Table 1.
Main properties of our galaxy sample.
Name | M* | δM* | Mgas | δMgas | Mbar | δMbar | j* | δj* | jgas | δjgas | jbar | δjbar | Rd | ℛ* ( † ) | ℛgas ( † ) | ℛbar ( † ) |
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
[108 M⊙] | [108 M⊙] | [108 M⊙] | [kpc km s−1] | [kpc km s−1] | [kpc km s−1] | [kpc] | ||||||||||
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13) | (14) | (15) | (16) | (17) |
DDO 50 | 1.80 | 0.48 | 7.19 | 1.34 | 8.99 | 1.42 | 58 | 26 | 142 | 28 | 126 | 38 | 0.90 | 1.00 | 0.97 | 0.97 |
DDO 52 | 0.88 | 0.23 | 2.44 | 0.43 | 3.31 | 0.48 | 66 | 13 | 153 | 17 | 130 | 31 | 0.94 | 0.99 | 0.70 | 0.75 |
DDO 87 | 0.41 | 0.26 | 2.04 | 1.24 | 2.44 | 1.27 | 83 | 34 | 141 | 53 | 132 | 118 | 1.13 | 0.25 | 0.79 | 0.77 |
DDO 126 | 0.33 | 0.10 | 1.45 | 0.31 | 1.78 | 0.33 | 40 | 20 | 62 | 8 | 58 | 18 | 0.82 | 0.98 | 0.85 | 0.88 |
DDO 133 | 0.43 | 0.29 | 1.16 | 0.77 | 1.59 | 0.82 | 49 | 24 | 65 | 26 | 60 | 54 | 0.80 | 0.90 | 0.92 | 0.92 |
DDO 168 | 0.84 | 0.22 | 2.71 | 0.52 | 3.55 | 0.57 | 64 | 14 | 109 | 13 | 98 | 26 | 1.03 | 0.99 | 0.87 | 0.89 |
NGC 4639 | 166.10 | 45.35 | 17.01 | 2.78 | 183.10 | 45.43 | 830 | 48 | 1394 | 70 | 882 | 63 | 1.68 | 0.99 | 0.90 | 0.97 |
NGC 4725 | 523.10 | 144.00 | 35.08 | 5.86 | 558.20 | 144.10 | 1914 | 160 | 3568 | 270 | 2018 | 170 | 3.39 | 1.00 | 0.98 | 1.00 |
NGC 5584 | 114.40 | 31.21 | 22.84 | 3.73 | 137.20 | 31.43 | 757 | 77 | 1022 | 83 | 802 | 89 | 2.63 | 0.97 | 0.93 | 0.96 |
Notes. (1) Name. (2) and (3) Stellar mass and uncertainty. (4) and (5) Gas mass and uncertainty. (6) and (7) Baryonic mass and uncertainty. (8) and (9) Stellar specific angular momentum and uncertainty. (10) and (11) Gas specific angular momentum and uncertainty. (12) and (13) Baryonic specific angular momentum and uncertainty. (14) Exponential disc scale length. (15)–(17) Convergence factor for the j*, jgas and jbar profiles. The complete version of this table is available at the CDS. ( † )These convergence criteria should be seen as an indication of the convergence of the j profiles rather than taken at face value to predict the exact value of j. In addition to this, values below 0.7 should be taken with extra caution as we find them to be low not necessarily because they are very far from convergence, but because they rely on an extrapolation of a polynomial that it is usually monotonically increasing for those profiles. Along this paper we used ℛ ≥ 0.8 to define a j profile as convergent.
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