Table 1.
Properties of our compiled dataset for NGC 1512, NGC 4535, and NGC 7496 (from PHANGS-MeerKAT; this work) and IC1954, NGC 1566, NGC 1672, NGC 3511, and NGC 5068 (from MHONGOOSE, de Blok et al. 2016).
| Galaxy | Morph. | RA | Dec | Dist. | Reff | r25 | i | PA | l⋆ | M⋆ | SFR |
|---|---|---|---|---|---|---|---|---|---|---|---|
| [°] | [°] | [Mpc] | [kpc] | [°] | [°] | [kpc] | [log(M⊙)] | [log(M⊙ yr−1)] | |||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | |
| IC 1954 | Sb | 52.522 | −52.074 | 12.8 | 2.4 | 5.6 | 57.1 | 63.4 | 1.5 | 9.7 | −0.4 |
| NGC 1512 | SB(r)ab | 60.976 | −43.349 | 18.8 | 4.8 | 23.1 | 42.5 | 261.9 | 6.2 | 10.7 | 0.1 |
| NGC 1566 | SABb | 65.002 | −54.938 | 17.7 | 3.2 | 18.6 | 29.5 | 214.7 | 3.9 | 10.8 | 0.7 |
| NGC 1672 | Sb | 71.427 | −59.247 | 19.4 | 3.4 | 17.4 | 42.6 | 134.3 | 5.8 | 10.7 | 0.9 |
| NGC 3511 | SABc | 165.238 | −22.817 | 13.9 | 3.0 | 12.3 | 75.1 | 256.8 | 2.4 | 10.4 | 0.1 |
| NGC 4535 | SAB(s)c | 188.585 | 8.198 | 15.8 | 6.3 | 18.7 | 44.7 | 179.7 | 3.8 | 10.5 | 0.3 |
| NGC 5068 | Sc | 199.728 | −21.039 | 5.2 | 2.0 | 5.7 | 35.7 | 342.4 | 1.3 | 9.4 | −0.6 |
| NGC 7496 | SBb | 347.447 | −43.428 | 18.7 | 3.8 | 9.1 | 35.9 | 193.7 | 1.5 | 10.0 | 0.4 |
Notes. We provide in columns from left to right the galaxy name, morphological type (Morph.), central right ascension (RA) and declination (Dec.), distance (Dist.), effective radius (Reff), optical radius (r25), inclination (i), position angle (P.A.), stellar scale length (l⋆), the total mass of stars (M⋆), and global star formation rate (SFR). (1): The morphological classifications are from HyperLEDA (Makarov et al. 2014). (2–3): Central positions are taken from Salo et al. (2015). (4): Source distances are taken from Anand et al. (2021). (5): Reff contains half of the stellar mass of the galaxy and is taken from Leroy et al. (2021b). (6): r25 is based on the radial position of the isophote at 25 mag arcsec−2 and is taken from Leroy et al. (2021b) that are drawn from RC3 (de Vaucouleurs et al. 1991) via HyperLEDA. (7–8): From Lang et al. (2020), based on PHANGS CO(2–1) kinematics for the inner disk. (9): The profile-based stellar scale length is taken from Leroy et al. (2021b). (10–11): Derived by Leroy et al. (2021b), using GALEX UV and WISE IR photometry, following a similar methodology to Leroy et al. (2019).
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