{{short description|One of a series of 30 quadrangle maps of Mars}} {{Infobox feature on celestial object |name = Syrtis Major [[quadrangle (geography)|quadrangle]] |image = [[File:USGS-Mars-MC-13-SyrtisMajorRegion-mola.png|300px]] |caption = Map of Syrtis Major quadrangle from [[Mars Orbiter Laser Altimeter]] (MOLA) data. The highest elevations are red and the lowest are blue. |coordinates = {{coord|15|N|292.5|W|globe:mars_type:landmark|display=inline,title}} }} [[File:Syrtis Major MC-13.jpg|thumb|300px|Image of the Syrtis Major Quadrangle (MC-13). The central part contains [[Syrtis Major Planum]]. The east includes [[Isidis basin]] and the west and north includes heavily cratered highlands.]] The '''Syrtis Major quadrangle''' is one of a series of [[list of quadrangles on Mars|30 quadrangle maps of Mars]] used by the [[United States Geological Survey]] (USGS) [[Astrogeology Research Program]]. The Syrtis Major quadrangle is also referred to as MC-13 (Mars Chart-13).<ref>{{cite book |last1=Davies |first1=M. E. |last2=Batson |first2=R. M. |last3=Wu |first3=S. S. C. |chapter=Geodesy and Cartography |editor1-last=Kieffer |editor1-first=H. H. |editor2-last=Jakosky |editor2-first=B. M. |editor3-last=Snyder |editor3-first=C. W. |editor4-last=Matthews |editor4-first=M. S. |title=Mars |publisher=University of Arizona Press |location=Tucson |year=1992 |isbn=0-8165-1257-4 }}</ref>
The [[quadrangle (geography)|quadrangle]] covers longitudes 270° to 315° west and latitudes 0° to 30° north on [[Mars]]. Syrtis Major quadrangle includes [[Syrtis Major Planum]] and parts of [[Terra Sabaea]] and [[Isidis Planitia]].
Syrtis Major is an old shield volcano with a central depression that is elongated in a north–south direction. It contains the calderas Meroe Patera and Nili Patera.<ref>{{Cite web|url=http://www.daviddarling.info/encyclopedia/S/SyrtisMajor.html|title=Syrtis Major|first=David|last=Darling|website=www.daviddarling.info}}</ref> Interesting features in the area include dikes and inverted terrain.
The ''[[Beagle 2]]'' lander was about to land near the quadrangle, particularly in the eastern part of [[Isidis Planitia]], in December 2003, when contact with the craft was lost. In January 2015, NASA reported the ''Beagle 2'' had been found on the surface in Isidis Planitia (location is about {{coord|11.5265|N|90.4295|E|globe:Mars}}).<ref name="TW-20150116"> {{cite web |last=Ellison |first=Doug |title=re Beagle 2 location on Mars => "Using HiView on image ESP_039308_1915_COLOR.JP2 I get 90.4295E 11.5265N" |url=https://twitter.com/doug_ellison/status/556201983443357696 |date=16 January 2015 |work=[[Twitter]] & [[JPL]] |access-date=19 January 2015 }}</ref><ref name="NASA-20150116-TG">{{cite web |last1=Grecicius |first1=Tony |last2=Dunbar |first2=Brian |title=Components of Beagle 2 Flight System on Mars |url=http://www.nasa.gov/jpl/mars/pia19106/ |date=16 January 2015 |work=[[NASA]] |access-date=18 January 2015 }}</ref> High-resolution images captured by the [[Mars Reconnaissance Orbiter]] identified [[Beagle 2#Discovery of Beagle 2 spacecraft on Mars|the lost probe]], which appears to be intact.<ref name="NASA-20150116">{{cite web |last=Webster |first=Guy |title='Lost' 2003 Mars Lander Found by Mars Reconnaissance Orbiter |url=http://www.nasa.gov/jpl/lost-2003-mars-lander-found-by-mars-reconnaissance-orbiter/ |date=16 January 2015 |work=[[NASA]] |access-date=16 January 2015 |archive-date=24 February 2017 |archive-url=https://web.archive.org/web/20170224145904/https://www.nasa.gov/jpl/lost-2003-mars-lander-found-by-mars-reconnaissance-orbiter/ |url-status=dead }}</ref><ref name="NYT-20150116"> {{cite news |agency=Associated Press |title=Mars Orbiter Spots Beagle 2, European Lander Missing Since 2003 |url=https://www.nytimes.com/2015/01/17/science/space/missing-lander-beagle-2-finally-located-on-mars.html |date=16 January 2015 |work=[[The New York Times]] |access-date=17 January 2015 }}</ref><ref name="BBC-20150116">{{cite news |last=Amos |first=Jonathan |title=Lost Beagle2 probe found 'intact' on Mars |url=https://www.bbc.co.uk/news/science-environment-30784886 |date=16 January 2015 |work=[[BBC]] |access-date=16 January 2015}}</ref>
In November 2018, NASA announced that Jezero crater was chosen as the landing site for the planned [[Mars 2020|Mars 2020 rover]] mission.<ref name="SPC-20181119">{{cite news |last=Wall |first=Mike |title=Jezero Crater or Bust! NASA Picks Landing Site for Mars 2020 Rover |url=https://www.space.com/42486-mars-2020-rover-jezero-crater-landing-site.html |date=19 November 2018 |work=[[Space.com]] |access-date=20 November 2018 }}</ref><ref>{{Cite news|url=https://gizmodo.com/nasas-mars-2020-rover-will-land-in-jezero-crater-1830540291|title=NASA's Mars 2020 Rover Will Land in Jezero Crater|last=Mandelbaum|first=Ryan F.|work=Gizmodo|access-date=2018-11-19}}</ref> [[Jezero (crater)|Jezero crater]] is in the Syrtis Major quadrangle at (at {{coord|18.855|N|77.519|E|globe:Mars}})<ref name="HR-20080606">{{cite web |last=Wray |first=James |title=Channel into Jezero Crater Delta |url=http://hirise.lpl.arizona.edu/PSP_007925_1990 |date=6 June 2008 |work=[[NASA]] |access-date=6 March 2015}}</ref>
==Discovery and name== The name [[Syrtis Major Planum|Syrtis Major]] is derived from the classical [[Ancient Rome|Roman]] name ''Syrtis maior'' for the [[Gulf of Sidra]] on the coast of [[Libya]] (classical [[Cyrenaica]]). It is near Cyrene which is the place where "Simon" who carried the cross of Jesus was from.<ref>{{Cite web|url=https://ferrelljenkins.blog/2011/03/30/libya-and-the-bible-%e2%80%94-more-than-you-think/|title=Libya and the Bible — more than you think|author=Andrew Petcher |work=Ferrell's Travel Blog |date=March 30, 2011}}</ref><ref>{{Citation|url=https://books.google.com/books?id=3JNQAQAAMAAJ&pg=PA18|title=The Cambridge Bible for Schools and Colleges|volume=59|year=1897}}</ref><ref>{{Cite web|url=https://books.google.com/books?id=jVIOAAAAQAAJ&pg=PA286|title = A history of the holy Bible, corrected and improved|first1=G.|last1=Gleig|last2 = Stackhouse|first2 = Thomas|year = 1817}}</ref>
Syrtis Major is a distinctly dark region standing out against the lighter surrounding highlands, and was the first documented surface feature of another [[planet]]. It was discovered by [[Christiaan Huygens]], who included it in a drawing of Mars in 1659. The feature was originally known as the '''Hourglass Sea''' but has been given different names by different [[cartographer]]s. In 1840, [[Johann Heinrich von Mädler]] compiled a map of Mars from his observations and called the feature '''Atlantic Canale'''. In [[Richard Proctor]]'s 1867 map it is called then '''Kaiser Sea''' (after [[Frederik Kaiser]] of the [[Leiden Observatory]]). [[Camille Flammarion]] called it the '''Mer du Sablier''' (French for "Hourglass Sea") when he revised Proctor's nomenclature in 1876. The name "Syrtis Major" was chosen by [[Giovanni Schiaparelli]] when he created a map based on observations made during Mars' close approach to Earth in 1877.<ref>{{cite book| title=Mapping Mars: Science, Imagination, and the Birth of a World| first=Oliver| last=Morton| publisher=Picador USA| location=New York| date=2002| isbn=0-312-24551-3| pages=[https://archive.org/details/mappingmarsscien00mort_0/page/14 14]–15| url-access=registration| url=https://archive.org/details/mappingmarsscien00mort_0}}</ref><ref>{{cite web|url=http://www.uapress.arizona.edu/onlinebks/mars/chap04.htm|title=The Planet Mars: A History of Observation and Discovery - Chapter 4: Areographers|author=William Sheehan|access-date=2007-09-07|archive-date=2017-07-01|archive-url=https://web.archive.org/web/20170701062415/http://www.uapress.arizona.edu/onlinebks/MARS/CHAP04.HTM|url-status=dead}}</ref>
== Igneous rocks == Syrtis Major is of great interest to geologists because several types of igneous rocks have been found there with orbiting spacecraft. Besides [[basalt]], [[dacite]] and [[granite]] have been found there. Dacite originates under [[volcanoes]] in [[magma]] chambers. Dacites form at the top of the chamber, after heavy minerals ([[olivine]] and [[pyroxene]]) containing [[iron]] and [[magnesium]] have settled to the bottom. Granite is formed by an even more complex process.<ref>Christensen, P. 2005. "The Many Faces of Mars". ''Scientific American''. July, 2005.</ref>
Some areas of Syrtis Major contain large amounts of the mineral olivine. Olivine turns into other minerals very rapidly in the presence of water, so a high abundance of olivine suggests that for a long time little water has been there.<ref>{{Cite web |url=https://themis.asu.edu/node/5396 |title=7. Olivine-rich rocks point to cold, dry martian past |publisher=Mars Space Flight Facility, Arizona State University |access-date=20 August 2024}}</ref>
==Minerals== A variety of important minerals have been discovered near [[Nili Fossae]], a major trough system in Syrtis major. Besides a large exposure of olivine located in Nili Fossae. Other minerals found there include carbonates, aluminum smectite, iron/magnesium smectite, hydrated silica, kaolinite group minerals, and iron oxides.<ref name="auto">{{Cite news|url=https://news.bbc.co.uk/2/hi/science/nature/7791060.stm|title=Nasa finds 'missing' Mars mineral|date=December 19, 2008|via=BBC News}}</ref><ref name="Murchie, S. 2009">{{cite journal | doi=10.1029/2009JE003342 | title=A synthesis of Martian aqueous mineralogy after 1 Mars year of observations from the Mars Reconnaissance Orbiter | date=2009 | last1=Murchie | first1=Scott L. | last2=Mustard | first2=John F. | last3=Ehlmann | first3=Bethany L. | last4=Milliken | first4=Ralph E. | last5=Bishop | first5=Janice L. | last6=McKeown | first6=Nancy K. | last7=Noe Dobrea | first7=Eldar Z. | last8=Seelos | first8=Frank P. | last9=Buczkowski | first9=Debra L. | last10=Wiseman | first10=Sandra M. | last11=Arvidson | first11=Raymond E. | last12=Wray | first12=James J. | last13=Swayze | first13=Gregg | last14=Clark | first14=Roger N. | last15=Des Marais | first15=David J. | last16=McEwen | first16=Alfred S. | last17=Bibring | first17=Jean-Pierre | journal=Journal of Geophysical Research: Planets | volume=114 | issue=E2 | article-number=2009JE003342 | bibcode=2009JGRE..114.0D06M }}</ref> In December 2008, [[NASA]]'s Mars Reconnaissance Orbiter found that rocks at Nili Fossae contain [[carbonate minerals]], a geologically significant discovery.<ref name="auto"/><ref>{{Cite web|url=http://www.space.com/30746-mars-missing-atmosphere-lost-in-space.html|title=Mars' Missing Atmosphere Likely Lost in Space|website=[[Space.com]]|date=5 October 2015}}</ref><ref>{{cite journal |last1=Edwards |first1=Christopher S. |last2=Ehlmann |first2=Bethany L. |title=Carbon sequestration on Mars |journal=Geology |date=October 2015 |volume=43 |issue=10 |pages=863–866 |doi=10.1130/G36983.1 |bibcode=2015Geo....43..863E }}</ref> Later research published in October 2010, described a large deposit of carbonate rocks found inside Leighton Crater at a level that was once buried 4 miles (6 km) below the surface. Finding carbonates in an underground location strongly suggests that Mars was warmer and had more atmospheric carbon dioxide and ancient seas. Because the carbonates were near silicate minerals and clays hydrothermal systems like the deep sea vents on Earth may have been present.<ref>{{cite web |last=<!--not stated--> |title=Exposed Rocks Point to Water on Ancient Mars |work=[[Astrobiology Magazine]] |date=2010-10-13 |url=http://www.astrobio.net/pressrelease/3646/exposed-rocks-point-to-water-on-ancient-mars |url-status=dead |archive-url=https://web.archive.org/web/20110629125815/http://www.astrobio.net/pressrelease/3646/exposed-rocks-point-to |archive-date=2011-06-29}}</ref><ref name="ReferenceA">{{cite journal | doi=10.1016/j.epsl.2010.06.018 | title=Hydrothermal formation of Clay-Carbonate alteration assemblages in the Nili Fossae region of Mars | date=2010 | last1=Brown | first1=Adrian J. | last2=Hook | first2=Simon J. | last3=Baldridge | first3=Alice M. | last4=Crowley | first4=James K. | last5=Bridges | first5=Nathan T. | last6=Thomson | first6=Bradley J. | last7=Marion | first7=Giles M. | last8=De Souza Filho | first8=Carlos R. | last9=Bishop | first9=Janice L. | journal=Earth and Planetary Science Letters | volume=297 | issue=1–2 | pages=174–182 | arxiv=1402.1150 | bibcode=2010E&PSL.297..174B }}</ref>
Other minerals found by the MRO are aluminum smectite, iron/magnesium smectite, hydrated silica, kaolinite group minerals, iron oxides, and talc.<ref name="Murchie, S. 2009"/><ref name="ReferenceA"/> NASA scientists discovered that Nili Fossae is the source of plumes of methane, raising the question of whether this source originates from biological sources.<ref>[http://dsc.discovery.com/news/2009/01/15/mars-methane-life.html Mars Methane Found, Raising Possibility of Life]</ref><ref>{{Cite news|url=https://news.bbc.co.uk/1/hi/sci/tech/7829315.stm|title=New light on Mars methane mystery|date=January 15, 2009|via=BBC News}}</ref>
Research published in the fall of 2010, describes the discovery of hydrated silica on the flanks of a volcanic cone. The deposit was from a steam [[fumarole]] or hot spring, and it represents a recent habitable microenvironment. The {{convert|100|m|ft|adj=mid|-high|sp=us}} cone rests on the floor of Nili Patera. Observations were obtained with NASA's Mars Reconnaissance Orbiter.<ref>{{Cite web|url=https://www.jpl.nasa.gov/news/silica-on-a-mars-volcano-tells-of-wet-and-cozy-past |title=Silica on Mars Volcano Tells of Wet and Cozy Past |publisher=JPL |date=31 October 2010 |access-date=20 August 2024}}</ref>
== Dikes == Narrow ridges occur in some places on Mars. They may be formed by different means, but some are probably caused by molten rock moving underground, cooling into hard rock, then being exposed by the erosion of softer, surrounding materials. Such a feature is termed a dike. They are common on Earth—some famous ones are [[Shiprock]], [[New Mexico]];<ref>{{Cite web|url=http://www.msss.com/mars_images/moc/2005/10/13/|title = Mars Global Surveyor MOC2-1249 Release}}</ref> around [[Spanish Peaks]], [[Colorado]];<ref>{{Cite book |isbn = 0-87842-105-X|title = Roadside Geology of Colorado|last1 = Chronic|first1 = Halka|date = January 1980| publisher=Mountain Press Publishing Company }}{{page needed|date=January 2026}}</ref><ref>{{Cite book |isbn = 0-7167-2438-3|title = Petrology, Second Edition: Igneous, Sedimentary, and Metamorphic|last1 = Blatt|first1 = Harvey|last2 = Tracy|first2 = Robert|date = 1995-12-15 | publisher=W. H. Freeman }}{{page needed|date=January 2026}}</ref> and the "Iron Dike" in [[Rocky Mountain National Park]], Colorado.<ref>{{Cite book|isbn = 0-8403-4619-0|title = Geology of National Parks|last1 = Harris|first1 = Ann G.|last2 = Tuttle|first2 = Esther|year = 1990| publisher=Kendall/Hunt Publishing Company }}{{page needed|date=January 2026}}</ref>
The discovery on Mars of dikes that were formed from molten rock is highly significant because dikes indicate the existence of intrusive igneous activity. On the Earth such activity is associated with precious metals like gold, silver, and [[tellurium]].<ref name="ccvgoldmining.com">{{Cite web |url=http://ccvgoldmining.com/Geology/geology.html |title=Geology of the Cripple Creek Mining District |access-date=2010-11-13 |archive-date=2011-05-16 |archive-url=https://web.archive.org/web/20110516160553/http://ccvgoldmining.com/Geology/geology.html |url-status=dead }}</ref> Dikes and other intrusive structures are common in the Cripple Creek Mining District of Colorado;<ref name="ccvgoldmining.com"/> the Battle Mountain-Eureka area in north-central Nevada, famous for gold and [[molybdenum]] deposits;<ref>{{Cite web |url=https://portergeo.com.au/database/mineinfo.asp?mineid=mn1127 |title=PorterGeo Database - Ore Deposit Description |publisher=PorterGeo |access-date=20 August 2024}}</ref> and around the [[Franklin dike swarm]] in Canada. Mapping the presence of dikes allows us to understand how [[magma]] (molten rock under the ground) travels and where it could have interacted with surrounding rock, thus producing valuable [[ores]]. Deposits of important minerals are also made by dikes and other igneous [[intrusion]]s heating water which then dissolves minerals that are deposited in cracks in nearby rock.<ref>Namowitz, S. and D. Stone. 1975. ''Earth Science-The World We Live In''. American Book Company. Ny, NY</ref> One would expect a great deal of intrusive igneous activity to occur on Mars because it is believed there is more igneous activity under the ground than on top, and Mars has many huge volcanoes.<ref>{{cite journal |last1=Crisp |first1=Joy A. |title=Rates of magma emplacement and volcanic output |journal=Journal of Volcanology and Geothermal Research |date=April 1984 |volume=20 |issue=3–4 |pages=177–211 |doi=10.1016/0377-0273(84)90039-8 |bibcode=1984JVGR...20..177C }}</ref>
==Jezero Crater discoveries with Perseverance==
The Perseverance rover landed in Jesero crater and has greatly increased our understanding of the crater. Although Jezero shows the classic signs of a lake, especially with its deltas, igneous rocks were found.<ref>{{cite report |last1=Schmidt |first1=M. E. |last2=Allwood |first2=A. |last3=Christian |first3=J. |last4=Clark |first4=B. C. |last5=Flannery |first5=D. |last6=Hennecke |first6=J. |last7=Herd |first7=C. D. K. |last8=Hurowitz |first8=J. A. |last9=Kizovski |first9=T. V. |last10=Liu |first10=Y. |last11=Mclennan |first11=S. M. |last12=Nachon |first12=M. |last13=Pedersen |first13=D. a. K. |last14=Shuster |first14=D. L. |last15=Simon |first15=J. I. |last16=Tice |first16=M. |last17=Tosca |first17=N. |last18=Treiman |first18=A. H. |last19=Udry |first19=A. |last20=Vanbommel |first20=S. |last21=Wadhwa |first21=M. |title=Highly Differentiated Basaltic Lavas Examined by PIXL in Jezero Crater |date=7 March 2022 |url=https://ntrs.nasa.gov/citations/20220000482 }}</ref> One would have expected just sedimentary rocks. Furthermore, some of the rocks had large crystals that indicated slow cooling. Large crystals are formed in maga bodies after a long period of cooling. The crystals were composed of the mineral olivine surrounded by another mineral called pyroxene. That arrangement happens in thick magma bodies and geologists call this type of texture "Cumulate."<ref name="bbc.com">{{cite web | title=Nasa's Perseverance Mars rover finds its 'baseline' rocks | date=16 December 2021 | url=https://www.bbc.com/news/science-environment-59677383 }}</ref> In addition basalt lava was found.<ref>{{cite web | title=NASA's Perseverance Rover Collects Puzzle Pieces of Mars' History - NASA | url=https://mars.nasa.gov/news/9036/nasas-perseverance-rover-collects-puzzle-pieces-of-mars-history/ }}</ref> Minerals that are produced with water, like carbonates, were found as well.<ref name="Ready to Roll">{{cite news |title=NASA's Perseverance Mars Rover Ready to Roll for Miles in Years Ahead |url=https://www.jpl.nasa.gov/news/nasas-perseverance-mars-rover-ready-to-roll-for-miles-in-years-ahead/ |work=NASA Jet Propulsion Laboratory (JPL) |date=17 December 2025 }}</ref><ref name="Williford Farley Carbonated ultramafic">{{cite journal |last1=Williford |first1=Kenneth H. |last2=Farley |first2=Kenneth A. |last3=Horgan |first3=Briony H.N. |last4=Garczynski |first4=Brad |last5=Treiman |first5=Allan H. |last6=Gupta |first6=Sanjeev |last7=Jones |first7=Alexander J. |last8=Siljeström |first8=Sandra |last9=Clavé |first9=Elise |last10=Mayhew |first10=Lisa |last11=Osterhout |first11=Jeffrey T. |last12=Ravanis |first12=Eleni |last13=Stack |first13=Kathryn M. |last14=Fagents |first14=Sarah |last15=Bedford |first15=Candice C. |last16=Bosak |first16=Tanja |last17=Bykov |first17=Sergei V. |last18=Flannery |first18=David |last19=Hand |first19=Kevin P. |last20=Jones |first20=Michael W. 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Uriah |last75=Yingst |first75=R. Aileen |title=Carbonated ultramafic igneous rocks in Jezero crater, Mars |journal=Science |date=17 December 2025 |article-number=eadu8264 |doi=10.1126/science.adu8264 |pmid=41405541 }}</ref> So at this point researchers have pieced together an understanding of the processes and their timing of how Jezero ended it to be how it is.<ref name="Ready to Roll"/><ref name="Williford Farley Carbonated ultramafic"/> After an impact created the Jezero Crater cavity, hot magma moved into weak parts of the crust and accumulated under the ground forming what are called intrusions. They may be called sills, dikes, or lacoliths depending on their shapes. In these chambers, magma underwent a slow cooling. The rocks with the large crystals were part of a group that was named the Seith Formation. Lava, then came into Jezero. The basalt from the lava flow was called the Maaza Formation.<ref name="bbc.com"/><ref>{{cite web | title=NASA's Perseverance Mars Rover Makes Surprising Discoveries | website=[[Jet Propulsion Laboratory]] | url=https://www.jpl.nasa.gov/news/nasas-perseverance-mars-rover-makes-surprising-discoveries }}</ref> Maaz is rich in the minerals pyroxene and plagioclase. It cooled quicker on the top of a mass of magma or lava. Water has altered the chemistry of the rock because carbonate, iron oxides, amorphous silicates, sulfates, halite, perchlorates, phosphates, and possible phyllosilicates were found in the rock.<ref>{{cite conference |last1=Sun |first1=V. Z. |last2=Hand |first2=K. P. |last3=Stack |first3=K. M. |last4=Farley |first4=K. A. |last5=Milkovich |first5=S. |last6=Kronyak |first6=R. |last7=Simon |first7=J. I. |last8=Hickman-Lewis |first8=K. |last9=Shuster |first9=D. |last10=J F Bell |first10=I. I. I. |last11=Gupta |first11=S. |last12=Herd |first12=C. D. K. |last13=Maurice |first13=S. |last14=Paar |first14=G. |last15=Wiens |first15=R. C. |title=Exploring the Jezero Crater Floor: Overview of Results from the Mars 2020 Perseverance Rover's First Science Campaign |date=7 March 2022 |conference=53rd Lunar and Planetary Science Conference |url=https://ntrs.nasa.gov/citations/20220000501 |bibcode=2022LPICo2678.1798S }}</ref> Erosion removed some of the upper parts of the intrusions, especially the Seith Formation. As a result of this erosion, instruments on Perseverance were able to analyze the minerals in Seith and discover the size and composition of its minerals. Eventually a large lake developed in the crater and made the carbonate minerals found by instruments on Perseverance.<ref name="Ready to Roll"/><ref name="Williford Farley Carbonated ultramafic"/><ref>{{cite journal |last1=Farley |first1=K. A. |last2=Stack |first2=K. M. |last3=Shuster |first3=D. L. |last4=Horgan |first4=B. H. N. |last5=Hurowitz |first5=J. 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Organic minerals that are probably aromatics or stable molecules of carbon and hydrogen connected to sulfates, were detected. Sulfate minerals can preserve information about the watery environments in which they formed. These molecules were found in a place called "Wildcat Ridge." It is believed to have formed as mud and sand settled in a saltwater lake that was evaporating. The Scanning Habitable Environments with Raman & Luminescence for Organics & Chemicals, or SHERLOC was used for the analysis.<ref>{{cite web | title=Perseverance rover finds organic matter 'treasure' on Mars | website=[[CNN]] | date=15 September 2022 | url=https://www.cnn.com/2022/09/15/world/perseverance-rover-mars-images-scn/index.html }}</ref><ref>{{cite web | title=NASA's Perseverance Rover Investigates Geologically Rich Mars Terrain | website=[[Jet Propulsion Laboratory]] | url=https://www.jpl.nasa.gov/news/nasas-perseverance-rover-investigates-geologically-rich-mars-terrain?utm_source=iContact&utm_medium=email&utm_campaign=nasajpl&utm_content=Daily-09152022 }}</ref>
Some rock and mineral fragments that are present in the Skinner Ridge sample hint at originating hundreds of miles outside Jezero Crater. This is from a distance that the rover will not be able to travel, but scientists will still get to examine them when the samples are returned to Earth.<ref>https://www.msn.com/en-us/news/technology/perseverance-rover-finds-organic-matter-treasure-on-mars/ar-AA11SJvX?ocid=mailsignout&cvid=d57c0d217b88485f8e8e25525f1a15ef</ref>
Perseverance may have discovered the remains of life. It found chemicals that may have been created by anaerobic organisms in the past. Speckles in rocks contained the minerals vivianite, an iron phosphate, and greigite, an iron sulfide. What's more both formed in close association with organic carbon. On Earth, vivianite frequently forms in lakes and coastal sediments where microbes use iron in their metabolism. They take iron (III) oxide, use it, and then give off Ferrous iron (II) as a waste. That ferrous iron reacts with phosphate to form vivianite.<ref>{{cite journal |last1=Yuan |first1=Qing |last2=Wang |first2=Shu |last3=Wang |first3=Xin |last4=Li |first4=Nan |title=Biosynthesis of vivianite from microbial extracellular electron transfer and environmental application |journal=Science of the Total Environment |date=March 2021 |volume=762 |article-number=143076 |doi=10.1016/j.scitotenv.2020.143076 |pmid=33129535 |bibcode=2021ScTEn.76243076Y }}</ref>
Greigite tends to form when microbes break down sulfate. They change sulfate to sulfide which unites with iron to produce greigite.<ref>{{cite journal |last1=Igarashi |first1=Kensuke |last2=Yamamura |first2=Yasuhisa |last3=Kuwabara |first3=Tomohiko |title=Natural synthesis of bioactive greigite by solid–gas reactions |journal=Geochimica et Cosmochimica Acta |date=October 2016 |volume=191 |pages=47–57 |doi=10.1016/j.gca.2016.07.005 |bibcode=2016GeCoA.191...47I |hdl=2241/00144219 |hdl-access=free }}</ref> When found together on Earth, these minerals and organic molecules are usually considered a sort of biosignature.<ref>{{cite journal |last1=Basilio |first1=Humberto |title=This Martian Rock Might Be the Closest We've Come to Finding Alien Life |journal=Scientific American |url=https://www.scientificamerican.com/article/is-there-life-on-mars-this-rock-may-hold-the-answer/ |url-access=subscription }}</ref> There are possible, but not probable ways, that these minerals may have been formed without microbes.<ref>{{cite journal |last1=Hurowitz |first1=Joel A. |last2=Tice |first2=M. M. |last3=Allwood |first3=A. C. |last4=Cable |first4=M. L. |last5=Hand |first5=K. P. |last6=Murphy |first6=A. E. |last7=Uckert |first7=K. |last8=Bell |first8=J. F. |last9=Bosak |first9=T. |last10=Broz |first10=A. P. |last11=Clavé |first11=E. |last12=Cousin |first12=A. |last13=Davidoff |first13=S. |last14=Dehouck |first14=E. |last15=Farley |first15=K. A. |last16=Gupta |first16=S. |last17=Hamran |first17=S.-E. |last18=Hickman-Lewis |first18=K. |last19=Johnson |first19=J. R. |last20=Jones |first20=A. J. |last21=Jones |first21=M. W. M. |last22=Jørgensen |first22=P. S. |last23=Kah |first23=L. C. |last24=Kalucha |first24=H. |last25=Kizovski |first25=T. V. |last26=Klevang |first26=D. A. |last27=Liu |first27=Y. |last28=McCubbin |first28=F. M. |last29=Moreland |first29=E. L. |last30=Paar |first30=G. |last31=Paige |first31=D. A. |last32=Pascuzzo |first32=A. C. |last33=Rice |first33=M. S. |last34=Schmidt |first34=M. E. |last35=Siebach |first35=K. L. |last36=Siljeström |first36=S. |last37=Simon |first37=J. I. |last38=Stack |first38=K. M. |last39=Steele |first39=A. |last40=Tosca |first40=N. J. |last41=Treiman |first41=A. H. |last42=VanBommel |first42=S. J. |last43=Wade |first43=L. A. |last44=Weiss |first44=B. P. |last45=Wiens |first45=R. C. |last46=Williford |first46=K. H. |last47=Barnes |first47=R. |last48=Barr |first48=P. A. |last49=Bechtold |first49=A. |last50=Beck |first50=P. |last51=Benzerara |first51=K. |last52=Bernard |first52=S. |last53=Beyssac |first53=O. |last54=Bhartia |first54=R. |last55=Brown |first55=A. J. |last56=Caravaca |first56=G. |last57=Cardarelli |first57=E. L. |last58=Cloutis |first58=E. A. |last59=Fairén |first59=A. G. |last60=Flannery |first60=D. T. |last61=Fornaro |first61=T. |last62=Fouchet |first62=T. |last63=Garczynski |first63=B. |last64=Goméz |first64=F. |last65=Hausrath |first65=E. M. |last66=Heirwegh |first66=C. M. |last67=Herd |first67=C. D. K. |last68=Huggett |first68=J. E. |last69=Jørgensen |first69=J. L. |last70=Lee |first70=S. W. |last71=Li |first71=A. Y. |last72=Maki |first72=J. N. |last73=Mandon |first73=L. |last74=Mangold |first74=N. |last75=Manrique |first75=J. A. |last76=Martínez-Frías |first76=J. |last77=Núñez |first77=J. I. |last78=O’Neil |first78=L. P. |last79=Orenstein |first79=B. J. |last80=Phelan |first80=N. |last81=Quantin-Nataf |first81=C. |last82=Russell |first82=P. |last83=Schulte |first83=M. D. |last84=Scheller |first84=E. |last85=Sharma |first85=S. |last86=Shuster |first86=D. L. |last87=Srivastava |first87=A. |last88=Wogsland |first88=B. V. |last89=Wolf |first89=Z. U. |title=Redox-driven mineral and organic associations in Jezero Crater, Mars |journal=Nature |date=11 September 2025 |volume=645 |issue=8080 |pages=332–340 |doi=10.1038/s41586-025-09413-0 |pmid=40931152 |pmc=12422973 |bibcode=2025Natur.645..332H }}</ref> They could have been made without biological reactions, including constant high temperatures, acidic conditions, and binding by organic compounds. But, the rocks in this place, called Bright Angel, do not show evidence that they experienced high temperatures or acidic conditions, and it is unknown whether the organic compounds present would’ve been capable of catalyzing the reaction at the expected low temperatures. This chemical evidence of past life appeared in some of the youngest sedimentary rocks the mission has examined. For a long time, we assumed signs of ancient life would be only found in older rock formations. This discovery may mean that Mars could have been habitable for a longer period or later in the planet's history than previously thought. Older rocks also might hold signs of life that are simply harder to detect.<ref>{{cite press release |last1=Taveau |first1=Jessica |title=NASA Says Mars Rover Discovered Potential Biosignature Last Year - NASA |url=https://www.nasa.gov/news-release/nasa-says-mars-rover-discovered-potential-biosignature-last-year/ |publisher=NASA |date=10 September 2025 }}</ref> The truth about these rocks may not be really known until the samples that were gathered are brought to the Earth.
===Linear ridge networks=== {{Main|Linear ridge networks}} [[File:Huo Hsing Vallis in Syrtis Major.JPG|thumb|upright=1.2|[[Huo Hsing Vallis]] in Syrtis Major, as seen by THEMIS. Straight ridges may be [[dike (geology)|dikes]] in which liquid rock once flowed.]] Some crater floors in the Syrtis Major area show elongated ridges in a lattice-like pattern.<ref>{{cite journal |last1=Kerber |first1=Laura |last2=Dickson |first2=James L. |last3=Head |first3=James W. |last4=Grosfils |first4=Eric B. |title=Polygonal ridge networks on Mars: Diversity of morphologies and the special case of the Eastern Medusae Fossae Formation |journal=Icarus |date=January 2017 |volume=281 |pages=200–219 |doi=10.1016/j.icarus.2016.08.020 |bibcode=2017Icar..281..200K }}</ref> Such patterns are typical of [[fault (geology)|faults]] and breccia [[Dike (geology)|dikes]] formed as a result of an impact. Some have suggested that these [[linear ridge networks]] are dikes made up of molten rock; others have advanced the idea that other fluids such as water were involved.<ref>{{cite journal |last1=Saper |first1=Lee |last2=Mustard |first2=John F. |title=Extensive linear ridge networks in Nili Fossae and Nilosyrtis, Mars: implications for fluid flow in the ancient crust |journal=Geophysical Research Letters |date=28 January 2013 |volume=40 |issue=2 |pages=245–249 |doi=10.1002/grl.50106 |bibcode=2013GeoRL..40..245S }}</ref> The ridges are found where there has been enhanced [[erosion]]. Pictures below show examples of these dikes. Water may flow along faults. The water often carries minerals that serve to cement rock materials thus making them harder. Later when the whole area undergoes erosion the dikes will remain as ridges because they are more resistant to erosion.<ref>{{cite news |last1=Okubo |first1=Chris |title=Ridges in Huo Hsing Vallis |url=https://hirise.lpl.arizona.edu/PSP_008189_2080 |work=HiRISE |date=21 May 2008 }}</ref> This discovery may be of great importance for future colonization of Mars because these types of faults and breccia dikes on earth are associated with key mineral resources.<ref>{{cite news |first1=Larry |last1=O'Hanlon |date=22 February 2010 |url=http://news.discovery.com/space/mars-prospecting-ores-gold.html |title=Mining Mars? Where's the Ore? |website=Discovery News |access-date=2010-06-11 |archive-date=2012-10-22 |archive-url=https://web.archive.org/web/20121022144808/http://news.discovery.com/space/mars-prospecting-ores-gold.html |url-status=dead }}</ref><ref>{{cite journal |last1=West |first1=Michael D. |last2=Clarke |first2=Jonathan D.A. |title=Potential martian mineral resources: Mechanisms and terrestrial analogues |journal=Planetary and Space Science |date=March 2010 |volume=58 |issue=4 |pages=574–582 |doi=10.1016/j.pss.2009.06.007 |bibcode=2010P&SS...58..574W }}</ref> It has been estimated that 25% of the Earth's impacts are connected to mineral production.<ref>{{cite journal |last1=Mory |first1=Arthur J. |last2=Iasky |first2=Robert P. |last3=Glikson |first3=Andrew Y. |last4=Pirajno |first4=Franco |title=Woodleigh, Carnarvon Basin, Western Australia: a new 120 km diameter impact structure |journal=Earth and Planetary Science Letters |date=15 April 2000 |volume=177 |issue=1–2 |pages=119–128 |doi=10.1016/S0012-821X(00)00031-5 |bibcode=2000E&PSL.177..119M }}</ref> The largest [[gold]] deposit on Earth is the [[Vredefort]] 300 km diameter impact structure in [[South Africa]].<ref>{{cite journal |last1=Evans |first1=Kevin R. |last2=Horton Jr. |first2=J. Wright |last3=Thompson |first3=Mark F. |last4=Warme |first4=John E. |title=The Sedimentary Record of Meteorite Impacts: An SEPM Research Conference |journal=The Sedimentary Record |date=31 March 2005 |volume=3 |issue=1 |pages=4–8 |doi=10.2110/sedred.2005.1.4 |doi-access=free }}</ref> Perhaps, when people live on Mars these kinds of areas will be mined as they are on earth.<ref>{{cite journal |last1=Head |first1=James W. |last2=Mustard |first2=John F. |title=Breccia dikes and crater-related faults in impact craters on Mars: Erosion and exposure on the floor of a crater 75 km in diameter at the dichotomy boundary |journal=Meteoritics & Planetary Science |date=October 2006 |volume=41 |issue=10 |pages=1675–1690 |doi=10.1111/j.1945-5100.2006.tb00444.x |bibcode=2006M&PS...41.1675H }}</ref>
== Streaks == Many areas of Mars change their shape and/or coloration. For many years, astronomers observing regular changes on Mars when the seasons changed, thought that what they saw was evidence of vegetation growing. After close-up inspection with a number of spacecraft, other causes were discovered. Basically, the changes are caused by the effects of the wind blowing dust around. Sometimes, fine bright dust settles on the dark basalt rock making the surface appear lighter, at other times the light-toned dust will be blown away; thus making the surface darken—just as if vegetation were growing. Mars has frequent regional or global dust storms that coat the surface with fine bright dust. In the [[THEMIS]] image below, white streaks are seen downwind of craters. The streaks are not too bright; they appear bright because of contrast with the dark volcanic rock [[basalt]] which makes up the surface.<ref>{{Cite web|url=http://themis.asu.edu/zoom-20020606a|title=Syrtis Major | Mars Odyssey Mission THEMIS|website=themis.asu.edu}}</ref>
== Inverted relief == [[File:Inverted Channel 012435.jpg|thumb|upright=1.2|Inverted Channel with many branches in Syrtis Major quadrangle]] Some places on Mars show [[inverted relief]]. In these locations, a stream bed may be a raised feature, instead of a valley. The inverted former stream channels may be caused by the deposition of large rocks or due to cementation. In either case erosion would erode the surrounding land and leave the old channel as a raised ridge because the ridge would be more resistant to erosion. Images below, taken with [[HiRISE]] show sinuous ridges that are old channels that have become inverted.<ref>{{Cite web |url=http://hiroc.lpl.arizona.edu/images/PSP/diafotizo.php?ID=PSP_002279_1735 |title=HiRISE | Sinuous Ridges Near Aeolis Mensae |access-date=2009-03-19 |archive-date=2016-03-05 |archive-url=https://web.archive.org/web/20160305025124/http://hiroc.lpl.arizona.edu/images/PSP/diafotizo.php?ID=PSP_002279_1735 |url-status=dead }}</ref>
== Methane == For several years, researchers have found [[methane]] in the atmosphere of Mars. After study, it was determined to be coming from a point in Syrtis Major, located at 10° N and 50° E.<ref>{{Cite web|url=http://www.space.com/scienceastronomy/mars-methane-gas-disappears-quickly-100920.html|title = Mystery on Mars: Why Methane Fades Away So Fast|website = [[Space.com]]|date = 20 September 2010}}</ref> A recent study indicates that to match the observations of methane, there must be something that quickly destroys the gas, otherwise it would be spread all through the atmosphere instead of being concentrated in one location. There may be something in the soil that oxidizes the gas before it has a chance to spread. If this is so, that same chemical would destroy organic compounds, thus life would be very difficult on Mars.<ref>{{Cite web |url=https://sci.esa.int/s/AqBLmnw |title=Reconciling Methane Variations on Mars |publisher=European Space Agency |date=6 August 2009 |access-date=20 August 2024}}</ref>
==Channels==
There is enormous evidence that water once flowed in river valleys on Mars.<ref>{{cite journal |last1=Baker |first1=V. |first2=Christopher W. |last2=Hamilton |first3=Devon M. |last3=Burr |display-authors=1 |year=2015 |title=Fluvial geomorphology on Earth-like planetary surfaces: a review |journal=Geomorphology |volume=245 |issue= |pages=149–182 |doi=10.1016/j.geomorph.2015.05.002 |pmid=29176917 |pmc=5701759 |bibcode=2015Geomo.245..149B }}</ref><ref>{{cite book |last1=Carr |first1=Michael H. |title=Water on Mars |date=1996 |doi=10.1093/oso/9780195099386.001.0001 |isbn=0-19-509938-9|publisher=Oxford University Press|pp=71-99|chapter=Valley Networks}}</ref> Images of curved channels have been seen in images from Mars spacecraft dating back to the early 1970s with the [[Mariner 9]] orbiter.<ref>{{cite book |last=Baker |first=V. |year=1982 |title=The Channels of Mars |publisher=Univ. of Tex. Press |location=Austin, TX |isbn=0-292-71068-2 }}{{page needed|date=January 2026}}</ref><ref>{{cite journal |last1=Baker |first1=V. |first2=R. |last2=Strom |first3=V. |last3=Gulick |first4=J. |last4=Kargel |first5=G. |last5=Komatsu |first6=V. |last6=Kale |display-authors=1 |year=1991 |title=Ancient oceans, ice sheets and the hydrological cycle on Mars |journal=Nature |volume=352 |issue= 6336|pages=589–594 |doi=10.1038/352589a0 |bibcode=1991Natur.352..589B |s2cid=4321529 }}</ref><ref>{{cite journal |last=Carr |first=M. |year=1979 |title=Formation of Martian flood features by release of water from confined aquifers |journal=J. Geophys. Res. |volume=84 |issue= |pages=2995–3007 |doi=10.1029/JB084iB06p02995 |bibcode=1979JGR....84.2995C }}</ref><ref>{{cite journal |last=Komar |first=P. |year=1979 |title=Comparisons of the hydraulics of water flows in Martian outflow channels with flows of similar scale on Earth |journal=Icarus |volume=37 |issue=1 |pages=156–181 |doi=10.1016/0019-1035(79)90123-4 |bibcode=1979Icar...37..156K }}</ref> Indeed, a study published in June 2017, calculated that the volume of water needed to carve all the channels on Mars was even larger than the proposed ocean that the planet may have had. Water was probably recycled many times from the ocean to rainfall around Mars.<ref>{{Cite web |first=Keith |last=Cowing |url=https://spaceref.com/science-and-exploration/how-much-water-was-needed-to-carve-valleys-on-mars/ |title=How Much Water Was Needed to Carve Valleys on Mars? |publisher=SpaceRef |date=5 June 2017 |access-date=20 August 2024}}</ref><ref>{{cite journal |last1=Luo |first1=W. |first2=Xuezhi |last2=Cang |first3=Alan D. |last3=Howard |display-authors=1 |year=2017 |title=New Martian valley network volume estimate consistent with ancient ocean and warm and wet climate |journal=Nature Communications |volume=8 |article-number=15766 |doi=10.1038/ncomms15766 |pmid=28580943 |pmc=5465386 |bibcode=2017NatCo...815766L |doi-access=free }}</ref>
{{Main|Valley networks (Mars)}} {{Main|Outflow channels}}
==See also== {{div col}} * {{annotated link|Flammarion (Martian crater)}} * {{annotated link|Geology of Mars}} * {{annotated link|Groundwater on Mars}} * {{annotated link|HiWish program}} * {{annotated link|Hydrothermal circulation}} * {{annotated link|Igneous differentiation}} * [[Jezero (crater)]] * {{annotated link|Lakes on Mars}} * {{annotated link|List of quadrangles on Mars}} * {{annotated link|MOC Public Targeting Program}} * {{annotated link|Ore genesis}} * {{annotated link|Ore resources on Mars}} * {{annotated link|Outflow channels}} *[[Perseverance (rover)]] * {{annotated link|Valley network (Mars)}} * {{annotated link|Vallis (planetary geology)|Vallis}} * {{annotated link|Water on Mars}} {{div col end}}
== References == {{reflist|colwidth=30em}}
== External links == {{commons category|Syrtis Major quadrangle}} {{Mars quadrangle layout}} {{Mars}} {{Portal bar|Solar System}}
{{DEFAULTSORT:Syrtis Major Quadrangle}} [[Category:Syrtis Major quadrangle| ]] [[Category:Mars]]