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Table 1.

Galaxy sample.

Name RA Dec i PA DC log(LIR/L⊙) SFR S​60/S​100 L1.4 S​i/S
(h m s) (° ′ ″) (°) (°) (Mpc) (M⊙ yr−1) (1021 W Hz−1) (%)
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)
ESO 005-G004 06 05 36.5 −86 37 53 89 −86.8 22.36 10.16 2.15 0.39 5.55 18.46
ESO 079-G003 00 32 02.0 −64 15 14 87 −48.5 35.31 10.51 4.84 0.40 8.81 38.09
ESO 163-G011 07 38 04.3 −55 11 27 84 3.3 38.7 10.5 4.74 0.47 8.49 –
ESO 209-G009 07 58 14.9 −49 51 09 88 −25.9 11.81 9.81 0.95 0.38 1.93 1.72
ESO 428-G028 07 23 38.3 −30 03 08 89 60.1 31.08 10.35 3.32 0.41 5.68 11.46
IC 3908 12 56 41.1 −07 33 46 82 −8.3 (−10.0) 20.28 10.07 1.74 0.51 3.35 11.85
IC 4595 16 20 44.4 −70 08 35 88 59.7 45.75 10.78 8.87 0.38 19.24 8.26
NGC 134 00 30 21.6 −33 14 38 81 49.6 15.9 10.37 3.46 0.38 6.52 0.79
NGC 1406 03 39 23.2 −31 19 20 85 16.6 18.98 10.22 2.46 0.47 5.80 44.65
NGC 1421 03 42 27.7 −13 29 23 82 0.9 21.2 10.25 2.62 0.48 5.54 21.11
NGC 1448 03 44 32.1 −44 38 41 87 41.7 11.47 9.78 0.90 0.32 1.80 2.23
NGC 1532 04 12 01.2 −32 53 11 83 34.2 15.51 10.01 1.51 0.31 3.32 0.98
NGC 2221 06 20 16.0 −57 34 43 80 −0.6 33.83 10.39 3.63 0.46 6.26 15.69
NGC 2613 08 33 23.2 −22 58 28 82 −72.0 20.18 10.18 2.27 0.29 3.05 0.59
NGC 2706 08 56 12.2 −02 33 47 83 −11.6 24.36 10.15 2.09 0.47 3.76 9.69
NGC 3175 10 14 42.9 −28 52 25 81 55.1 13.45 9.96 1.37 0.44 1.80 39.36
NGC 3263 10 29 12.3 −44 07 13 81 −78.0 38.79 10.66 6.78 0.45 25.21 59.66
NGC 3717 11 31 31.2 −30 18 24 85 32.0 21.39 10.29 2.90 0.46 4.17 61.75
NGC 4666 12 45 07.7 −00 27 41 81 40.6 12.82 10.36 3.42 0.43 8.76 2.86
NGC 4835 12 58 08.2 −46 15 56 81 −30.5 23.96 10.57 5.48 0.44 13.30 2.96
NGC 5073 13 19 18.5 −14 50 30 88 −31.1 37.09 10.6 5.95 0.62 6.77 74.65
NGC 7090 21 36 28.4 −54 33 30 88 −51.8 7.65 9.22 0.25 0.41 0.36 –
UGCA 150 09 10 49.5 −08 53 36 87 29.5 26.85 10.3 2.96 0.29 4.01 3.07
UGCA 394 14 47 24.1 −17 26 49 88 −3.9 (−10.0) 30.02 10.26 2.67 0.55 3.71 48.75
UGCA 402 15 13 30.6 −20 40 29 85 61.8 30.94 10.34 3.21 0.40 6.95 6.76

Notes. (1) Galaxy name. (2) J2000 coordinates of the IRAS source. (3) Inclination calculated using INCLINET. (4) Position angle, measured from the north, between 90° and −90°. Obtained from HYPERLEDA (http://leda.univ-lyon1.fr/; Makarov et al. 2014). For IC 3908 and UGCA 394 we had to use slightly different values, shown in parenthesis, to ensure that the major axis was horizontal after rotating them. (5) Comoving distance, taken from Condon et al. (2021). (6) Logarithm of the absolute IR (8 < λ[μm]< 1000) luminosity in units of the solar bolometric luminosity L⊙ = 3.83 × 1026 W, taken from Sanders & Mirabel (1996). (7) The SFR calculated as SFR = 0.39 LIR/1043 erg s−1 (Heesen et al. 2018). (8) 60 μm to 100 μm IR IRAS flux ratio (Dahlem et al. 2001). (9) Total 1.4 GHz luminosity obtained from the MeerKAT 1.28 GHz flux densities. We assumed that S​1.4 ≈ 0.94 S​1.28 given that most star-forming galaxies have spectral indices near α ≈ −0.7, with S(ν)∝να (Condon 1992). (10) Contribution of the compact central source to the total flux density of the galaxy (Condon et al. 2021).

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