005007 | Dwarf | 18 ± 1 | 0.5 ± 0.1 | 18.3 ± 0.9 | 63 ± 4 | – | – | 108 ± 3 | 2.1 ± 0.3 | 1 |
NGC 1222 | 03:08:56.74 | −02:57:18.6 | 0.008079 | SB | 22.2 ± 0.5 | 2.1 ± 0.2 | 81 ± 1 | 89 ± 2 | – | – | – | 5.8 ± 0.7 | 4 |
SBS 0335-052 | 03:37:44.06 | −05:02:40.19 | 0.013519 | Dwarf | 1.48 ± 0.04 | – | 0.07 ± 0.01 | 1.24 ± 0.07 | – | – | 4.4 ± 0.3 | – | 1 |
Notes. For each galaxy we provide the name, coordinates, redshift, spectral type (dwarf galaxy, starburst, or ULIRG), the mid-IR line fluxes in units of 10−17 W m−2, and the references in the literature where these measurements were compiled. The complete version of the table is available at the CDS.
References. (1) Cormier et al. (2015); (2) Veilleux et al. (2009); (3) Pereira-Santaella et al. (2017); (4) Bernard-Salas et al. (2009); (5) Goulding & Alexander (2009); (6) Fernández-Ontiveros et al. (2016).
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