Table 3.
Population of SySts and SNe Ia rate from symbiotic progenitors for galaxies in the LG.
| Galaxy | MV | fbin | #SySt | known | SNe rate [yr−1] |
|---|---|---|---|---|---|
| Milky Way | −20.9 | function& | (53 ± 6)×103 | 283 | (2.8 ± 0.1)×10−5 |
| LMC | −18.5 | 0.30† | 2300 ± 300 | 10 | (1.2 ± 0.1)×10−6 |
| SMC | −17.1 | 0.30† | 650 ± 80 | 12 | (3.4 ± 0.2)×10−7 |
| NGC 205 | −16.4 | (0.25–0.75)* | 340 ± 40 | 1 | (1.8 ± 0.1)×10−7 |
| IC 10 | −16.3 | (0.25–0.75)* | 310 ± 40 | 1 | (1.6 ± 0.1)×10−7 |
| NGC 6822 | −16.0 | (0.25–0.75)* | 230 ± 30 | 1 | (1.2 ± 0.1)×10−7 |
| NGC 185 | −15.6 | (0.25–0.75)* | 160 ± 20 | 1 | (8.7 ± 0.4)×10−8 |
| IC 1613 | −15.3 | (0.25–0.75)* | 120 ± 20 | 0 | (6.6 ± 0.3)×10−8 |
| NGC 147 | −15.1 | (0.25–0.75)* | 100 ± 10 | 0 | (5.4 ± 0.3)×10−8 |
| WLM | −14.4 | (0.25–0.75)* | 50 ± 6 | 0 | (2.9 ± 0.1)×10−8 |
| Sagittarius | −13.8 | (0.36–0.40)‡ | 30 ± 4 | 0 | (1.6 ± 0.1)×10−8 |
| Fornax | −13.1 | 0.44c–0.87a | 16 ± 2 | 0 | (8.6 ± 0.4)×10−9 |
| Leo II | −10.1 | 0.33b–0.36a | 1 | 0 | (5.5 ± 0.3)×10−10 |
| Sculptor | −9.8 | 0.58a–0.59c | 0 | 0 | (3.0 ± 0.2)×10−10 |
| Sextans | −9.5 | 0.68c–0.71a | 0 | 0 | (3.2 ± 0.2)×10−10 |
| Carina | −9.4 | 0.14c–0.20a | 0 | 0 | (2.9 ± 0.1)×10−10 |
| Draco | −8.6 | 0.50a | 0 | 1 | (1.4 ± 0.1)×10−10 |
| Ursa Minor | −8.5 | 0.78a | 0 | 0 | (1.3 ± 0.1)×10−10 |
| Hercules | −6.6 | 0.47d | 0 | 0 | (2.2 ± 0.1)×10−11 |
| Leo IV | −5.5 | 0.47d | 0 | 0 | (8.2 ± 0.5)×10−12 |
Notes. The first column gives the galaxies’ designations. The second column, the visual absolute magnitudes, MV (McConnachie 2012). The third column the binary fractions. SySt populations, # SySt, are rounded and given in the fourth column. The fifth column displays the confirmed SySt population, from the literature (Akras et al. 2019; Merc et al. 2019a,b). And the sixth column the derived SNe Ia rates. Starting on Sagittarius, to the bottom of the table, all galaxies are dwarf spheroidals. &: multiplicity frequency as a function of M1 (Duchêne & Kraus 2013).*: Range of values used on absence of observed ones. †: Assumed based on the mean binary fraction value for LMC globular clusters (Milone et al. 2009), and in accordance with stellar formation history for SMC and LMC as commented by Rubele et al. (2011) and references therein. ‡: Derived from radial velocity dispersion, but with high uncertainty (Bonidie et al. 2022). a: Spencer et al. (2018); b: Spencer et al. (2017); c: Minor (2013); d: Geha et al. (2013).
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