Table 1
Summary of γ-ray line fluxes from the Local Bubble.
| Model | Line | Total | Isotropic | Isotro- |
|---|---|---|---|---|
| energy | flux | flux | pic ratio | |
| (keV) | (ph cm−2 s−1) | (ph cm−2 s−1 ) | (%) | |
| LB 1a | 1809 | 3.3 × 10−6 | 1.3 × 10−6 | 39 |
| LB 1b | 1809 | 3.4 × 10−6 | 1.6 × 10−6 | 48 |
| LB 2a | 1809 | 19.5 × 10−6 | 8.7 × 10−6 | 44 |
| LB 2b | 1809 | 6.7 × 10−6 | 1.9 × 10−6 | 28 |
| LB 1a | 1332 | 4.6 × 10−6 | 1.7 × 10−6 | 36 |
| LB 1b | 1332 | 4.7 × 10−6 | 2.1 × 10−6 | 43 |
| LB 2a | 1332 | 42.2 × 10−6 | 13.3 × 10−6 | 31 |
| LB 2b | 1332 | 32.2 × 10−6 | 6.2 × 10−6 | 19 |
| LB 1a | 511 | 21.4 × 10−6 | 5.3 × 10−6 | 25 |
| LB 1b | 511 | 20.6 × 10−6 | 7.9 × 10−6 | 39 |
| LB 2a | 511 | 2.0 × 10−6 | 0.2 × 10−6 | 13 |
| LB 2b | 511 | 1.7 × 10−6 | 0.2 × 10−6 | 12 |
Notes. Shown are fluxes for the two model assumptions of the Local Bubble, each with two different model-specific changes. 1) Geometric model: a) lmax = 40, b) lmax = 6 (see Fig. 1). 2) Hydrodynamics simulation: a) 14 SNe, b) 13 SNe. The four cases studied here provide a reasonable range of plausible fluxes. For cases 1a and 1b, we assume ejecta masses of 10−4 M⊙ for both isotopes (see Sect. 3.1.1 for details about the ejecta masses). In cases 2a and 2b, on the other hand, the ejecta mass is the difference between the instantaneous mass of the star at the last data point of the (rotating) stellar evolution model used and its predicted remnant mass, and thus depends on the initial mass of the star. Further systematic uncertainties are discussed in Sect. 6.
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