Table A.1
The sample of spatially resolved galaxies in the MUSE-HDFS.
ID | z | i | PAmor | R d | PAkin | V max | σ | Int. | log (Mstar) | log (SFR) |
(°) | (°) | (″/kpc) | (°) | (km s-1) | (km s-1) | (M⊙) | (M⊙ yr-1) | |||
[1] | [2] | [3] | [4] | [5] | [6] | [7] | [8] | [9] | [10] | [11] |
|
||||||||||
1 | 0.1723 | 75 | 31.3 ± 0.1 | 0.46 / 1.34 ± 0.01 | 33 ± 2 | 74 ± 4 | 30 ± 3 | 0 | 8.78 ± 0.42 | − 1.01 ± 0.67 |
3 | 0.5637 | 16 | − 18.8 ± 3.0 | 0.66 / 4.28 ± 0.04 | 64 ± 2 | 103 ± 20 | 34 ± 1 | 0 | 9.66 ± 0.14 | 0.24 ± 0.37 |
4 | 0.5638 | 75 | 35.8 ± 0.1 | 0.62 / 4.01 ± 0.03 | 34 ± 1 | 204 ± 20 | 48 ± 3 | 0 | 9.86 ± 0.17 | 0.54 ± 0.35 |
5 | 0.5798 | 68 | 6.9 ± 0.2 | 0.25 / 1.67 ± 0.02 | 37 ± 6 | 47 ± 16 | 54 ± 3 | 0 | 9.82 ± 0.17 | 0.59 ± 0.38 |
6 | 0.4230 | 29 | 45.0 ± 2.0 | 0.46 / 2.54 ± 0.03 | 9 ± 7 | 80 ± 4 | 29 ± 3 | 1 | 9.23 ± 0.10 | − 0.61 ± 0.50 |
7 | 0.4637 | 41 | 43.0 ± 0.7 | 0.44 / 2.55 ± 0.03 | 50 ± 3 | 76 ± 2 | 27 ± 15 | 1 | 9.31 ± 0.12 | − 0.51 ± 0.54 |
8 | 0.5772 | 61 | − 29.4 ± 0.4 | 0.18 / 1.20 ± 0.01 | − 20 ± 2 | 124 ± 20 | 84 ± 12 | 1 | 9.88 ± 0.23 | 1.39 ± 0.58 |
9 | 0.5638 | 61 | − 34.8 ± 0.4 | 0.25 / 1.60 ± 0.02 | − 37 ± 2 | 125 ± 3 | 54 ± 3 | 0 | 9.31 ± 0.20 | 0.80 ± 0.41 |
10 | 1.2840 | 26 | 39.9 ± 4.1 | 0.24 / 2.05 ± 0.06 | 107 ± 15 | 98 ± 14 | 116 ± 3 | 2 | 10.77 ± 0.11 | 0.30 ± 0.89 |
11 | 0.5779 | 62 | 27.3 ± 0.5 | 0.10 / 0.67 ± 0.01 | 29 ± 3 | 61 ± 12 | 49 ± 1 | 0 | 9.22 ± 0.18 | 0.08 ± 0.49 |
12 | 0.6701 | 37 | − 144.0 ± 4.9 | 0.04 / 0.29 ± 0.01 | − 145 ± 30 | 48 ± 12 | 59 ± 1 | 2 | 9.02 ± 0.27 | 0.82 ± 0.67 |
13 | 1.2900 | 33 | − 45.9 ± 1.9 | 0.15 / 1.25 ± 0.02 | − 13 ± 2 | 24 ± 4 | 48 ± 1 | 0 | 9.89 ± 0.11 | 1.89 ± 0.18 |
16 | 0.4647 | 20 | − 40.0 ± 7.6 | 0.40 / 2.35 ± 0.06 | − 53 ± 10 | 91 ± 3 | 34 ± 3 | 0 | 8.74 ± 0.21 | − 0.65 ± 0.55 |
17 | 0.5810 | 45 | 77.3 ± 1.2 | 0.26 / 1.73 ± 0.04 | 95 ± 15 | 87 ± 30 | 41 ± 6 | 0 | 9.06 ± 0.17 | − 0.13 ± 0.84 |
20 | 0.4275 | 73 | − 38.8 ± 0.5 | 0.49 / 2.77 ± 0.10 | − 121 ± 4 | 41 ± 15 | 21 ± 3 | 0 | 8.71 ± 0.06 | − 1.16 ± 0.50 |
23 | 0.5641 | 24 | 78.3 ± 4.9 | 0.51 / 3.38 ± 0.09 | 14 ± 8 | 32 ± 6 | 31 ± 3 | 0 | 8.72 ± 0.27 | − 0.19 ± 0.70 |
24 | 0.9723 | 14 | − 1.2 ± 13.8 | 0.18 / 1.44 ± 0.05 | − 68 ± 3 | 164 ± 21 | 45 ± 3 | 0 | 9.61 ± 0.24 | 0.77 ± 0.73 |
26 | 0.2249 | 70 | 15.0 ± 0.4 | 0.46 / 1.66 ± 0.05 | 14 ± 4 | 75 ± 9 | 16 ± 3 | 0 | 7.95 ± 0.35 | − 1.87 ± 0.63 |
27 | 1.2853 | 71 | − 9.4 ± 0.5 | 0.48 / 4.00 ± 0.05 | 5 ± 2 | 168 ± 15 | 99 ± 6 | 1,2 | 10.32 ± 0.19 | 1.06 ± 0.95 |
28 | 0.3179 | 32 | 84.9 ± 3.0 | 0.21 / 0.99 ± 0.04 | 75 ± 22 | 47 ± 10 | 29 ± 3 | 0 | 7.99 ± 0.14 | − 1.24 ± 0.38 |
32 | 0.5644 | 68 | 122.0 ± 0.5 | 0.28 / 1.83 ± 0.06 | 112 ± 8 | 70 ± 7 | 50 ± 3 | 0 | 8.57 ± 0.17 | − 1.07 ± 0.39 |
35 | 1.2806 | 41 | 44.3 ± 2.5 | 0.17 / 1.40 ± 0.06 | 34 ± 7 | 214 ± 30 | 87 ± 12 | 0 | 10.12 ± 0.26 | 1.37 ± 0.96 |
37 | 1.0978 | 72 | 6.1 ± 0.7 | 0.12 / 0.98 ± 0.02 | 46 ± 20 | 21 ± 7 | 66 ± 3 | 0 | 9.12 ± 0.17 | 0.89 ± 0.43 |
38 | 1.0217 | 57 | − 29.0 ± 1.2 | 0.23 / 1.82 ± 0.08 | − 23 ± 6 | 98 ± 10 | 45 ± 6 | 0 | 8.86 ± 0.14 | 0.17 ± 0.42 |
49 | 0.9991 | 68 | − 68.8 ± 1.0 | 0.19 / 1.52 ± 0.08 | − 69 ± 6 | 86 ± 20 | 51 ± 6 | 1 | 8.83 ± 0.21 | − 0.02 ± 0.72 |
68 | 0.9715 | 78 | 26.3 ± 0.9 | 0.16 / 1.29 ± 0.06 | 9 ± 7 | 70 ± 13 | 39 ± 6 | 0 | 8.29 ± 0.24 | − 0.51 ± 0.53 |
72 | 0.8391 | 74 | − 90.0 ± 1.0 | 0.16 / 1.22 ± 0.07 | − 87 ± 8 | 135 ± 9 | 24 ± 21 | 0 | 8.68 ± 0.25 | − 0.62 ± 0.42 |
88 | 1.3600 | 77 | 8.8 ± 2.0 | 0.21 / 1.76 ± 0.22 | − 64 ± 12 | 51 ± 9 | 34 ± 12 | 2 | 8.71 ± 0.14 | − 0.45 ± 0.37 |
Notes. Column (1): identification number according to Bacon et al. (2015); Col. (2): spectroscopic redshift from MUSE according to Bacon et al. (2015); Cols. (3), (4), (5): disk inclination (with typical uncertainties of ±5°), position angle of the disk major axis, and disk scale length (both in arcsec and kpc, but uncertainties are given in kpc only) derived from Galfit modeling on HST F814W images (see Sect. 3); Cols. (6), (7), (8): position angle of the disk major axis, maximum rotation velocity, and velocity dispersion derived from kinematic modeling of MUSE data cubes (see Sect. 4); Col. (9): flag indicating the level of gravitational interactions: 0 = isolated, 1 = minor pair/interaction, 2 = major pair/interaction or clear merger remnant (see Sect. 5.1.3); Cols. (10, 11): stellar mass and star formation rate derived from SED fitting on visible+NIR photometry (see Sect. 2.2.2).
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