Compare commits
No commits in common. "0bb3ef1ec4974f7fe0d43f7687c3ee948365662a" and "0f7a63a6b5f4870054ca3b528323958b89c914a4" have entirely different histories.
0bb3ef1ec4
...
0f7a63a6b5
4 changed files with 54 additions and 81 deletions
Binary file not shown.
|
Before Width: | Height: | Size: 190 KiB |
|
|
@ -104,16 +104,13 @@ Status: \docstatus
|
|||
|
||||
%---> change abstract as required
|
||||
\begin{abstract}\normalsize
|
||||
%This document provides a concise summary of the key findings of the \acs{AHEPaM} \acs{DM} project.
|
||||
This document provides a concise summary of the key findings of the \acs{AHEPaM} \acs{DM} project.
|
||||
|
||||
This document summarizes the work performed at the University of Kiel (\acs{CAU}) for the \acs{ATHENA} High Energy Particle Monitor (\acs{AHEPaM}) demonstration model (\acs{DM}) project. It provides the key properties of \acs{AHEPaM}, describes the design of \acs{AHEPaM}, compares its expected performance with the original measurement requirements, discusses possible future trade studies, and gives an assessment of the current Technology Readiness Level (\acs{TRL}) of \acs{AHEPaM}.
|
||||
|
||||
|
||||
%\textcolor{red}{PK, from contract: "4.1.4. Executive Summary Report
|
||||
%The Executive Summary Report shall concisely summarise the findings of the Contract.
|
||||
%It shall be suitable for non-experts in the field and should also be appropriate for publication.
|
||||
%For this reason, it shall not exceed five (5) pages of text and ten (10) pages in total (one
|
||||
%thousand five hundred (1500) to three thousand (3000) words)."}
|
||||
\textcolor{red}{PK, from contract: "4.1.4. Executive Summary Report
|
||||
The Executive Summary Report shall concisely summarise the findings of the Contract.
|
||||
It shall be suitable for non-experts in the field and should also be appropriate for publication.
|
||||
For this reason, it shall not exceed five (5) pages of text and ten (10) pages in total (one
|
||||
thousand five hundred (1500) to three thousand (3000) words)."}
|
||||
\end{abstract}
|
||||
|
||||
%\newpage
|
||||
|
|
|
|||
|
|
@ -8,24 +8,40 @@
|
|||
\end{itemize}
|
||||
|
||||
|
||||
\acs{ATHENA}, the Advanced Telescope for High Energy Astrophysics, is the second large-class
|
||||
mission (L2) within the \acs{ESA} Cosmic Vision program. Due to steadily increasing cost, ATHENA was redefined into NewAthena in 2023. While the \acs{ATHENA} scientific community had requested the addition of a \acs{ATHENA} High Energy Particle Monitor (\acs{AHEPaM}) to the \acs{ATHENA} spacecraft (\acs{S/C}), this has now been removed from \acs{ESA}'s responsibility. If possible, \acs{AHEPaM} should be provided as a member-state contribution to NewAthena. This document gives a top-level summary of the development of \acs{AHEPaM} for the original \acs{ATHENA} mission.
|
||||
ATHENA, the Advanced Telescope for High Energy Astrophysics, is the second large-class
|
||||
mission (L2) within the ESA Cosmic Vision program. Due to steadily increasing cost, ATHENA was redefined into NewAthena in 2023. While the ATHENA scientific community had requested the addition of a ATHENA High Energy Particle Monitor (AHEPaM) to the ATHENA SC, this has now been removed from ESA's responsibility. If possible, AHEPaM should be provided as a member-state contribution to NewA
|
||||
|
||||
\acs{ATHENA} (and NewAthena) will observe the hot and energetic Universe in the X-ray spectral region and has been conceived to address two key questions in modern astrophysics:
|
||||
The mission will observe the hot and energetic Universe in the X-ray spectral region and
|
||||
has been conceived to address two key questions in modern astrophysics:
|
||||
How does ordinary matter form the large-scale structures that we see today?
|
||||
How do black holes grow and shape the Universe?
|
||||
ATHENA will comprise two instruments, the Wide Field Imager (\acs{WFI}) and the X-ray
|
||||
Integral Field Unit (\acs{X-IFU}).
|
||||
The \acs{WFI} consists of an active pixel sensor camera with a field of view of 40' x 40' (50' goal), a high count-rate capability and high time resolution.
|
||||
The \acs{X-IFU} provides spatially resolved high resolution (2.5 eV) spectroscopy within a field of view of 5' diameter (7' goal). The cooled Transition Edge Sensor (TES) technology of this instrument provides the necessary energy resolution, while providing exceptional efficiency compared to dispersive spectrometers flown on the current generation of X-ray observatories.
|
||||
ATHENA will comprise two instruments, the Wide Field Imager (WFI) and the X-ray
|
||||
Integral Field Unit (X-IFU).
|
||||
The WFI consists of an active pixel sensor camera with a field of view of 40' x 40' (50' goal),
|
||||
a high count-rate capability and high time resolution.
|
||||
The X-IFU provides spatially resolved high resolution (2.5 eV) spectroscopy within a field
|
||||
of view of 5' diameter (7' goal). The cooled Transition Edge Sensor (TES) technology of this
|
||||
instrument provides the necessary energy resolution, while providing exceptional efficiency
|
||||
compared to dispersive spectrometers flown on the current generation of X-ray
|
||||
observatories.
|
||||
|
||||
%The ATHENA scientific community requested the addition of a \acs{ATHENA} High Energy Particle Monitor (\acs{AHEPaM}) to the \acs{ATHENA} spacecraft.
|
||||
The need for \acs{AHEPaM} is driven by the calibration requirements [CAL-BKG-R-001] and [CAL-BKG-R-002] in \cite{cal-req-esa}. These are translated into 1\% knowledge on the energy ranges of protons (0.1-2 GeV), Helium ions (1-3 GeV), and electrons (0.05-1 GeV).
|
||||
The ATHENA scientific community has requested the addition of a ATHENA High Energy Particle
|
||||
Monitor (AHEPaM) to the ATHENA SC. AHEPaM driven by the calibration requirements [CAL-BKG-
|
||||
R-001] and [CAL-BKG-R-002] in [RD01]. These are translated into 1% knowledge on the ranges 0.1-2
|
||||
GeV, Helium ions of 1-3 GeV and electrons of 0.05-1 GeV
|
||||
|
||||
The main goal of AHEPaM is to ensure that the requirements on the
|
||||
knowledge of the “Non-X-ray Background” (NXB) are met. The NXB (a.k.a.
|
||||
“internal particle background”) is due to high-energy particles (primarily Galactic cosmic
|
||||
rays) that interact with the spacecraft and instruments and create showers of secondary
|
||||
particles. Many of the latter are detected as soft X-ray events. In this document, we will
|
||||
consider as “background” only this component. Cosmic ray particles are modulated by the
|
||||
solar cycle because the heliospheric magnetic field and the solar particle flux modulate the
|
||||
cosmic ray flux within the solar system. In particular, the cosmic ray flux is at a minimum
|
||||
when the solar cycle is at the maximum and, conversely, the cosmic ray flux is at a
|
||||
maximum during minima of the solar cycle.
|
||||
|
||||
The main goal of \acs{AHEPaM} was to ensure that the requirements on the knowledge of the “Non-X-ray Background” (\acs{NXB}) are met. The NXB (also known as “internal particle background”) is due to high-energy particles (primarily Galactic Cosmic Rays (\acs{GCR})) that interact with the spacecraft and instruments and create showers of secondary
|
||||
particles. Many of the latter are detected as soft X-ray events. Cosmic ray particles are modulated by the solar cycle because the heliospheric magnetic field, occasianally interrupted by solar particle events which can results in an additional \acs{NXB}. In particular, the \acs{GCR} flux is at a minimum during solar activity maximum and, conversely, the cosmic ray flux is at a maximum during solar activity minimum.
|
||||
|
||||
This executive report summarizes the findings of the work performed at \acs{CAU} in a manner suitable for non-experts in the field and is appropriate for publication. It summarizes the key properties of the \acs{AHEPaM} (in Tab.~\ref{tab:key-properties}, describes the design of \acs{AHEPaM}, compares its expected performance with the original measurement requirements, discusses possible future trade studies, and gives an assessment of the current Technology readiness Level (\acs{TRL}).
|
||||
|
||||
\begin{table}[h]
|
||||
\centering
|
||||
|
|
@ -56,37 +72,9 @@ This executive report summarizes the findings of the work performed at \acs{CAU}
|
|||
|
||||
|
||||
\section{AHEPaM Design}
|
||||
|
||||
The design of \acs{AHEPaM} was driven by the original measurement requirements which are summarized in Tab.~\ref{tab:orig-meas-req}. The statistical accuracy of 1\% in 2 energy bands within 3 ks for protons and 5\% for electrons in the ~1 GeV energy range determined the size, and thus mass, and envelope of \acs{AHEPaM}. Figure~\ref{fig:GCR-spec} shows typical \acs{GCR} spectra of protons and electrons as well as two straight-forward fits of a force-field solution to the data. The peak flux of protons can be seen as between one and two particles per m$²$
|
||||
|
||||
The large energy range to be covered includes relativistic, highly penetrating particles...
|
||||
|
||||
\begin{figure}
|
||||
\centering
|
||||
\includegraphics{cau-ath-er_i1-0/adriani-etal-combined-e-p.png}
|
||||
\caption{Measurements of galactic cosmic ray protons and electrons and fitted force field solutions.}
|
||||
\label{fig:GCR-spec}
|
||||
\end{figure}
|
||||
|
||||
\begin{table}[]
|
||||
\centering
|
||||
\begin{tabular}{|c|c|c|c|c|} \hline\\
|
||||
Requirement & Protons & Electrons & He ions & Motivation \\
|
||||
Energy range & 0.1 - 2.0 GeV & 0.05 - 1.0 GeV & 1 - 3 GeV & Fluxes \\
|
||||
Abs. Precision & \acs{N/A} & \acs{N/A} & \acs{N/A} & Abs. calibration \\
|
||||
Rel. Precision & 0.5\% & 1\% & \acs{N/A} & Spectral shape \\
|
||||
Rel. to prot. prec. & \acs{N/A} & 2.5\% & 5\% & Normalization \\
|
||||
Stat. acc. $>$3ks & 1\% in 2 bands & 5\% in 2 bands & 10\% in 1 band & Temporal variations \\
|
||||
Stat. acc. $>$10ks & 1\% in 5 bands & 5\% in 5 bands & \acs{N/A} & Spectro-temp. variations \\\hline
|
||||
\end{tabular}
|
||||
\caption{Original measurement requirements.}
|
||||
\label{tab:orig-meas-req}
|
||||
\end{table}
|
||||
|
||||
|
||||
Explain how we arrived at the current design. Justify.
|
||||
|
||||
Key properties such as mass, power, volume, etc.\,of the AHEPaM developed under this contract are given in Tab.~\ref{tab:key-properties}.
|
||||
Summarize key properties of AHEPaM such as mass, power, volume, etc. in a table
|
||||
|
||||
Explain interface of AHEPaM to S/C: simple, straightforward. Structural \& thermal modeling results.
|
||||
|
||||
|
|
@ -103,27 +91,6 @@ Identify design drivers (large detectors, number of channels, mass of BGO, compl
|
|||
|
||||
The proposed sensor design of the \acs{AHEPaM} is sketched in fig. \ref{fig:telescope-specs}. \ac{AHEPaM} utilizes a combination of \ac{SSD}, \ac{BGO} scintilators and Cherenkov detectors. The combination of these different measurement techniques allows for a separation of high energy electrons and protons. Fig. \ref{fig:basic-arrangement} shows the combination of those different sensors and their mounting (blue) on top of the housing of the different electronics boards (green). The entire instrument will be covered (purple) for thermal reasons. \\
|
||||
|
||||
|
||||
|
||||
|
||||
|
||||
\begin{figure}[ht]
|
||||
\begin{subfigure}[]{0.5\linewidth}
|
||||
\includegraphics[width=\linewidth]{cau-ath-ddc-0006_i1-0/media/ahepam_with-cover.png}
|
||||
\caption{\centering{\acs{AHEPaM} with its instrument cover (purple) attached to the top of the \acs{EBox} (green).}}
|
||||
\label{fig:ahepam-with-cover}
|
||||
\end{subfigure}
|
||||
\hfill
|
||||
\begin{subfigure}[]{0.5\linewidth}
|
||||
\includegraphics[width=\linewidth]{cau-ath-ddc-0006_i1-0/media/ahepam_without-cover.png}
|
||||
\caption{\centering{The instrument cover (not visible) shields the telescope (blue) against light and electronic noise.}}
|
||||
\label{fig:ahepam-wo-cover}
|
||||
\end{subfigure}
|
||||
\caption[Two pictures showing \acs{AHEPaM}'s telescope on top of the \acs{EBox}. With and without instrument cover.]{\acs{CAD-views} of AHEPaM's principle arrangement, with and without cover.}
|
||||
\label{fig:basic-arrangement}
|
||||
\end{figure}
|
||||
|
||||
|
||||
\begin{figure}[h]
|
||||
\begin{subfigure}[]{0.5\linewidth}
|
||||
\includegraphics[width=\linewidth]{cau-ath-ddc-0006_i1-0/media/cau-ath-icd-0009_i2-0_telescope.pdf}
|
||||
|
|
@ -144,6 +111,24 @@ The proposed sensor design of the \acs{AHEPaM} is sketched in fig. \ref{fig:tele
|
|||
|
||||
|
||||
|
||||
\begin{figure}[ht]
|
||||
\begin{subfigure}[]{0.5\linewidth}
|
||||
\includegraphics[width=\linewidth]{cau-ath-ddc-0006_i1-0/media/ahepam_with-cover.png}
|
||||
\caption{\centering{AHEPaM with its instrument cover (purple) on top of the \acs{EBox} (green).}}
|
||||
\label{fig:ahepam-with-cover}
|
||||
\end{subfigure}
|
||||
\hfill
|
||||
\begin{subfigure}[]{0.5\linewidth}
|
||||
\includegraphics[width=\linewidth]{cau-ath-ddc-0006_i1-0/media/ahepam_without-cover.png}
|
||||
\caption{\centering{The instrument cover (not visible) shields the telescope (blue) against light and electronics noise.}}
|
||||
\label{fig:ahepam-wo-cover}
|
||||
\end{subfigure}
|
||||
\caption[Two pictures showing AHEPaM's telescope on top of the ebox. With and without instrument cover.]{CAD-views of AHEPaM's principle arrangement.}
|
||||
\label{fig:basic-arrangement}
|
||||
\end{figure}
|
||||
|
||||
|
||||
|
||||
\begin{figure}
|
||||
\centering
|
||||
\includegraphics[width=7cm]{../cau-ath-djf-0007_i1-0/media/figs_sim/sim_model_invert.png}
|
||||
|
|
|
|||
|
|
@ -16,15 +16,6 @@ year = {2020},
|
|||
keywords = {applicable},
|
||||
}
|
||||
|
||||
@techreport{cal-req-esa,
|
||||
author = {European Space Agency},
|
||||
title = {ATHENA – Calibration Requirements Document},
|
||||
number = {ESA-ATHENA-ESTEC-SCI-RS-0002},
|
||||
note = {Issue 1.1},
|
||||
year = {2020},
|
||||
keywords = {applicable},
|
||||
}
|
||||
|
||||
@techreport{sow-esa,
|
||||
author = {European Space Agency},
|
||||
title = {Statement of Work, Athena High-Energy Particle Monitor Interface Definition C204-133EP},
|
||||
|
|
|
|||
Loading…
Add table
Add a link
Reference in a new issue