Table 1
Galaxy sample.
| Name | Alternative | Dist | M ∗ | M R | M ∗ / L R | b | SFR p | t p | ΣSFR(tp) | 12+log(O/H) | Ref. |
| name | (Mpc) | (107M⊙) | (M⊙/L⊙) | (10-3M⊙ yr-1) | (Myr) | (10-3M⊙ yr-1 kpc-2) | |||||
|
|
|||||||||||
| NGC 625 | ESO 297-G005 | 3.9 ± 0.4 | 26 ± 10 | −17.25 ± 0.24 | >0.6 | 3.0 ± 0.1 | 86 ± 20 | 820 ± 180 | 2.5 ± 0.6 | 8.08 ± 0.12 | a, g, l |
| NGC 1569 | UGC 3056 | 3.4 ± 0.2 | 70 ± 7 | −17.14 ± 0.25 | 1.7 ± 0.2 | 21 ± 1 | 240 ± 10 | 40 ± 10 | 8.5 ± 0.3 | 8.19 ± 0.02 | a, h, m |
| NGC 1705 | ESO 158-G013 | 5.1 ± 0.6 | >20 | −16.35 ± 0.26 | >1 | ~6 | 314 ± 78 | ~3 | 44 ± 11 | 8.21 ± 0.05 | b, i, l |
| NGC 2366 | UGC 3851 | 3.2 ± 0.4 | 26 ± 3 | −16.64 ± 0.27 | 1.0 ± 0.1 | 5.6 ± 0.4 | 160 ± 10 | 450 ± 50 | 2.6 ± 0.2 | 7.91 ± 0.05 | a, h, l |
| NGC 4068 | UGC 7047 | 4.3 ± 0.1 | 22 ± 3 | −15.67 ± 0.05 | 2.0 ± 0.3 | 4.7 ± 0.3 | 42 ± 3 | 360 ± 40 | 4.5 ± 0.3 | ... | a, h |
| NGC 4163 | UGC 7199 | 3.0 ± 0.1 | 10 ± 3 | −14.81 ± 0.10 | 2.0 ± 0.6 | 2.9 ± 0.6 | 12 ± 3 | 450 ± 50 | 3.8 ± 0.9 | 7.56 ± 0.14 | a, h, l |
| NGC 4214 | UGC 7278 | 2.7 ± 0.2 | >28 | −17.77 ± 0.24 | >0.4 | 3.1 ± 0.9 | 130 ± 40 | 450 ± 50 | 8.5 ± 2.6 | 8.22 ± 0.05 | a, h, l |
| NGC 4449 | UGC 7592 | 4.2 ± 0.5 | 210 ± 35 | −18.88 ± 0.26 | 1.0 ± 0.2 | 6.0 ± 0.5 | 970 ± 70 | 5 ± 3 | 28 ± 2 | 8.26 ± 0.09 | a, h, l |
| NGC 5253 | Haro 10 | 3.5 ± 0.4 | 154 ± 21 | −17.61 ± 0.27 | 2.4 ± 0.3 | 9.0 ± 0.9 | 400 ± 40 | 450 ± 50 | 29 ± 3 | 8.12 ± 0.05 | a, g, k |
| NGC 6789 | UGC 11425 | 3.6 ± 0.2 | 7 ± 2 | −15.09 ± 0.14 | 1.1 ± 0.3 | 3.8 ± 1.3 | 15 ± 5 | 565 ± 65 | 9.7 ± 3.2 | ... | a, i |
| UGC 4483 | ... | 3.2 ± 0.2 | 1.0 ± 0.2 | −12.97 ± 0.19 | 1.1 ± 0.3 | 14 ± 3 | 11 ± 2 | 565 ± 65 | 8.8 ± 3.5 | 7.56 ± 0.03 | a, i, l |
| UGC 6456 | VII Zw 403 | 4.3 ± 0.1 | 5 ± 2 | −14.41 ± 0.05 | 1.5 ± 0.6 | 7.6 ± 1.1 | 23 ± 3 | 16 ± 8 | 5.1 ± 0.7 | 7.69 ± 0.01 | a, j, n |
| UGC 6541 | Mrk 178 | 4.2 ± 0.2 | >0.8 | −14.61 ± 0.10 | >0.2 | ~3 | ~3 | ... | 1.2 ± 0.6 | 7.82 ± 0.06 | c, j, l |
| UGC 9128 | DDO 187 | 2.2 ± 0.1 | 1.3 ± 0.2 | −12.82 ± 0.12 | 1.6 ± 0.2 | 6.3 ± 1.4 | 5 ± 1 | 150 ± 50 | 4.4 ± 0.9 | 7.75 ± 0.05 | a, h, l |
| UGCA 290 | Arp 211 | 6.7 ± 0.4 | >1.0 | −14.09 ± 0.18 | >0.4 | ~3 | 42 ± 15 | ~15 | 16 ± 6 | ... | d, i |
| I Zw 18 | Mrk 116 | 18.2 ± 1.4 | >1.7 | −14.99 ± 0.26 | >0.3 | ~30 | ~100 | ~10 | ~127 | 7.20 ± 0.01 | e, j, k |
| I Zw 36 | Mrk 209 | 5.9 ± 0.5 | >0.8 | −14.88 ± 0.23 | >0.1 | ~7 | ~25 | ... | ~9.8 | 7.77 ± 0.01 | f, i, k |
| SBS 1415+437 | ... | 13.6 ± 1.4 | 17 ± 3 | −15.90 ± 0.25 | 1.3 ± 0.2 | 12 ± 2 | 150 ± 10 | 450 ± 50 | 8.3 ± 0.5 | 7.62 ± 0.03 | a, i, o |
Notes. Distances are derived from the TRGB. Stellar masses are calculated
integrating the SFHs and assuming i) a Salpeter IMF from 0.1 to 100 M⊙; and ii)
a gas-recycling efficiency of 30%. The birthrate parameter b is defined as
,
where SFRp is
the peak SFR over the past 1 Gyr and 
is
the mean SFR over the past 6 Gyr (see McQuinn et al.
2010a). tp is the look-back time at
SFRp.
ΣSFR(tp) is the SFR
surface density at tp, calculated as SFRp/
where Ropt is the
optical radius (see Table 3). The last column
provides references for the HST studies of the resolved stellar populations, the
integrated photometry, and the ionized gas metallicity, respectively.
Reference. (a) McQuinn et al. (2010a); (b) Annibali et al. (2003); (c) Schulte-Ladbeck et al. (2000); (d) Crone et al. (2002); (e) Annibali et al. (2013); (f) Schulte-Ladbeck et al. (2001); (g) Lauberts & Valentijn (1989); (h) Swaters & Balcells (2002); (i) Gil de Paz et al. (2003); (j) Papaderos et al. (2002); (k) Izotov & Thuan (1999); (l) Berg et al. (2012); (m) Kobulnicky & Skillman (1997); (n) Thuan & Izotov (2005); (o) Guseva et al. (2003).
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