AHEAD2020 · Horizon 2020 Research and Innovation Programme · GA 871158
AHEAD2020 · Horizon 2020 Research and Innovation Programme · GA 871158
WP 9.3.c "Understanding the interaction between soft protons and X-ray mirrors"
WP 9.3.c "Understanding the interaction between soft protons and X-ray mirrors"
* Authors: V.Fioretti(1), T. Mineo(2), R. Amato(2), S. Lotti(3), C. Macculi(3), S. Molendi(4), F. Gastaldello(4), M. Cappi(1), M. Dadina(1), S. Ettori(1)
* Authors: V.Fioretti(1), T. Mineo(2), R. Amato(2), S. Lotti(3), C. Macculi(3), S. Molendi(4), F. Gastaldello(4), G. Lanzuisi(1), M. Cappi(1), M. Dadina(1), S. Ettori(1)
* Description: The proton response matrix for the ATHENA telescope is composed by a Redistribution Matrix File (RMF)
* Description: The proton response matrix for the ATHENA telescope is composed by a Redistribution Matrix File (RMF)
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@@ -41,6 +42,10 @@ collecting the grasp of the optics, the filter transmission efficiency and the d
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@@ -41,6 +42,10 @@ collecting the grasp of the optics, the filter transmission efficiency and the d
* The files are formatted according to the NASA OGIP (Office of Guest Investigators Program) calibration database (caldb) format, and they are tested with the NASA HEASARC XSPEC analysis software tool.
* The files are formatted according to the NASA OGIP (Office of Guest Investigators Program) calibration database (caldb) format, and they are tested with the NASA HEASARC XSPEC analysis software tool.
### Documentation
The detailed description of the activity, including the verification and validation, can be found in the [WP 9.8 Technical Note](https://www.ict.inaf.it/gitlab/proton_response_matrix/xmm-newton-proton-response-files/-/blob/main/docs/AHEAD2020_WP9.8_SOFTPROTONS_report_FINAL_v1.2.pdf).
### Built with
### Built with
The current release of the proton response files is based on:
The current release of the proton response files is based on:
* Geant4 v10.4 [Agostinelli et al. NIMPA, 506, 250, 2003; Allison et al. ITNS, 53, 270, 2006; Allison et al. NIMPA, 835, 186, 2016]
* Geant4 v10.4 [Agostinelli et al. NIMPA, 506, 250, 2003; Allison et al. ITNS, 53, 270, 2006; Allison et al. NIMPA, 835, 186, 2016]
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@@ -54,6 +59,8 @@ The current release of the proton response files is based on:
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@@ -54,6 +59,8 @@ The current release of the proton response files is based on:
* The RMF and ARF files can be loaded with any X-ray analysis software compliant with the NASA caldb format.
* The RMF and ARF files can be loaded with any X-ray analysis software compliant with the NASA caldb format.
* Since the accuracy of the Geant4 modeling of the proton stopping power degrades below 1 keV (20% at 1 keV reported in the Geant4 Physics Reference Manual), the energy redistribution is modelled from 1 keV to the upper threshold of the instrument X-ray RMF.
* Since the accuracy of the Geant4 modeling of the proton stopping power degrades below 1 keV (20% at 1 keV reported in the Geant4 Physics Reference Manual), the energy redistribution is modelled from 1 keV to the upper threshold of the instrument X-ray RMF.
* contrary to the X-ray ARFs, the proton ARF stores the grasp, in cm2 sr. For this reason, the input proton model obtained by deconvolving the observed spectrum with the response files is in units of protons/s/keV/sr.
* The spectra obtained from the response files are normalized for the simulated detection area, stored in the header of the response files. This area can be different from the actual detection area and the observed spectra must be corrected in order to be normalized for the simulated and not the in-flight observation area.
* The WFI response files are available with two optical filter configurations:
* The WFI response files are available with two optical filter configurations:
