Table 1: Effective areas and transmission factors of the SPI gamma-ray camera for the observation conditions of the flare obtained by MGGPOD simulations with a detailed model of SPI and the spacecraft.
$E_{\gamma}$ (keV) origin eff. area (cm²) transmission (%)

1369 ²⁴Mg $^{\star}_{1369}$ 3.6 2.8

1634 ²⁰Ne $^{\star}_{1634}$ 4.6 4.0

1779 ²⁸Si $^{\star}_{1779}$ 5.0 4.5

2223 ¹H(n, $\gamma$ )²H 5.4 5.7

4438 ¹²C $^{\star}_{4439}$ 5.2 8.7

6129 ¹⁶O $^{\star}_{6130}$ 4.1 9.3

6916 ¹⁶O $^{\star}_{6917}$ 3.6 9.4

7115 ¹⁶O $^{\star}_{7117}$ 3.6 9.4

**Table 1:** Effective areas and transmission factors of the SPI gamma-ray camera for the observation conditions of the flare obtained by MGGPOD simulations with a detailed model of SPI and the spacecraft.
$E_{\gamma}$ (keV)	origin	eff. area (cm²)	transmission (%)
1369	²⁴Mg $^{\star}_{1369}$	3.6	2.8
1634	²⁰Ne $^{\star}_{1634}$	4.6	4.0
1779	²⁸Si $^{\star}_{1779}$	5.0	4.5
2223	¹H(n, $\gamma$ )²H	5.4	5.7
4438	¹²C $^{\star}_{4439}$	5.2	8.7
6129	¹⁶O $^{\star}_{6130}$	4.1	9.3
6916	¹⁶O $^{\star}_{6917}$	3.6	9.4
7115	¹⁶O $^{\star}_{7117}$	3.6	9.4

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