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Table 1.

Main properties of the DWALIN galaxy sample.

Galaxy RA (J2000) Dec (J2000) D (M,SFR)
h m s ° ′ ″ Mpc kpc method
(1) (2) (3) (4) (5) (6) (7) (8)
CGCG007-025 09 44 01.9 −00 38 32 23 ± 5FM 8.07 ± 0.24 −0.64 ± 0.13 0.85 ± 0.03 1
ESO 154-G023 02 56 50.4 −54 34 17 6.0 ± 0.5CF3 8.18 ± 0.22 −1.39 ± 0.10 3.19 ± 0.08 1
ESO 320-G014 11 37 53.2 −39 13 13 6.0 ± 0.5CF3 6.98 ± 0.20 −2.92 ± 0.14 0.24 ± 0.02 4
ESO 321-G014 12 13 49.6 −38 13 53 3.3 ± 0.2CF3 6.98 ± 0.20 −3.00 ± 0.10 0.30 ± 0.01 4
ESO 349-G031 00 08 13.4 −34 34 42 3.2 ± 0.3CF3 6.55 ± 0.20 −3.34 ± 0.10 0.27 ± 0.01 4
ESO 379-G007 11 54 43.5 −33 33 36 5.4 ± 0.5CF3
ESO 379-G024 12 04 56.7 −35 44 35 5.5 ± 0.2STD 6.71 ± 0.22 −2.90 ± 0.11 0.38 ± 0.04 5
ESO 489-G56 06 26 17.6 −26 15 56 6.3 ± 0.6CF3 7.47 ± 0.15 −3.11 ± 0.17 0.63 ± 0.04 3
HIPASS J1133-32 11 33 10.9 −32 57 45 5.6 ± 0.5CF3 6.69 ± 0.21 −3.09 ± 0.11 0.27 ± 0.03 5
HIPASS J1337-39 13 37 25.3 −39 53 48 5.1 ± 0.5CF3 5.99 ± 0.27 −2.73 ± 0.09 0.25 ± 0.02 1
Haro 11 00 36 52.7 −33 33 17 86 ± 17FM 10.24 ± 0.25 1.78 ± 0.16 2.23 ± 0.15 1
Henize 2-10 08 36 15.1 −26 24 34 8.2 ± 0.8CF3 9.05 ± 0.32 0.22 ± 0.17 0.69 ± 0.01 3
IC 2828 11 27 11.2 +08 43 53 13 ± 2FM 8.05 ± 0.22 −1.49 ± 0.11 0.52 ± 0.02 1
IC 3077 12 15 56.3 +14 25 59 5 ± 2TFR 7.78 ± 0.20 −3.94 ± 0.38 0.51 ± 0.01 4
IC 4870 19 37 37.6 −65 48 43 8.5 ± 0.8CF3 8.53 ± 0.20 −1.28 ± 0.09 0.64 ± 0.03 1
IIZw40 05 55 42.6 +03 23 32 14 ± 3FM 9.03 ± 0.25 0.37 ± 0.25 1.31 ± 0.11 1
J0405-3648 04 05 20.3 −36 49 01 9 ± 2FM 7.03 ± 0.20 −2.31 ± 0.10 0.29 ± 0.01 4
J0921+0721 09 21 27.2 +07 21 53 21 ± 4FM 8.03 ± 0.22 −1.64 ± 0.10 1.47 ± 0.03 4
J1044+0353 10 44 58.0 +03 53 13 52 ± 10FM 7.83 ± 0.24 −0.76 ± 0.11 0.80 ± 0.08 1
J1418+2102 14 18 49.9 +21 02 26 29 ± 6FM 6.59 ± 0.36 −1.32 ± 0.17 5.95 ± 0.14 3
KK182 13 05 02.8 −40 04 59 5.9 ± 0.5CF3 6.50 ± 0.24 −2.47 ± 0.10 0.49 ± 0.03 1
KK195 13 21 08.0 −31 31 48 5.6 ± 0.3STD - −3.33 ± 0.70 0.63 ± 0.02 4
KKH046 09 08 36.5 +05 17 27 12 ± 2FM 7.09 ± 0.20 −2.37 ± 0.10 0.74 ± 0.02 4
Leo P 10 21 45.1 +18 05 17 1.6 ± 0.1a 5.75 ± 0.30a −4.40 ± 0.38 0.07 ± 0.01 5
NGC 0337 00 59 50.1 −07 34 41 19 ± 3CF3 9.75 ± 0.21 0.12 ± 0.12 3.05 ± 0.03 1
NGC 0625 01 35 04.6 −41 26 10 4.0 ± 0.4CF3 8.60 ± 0.19 −1.20 ± 0.14 0.61 ± 0.03 1
NGC 1487 03 55 46.1 −42 22 05 9 ± 2FM 9.00 ± 0.21 −0.68 ± 0.10 1.16 ± 0.04 1
NGC 1705 04 54 13.5 −53 21 40 5.5 ± 0.4CF3 8.13 ± 0.24 −1.31 ± 0.09 0.21 ± 0.01 1
NGC 1741 05 01 38.3 −04 15 25 56 ± 11FM 9.80 ± 0.25 0.85 ± 0.14 3.39 ± 0.23 1
NGC 2915 09 26 11.5 −76 37 35 4.3 ± 0.4CF3 8.21 ± 0.20 −1.47 ± 0.09 0.44 ± 0.01 1
NGC 3125 10 06 33.4 −29 56 05 15 ± 3FM 8.91 ± 0.24 −0.15 ± 0.14 0.68 ± 0.04 1
NGC 5253 13 39 56.0 −31 38 24 3.5 ± 0.2CF3 8.64 ± 0.24 −0.26 ± 0.15 0.32 ± 0.01 1
SBS 0335-052 03 37 44.1 −05 02 40 59 ± 12FM 8.32 ± 0.24 0.07 ± 0.13 0.86 ± 0.01 1
Tol 1214-277 12 17 17.1 −28 02 33 100 ± 20FM 7.82 ± 0.30 −0.45 ± 0.10 1.46 ± 0.03 1
Tol 1924-416 19 27 58.2 −41 34 32 33 ± 6FM 8.87 ± 0.24 0.31 ± 0.11 0.96 ± 0.05 1
Tol 65 12 25 46.5 −36 14 01 33 ± 6FM 7.41 ± 0.24 −1.04 ± 0.11 0.54 ± 0.08 1
UGC 07983 12 49 47.0 +03 50 32 6 ± 1FM 7.08 ± 0.20 −3.02 ± 0.11 0.42 ± 0.01 4
UM 228 00 21 01.0 +00 52 48 423 ± 84FM 10.60 ± 0.29 1.37 ± 0.12 6.58 ± 0.97 1
UM 461 11 51 33.3 −02 22 22 19 ± 4FM 7.56 ± 0.24 −1.21 ± 0.12 0.53 ± 0.03 1
UM 462 11 52 37.2 −02 28 10 19 ± 4FM 8.36 ± 0.25 −0.60 ± 0.10 0.64 ± 0.01 1
VCC 2037 12 46 15.3 +10 12 20 9.6 ± 0.9STD 7.66 ± 0.16 −2.29 ± 0.09 0.57 ± 0.05 1

Notes. (1) Galaxy name. Systems studied in this work are highlighted in boldface. (2)–(3) Celestial coordinates in J2000 from NED; (4) Galaxy distance from the Extragalactic Distance Database, based on: CF3 – Cosmicflow-3 catalogue (Tully et al. 2016); FM – flow model (Kourkchi et al. 2020); STD – stellar distances from Jacobs et al. (2009) and Anand et al. (2021); TFR – Tully–Fisher relation distance from Kourkchi et al. (2022); (5)–(6) M and SFR as determined in this work; (7) Half-light radius in the GALEX NUV band or, when this is not available, in the WISE W4 band; (8) Method used to determine M and SFR, following the notation of Table 2. The a distance and M for Leo P are taken from McQuinn et al. (2015).

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