From b08f911ac638a10b8843fc86cc5090d9b7be1949 Mon Sep 17 00:00:00 2001
From: Roy Smart <roytsmart@gmail.com>
Date: Thu, 5 Oct 2023 15:29:50 -0600
Subject: [PATCH 1/2] Started rewriting the first few sentences in the
introduction of the instrument paper.
---
.../papers/instrument/sections/introduction.py | 14 ++++++++------
1 file changed, 8 insertions(+), 6 deletions(-)
diff --git a/esis/science/papers/instrument/sections/introduction.py b/esis/science/papers/instrument/sections/introduction.py
index 0dd14aa..a8e0fe8 100644
--- a/esis/science/papers/instrument/sections/introduction.py
+++ b/esis/science/papers/instrument/sections/introduction.py
@@ -10,12 +10,14 @@ def section() -> pylatex.Section:
result.escape = False
result.append(
r"""
-The solar \TR\ and corona, as viewed from space in its characteristic short wavelengths (\FUV, \EUV, and soft X-ray),
-is a three-dimensional scene evolving in time: $I(x, y, \lambda, t)$.
-Here, the helioprojective cartesian coordinates, $x$ and $y$ \citep{Thompson2006}, and the wavelength axis, $\lambda$,
-comprise the three dimensions of the scene, while $t$ represents the temporal axis.
-An ideal instrument would capture a spatial/spectral data cube, at a rapid temporal cadence, however, practical
-limitations lead us to accept various compromises of the sampling rate along each of these four dimensions.
+The light emitted by the solar \TR\ and corona varies significantly as a function
+of position, wavelength, and time.
+When viewed from Earth, the spectral radiance from the Sun can be written as: $I(x, y, \lambda, t)$,
+where $x$ and $y$ are the helioprojective Cartesian coordinates \citep{Thompson2006}, $\lambda$ is wavelength, and $t$ is time.
+The ideal solar imaging spectrograph would capture $I(x, y, \lambda, t)$ with high resolution in $x$, $y$, $\lambda$, and $t$
+\textit{and} over a wide \FOV\, wavelength range, and time period.
+However, physical limitations in sensors and materials mean that we must make compromises on either the sampling rate
+or the sampling rangle along each of these four dimensions.
Approaching this ideal is the fast tunable filtergraph (\ie\ fast tunable Fabry--P\'erot etalons, \eg\ the GREGOR
Fabry--P{\'e}rot Interferometer, \citep{Puschmann12}), but the materials do not exist to extend this technology to
\EUV\ wavelengths shortward of $\sim$\SI{150}{\nano\meter}~\citep{2000WuelserFP}.
From af2e6dfb2ed9af77206a9c79a2087e68738f367e Mon Sep 17 00:00:00 2001
From: Roy Smart <roytsmart@gmail.com>
Date: Thu, 19 Oct 2023 16:27:51 -0600
Subject: [PATCH 2/2] Edits to the Fabry-Perot paragraph of the Instrument
paper introduction.
---
.../instrument/sections/introduction.py | 23 +++++++++++++++----
1 file changed, 18 insertions(+), 5 deletions(-)
diff --git a/esis/science/papers/instrument/sections/introduction.py b/esis/science/papers/instrument/sections/introduction.py
index a8e0fe8..51aad1b 100644
--- a/esis/science/papers/instrument/sections/introduction.py
+++ b/esis/science/papers/instrument/sections/introduction.py
@@ -13,11 +13,24 @@ def section() -> pylatex.Section:
The light emitted by the solar \TR\ and corona varies significantly as a function
of position, wavelength, and time.
When viewed from Earth, the spectral radiance from the Sun can be written as: $I(x, y, \lambda, t)$,
-where $x$ and $y$ are the helioprojective Cartesian coordinates \citep{Thompson2006}, $\lambda$ is wavelength, and $t$ is time.
-The ideal solar imaging spectrograph would capture $I(x, y, \lambda, t)$ with high resolution in $x$, $y$, $\lambda$, and $t$
-\textit{and} over a wide \FOV\, wavelength range, and time period.
-However, physical limitations in sensors and materials mean that we must make compromises on either the sampling rate
-or the sampling rangle along each of these four dimensions.
+where $x$ and $y$ are the helioprojective Cartesian coordinates \citep{Thompson2006},
+$\lambda$ is wavelength, and $t$ is time.
+The ideal solar imaging spectrograph would capture $I(x, y, \lambda, t)$ with high resolution in $x$, $y$, $\lambda$,
+and $t$ \textit{and} over a wide \FOV\, wavelength range, and time period.
+Of course, the temporal dimension is privileged, so we often reduce the problem to capturing a 3D spatial/spectral
+cube at a particular time $t_0$: $I(x, y, \lambda, t_0)$.
+Since we use 2D detectors, this means that we must find a way to flatten the 3D cube into two dimensions
+without losing information.
+
+One obvious way to accomplish this is to multiplex one of the three remaining dimensions in time.
+Narrowband, tunable filters,
+such as the GREGOR Fabry--P{\'e}rot Interferometer \citep{Puschmann12},
+multiplex the wavelength dimension in time,
+and can change the selected wavelength in \SI{100}{\milli\second} or less \citep{vanNoort2022},
+but the technology does not exist to use this technique for wavelengths shorter than
+$\sim$\SI{150}{\nano\meter}~\citep{2000WuelserFP}.
+
+
Approaching this ideal is the fast tunable filtergraph (\ie\ fast tunable Fabry--P\'erot etalons, \eg\ the GREGOR
Fabry--P{\'e}rot Interferometer, \citep{Puschmann12}), but the materials do not exist to extend this technology to
\EUV\ wavelengths shortward of $\sim$\SI{150}{\nano\meter}~\citep{2000WuelserFP}.