Table 1.
Parameters of the sample galaxies.
| Name | Distance | TC | Vrot | Diameter | M⋆ | MHI | SFR | ΣSFR |
|---|---|---|---|---|---|---|---|---|
| (Mpc) | (km s−1) | (kpc) | (× 1010 M⊙) | (× 1010 M⊙) | (M⊙ yr−1) | (×10−3 M⊙ yr−1 kpc−2) | ||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) |
| NGC 2613 | 23.4 | 3.0 ± 0.3 | 290.6 | 33.7 | 12.0 ± 0.2 | 0.712 (a) | 3.36 ± 0.35 | 3.77 ± 0.39 |
| NGC 2683 | 6.27 | 3.0 ± 0.3 | 202.6 | 9.39 | 1.49 ± 0.02 | 0.052 (b) | 0.25 ± 0.03 | 3.54 ± 0.40 |
| NGC 2820 | 26.5 | 5.0 ± 0.5 | 162.8 | 13.8 | 0.467 ± 0.013 | 1.424 (c) | 1.35 ± 0.14 | 9.00 ± 0.96 |
| NGC 2992 | 34.0 | 1.0 ± 0.3 | 58.7 | 12.5 | 5.26 ± 0.09 | 0.738 (d) | 5.91 ± 0.54 | 48.2 ± 4.4 |
| NGC 3003 | 25.4 | 4.0 ± 0.6 | 120.6 | 27.7 | 0.485 ± 0.010 | 1.072 (b) | 1.56 ± 0.16 | 2.59 ± 0.27 |
| NGC 3044 | 20.3 | 5.0 ± 0.5 | 152.6 | 18.1 | 0.660 ± 0.013 | 0.363 (b) | 1.75 ± 0.16 | 6.79 ± 0.60 |
| NGC 3432 | 9.42 | 9.0 ± 0.3 | 109.9 | 9.96 | 0.100 ± 0.002 | 0.222 (c) | 0.51 ± 0.06 | 6.36 ± 0.69 |
| NGC 3448 | 24.5 | 5.0 ± 0.0 | 119.5 | 12.5 | 0.564 ± 0.011 | 0.832 (b) | 1.78 ± 0.18 | 14.5 ± 1.5 |
| NGC 3556 | 14.1 | 6.0 ± 0.3 | 153.2 | 24.9 | 2.81 ± 0.04 | 0.479 (b) | 3.57 ± 0.30 | 7.32 ± 0.62 |
| NGC 3735 | 42.0 | 5.0 ± 0.5 | 241.1 | 34.4 | 14.9 ± 0.2 | 1.160 (c) | 6.23 ± 0.57 | 6.71 ± 0.61 |
| NGC 3877 | 17.7 | 5.0 ± 0.3 | 155.1 | 18.5 | 2.74 ± 0.04 | 0.148 (b) | 1.35 ± 0.12 | 5.04 ± 0.44 |
| NGC 4096 | 10.3 | 5.0 ± 0.3 | 144.8 | 11.8 | 0.613 ± 0.010 | 0.145 (b) | 0.71 ± 0.08 | 6.52 ± 0.77 |
| NGC 4157 | 15.6 | 3.0 ± 0.5 | 188.9 | 16.6 | 2.92 ± 0.04 | 0.525 (b) | 1.76 ± 0.18 | 8.15 ± 0.83 |
| NGC 4217 | 20.6 | 3.0 ± 0.3 | 187.6 | 23.4 | 4.74 ± 0.07 | 0.275 (b) | 1.89 ± 0.18 | 4.40 ± 0.42 |
| NGC 4244 | 4.40 | 6.0 ± 0.3 | 97.8 | 14.8 | 0.090 ± 0.002 | 0.067 (c) | 0.06 ± 0.01 | 0.37 ± 0.04 |
| NGC 4302 | 19.4 | 5.0 ± 0.5 | 167.4 | 3.82 | 3.43 ± 0.05 | 0.174 (b) | 0.92 ± 0.08 | 2.52 ± 0.21 |
| NGC 4594 | 12.7 | 1.0 ± 0.3 | 408.0 | 22.0 | 26.1 ± 0.4 | 0.033 (c) | 0.43 ± 0.04 | 1.14 ± 0.10 |
| NGC 4666 | 27.5 | 5.0 ± 0.3 | 192.9 | 32.3 | 12.5 ± 0.2 | 1.096 (b) | 10.5 ± 0.9 | 12.8 ± 1.1 |
| NGC 4845 | 17.0 | 2.0 ± 0.3 | 176.0 | 10.4 | 2.89 ± 0.05 | 0.009 (c) | 0.62 ± 0.06 | 7.33 ± 0.68 |
| NGC 5084 | 23.4 | −2.0 ± 0.3 | 312.9 | 4.99 | 12.3 ± 0.2 | 0.912 (b) | − | − |
| NGC 5297 | 40.4 | 4.5 ± 0.5 | 189.5 | 25.9 | 3.69 ± 0.07 | 1.992 (e) | 3.00 ± 0.33 | 5.70 ± 0.62 |
| NGC 5792 | 31.7 | 3.0 ± 0.3 | 208.6 | 23.7 | 8.89 ± 0.16 | 1.413 (b) | 4.41 ± 0.37 | 10.0 ± 0.8 |
| UGC10288 | 34.1 | 5.3 ± 0.6 | 167.1 | 21.3 | 2.03 ± 0.05 | 0.955 (b) | 0.66 ± 0.07 | 1.85 ± 0.21 |
Notes. Galaxy parameters. (1) Galaxy name. (2) Distance, obtained from Vargas et al. (2019). (3) TC, the morphological type code from de Vaucouleurs et al. (1991), except for NGC 3448, which is from Huchra et al. (2012). (4) Vrot is the maximum atomic gas rotation velocity corrected for inclination obtained from HyperLeda (http://leda.univ-lyon1.fr/), as also noted in Makarov et al. (2014). (5) Diameter, derived from 22 μm data by Wiegert et al. (2015). (6) M⋆ is the stellar mass from Li et al. (2016a), which is derived from the 2MASSK-band apparent magnitude (Skrutskie et al. 2006). (7) MHI, the total atomic gas mass, is directly available for 14 galaxies from Zheng et al. (2022). The source of the H I flux is indicated by superscript, and the detailed calculation methods are summarised in Sect. 4.1. References and corresponding observational instruments are as follows:
Chaves & Irwin (2001) with VLA L-band CnB-array;
Zheng et al. (2022) with VLA L-band C-array;
Courtois & Tully (2015), who uniformly processed data from various telescopes (NGC 2820 and NGC 3735 from Green Bank 42 m; NGC 3432, NGC 4244, and NGC 4594 from Robert C. Byrd Green Bank Telescope; NGC 4845 from Arecibo with line feed system.);
Huchtmeier (1982) with NRAO 91 m;
Davis & Seaquist (1983) with NRAO 91 m. (8) SFR is the revised star formation rate from Vargas et al. (2019), calculated using a combination of Hα and 22 μm data. (9) ΣSFR is the surface density of SFR and calculated using the 22 μm diameter and obtained from Vargas et al. (2019).
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