Table 1.
Distances, SFRs, IR, and γ-ray fluxes and luminosities for all γ-ray emitting SFGs known.
| Galaxy | DL | Fγ | FIR | Ṁ∗ | log(Lγ) | log(LIR/L⊙) |
|---|---|---|---|---|---|---|
| [0.1 − 100 GeV] | [8 − 1000 μm] (l) | [0.1 − 100 GeV] | [8 − 1000 μm] | |||
| (Mpc) | (10−12 erg cm−2 s−1) | (10−9 erg cm−2 s−1) | (M⊙ yr−1) | (erg s−1) | ||
| M 31 | 0.77 ± 0.04 (a) | 2.29 ± 0.70 (f) | 127.2 ± 6.4 | 0.26 ± 0.02 (h) | 38.21 ± 0.14 | 9.37 ± 0.05 |
| NGC 253 | 3.56 ± 0.26 (a) | 8.78 ± 0.60 (f) | 92.5 ± 4.6 | 5.03 ± 0.76 (h) | 40.12 ± 0.07 | 10.56 ± 0.07 |
| SMC | 0.060 ± 0.003 (a) | 29.2 ± 1.2 (f) | 622 ± 31 | 0.027 ± 0.003 (i) | 37.10 ± 0.05 | 7.85 ± 0.05 |
| M 33 | 0.91 ± 0.04 (a) | 2.02 ± 0.38 (g) | 53.8 ± 2.7 | 0.29 ± 0.02 (h) | 38.30 ± 0.09 | 9.14 ± 0.04 |
| NGC 1068 | 10.1 ± 1.8 (b) | 7.46 ± 0.55 (f) | 31.6 ± 1.6 | 22.7 ± 8.1 (h) | 40.96 ± 0.16 | 11.00 ± 0.16 |
| LMC | 0.050 ± 0.003 (a) | 195.1 ± 8.5 (f) | 6777 ± 339 | 0.20 ± 0.03 (i) | 37.77 ± 0.06 | 8.72 ± 0.06 |
| NGC 2146 | 17.2 ± 3.2 (c) | 1.83 ± 0.36 (f) | 13.71 ± 0.69 | 14.0 ± 5.2 (h) | 40.81 ± 0.18 | 11.10 ± 0.16 |
| NGC 2403 | 3.18 ± 0.18 (a) | 1.22 ± 0.28 (g) | 4.73 ± 0.24 | 0.37 ± 0.03 (h) | 39.17 ± 0.11 | 9.17 ± 0.05 |
| M 82 | 3.53 ± 0.26 (a) | 10.36 ± 0.52 (f) | 143.6 ± 7.2 | 10.4 ± 1.6 (h) | 40.19 ± 0.07 | 10.75 ± 0.07 |
| NGC 3424 | 25.6 ± 1.8 (d) | 1.59 ± 0.35 (f) | 0.910 ± 0.046 | 1.59 ± 0.23 (j) | 41.10 ± 0.11 | 10.27 ± 0.07 |
| Arp 299 | 46.8 ± 3.3 (d) | 1.10 ± 0.33 (g) | 10.50 ± 0.52 | 97 ± 14 (k) | 41.46 ± 0.14 | 11.86 ± 0.07 |
| NGC 4945 | 3.72 ± 0.27 (a) | 11.51 ± 0.79 (f) | 63.6 ± 3.2 | 1.22 ± 0.16 (i) | 40.28 ± 0.07 | 10.44 ± 0.07 |
| Circinus | 4.21 ± 0.70 (e) | 7.1 ± 1.2 (f) | 29.8 ± 1.5 | 2.05 ± 0.63 (i) | 40.18 ± 0.16 | 10.22 ± 0.15 |
| Arp 220 | 80.9 ± 5.7 (d) | 2.91 ± 0.48 (f) | 7.80 ± 0.39 | 214 ± 32 (k) | 42.36 ± 0.09 | 12.20 ± 0.07 |
| Milky way | * | * | * | 1.90 ± 0.04 (m) | 38.91 ± 0.13 (n) | 10.15 ± 0.21 (n) |
References.
Derived from Ajello et al. (2020).
Computed from FUV (Gil de Paz et al. 2007) + IRAS 25 μm (Sanders et al. 2003) fluxes.
Computed from FUV (Cortese et al. 2012) + IRAS 25 μm (Sanders et al. 2003) fluxes.
Computed from Hα (Kennicutt et al. 2008) + IRAS 25 μm (Sanders et al. 2003) fluxes.
Computed from IRAS 12, 25, 60, and 100 μm fluxes of Brauher et al. (2008, for Circinus) and Sanders et al. (2003, for the remaining galaxies).
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