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Jezero Crater

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Image
Artist’s reconstruction of Jezero Crater, Mars, as it may have looked billions of years ago when it was a lake. Image credit: NASA/JPL-Caltech
Published: 01 February 2023
Artist’s reconstruction of Jezero Crater, Mars, as it may have looked billions of years ago when it was a lake. I mage credit : NASA/JPL-C altech
Image
(left) Color image of the delta in Jezero Crater taken by the High-Resolution Stereo Camera aboard the European Space Agency Mars Express orbiter (ESA/DLR/FU-Berlin). (A–F) Stratigraphic relationships observed in Kodiak butte, which is an isolated erosional remnant of the delta imaged by the Perseverance rover shortly after landing in Jezero Crater. Reproduced from Mangold et al. (2021) with permission from The American Association for the Advancement of Science. Elevation scales are inferred from a digital elevation model and have systematic uncertainties of ±2 m. White boxes indicate regions shown in more detail in other panels. (B), (E) Interpreted line drawings of the main visible beds (blue lines for individual beds and red lines for discontinuities), overlain on the images from (A) and (D). (C) Zoomed image of k1 showing the change in dip from sub-horizontal beds (topsets) to inclined beds (foresets). (F) Zoomed image of the foresets in k3. This unit has a coarse texture with several cobble-size clasts. The erosional truncation of k3 by k4 is labeled.
Published: 01 February 2023
Figure 2. ( left ) Color image of the delta in Jezero Crater taken by the High-Resolution Stereo Camera aboard the European Space Agency Mars Express orbiter (ESA/DLR/FU-Berlin). ( A–F ) Stratigraphic relationships observed in Kodiak butte, which is an isolated erosional remnant of the delta
Image
False-color delta deposits in Jezero Crater on Mars, as seen by NASA’s Mars Reconnaissance Orbiter. The green color shows Fe/Mg smectites deposited in the ancient crater lake. The Mars 2020 rover is scheduled to explore whether these deposits contain trapped organic biosignatures. Image credit: NASA/JPL-Caltech/MSSS/JHU-APL.
Published: 01 February 2020
Figure 1. False-color delta deposits in Jezero Crater on Mars, as seen by NASA’s Mars Reconnaissance Orbiter . The green color shows Fe/Mg smectites deposited in the ancient crater lake. The Mars 2020 rover is scheduled to explore whether these deposits contain trapped organic biosignatures. I
Image
A: Olivine-rich unit superposing rim of Jezero crater (Mars; 18.4°N, 77.7°E) in digital elevation model. Inset shows olivine-rich mesa (outlined) ∼675 m above surrounding terrain, similar in morphology to in-place olivine-rich mesas elsewhere. Red to green shading denotes elevation, ranging from –1022 m (floor of Jezero) to –1300 m (rim of Jezero, foreground). B: Unit’s measured topographic distribution along line of section z-z′ in A, inferred from morphology and spectroscopy. Unit’s minimum elevation above surrounding terrain is noted. C: Unit’s topographic range in circum-Isidis region, derived from Mars Orbiter Laser Altimeter on Mars Global Surveyor, relative to Mars datum and binned by area. Libya Montes area (black) is small. Imagery identification details and more examples are shown in Figure DR9 (see footnote 1).
Published: 22 May 2019
Figure 3. A: Olivine-rich unit superposing rim of Jezero crater (Mars; 18.4°N, 77.7°E) in digital elevation model. Inset shows olivine-rich mesa (outlined) ∼675 m above surrounding terrain, similar in morphology to in-place olivine-rich mesas elsewhere. Red to green shading denotes elevation
Image
Olivine-bearing rocks in and near the Nili Fossae region of Mars. (A) Digital terrain model (DTM) of Jezero Crater and Nili Planum, with landing site (“x”) and traverse of the Perseverance rover in white. Much of the region is covered in a thin (~1–10 m) layer of olivine-rich rock. (B) Outcrops of olivine-rich basaltic rocks at Jezero Crater (DTM from rover images). (C) Olivine grains from rock in (A) and (B). (D) Layered olivine-rich rock, stratigraphically correlated with rocks in/near Jezero Crater (DTM from orbital data).
Published: 01 June 2023
Figure 4. Olivine-bearing rocks in and near the Nili Fossae region of Mars. ( A ) Digital terrain model (DTM) of Jezero Crater and Nili Planum, with landing site (“x”) and traverse of the Perseverance rover in white. Much of the region is covered in a thin (~1–10 m) layer of olivine-rich rock
Journal Article
Journal: Elements
Published: 01 February 2023
Elements (2023) 19 (1): 37–44.
...Artist’s reconstruction of Jezero Crater, Mars, as it may have looked billions of years ago when it was a lake. I mage credit : NASA/JPL-C altech ...
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Journal Article
Journal: Geophysics
Published: 14 February 2023
Geophysics (2023) 88 (2): A7–A12.
... collected in the Jezero crater during the Mars2020 mission of the Perseverance rover, showing successful performances and robustness. After selecting data from the entire RIMFAX data set (from SOL 072 to SOL 204) to avoid redundant data due to continuing data acquisition during rover stops based...
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Image
Potential for extraformational, recycled sediment at the planned Perseverance rover site in Jezero crater, located at 18.6°N, 282.4°W (18.4°N, 77.7°E). C–G are presented at the same scale. (A) Jezero crater and local context. The locations of B–E are indicated. Blue traces indicate inlet valleys (Neretva and Sava); purple trace indicates an outlet valley (Pliva). West of Jezero crater, olivine- and carbonate-bearing rock is cut by Neretva Vallis and Sava Vallis (Goudge et al., 2015). (B) Lithified, deltaic sediment of the “western delta” in Jezero crater. (C) Detailed view of the geomorphic expression of rock cut by Neretva Vallis. (D) Detailed view of the geomorphic expression of rock cut by Sava Vallis. (E) Detailed view of the geomorphic expression of rock cut by Neretva Vallis. (F) Compare with D; detailed view of an outcrop of the fine-grained (largely mudstone) Murray formation in Gale crater; dark-toned materials are windblown sands, and lighter-toned features are blocks of mudstone slightly displaced in outcrop expression. Yellow trace indicates the Curiosity rover traverse; yellow dots indicate locations where the rover parked after each drive; white numbers indicate the sols that bracketed this portion of the traverse. Color inset from Mars Hand Lens Imager (MAHLI) shows a dust-coated mudstone surface investigated along this traverse (arrow); the bands are a stair-stepped expression of fine laminae. (G) Compare with E; detailed view of a dust-coated outcrop of the Sheepbed (mudstone) member of the Yellowknife Bay formation in Gale crater (see Schieber et al., 2017). Yellow trace and dots indicate rover traverse through the area between sols 121 and 309. Color inset from MAHLI shows the very fine–grained nature of the mudstone; the larger, lighter-toned objects are dust clumps stirred by the rover’s wire brush tool; the finer, speckled surface illustrates silt-sized grains.
Published: 06 October 2020
Figure 19. Potential for extraformational, recycled sediment at the planned Perseverance rover site in Jezero crater, located at 18.6°N, 282.4°W (18.4°N, 77.7°E). C–G are presented at the same scale. (A) Jezero crater and local context. The locations of B–E are indicated. Blue traces indicate
Image
Examples of possible ancient lacustrine environments on Mars. Some putative crater lakes exhibit clear evidence of sedimentary strata bearing clay minerals, such as: (a) the deltaic deposits in the closed-basin Eberswalde Crater (Milliken and Bish, 2010); and (b) deposits in the open-basin Jezero Crater (Fassett and Head, 2008; Ehlmann et al., 2008a). Other craters exhibit geomorphic evidence (e.g. inlets and outlets) for standing bodies of water but currently lack clear sedimentological and/or mineralogical evidence for lacustrine deposits, such as (c) Gusev Crater (Cabrol et al., 1996) and (d) a crater located at −9.5ºS, 135ºE (Cabrol and Grin, 1999; Fassett and Head, 2008). Arrows point North. (e) Topographic map of Mars based on Mars Orbiter Laser Altimeter (MOLA) data (produced by the MOLA team) showing the locations of sites in Figures 1 and 2.
Published: 01 August 2011
-basin Jezero Crater ( Fassett and Head, 2008 ; Ehlmann et al. , 2008a ). Other craters exhibit geomorphic evidence ( e.g. inlets and outlets) for standing bodies of water but currently lack clear sedimentological and/or mineralogical evidence for lacustrine deposits, such as (c) Gusev Crater ( Cabrol
Journal Article
Published: 01 January 2025
American Mineralogist (2025) 110 (1): 34–47.
... abundance estimates rather than mineral species determination. Since the arrival of the Perseverance rover to Jezero crater, scientific investigations have focused on two geologic units called the Máaz and the Séítah formations ( Bell et al. 2022 ; Liu et al. 2022 ; Farley et al. 2022 ). The Máaz...
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Image
Distribution of paleolakes on Mars from Goudge et al. (2016). Open- and closed-basin valley network-fed lakes (black and white symbols, respectively) were primarily formed earlier in Martian geological history, prior to 3.7 Ga. Closed-basin paleolakes with isolated inlet valleys (red symbols) primarily formed subsequent to the era of major valley network formation, after 3.7 Ga. Closed-basin lakes indicated by stars are hosted by craters with continuous ejecta deposits or have inlet valleys that incise continuous ejecta deposits of nearby craters, indicating more recent activity than their counterparts that are mapped with circular symbols. The location of Jezero Crater (white circle with label) is indicated. The background shows the Mars Orbiter Laser Altimeter (MOLA) gridded topography, in which white represents the highest elevations and purple the lowest, overlain on a MOLA-derived hillshade map.
Published: 01 February 2023
their counterparts that are mapped with circular symbols. The location of Jezero Crater (white circle with label) is indicated. The background shows the Mars Orbiter Laser Altimeter (MOLA) gridded topography, in which white represents the highest elevations and purple the lowest, overlain on a MOLA-derived hillshade
Journal Article
Journal: Geology
Published: 22 May 2019
Geology (2019) 47 (7): 677–681.
...Figure 3. A: Olivine-rich unit superposing rim of Jezero crater (Mars; 18.4°N, 77.7°E) in digital elevation model. Inset shows olivine-rich mesa (outlined) ∼675 m above surrounding terrain, similar in morphology to in-place olivine-rich mesas elsewhere. Red to green shading denotes elevation...
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Image
Fluvial ridge morphology on Mars and relationships with adjacent units. (A) NASA Context Camera (CTX) mosaic of Arabia Terra with Mars Orbiter Laser Altimeter (MOLA) topography of fluvial ridges (black arrows) emanating downslope from valley networks and eroding out of a broader sedimentary unit (Davis et al., 2016). 7.6°N, 26.3°E. Inset: High Resolution Imaging Science Experiment (HiRISE) orbit ESP_058721_1875. (B) Flat-topped fluvial ridges within Aeolis Dorsum in CTX data. These ridges show branching and meandering patterns. 4.9°S, 155.0°E. In our mapping, systems of ridges are represented by a single marker in Figure 3. (C) CTX mosaic of fluvial ridges in direct contact with exhumed crater fills in Arabia Terra. 16.1°N, 50.0°E. (D) Anastomosing ridges observed in CTX data in cratered plains west of Alba Patera. 43.7°N, 232.4°E. (E) Fluvial ridge in CTX data confined within an existing valley upstream of the western fan within Jezero crater. 18.8°N, 76.9°E.
Published: 21 December 2020
an existing valley upstream of the western fan within Jezero crater. 18.8°N, 76.9°E.
Journal Article
Journal: Elements
Published: 01 April 2021
Elements (2021) 17 (2): 143.
... or lack thereof between the degree of shock metamorphism extrapolation of the lunar record. But how to choose the right rock for and the amount of Pb loss in baddeleyite, demonstrating that micro- this? Studies of the floor of Jezero Crater (Perseverance s landing site) structural studies of baddeleyite...
Journal Article
Journal: Elements
Published: 01 June 2023
Elements (2023) 19 (3): 173–179.
...Figure 4. Olivine-bearing rocks in and near the Nili Fossae region of Mars. ( A ) Digital terrain model (DTM) of Jezero Crater and Nili Planum, with landing site (“x”) and traverse of the Perseverance rover in white. Much of the region is covered in a thin (~1–10 m) layer of olivine-rich rock...
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Journal Article
Journal: Elements
Published: 01 April 2022
Elements (2022) 18 (2): 75.
... materials, which we already know are present in Gale crater mud stones, surfaces of rocks in Jezero crater, and in trace amounts in some Martian meteorites. These organics just might be the trace residues of past Martians. Or, they might be something less exciting, like organics from chondritic meteorites...
FIGURES
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Olivine records nebular and planetary processes across the galaxy. Following the arrow, inset images are: presolar olivine grain, TEM (Messenger et al. 2005); Maralinga barred olivine (BO) chondrule, crossed polars (Photo: Laurence Garvie, Buseck Center for Meteorite Studies, ASU); Seymchan pallasite (Photo: Laurence Garvie); lunar troctolite 76535 (NASA); Apollo 17 orange glass deposit, transmitted light (Photo: Emily First); phosphorous distribution in olivine in Martian meteorite Yamato 980459 (Photo: Emily First); Dourbes abrasion patch on altered olivine-rich rock in Jezero Crater, Mars (NASA). Background images are for illustrative purposes only. Their origins are: stellar nursery Cepheus B (NASA/CXC/PSU/K/JPL-Caltech/CfA); star HL Tau and its protoplanetary disk (ESO/NAOJ/NRAO/C. Brogan/B. Saxton/AUI/NSF); asteroid Vesta (NASA/JPL-Caltech/UCAL/MPS/DLR/IDA); artist’s rendering of Jupiter Trojan asteroids (NASA/JPL-Caltech); artist’s rendering of a cooling planet (NASA/JPL-Caltech); Mars (ESA/DLR/FU/Berlin/Justin Cowart; CC BY 3.0).
Published: 01 June 2023
on altered olivine-rich rock in Jezero Crater, Mars (NASA). Background images are for illustrative purposes only. Their origins are: stellar nursery Cepheus B (NASA/CXC/PSU/K/JPL-C altech /C f A); star HL Tau and its protoplanetary disk (ESO/NAOJ/NRAO/C. B rogan /B. S axton /AUI/NSF); asteroid Vesta (NASA
Journal Article
Journal: GSA Bulletin
Published: 28 August 2023
GSA Bulletin (2024) 136 (5-6): 2007–2018.
... ). Understanding the origin of clay minerals and their implications for habitability is critical for NASA’s Mars 2020 Perseverance rover mission. The landing site for the Perseverance rover is within the Jezero Crater basin situated in the clay-rich Nili Fossae region, which is proximal to one of the largest...
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Journal Article
Journal: Geosphere
Published: 11 March 2024
Geosphere (2024) 20 (2): 547–576.
... ( Sautter et al., 2015 ; Cousin et al., 2017 ; Berger et al., 2020 ), and basaltic lava samples from Jezero Crater ( Farley et al., 2022 ; Liu et al., 2022 ; Wiens et al., 2022 ; Simon et al., 2023 ). We also included data from shergottite meteorites as compiled in Udry et al. (2020...
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Journal Article
Published: 26 September 2023
Journal of the Geological Society (2023) 180 (5): jgs2022-152.
... ), there is a relative lack of carbonate deposits at the surface of the planet ( Bridges et al. 2001 ; Ehlmann et al. 2008 ; Horgan et al. 2020 ). Most of the sedimentary carbonates identified on Mars are magnesium carbonates, such as those at Columbia Hills, Gusev Crater ( Morris et al. 2010 ) and Jezero...
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