Pre-flight Background Estimates for COSI
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| Main Authors: | , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2025
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| author | Gallego, Savitri Oberlack, Uwe Lommler, Jan Karwin, Christopher M. Fenu, Francesco Fioretti, Valentina Zoglauer, Andreas Follega, F. M. Perinelli, A. Battiston, Roberto Iuppa, Roberto Boggs, E. Steven Mittal, Saurabh Jean, Pierre Kierans, Carolyn Hartmann, H. Dieter Tomsick, A. John |
| author_facet | Gallego, Savitri Oberlack, Uwe Lommler, Jan Karwin, Christopher M. Fenu, Francesco Fioretti, Valentina Zoglauer, Andreas Follega, F. M. Perinelli, A. Battiston, Roberto Iuppa, Roberto Boggs, E. Steven Mittal, Saurabh Jean, Pierre Kierans, Carolyn Hartmann, H. Dieter Tomsick, A. John |
| contents | The Compton Spectrometer and Imager (COSI) is a Compton telescope designed to survey the 0.2 - 5 MeV sky, consisting of a compact array of cross-strip germanium detectors. It is planned to be launched in 2027 into an equatorial low-Earth (530 km) orbit with a prime mission duration of 2 years. The observation of MeV gamma rays is dominated by background, mostly from extragalactic and atmospheric photon but also from the activation of the detector materials induced by cosmic-ray interactions. Thus, background simulation and identification are crucial for the data analysis. In this work we perform Monte Carlo simulations of the background for the first 3 months in orbit, and we extrapolate the results to 2 years in orbit, in order to determine the build-up of the activation due to long-lived isotopes. We determine the rates of events induced by the background that are reconstructed as Compton events in the simulated COSI data. We find that the extragalactic background photons dominate at low energies (<660 keV), while delayed activation from cosmic-ray primaries (proton/alpha) and albedo photons dominate at higher energies. As part of this work, a comparison at low latitude (<1 deg) between recent measurement of the SAA by the High-Energy Particle Detector (HEPD-01) on board the China Seismo-Electromagnetic Satellite (CSES-01) and the AP9/AE9 model has been made, showing an overestimation of the flux by a factor 9 by the model. The systematic uncertainties associated with these components are quantified. This work marks a major step forward in estimating and understanding the expected background rates for the COSI satellite mission. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2510_25304 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Pre-flight Background Estimates for COSI Gallego, Savitri Oberlack, Uwe Lommler, Jan Karwin, Christopher M. Fenu, Francesco Fioretti, Valentina Zoglauer, Andreas Follega, F. M. Perinelli, A. Battiston, Roberto Iuppa, Roberto Boggs, E. Steven Mittal, Saurabh Jean, Pierre Kierans, Carolyn Hartmann, H. Dieter Tomsick, A. John Instrumentation and Methods for Astrophysics The Compton Spectrometer and Imager (COSI) is a Compton telescope designed to survey the 0.2 - 5 MeV sky, consisting of a compact array of cross-strip germanium detectors. It is planned to be launched in 2027 into an equatorial low-Earth (530 km) orbit with a prime mission duration of 2 years. The observation of MeV gamma rays is dominated by background, mostly from extragalactic and atmospheric photon but also from the activation of the detector materials induced by cosmic-ray interactions. Thus, background simulation and identification are crucial for the data analysis. In this work we perform Monte Carlo simulations of the background for the first 3 months in orbit, and we extrapolate the results to 2 years in orbit, in order to determine the build-up of the activation due to long-lived isotopes. We determine the rates of events induced by the background that are reconstructed as Compton events in the simulated COSI data. We find that the extragalactic background photons dominate at low energies (<660 keV), while delayed activation from cosmic-ray primaries (proton/alpha) and albedo photons dominate at higher energies. As part of this work, a comparison at low latitude (<1 deg) between recent measurement of the SAA by the High-Energy Particle Detector (HEPD-01) on board the China Seismo-Electromagnetic Satellite (CSES-01) and the AP9/AE9 model has been made, showing an overestimation of the flux by a factor 9 by the model. The systematic uncertainties associated with these components are quantified. This work marks a major step forward in estimating and understanding the expected background rates for the COSI satellite mission. |
| title | Pre-flight Background Estimates for COSI |
| topic | Instrumentation and Methods for Astrophysics |
| url | https://arxiv.org/abs/2510.25304 |