Table 1.
MUSE observational parameters listed for each object in the BGG sample.
| Group | BGG | z | Scale | Exp. time | Seeing | αJ2000 | δJ2000 | R | G. | Hα info | Emission lines |
|---|---|---|---|---|---|---|---|---|---|---|---|
| (kpc/″) | (s) | (″) | Type | detected | |||||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) |
| LGG 9 | NGC 193 | 0.014723 | 0.359 | 3 × 900 | 1.98 | 00:39:18.6 | +03:19:52 | 7 | E | Emission | Hα, [NII], [OIII], Hβ, [SII] |
| LGG 18 | NGC 410 | 0.017659 | 0.373 | 3 × 900 | 1.10 | 01:10:58.9 | +33:09:07 | 6 | E2 | Emission | Hα, [NII], [OIII], Hβ, [SII] |
| LGG 27 | NGC 584 | 0.006011 | 0.121 | 3 × 900 | 1.59 | 01:31:20.7 | −06:52:05 | 4 | S0 | Abs/Emis | Hα, [NII], [OIII], Hβ, [SII] |
| LGG 31 | NGC 677 | 0.017012 | 0.378 | 3 × 900 | 0.65 | 01:49:14.0 | +13:03:19 | 7 | E3 | Emission | Hα, [NII], [OIII], Hβ, [SII], [OI] |
| LGG 42 | NGC 777 | 0.016728 | 0.354 | 3 × 900 | 0.86 | 02:00:14.9 | +31:25:46 | 5 | E1 | Abs/Emis | Hα, [NII] |
| LGG 58 | NGC 940 | 0.017075 | 0.359 | 3 × 900 | 0.77 | 02:29:27.5 | +31:38:27 | 3 | S0 | Abs/Emis | Hα, [NII], [OIII], Hβ, [SII] |
| LGG 61 | NGC 924 | 0.014880 | 0.310 | 3 × 900 | 0.73 | 02:26:46.8 | +20:29:51 | 3 | S0 | Emission | Hα, [NII], [OIII], Hβ, [SII], [OI] |
| LGG 66 | NGC 978 | 0.015794 | 0.334 | 3 × 900 | 1.16 | 02:34:47.6 | +32:50:37 | 7 | E/S0 | Abs/Emis | Hα, [NII], [OIII], Hβ, [SII], [OI] |
| LGG 72 | NGC 1060 | 0.017312 | 0.368 | 3 × 900 | 0.43 | 02:43:15.0 | +32:25:30 | 8 | E/S0 | Abs/Emis | Hα, [NII], [OIII], [SII] |
| LGG 103 | NGC 1453 | 0.012962 | 0.305 | 3 × 900 | 0.80 | 03:46:27.2 | −03:58:08 | 4 | E3 | Emission | Hα, [NII], [OIII], Hβ, [SII], [OI] |
| LGG 117 | NGC 1587 | 0.012322 | 0.247 | 3 × 900 | 0.97 | 04:30:39.9 | +00:39:42 | 4 | E1 | Abs/Emis | Hα, [NII], [OIII], Hβ, [SII], [OI] |
| LGG 262 | NGC 4008 | 0.012075 | 0.262 | 3 × 900 | 0.79 | 11:58:17.0 | +28:11:33 | 4 | E5 | Abs/Emis | Hα, [NII], Hβ |
| LGG 276 | NGC 4169 | 0.012622 | 0.218 | 3 × 900 | 0.68 | 12:12:18.8 | +29:10:46 | 4 | S0a | Emission | Hα, [NII], [OIII], Hβ, [SII], [OI] |
| LGG 278 | NGC 4261 | 0.007378 | 0.155 | 3 × 880 | 0.78 | 12:19:23.2 | +05:49:31 | 7 | E2 | Emission | Hα, [NII], [OIII], Hβ, [SII], [OI] |
| LGG 393 | NGC 5846 | 0.005711 | 0.126 | 7 × 880 | 0.90 | 15:06:29.3 | +01:36:20 | 5 | E0 | Emission | Hα, [NII], [OIII], Hβ, [SII], [OI] |
| LGG 421 | NGC 6658 | 0.014243 | 0.305 | 3 × 870 | 1.82 | 18:33:55.6 | +22:53:18 | 4 | E2 | Absorption | – |
| LGG 473 | NGC 7619 | 0.012549 | 0.262 | 3 × 870 | 0.47 | 23:20:14.5 | +08:12:22 | 8 | E3 | Abs/Emis | Hα, [NII], [SII], [OI] |
| LGG 310 | ESO 507-25 | 0.010788 | 0.218 | 3 × 900 | 1.90 | 12:51:31.8 | −26:27:07 | 4 | S0 | Emission | Hα, [NII], [OIII], Hβ, [SII], [OI] |
Notes. (1) Group name (LGG: Lyon Groups of Galaxies). (2) BGG name. (3) Redshifts of each group, taken from O’Sullivan et al. (2015, 2018b). (4) Scale. (5) MUSE exposure time on source. (6) Average DIMM seeing of the MUSE observations. (7) and (8) Right Ascension and Declination of each group. (9) Richness R values for each source O’Sullivan et al. (2017). (10) Morphological classification of the galaxy based on de Vaucouleurs et al. (1991). (11) In some cases, the Hα line appears very weak or even completely absent from some parts of the cube where it is otherwise expected to exist (such as regions where the other ionized lines are stronger, e.g., [NII]λ6583). This is because the stellar continuum is very high, and the Hα flux is low. Those systems are being labeled with Hα in absorption. Some of the Hα flux is recovered after the stellar continuum subtraction (see Fig. 1 for an example), however, it is possible that we are not able to recover entirely the underlying Hα emission in some cases. (12) Emission lines detected on the MUSE data cube.
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