Table B.1
Properties of the galaxy sample.
| Galaxy | i | PA | Morph. | Dist. | Reff | Metal. | MHI | MH2 | M⋆ | SFR |
|---|---|---|---|---|---|---|---|---|---|---|
| ° | ° | Mpc | kpc | 12+log(O/H) | log(M⊙) | log(M⊙) | log(M⊙) | log(M⊙ yr−1) | ||
| (a) | (a) | (b) | (c) | (d) | (e) | (f) | (g) | (h) | (h) | |
| IC 5332 | 26.9 | 74.4 | SABc | 9.0 | 3.6 | 8.37 | 9.3 | − | 9.7 | −0.4 |
| NGC 0628* | 8.9 | 20.7 | Sc | 9.8 | 3.9 | 8.48 | 9.7 | 9.4 | 10.3 | 0.2 |
| NGC 1087 | 42.9 | 359.1 | Sc | 15.9 | 3.2 | 8.40 | 9.1 | 9.2 | 9.9 | 0.1 |
| NGC 1300 | 31.8 | 278.0 | Sbc | 19.0 | 6.5 | 8.52 | 9.4 | 9.4 | 10.6 | 0.1 |
| NGC 1365 | 55.4 | 201.1 | Sb | 19.6 | 2.8 | 8.53 | 9.9 | 10.3 | 11.0 | 1.2 |
| NGC 1385 | 44.0 | 181.3 | Sc | 17.2 | 3.4 | 8.42 | 9.2 | 9.2 | 10.0 | 0.3 |
| NGC 1433 | 28.6 | 199.7 | SBa | 18.6 | 4.3 | 8.54 | 9.4 | 9.3 | 10.9 | 0.1 |
| NGC 1512 | 42.5 | 261.9 | Sa | 18.8 | 4.8 | 8.55 | 9.9 | 9.1 | 10.7 | 0.1 |
| NGC 1566 | 29.5 | 214.7 | SABb | 17.7 | 3.2 | 8.55 | 9.8 | 9.7 | 10.8 | 0.7 |
| NGC 1672 | 42.6 | 134.3 | Sb | 19.4 | 3.4 | 8.54 | 10.2 | 9.9 | 10.7 | 0.9 |
| NGC 2835 | 41.3 | 1.0 | Sc | 12.2 | 3.3 | 8.38 | 9.5 | 8.8 | 10.0 | 0.1 |
| NGC 3351 | 45.1 | 193.2 | Sb | 10.0 | 3.0 | 8.59 | 8.9 | 9.1 | 10.4 | 0.1 |
| NGC 3627 | 57.3 | 173.1 | Sb | 11.3 | 3.6 | 8.55 | 9.1 | 9.8 | 10.8 | 0.6 |
| NGC 4254 | 34.4 | 68.1 | Sc | 13.1 | 2.4 | 8.53 | 9.5 | 9.9 | 10.4 | 0.5 |
| NGC 4303 | 23.5 | 312.4 | Sbc | 17.0 | 3.4 | 8.56 | 9.7 | 9.9 | 10.5 | 0.7 |
| NGC 4321 | 38.5 | 156.2 | SABb | 15.2 | 5.5 | 8.56 | 9.4 | 9.9 | 10.7 | 0.6 |
| NGC 4535 | 44.7 | 179.7 | Sc | 15.8 | 6.3 | 8.54 | 9.6 | 9.6 | 10.5 | 0.3 |
| NGC 5068 | 35.7 | 342.4 | Sc | 5.2 | 2.0 | 8.30 | 8.8 | 8.4 | 9.4 | −0.6 |
| NGC 7496 | 35.9 | 193.7 | Sb | 18.7 | 3.8 | 8.49 | 9.1 | 9.3 | 10.0 | 0.4 |
Notes. We show in columns from left to right the galaxy name, inclination (i), position angle (PA), morphological type (Morph.), distance (Dist.), effective radius (Reff), globally averaged metallicity (12 + log(O/H)), total mass of atomic gas (MHI), molecular gas (MH2) and stars (M⋆), and global star formation rate (SFR). *We only make use of the archival "central" pointing observed with the F658N ACS HST filter, due to the lack of cross-over between the MUSE and newer F658N WFC3 HST filter "east" pointing (see Chandar et al. 2025). (a) From Lang et al. (2020), based on PHANGS CO(2–1) kinematics. For IC 5332, we use values from Salo et al. (2015). (b) Morphological classification taken from HyperLEDA (Makarov et al. 2014). (c) Source distances are taken from the compilation of Anand et al. (2021b,a). (d) Reff that contains half of the stellar mass of the galaxy (Leroy et al. 2021). (e) Averaged metallicity within the area mapped by MUSE, computed using the Scal method of Pilyugin & Grebel (2016); see Kreckel et al. (2019) for more details. (f) Total atomic gas mass taken from HYPERLEDA (Makarov et al. 2014). (g) Molecular gas mass determined from PHANGS CO(2–1) observations (see Leroy et al. 2021). CO was not detected at high enough significance in IC 5332 to allow a molecular gas mass to be determined. (h) Derived by Leroy et al. (2021), using GALEX UV and WISE IR photometry, following a similar methodology to Leroy et al. (2019).
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