From d025548fbfc6c71e03e249b87f2ae314e46c1741 Mon Sep 17 00:00:00 2001 From: Jeff Moe Date: Tue, 30 Aug 2022 17:48:27 -0600 Subject: [PATCH] Process list --- src/Glossary.tex | 11 +++++++++-- src/SNOUG.bib | 9 +++++++++ src/SatNOGS_Optical.tex | 13 +++++++++++-- src/Satellites.tex | 4 ++-- src/Software.tex | 3 +++ 5 files changed, 34 insertions(+), 6 deletions(-) diff --git a/src/Glossary.tex b/src/Glossary.tex index 2efd668..29d0377 100644 --- a/src/Glossary.tex +++ b/src/Glossary.tex @@ -67,7 +67,7 @@ {GPL}{GPL}{GNU General Public License} \newacronym[ - description={Simplified General Perturbations models apply to near earth objects with an orbital period of less than 225 minutes. Simplified \glspl{perturbation} models are a set of five mathematical models (SGP, SGP4, SDP4, SGP8 and SDP8) used to calculate orbital state vectors of satellites and space debris relative to the Earth-centered inertial coordinate system. This set of models is often referred to collectively as SGP4 due to the frequency of use of that model particularly with \gls{TLE} sets produced by \gls{NORAD} and \gls{NASA}. These models predict the effect of \glspl{perturbation} caused by the Earth's shape, drag, radiation, and gravitation effects from other bodies such as the sun and moon. See also: \gls{SDP}.% + description={Simplified General Perturbations models apply to near earth objects with an orbital period of less than 225 minutes. Simplified \glspl{perturbation} models are a set of five mathematical models (SGP, SGP4, SDP4, SGP8 and SDP8) used to calculate orbital state vectors of \glspl{satellite} and space debris relative to the Earth-centered inertial coordinate system. This set of models is often referred to collectively as SGP4 due to the frequency of use of that model particularly with \gls{TLE} sets produced by \gls{NORAD} and \gls{NASA}. These models predict the effect of \glspl{perturbation} caused by the Earth's shape, drag, radiation, and gravitation effects from other bodies such as the sun and moon. See also: \gls{SDP}.% \footnote{\cite{enwiki:Simplified_perturbations_models}} }] {SGP}{SGP}{Simplified General Perturbations} @@ -129,6 +129,7 @@ \newacronym[description={Commodity off the shelf.}]{COTS}{COTS}{Commodity off the shelf} \newacronym[description={Free open-source hardware. See also: \gls{OSH}.}]{FOSH}{FOSH}{Free open-source hardware} \newacronym[description={Free/libre and open-source software. See also: \gls{FOSS}.}]{FLOSS}{FLOSS}{Free/libre and open-source software} +\newacronym[description={Simple Imaging Polynomial.}]{SIP}{SIP}{Simple Imaging Polynomial} %%%%%%%%%%% % Acronyms with citations @@ -316,7 +317,7 @@ \newglossaryentry{orbit} { name={orbit}, - description={is the curved trajectory of an object such as the trajectory of a planet around a star, or of a natural satellite around a planet, or of an artificial satellite around an object or position in space such as a planet, moon, asteroid, or Lagrange point. Normally, orbit refers to a regularly repeating trajectory, although it may also refer to a non-repeating trajectory. To a close approximation, planets and satellites follow elliptic orbits, with the center of mass being orbited at a focal point of the ellipse, as described by Kepler's laws of planetary motion. For most situations, orbital motion is adequately approximated by Newtonian mechanics, which explains gravity as a force obeying an inverse-square law. However, Albert Einstein's general theory of relativity, which accounts for gravity as due to curvature of spacetime, with orbits following geodesics, provides a more accurate calculation and understanding of the exact mechanics of orbital motion.% + description={is the curved trajectory of an object such as the trajectory of a planet around a star, or of a natural satellite around a planet, or of an artificial satellite around an object or position in space such as a planet, moon, asteroid, or Lagrange point. Normally, orbit refers to a regularly repeating trajectory, although it may also refer to a non-repeating trajectory. To a close approximation, planets and \glspl{satellite} follow elliptic orbits, with the center of mass being orbited at a focal point of the ellipse, as described by Kepler's laws of planetary motion. For most situations, orbital motion is adequately approximated by Newtonian mechanics, which explains gravity as a force obeying an inverse-square law. However, Albert Einstein's general theory of relativity, which accounts for gravity as due to curvature of spacetime, with orbits following geodesics, provides a more accurate calculation and understanding of the exact mechanics of orbital motion.% \footnote{\cite{enwiki:Orbit}} }} @@ -356,6 +357,12 @@ \footnote{\cite{enwiki:Gratis-versus-libre}} }} +\newglossaryentry{plate-solver} +{ name={plate solver}, + description={is software implementing a technique used in astronomy and applied on celestial images. Solving an image is finding match between the imaged stars and a star catalogue. The solution is a math model describing the corresponding astronomical position of each image pixel. The position of reference catalogue stars has to be known to a high accuracy so an astrometric reference catalogue is used. The image solution contains a reference point, often the image centre, image scale, image orientation and in some cases an image distortion model. With the astrometric solution it is possible to: 1) Calculate the celestial coordinates of any object on the image. 2) Synchronize the telescope mount or satellite pointing position to the center of the image taken. Astrometric solving programs extract the star x,y positions from the celestial image, groups them in three-star triangles or four-star quads. Then it calculates for each group a geometric hash code based on the distance and/or angles between the stars in the group. It then compares the resulting hash codes with the hash codes created from catalogue stars to find a match. If it finds sufficient statistically reliable matches, it can calculate transformation factors. There are several conventions to model the transformation from image pixel location to the corresponding celestial coordinates. The simplest linear model is called the \gls{WCS}. A more advanced convention is \gls{SIP} describing the transformation in polynomials to cope with non-linear geometric distortion in the celestial image, mainly caused by the optics.% + \footnote{\cite{enwiki:Astrometric-solving}} + }} + % TO ADD % RamSat % Dashboard diff --git a/src/SNOUG.bib b/src/SNOUG.bib index 15920ee..5c59e2a 100644 --- a/src/SNOUG.bib +++ b/src/SNOUG.bib @@ -307,4 +307,13 @@ year = {2022}, } +@Misc{enwiki:Astrometric-solving, + author = {{Wikipedia contributors}}, + title = {Astrometric solving --- {Wikipedia}{,} The Free Encyclopedia}, + howpublished = {\url{https://en.wikipedia.org/w/index.php?title=Astrometric_solving&oldid=1099832612}}, + note = {[Online; accessed 30-August-2022]}, + modificationdate = {2022-08-30T17:39:16}, + year = {2022}, +} + @Comment{jabref-meta: databaseType:biblatex;} diff --git a/src/SatNOGS_Optical.tex b/src/SatNOGS_Optical.tex index 510fb73..9a2ef18 100644 --- a/src/SatNOGS_Optical.tex +++ b/src/SatNOGS_Optical.tex @@ -12,14 +12,23 @@ SatNOGS Optical is the nascent distributed network of optical ground stations. -This chapter reviews what is needed in terms of hardware and +This chapter gives a top level review what is needed in terms of hardware and software to build an operating optical ground station. \section{Toolchain} SatNOGS Optical Process Overview.% \footnote{\url{https://spacecruft.org/spacecruft/SNOPO}} -See figure \ref{fig:snopo}, page \pageref{fig:snopo}. +See figure \ref{fig:snopo}, page \pageref{fig:snopo}, described below. + +\begin{enumerate} + \item Hardware --- Hardware, such as cameras and computers, is to be selected and set up. + \item Software --- The best currently available software is to be downloaded, installed, and configured. + \item Acquire --- Data samples, typically in the form of \gls{FITS} file photographs, need to be acquired by running a camera outside at night taking pictures of the sky. + \item \Gls{plate-solver} --- Acquired data samples need to be processed by a \gls{plate-solver}. See \ref{sec:plate-solver}, page \pageref{sec:plate-solver}. + \item Detect \glspl{satellite} --- Using \glspl{TLE} and the ``solved'' plates, detect \glspl{satellite}. See \ref{sec:satellite-detection}, page \pageref{sec:satellite-detection}. + \item Identify \glspl{satellite} --- With \glspl{satellite} detected in the previous step, identify what they are. See \ref{sec:overview-identify}, page \pageref{sec:overview-identify}. +\end{enumerate} \begin{figure}[h!] \includegraphics[keepaspectratio=true,height=1.10\textheight,width=1.00\textwidth,angle=0]{SNOPO.png} diff --git a/src/Satellites.tex b/src/Satellites.tex index cdd4891..1737b49 100644 --- a/src/Satellites.tex +++ b/src/Satellites.tex @@ -10,8 +10,8 @@ % \section{Overview of Satellites} -\label{sec:overview-satellites} -\index{satellites} +\label{sec:overview-satellite} +\index{satellite} \Glspl{artificial satellite} are rocks with modems. diff --git a/src/Software.tex b/src/Software.tex index acb6b5c..e17fc76 100644 --- a/src/Software.tex +++ b/src/Software.tex @@ -184,6 +184,9 @@ inparallel \section{skymap} Use \gls{skymap} for viewing \gls{satellite} \glspl{orbit} tracks projected on a map of of the sky. Skymap is part of \gls{sattools}. +\Gls{skymap} isn't a required part of the toolchain, but it is useful +to see what \glspl{satellite} are visibile at a particular time and +location. Source: