Merge pull request #89 from chhoumann/thesis-introduction-feedback-co…

…rrections

report_thesis/src/references.bib

@@ -54,6 +54,25 @@ @article{andersonPostlandingMajorElement2022
   langid       = {english}
 }
 
+@article{wiensChemcam2012,
+  title        = {The {ChemCam} Instrument Suite on the Mars Science Laboratory ({MSL}) Rover: Body Unit and Combined System Tests},
+  volume       = {170},
+  issn         = {1572-9672},
+  url          = {https://doi.org/10.1007/s11214-012-9902-4},
+  doi          = {10.1007/s11214-012-9902-4},
+  shorttitle   = {The {ChemCam} Instrument Suite on the Mars Science Laboratory ({MSL}) Rover},
+  abstract     = {The {ChemCam} instrument suite on the Mars Science Laboratory ({MSL}) rover Curiosity provides remote compositional information using the first laser-induced breakdown spectrometer ({LIBS}) on a planetary mission, and provides sample texture and morphology data using a remote micro-imager ({RMI}). Overall, {ChemCam} supports {MSL} with five capabilities: remote classification of rock and soil characteristics; quantitative elemental compositions including light elements like hydrogen and some elements to which {LIBS} is uniquely sensitive (e.g., Li, Be, Rb, Sr, Ba); remote removal of surface dust and depth profiling through surface coatings; context imaging; and passive spectroscopy over the 240–905 nm range. {ChemCam} is built in two sections: The mast unit, consisting of a laser, telescope, {RMI}, and associated electronics, resides on the rover’s mast, and is described in a companion paper. {ChemCam}’s body unit, which is mounted in the body of the rover, comprises an optical demultiplexer, three spectrometers, detectors, their coolers, and associated electronics and data handling logic. Additional instrument components include a 6 m optical fiber which transfers the {LIBS} light from the telescope to the body unit, and a set of onboard calibration targets. {ChemCam} was integrated and tested at Los Alamos National Laboratory where it also underwent {LIBS} calibration with 69 geological standards prior to integration with the rover. Post-integration testing used coordinated mast and instrument commands, including {LIBS} line scans on rock targets during system-level thermal-vacuum tests. In this paper we describe the body unit, optical fiber, and calibration targets, and the assembly, testing, and verification of the instrument prior to launch.},
+  pages        = {167--227},
+  number       = {1},
+  journaltitle = {Space Science Reviews},
+  shortjournal = {Space Sci Rev},
+  author       = {Wiens, Roger C. and Maurice, Sylvestre and Barraclough, Bruce and Saccoccio, Muriel and Barkley, Walter C. and Bell, James F. and Bender, Steve and Bernardin, John and Blaney, Diana and Blank, Jennifer and Bouyé, Marc and Bridges, Nathan and Bultman, Nathan and Caïs, Phillippe and Clanton, Robert C. and Clark, Benton and Clegg, Samuel and Cousin, Agnes and Cremers, David and Cros, Alain and {DeFlores}, Lauren and Delapp, Dorothea and Dingler, Robert and D’Uston, Claude and Darby Dyar, M. and Elliott, Tom and Enemark, Don and Fabre, Cecile and Flores, Mike and Forni, Olivier and Gasnault, Olivier and Hale, Thomas and Hays, Charles and Herkenhoff, Ken and Kan, Ed and Kirkland, Laurel and Kouach, Driss and Landis, David and Langevin, Yves and Lanza, Nina and {LaRocca}, Frank and Lasue, Jeremie and Latino, Joseph and Limonadi, Daniel and Lindensmith, Chris and Little, Cynthia and Mangold, Nicolas and Manhes, Gerard and Mauchien, Patrick and {McKay}, Christopher and Miller, Ed and Mooney, Joe and Morris, Richard V. and Morrison, Leland and Nelson, Tony and Newsom, Horton and Ollila, Ann and Ott, Melanie and Pares, Laurent and Perez, René and Poitrasson, Franck and Provost, Cheryl and Reiter, Joseph W. and Roberts, Tom and Romero, Frank and Sautter, Violaine and Salazar, Steven and Simmonds, John J. and Stiglich, Ralph and Storms, Steven and Striebig, Nicolas and Thocaven, Jean-Jacques and Trujillo, Tanner and Ulibarri, Mike and Vaniman, David and Warner, Noah and Waterbury, Rob and Whitaker, Robert and Witt, James and Wong-Swanson, Belinda},
+  urldate      = {2023-10-03},
+  date         = {2012-09-01},
+  langid       = {english},
+  keywords     = {{ChemCam}, Curiosity, Gale Crater, Laser induced breakdown spectroscopy, Laser plasma, {LIBS}, Mars, Mars Science Laboratory, {MSL}, {RMI}}
+}
+
 @article{song_DF-K-ELM,
 	title = {Incorporating domain knowledge into machine learning for laser-induced breakdown spectroscopy quantification},
 	volume = {195},

report_thesis/src/sections/introduction.tex

@@ -1,19 +1,20 @@
 \section{Introduction}\label{sec:introduction}
-The NASA Viking missions in the 1970s were the first to successfully land a rover on Mars, aiming to determine if life existed on the planet.
-One experiment suggested the presence of life, but the results were ambiguous and inconclusive, and NASA was unable to repeat the experiment due to budget constraints\cite{marsnasagov_vikings}.
+The NASA Viking missions in the 1970s were the first to successfully land on Mars, aiming to determine if life existed on the planet.
+One experiment suggested the presence of life, but the results were ambiguous and inconclusive, and NASA was unable to repeat the experiment.
+Nevertheless, these missions were deemed a monumental success and advanced our knowledge of the Martian envi-\\ronment.\cite{marsnasagov_vikings}
 
-A few decades later, the philosophy of Martian exploration had shifted from searching for life to investigating whether Mars ever had the conditions to support life as we know it.
-The \gls{mer} mission, which included the Spirit and Opportunity rovers, discovered clear evidence that water once flowed on Mars.
-As water alone is not enough to support life, NASA shifted their focus to search for organic material as well\cite{marsnasagov_observer, marsnasagov_spirit_opportunity}.
+Leveraging the knowledge gained from the Viking missions, NASA launched the \gls{mer} mission in 2003 to investigate whether Mars ever had the conditions to support life as we know it.
+The mission landed two rovers, Spirit and Opportunity, on Mars in January 2004, and they quickly discovered clear evidence that water once flowed on Mars.
+However, since water alone is not enough to support life, the next objective was to search for organic material as well.\cite{marsnasagov_observer, marsnasagov_spirit_opportunity}
 
 The Curiosity rover landed on Mars in August 2012 inside Gale Crater as part of the \gls{msl} mission with this very purpose.
-Its sophisticated equipment quickly discovered that the conditions to support life as we know it had existed on Mars through chemical and mineral evidence.\cite{marsnasagov_chemcam}
+Thanks to its sophisticated equipment, Curiosity was able to find evidence of past habitable environments on Mars based on chemical and mineral findings early in its mission.\cite{marsnasagov_chemcam}
 
 One of the instruments aboard the rover is the \gls{chemcam} instrument, which is a remote-sensing laser instrument used to gather \gls{libs} data from geological samples on Mars.
-\gls{libs} is a non-invasive technique that enables rapid analysis without the need for sample preparation by using a laser to ablate and remove surface contaminants to expose the underlying material and generate a plasma plume from the now-exposed sample material.
+\gls{libs} is a technique that enables rapid analysis by using a laser to ablate and remove surface contaminants to expose the underlying material and generate a plasma plume from the now-exposed sample material\cite{wiensChemcam2012}.
 This plasma plume emits light that is captured through three distinct spectrometers to collect a series of spectral readings.
 These spectra consist of emission lines that can be associated with the concentration of a specific element, and their intensity reflects the concentration of that element in the sample.
-Consequently, a spectra serves as a complex, multi-dimensional fingerprint of the elemental composition of the examined geological formations.\cite{cleggRecalibrationMarsScience2017}
+Consequently, a spectra serves as a complex, multi-dimensional fingerprint of the elemental composition of the examined geological samples.\cite{cleggRecalibrationMarsScience2017}
 
 Analyzing \gls{libs} data is computationally challenging due to high multicollinearity within spectral data, which diminishes the effectiveness of traditional linear analysis.
 The multicollinearity, which stems from correlations among spectral channels and elemental emission characteristics, complicates data interpretation.