DOCSLIB.ORG

Mest Ceresglobalmapping.Pdf

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Mest Ceresglobalmapping.Pdf Scott C. Mest1 1Planetary Science Institute, Tucson, AZ 1 David A. Crown 2School of Earth & Space Exploration, R. Aileen Yingst1 Arizona State University, Tempe, AZ 1 Daniel C. Berman 3JHU-APL, Laurel, MD 2 David A. Williams 4 3 NASA JPL, California Institute of Debra L. Buczkowski Technology, Pasadena, CA Jennifer E.C. Scully4 5MPI for Solar System Research, Thomas Platz1,5 Göttingen, Germany H. Hiesinger6 6 J.H. Pasckert6 Institute for Planetology, WWU, Münster, Germany A. Neesemann7 7 Ralf Jaumann8 Freie Universität, Berlin, Germany Thomas Roatsch8 8DLR, Berlin, Germany Frank Preusker8 9UCLA, Los Angeles, CA, USA Andreas Nathues5 Carol A. Raymond4, 9 Christopher T. Russell Planetary Geologic Mappers Meeting/Planetary Data Workshop June 12-15, 2017 Outline Objectives Background HAMO-phase mapping Global mapping datasets Methodology (scale, feature sizes, unit identification) Current state of the map / Mapping highlights Publication and archiving Cerean Chronostratigraphy Ongoing work This work is supported by the NASA Dawn at Ceres Guest Investigator Program. June 12-15, 2017 PGMM/PDW 2 Objectives Through mapping, we are …evaluating the global geology of Ceres where important spatial and temporal relationships between geologic processes are preserved. …characterizing and analyzing stratigraphy of mapped geologic units …addressing outstanding science questions regarding the nature and stratigraphy of its impact record, potential past (cryo)volcanic activity and other geologic processes. Specific scientific objectives of this investigation include: Evaluate the timing and sequence of impact events by characterizing the spatial and temporal relationships between impact craters and other surface materials. Evaluate the nature of surface materials via assessment of surface and feature morphology, and unit extent and distribution. Determine relative ages of mapped units and features via analysis of crater size-frequency distribution statistics and stratigraphic relations (e.g., superposition, cross-cutting); develop a cerean time-stratigraphic system. June 12-15, 2017 PGMM/PDW 3 HAMO-phase mapping plan Construct geologic map at 1:2.5M scale. • Build upon Survey map [Buczkowski et al., 2016, Science, v353] using HAMO data (FC base, DTM, color maps), and informed by LAMO images (for unit characterization) Evaluate global geologic history and develop cerean time-stratigraphic system • Relative ages determined from stratigraphic relationships (superposition, cross-cutting, embayment). • “Absolute” ages estimated from lunar- and asteroid-based chronologies; both will be reported. Publish map, map text, and timescale in a journal (e.g., Icarus) Archive geologic map and ancillary data layers (e.g., linear feature map, impact crater location map, lobate feature map) with PDS June 12-15, 2017 PGMM/PDW 4 Global datasets Framing Camera mosaic Clear filter map base Survey mosaic HAMO mosaic (400 m/pixel) (140 m/pixel) VENDIMIA HANAMI Occator PLANITIA PLANUM Kerwan Urvara Yalode June 12-15, 2017 PGMM/PDW 5 Supplemental datasets - topography FC-derived DTM (~137 m/pixel) • Used to identify geologic structures, characterize relationships between geologic units and topography Surface exhibits ~15 km in relief (+7.5 km, knobs in north; -7.5 km, floor of Urvara) • Broad expanses of low-lying terrain – shaped largely by impacts (e.g., Vendimia Planitia) • Areas of elevated terrain – “high” areas composed of knobs and crater rims (eg., Hanami Planum) HAMO DTM VENDIMIA HANAMI Occator PLANITIA PLANUM Kerwan Yalode Urvara June 12-15, 2017 PGMM/PDW 6 Supplemental datasets - spectral Spectral data is used to (a) assist in mapping unit contacts, and (b) FC Color (0.44-0.96 μm) provide useful and unique compositional information in unit – Color filter maps (DLR) descriptions that can help – Color ratio maps - Ceres Color Composite maps (MPS) Ceres Color Composite A: R=965/750, G=750, B=440/750 distinguish geologic units. June 12-15, 2017 PGMM/PDW 7 Supplemental datasets - spectral Spectral data is used to (a) assist in mapping unit contacts, and (b) FC Color (0.44-0.96 μm) provide useful and unique compositional information in unit – Color filter maps (DLR) descriptions that can help – Color ratio maps - Ceres Color Composite maps (MPS) Ceres Color Composite A: R=965/750, G=750, B=440/750 distinguish geologic units. June 12-15, 2017 PGMM/PDW 8 HAMO-based point and linear features Linework length > 20 km Crater diameter > 20 km O K Y U June 12-15, 2017 PGMM/PDW 9 HAMO-based contacts and units Unit area > 100 km2 O K Y U June 12-15, 2017 PGMM/PDW 10 HAMO-based geologic map Regional units (ct, s) unconstrained by topography Color data useful for estimating extents of proximal ejecta of “fresh” craters FC HAMO DTM FC color CCC A June 12-15, 2017 PGMM/PDW 11 Impact craters Most pervasive features on Ceres Sizes range from limits of FC resolution to largest craters, e.g., Kerwan (280 km), Yalode (260 km), Urvara (170 km) Morphology – well-preserved, degraded, and buried Well-preserved craters Gaue (80 km) • rims nearly circular and raised above surrounding terrain • small craters (D<15 km) are bowl-shaped • larger well-preserved craters display steep walls, slump terraces along their walls, scalloped rims • Some display flat floors, some floors fractured (e.g., Occator and Dantu); most contain hummocky floor deposits, debris lobes on their floors • Most have well-preserved ejecta deposits Degraded craters • irregularly shaped • Rims are rounded and at or near level of surrounding terrain Dantu (126 km) • Most nearly filled June 12-15, 2017 PGMM/PDW 12 Rayed craters (D>30 km) Azacca, Dantu, Haulani, Occator (D<30 km) Cacaguati, Kupalo, Oxo, Takel Well-preserved rims and ejecta Steep walls, terrace deposits, lobate deposits Smooth floors; fractures High albedo rays in ejecta, bluish in CCC-A Stratigraphically important impact structures; represent some of youngest impacts on Ceres June 12-15, 2017 13 PGMM/PDW Urvara and Yalode 170 km and 260 km in diameter Extensive ejecta deposits; smooth and rugged (Urvara), hummocky (Yalode) Structures (troughs, grooves, secondary chains) within Yalode ejecta help reveal extent Relatively smooth floor deposits; fractures, grooves Stratigraphically important impact structures June 12-15, 2017 PGMM/PDW 14 Urvara and Yalode 170 km and 260 km in diameter Extensive ejecta deposits; smooth and rugged facies (Urvara), hummocky and etched? textures (Yalode) Structures (troughs, grooves, secondary chains) within Yalode ejecta help reveal extent Relatively smooth floor deposits; fractures, grooves Stratigraphically important impact structures June 12-15, 2017 PGMM/PDW 15 Smooth and featureless; superposed by craters and secondary craters Smooth material Moderate albedo Underlaying hummocky texture in west No clear source, emplacement process June 12-15, 2017 PGMM/PDW 16 Cratered terrain Covers most of Ceres’ surface Rugged surfaces formed by structures and deposits of impacts Moderate albedo June 12-15, 2017 PGMM/PDW 17 Chronostratigraphy of Ceres Organizing major geologic events that are separated in time into distinct time- stratigraphic periods Relative ages determined from stratigraphic relations Superposition, cross cutting, embayment Key relationships missing, e.g., between major impact events and smooth material Absolute model ages determined from calculating crater size-frequency distribution statistics Counts from a number of Dawn Science Team sources Ages from Lunar-derived Model (LDM) and Asteroid-derived Model (ADM) will be reported. June 12-15, 2017 PGMM/PDW 18 Chronostratigraphy of Ceres Major referents to be used to define Chronostratigraphic Series: Azacca crater materials – represents base of “Era of rayed craters” Urvara Formation Yalode Formation Kerwan smooth material Cratered terrain – represents oldest known crust Preliminary absolute model ages (based on sub-sets of unit areas) derived for major geologic units used to represent the cerean chronostratigraphic time periods. June 12-15, 2017 PGMM/PDW 19 Chronostratigraphy of Ceres Preliminary geologic timescale based on absolute model ages derived for referents. Ages being recalculated for full unit areas - Results will inform us if sub-unit areas should be counted to smaller diameters Considering combining Urvaran and Yalodean Tanaka et al. (1992) Mars Crater-Density Absolute-Age Range Range N(D) = no.>D/106 (Myr) km2 Epoch N(1) N(2) N(5) N(16) LDM ADM Azaccan Y Y -- -- 110-0 38-0 Urvaran Y Y Y -- 160-110 100-38 Yalodean -- Y Y Y 840-160 180-100 KerwananJune 12-15, 2017-- Y Y Y 2,500-840 PGMM/PDW2,400-180 20 Pre-Kerwanan -- -- Y Y 4,600-2,500 4,600-2,000 June 12-15, 2017 PGMM/PDW 21.
Load more

Recommended publications
  • The Puzzle of the Missing Large Craters. S
    47th Lunar and Planetary Science Conference (2016) 1281.pdf CRATERING ON CERES: THE PUZZLE OF THE MISSING LARGE CRATERS. S. Marchi1, D. P. O'Brien2, P. Schenk3, R. Fu4, A. Ermakov5, M. C. De Sanctis6, E. Ammannito7, D. A. Williams8, S. C. Mest2, C. A. Raymond9, C. T. Russell7; 1Southwest Research Institute ([email protected]), Boulder, CO; 2Planetary Science Institute, Tucson, AZ; 3Lunar and Planetary Institute, Houston, TX; 4Lamont-Doherty Earth Ob- servatory, Palisades, NY; 5Massachusetts Institute of Technology, Cambridge, MA; 6Istituto Nazionale d'Astrofisica, Rome, Italy; 7University of California, Los Angeles, CA; 8Arizona State University, Tempe, AZ; 9JPL, Caltech, Pasadena, CA. Introduction: Data acquired by the Dawn space- hemisphere, although heavily craters terrains are also craft revealed a portrait of Ceres's surface that, in many found at low latitudes. This observation tells us that to- ways, challenges our preconceived expectations. pographic relaxation due to the presence of an ice-rich Ceres is the largest object in the main belt of aster- shell has to be limited. Furthermore, an improved oids. As such, extensive ground-based and Hubble model of topographic relaxation has constrained the Space Telescope observations have provided a wealth fraction of ice to be <30% in the outer shell [9]. of information [e.g. 1,2] Ceres' surface has a very low A second major finding is the lack of larger craters. albedo (~9 %) [2], while the lack of significant absorp- The largest well recognizable craters are 260-280 km tions bands at visible and near-infrared wavelengths in diameter. Although large scale topography relaxes points toward a more pristine composition [e.g., 3,4] if faster than at small scales, the lack of large craters compared to many siblings in the asteroid belt (and no- seems at odds with the presence of heavily cratered ter- tably to the large asteroid Vesta).
    [Show full text]
  • March 21–25, 2016
    FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk,
    [Show full text]
  • THE PLANETARY REPORT JUNE SOLSTICE 2016 VOLUME 36, NUMBER 2 Planetary.Org
    THE PLANETARY REPORT JUNE SOLSTICE 2016 VOLUME 36, NUMBER 2 planetary.org ILLUMINATING CERES DAWN SHEDS NEW LIGHT ON AN ENIGMATIC WORLD BREAKTHROUGH STARSHOT C LIGHTSAIL 2 TEST C MEMBERSHIP UPGRADES SNAPSHOTS FROM SPACE EMILY STEWART LAKDAWALLA blogs at planetary.org/blog. Black Sands of Mars ON SOL 1192 (December 13, 2015), Curiosity approached the side of Namib, a Faccin and Marco Bonora Image: NASA/JPL/MSSS/Elisabetta massive barchan sand dune. Namib belongs to a field of currently active dark basaltic sand dunes that form a long barrier between the rover and the tantalizing rocks of Mount Sharp. This view, processed by Elisabetta Bonora and Marco Faccin, features wind-carved yardangs (crests or ridges ) of Mount Sharp in the background. After taking this set of photos, Curiosity went on to sample sand from the dune, and it is now working its way through a gap in the dune field on the way to the mountain. —Emily Stewart Lakdawalla SEE MORE AMATEUR-PROCESSED SPACE IMAGES planetary.org/amateur SEE MORE EVERY DAY! planetary.org/blogs 2 THE PLANETARY REPORT C JUNE SOLSTICE 2016 CONTENTS JUNE SOLSTICE 2016 COVER STORY Unveiling Ceres 6 Simone Marchi on why Ceres is a scientific treasure chest for Dawn. Pathway to the Stars Looking back at years of Society-led solar sail 10 development as Breakthrough Starshot is announced. Life, the Universe, and Everything 13 Planetary Radio in Death Valley. ADVOCATING FOR SPACE Partisan Peril 18 Casey Dreier looks at the U.S. President’s impact on space policy and legislation. DEVELOPMENTS IN SPACE SCIENCE Update on LightSail 2 20 Bruce Betts details the progress we’ve made in the year since LightSail 1 launched.
    [Show full text]
  • Jjmonl 1802.Pmd
    alactic Observer John J. McCarthy Observatory G Volume 11, No. 2 February 2018 A porpoise or a penguin or a puppet on a string? — Find out on page 19 The John J. McCarthy Observatory Galactic Observer New Milford High School Editorial Committee 388 Danbury Road Managing Editor New Milford, CT 06776 Bill Cloutier Phone/Voice: (860) 210-4117 Production & Design Phone/Fax: (860) 354-1595 www.mccarthyobservatory.org Allan Ostergren Website Development JJMO Staff Marc Polansky Technical Support It is through their efforts that the McCarthy Observatory Bob Lambert has established itself as a significant educational and recreational resource within the western Connecticut Dr. Parker Moreland community. Steve Barone Jim Johnstone Colin Campbell Carly KleinStern Dennis Cartolano Bob Lambert Route Mike Chiarella Roger Moore Jeff Chodak Parker Moreland, PhD Bill Cloutier Allan Ostergren Doug Delisle Marc Polansky Cecilia Detrich Joe Privitera Dirk Feather Monty Robson Randy Fender Don Ross Louise Gagnon Gene Schilling John Gebauer Katie Shusdock Elaine Green Paul Woodell Tina Hartzell Amy Ziffer In This Issue OUT THE WINDOW ON YOUR LEFT .................................... 4 REFERENCES ON DISTANCES ............................................ 18 VALENTINE DOME .......................................................... 4 INTERNATIONAL SPACE STATION/IRIDIUM SATELLITES .......... 18 PASSING OF ASTRONAUT JOHN YOUNG ............................... 5 SOLAR ACTIVITY ........................................................... 19 FALCON HEAVY DEBUT ..................................................
    [Show full text]
  • 1950 Da, 205, 269 1979 Va, 230 1991 Ry16, 183 1992 Kd, 61 1992
    Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. Burbine Index More Information 356 Index 1950 DA, 205, 269 single scattering, 142, 143, 144, 145 1979 VA, 230 visual Bond, 7 1991 RY16, 183 visual geometric, 7, 27, 28, 163, 185, 189, 190, 1992 KD, 61 191, 192, 192, 253 1992 QB1, 233, 234 Alexandra, 59 1993 FW, 234 altitude, 49 1994 JR1, 239, 275 Alvarez, Luis, 258 1999 JU3, 61 Alvarez, Walter, 258 1999 RL95, 183 amino acid, 81 1999 RQ36, 61 ammonia, 223, 301 2000 DP107, 274, 304 amoeboid olivine aggregate, 83 2000 GD65, 205 Amor, 251 2001 QR322, 232 Amor group, 251 2003 EH1, 107 Anacostia, 179 2007 PA8, 207 Anand, Viswanathan, 62 2008 TC3, 264, 265 Angelina, 175 2010 JL88, 205 angrite, 87, 101, 110, 126, 168 2010 TK7, 231 Annefrank, 274, 275, 289 2011 QF99, 232 Antarctic Search for Meteorites (ANSMET), 71 2012 DA14, 108 Antarctica, 69–71 2012 VP113, 233, 244 aphelion, 30, 251 2013 TX68, 64 APL, 275, 292 2014 AA, 264, 265 Apohele group, 251 2014 RC, 205 Apollo, 179, 180, 251 Apollo group, 230, 251 absorption band, 135–6, 137–40, 145–50, Apollo mission, 129, 262, 299 163, 184 Apophis, 20, 269, 270 acapulcoite/ lodranite, 87, 90, 103, 110, 168, 285 Aquitania, 179 Achilles, 232 Arecibo Observatory, 206 achondrite, 84, 86, 116, 187 Aristarchus, 29 primitive, 84, 86, 103–4, 287 Asporina, 177 Adamcarolla, 62 asteroid chronology function, 262 Adeona family, 198 Asteroid Zoo, 54 Aeternitas, 177 Astraea, 53 Agnia family, 170, 198 Astronautica, 61 AKARI satellite, 192 Aten, 251 alabandite, 76, 101 Aten group, 251 Alauda family, 198 Atira, 251 albedo, 7, 21, 27, 185–6 Atira group, 251 Bond, 7, 8, 9, 28, 189 atmosphere, 1, 3, 8, 43, 66, 68, 265 geometric, 7 A- type, 163, 165, 167, 169, 170, 177–8, 192 356 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H.
    [Show full text]
  • Fracture Geometry and Statistics of Ceres' Floor Fractures
    1 Fracture Geometry and Statistics of Ceres’ Floor Fractures 2 3 K. Krohn1, D. L. Buczkowski2, I. von der Gathen1, R. Jaumann1,3, F. Schulzeck1, K. Stephan1, R. 4 Wagner1, J. E. C. Scully4, C. A. Raymond4, C. T. Russell5 5 6 1Institute of Planetary Research, German Aerospace Center, Berlin, Germany; 2Johns Hopkins 7 University Applied Physics Laboratory, Laurel, MD, USA; 3Freie Universiät Berlin, Germany; 8 4NASA JPL, California Institute of Technology, Pasadena, California, USA; 5UCLA, Institute of 9 Geophysics, Los Angeles, CA, USA 10 11 Corresponding author: Katrin Krohn, [email protected], Rutherfordstraße 2, 12489 Berlin, Germany 12 13 Keywords: Ceres, dwarf planet, floor fractured craters 14 15 16 Highlights: 17 18 We measured 2336 fractures in thirteen floor-fractured craters (FFC) on Ceres. 19 20 Floor-fractured craters on Ceres share similarities with FFCs on other planetary bodies 21 especially those on the Moon and Mars. 22 23 On Ceres some floor-fractured craters are impact-driven; other appear to be related to cooling- 24 melting processes, outgassing and/or tectonics such as doming of the subsurface. 25 26 Fracture studies point out brittle surface materials. 27 28 29 30 Abstract 31 32 Floor-fractured craters are one of the most distinct features on Ceres. Most of the fractures are located 33 on the crater floors. The floor-fractures are concentric, radial or polygonal and share similarities with 34 Class 1 and 4 floor-fractured craters (FFC) on the Moon (e.g., Buczkowski et al., 2018; Schultz, 1976) 35 In total we measured 2336 fractures in thirteen craters.
    [Show full text]
  • Mineralogical Mapping of the Kerwan Quadrangle on Ceres
    Icarus 318 (2019) 188–194 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Mineralogical mapping of the Kerwan quadrangle on Ceres ∗ E. Palomba a,e, , A. Longobardo a, M.C. De Sanctis a, F.G. Carrozzo a, A. Galiano a,b, F. Zambon a, A. Raponi a, M. Ciarniello a, K. Stephan c, D.A. Williams d, E. Ammannito a,g, M.T. Capria a,e, S. Fonte a, M. Giardino a, F. Tosi a, C.A. Raymond f, C.T. Russell g a Istituto di Astrofisica e Planetologia Spaziali, INAF, via del fosso del Cavaliere, 100, 00133, Rome, Italy b Università di Roma Tor Vergata, Department of Physics, via della ricerca scientifica, 1, 00133 Rome, Italy c Institute of Planetary Research, German Aerospace Center (DLR), Rutherfordstrasse 2, d-12489 Berlin, Germany d School of Earth & Space Exploration, Arizona State University, Tempe, AZ 85287-1404, USA e Space Science Data Center (SSDC) - Agenzia Spaziale Italiana (ASI), Via del Politecnico snc, Edificio D, 00133 Roma, Italy f Jet Propulsion Laboratory, Pasadena, CA 91109, USA g Institute of Geophysics and Planetary Physics, University of California, Los Angeles, CA 90095-1567, USA a r t i c l e i n f o a b s t r a c t Article history: The Ceres surface is globally composed of Mg-phyllosilicates, ammoniated clays, carbonates and dark Received 28 April 2017 components. To obtain a more detailed mineralogical and geological investigation, the dwarf planet sur- Revised 11 July 2017 face has been divided into fifteen quadrangles. The aim of this work is to investigate the abundance of Accepted 25 July 2017 phyllosilicates and ammoniated clays in the Kerwan quadrangle, classified as Ac-H-7 and spanning from Available online 25 July 2017 22 °S to 22 °N in latitude and from 72 °E to 144 °E in longitude.
    [Show full text]
  • Results from the NASA Dawn Mission to Vesta and Ceres
    EPSC Abstracts Vol. 13, EPSC-DPS2019-5-1, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. The Geologic Mapping of Small Bodies: Results from the NASA Dawn Mission to Vesta and Ceres Williams, David A. and the Dawn Science Team School of Earth and Space Exploration, Arizona State University, Tempe, Arizona, USA, ([email protected]) Abstract 2. Ceres mapping & chronostratigraphy NASA’s Dawn mission was a Discovery-class robotic mission to send an orbiter to the two most massive The geologic mapping of Ceres was described in [5] objects in the Main Asteroid Belt, asteroid (4) Vesta and its chronostratigraphy is still being finalized at the and dwarf planet (1) Ceres [1]. Dawn orbited Vesta time of this writing. Ceres has a globally distributed from July 2011 to September 2012, and it remains in cratered terrain, with three large, ill-defined orbit of Ceres since it arrived in March 2015. As part topographic depressions that could be ancient basins. of the spacecraft’s nominal mission, the Dawn Science Kerwan crater (285 km diameter) is the largest Team requested geologic mapping campaigns of both identifiable impact crater, infilled and surrounded by Vesta and Ceres, which included global mapping a unique smooth material that marks this oldest crater. using High Altitude Mapping Orbit (HAMO) images In the southeastern hemisphere Yalode and Urvara (Vesta: 70 m/px; Ceres: 140 m/px) and quadrangle craters mark the next two youngest basins, with mapping using Low Altitude Mapping Orbit (LAMO) complex ejecta units. Intermediate and younger aged images (Vesta: 25/m/px; Ceres: 35 m/px).
    [Show full text]
  • New Animation Takes a Colorful Flight Over Ceres 29 January 2016
    New animation takes a colorful flight over Ceres 29 January 2016 "The simulated overflight shows the wide range of crater shapes that we have encountered on Ceres. The viewer can observe the sheer walls of the crater Occator, and also Dantu and Yalode, where the craters are a lot flatter," said Ralf Jaumann, a Dawn mission scientist at DLR. Dawn is the first mission to visit Ceres, the largest object in the main asteroid belt between Mars and Jupiter. After orbiting asteroid Vesta for 14 months in 2011 and 2012, Dawn arrived at Ceres in March 2015. The spacecraft is currently in its final and lowest mapping orbit, at about 240 miles (385 Occator Crater (57 miles, 92 kilometers) on Ceres, home kilometers) from the surface. of the brightest spots on the dwarf planet, in a simulated view using Dawn images. Credit: NASA/JPL- Caltech/UCLA/MPS/DLR/IDA Provided by NASA A colorful new animation shows a simulated flight over the surface of dwarf planet Ceres, based on images from NASA's Dawn spacecraft. The movie shows Ceres in enhanced color, which helps to highlight subtle differences in the appearance of surface materials. Scientists believe areas with shades of blue contain younger, fresher material, including flows, pits and cracks. The animated flight over Ceres emphasizes the most prominent craters, such as Occator, and the tall, conical mountain Ahuna Mons. Features on Ceres are named for earthly agricultural spirits, deities and festivals. The movie was produced by members of Dawn's framing camera team at the German Aerospace Center, DLR, using images from Dawn's high- altitude mapping orbit.
    [Show full text]
  • Ceres Subsurface Mineral Composition Detected by Spectral Analysis of Crater Central Peak Material (Ccp)
    49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083) 1523.pdf CERES SUBSURFACE MINERAL COMPOSITION DETECTED BY SPECTRAL ANALYSIS OF CRATER CENTRAL PEAK MATERIAL (CCP). A. Galiano1,2, E. Palomba1,3, A. Longobardo1, M. C. De Sanc- tis1, F. G. Carrozzo1, A. Raponi1, E. Ammannito4, F. Tosi1, C. A. Raymond5, C. T. Russell6 and the VIR team. 1IAPS-INAF Istituto di Astrofisica e Planetologia Spaziali, Rome, Italy ([email protected]), 2Università degli Studi di Roma Tor Vergata, Rome, Italy, 3ASDC-ASI, Rome, Italy, 4ASI-URS, Rome, Italy, 5Jet Propulsion Labora- tory, Californi Institute of Technology, Pasadena, CA, USA, 6University of California at Los Angles, Los Angeles, CA, USA. Introduction: The dwarf planet Ceres is the sec- Selection of ccp and parameters retrieved: A to- ond target of NASA Dawn mission since March 2015, tal of 32 craters with a clear peak arising from the floor which acquired images and hyperspectral data of its have been identified from the geologic maps of Ceres surface by using the Framing Camera (FC) and the [5] and the area of peak has been defined by selecting Visible and Infrared Mapping Spectrometer (VIR), the minimum and maximum value of both latitude and respectively. The Ceres surface is mainly composed of longitude. The selected area has been spectrally ana- a dark component, lowering the albedo, and Mg- lyzed by using VIR data at high resolution, i.e. data phyllosilicates, NH4-phyllosilicates and Mg/Ca- acquired during the HAMO and LAMO mission phas- carbonates, as inferred from the occurrence of absorp- es. For each ccp unit, the mean value of 2.7-, 3.1-, 3.4- tion bands located at 2.7, 3.1, 3.4 and 4.0 µm in VIR and 4.0-µm band depths, together with their respective reflectance spectra [1].
    [Show full text]
  • The Geometry and Possible Origin of Fractures in Floor-Fractured Craters on Ceres
    Lunar and Planetary Science XLVIII (2017) 1390.pdf THE GEOMETRY AND POSSIBLE ORIGIN OF FRACTURES IN FLOOR-FRACTURED CRATERS ON CERES. I. von der Gathen1, K. Krohn1, F. Schulzeck1, R. Jaumann1,2, D. L. Buczkowski3, J. E. C. Scully4, K. Stephan1, R. Wagner1, C. A. Raymond4, C. T. Russell5, 1German Aerospace Center, institute of Planetary Research, Berlin, Ger- many; 2Institute of Geological Sciences, Freie Universität Berlin, Berlin, Germany; 3Johns Hopkins University Ap- plied Physics Laboratory, Laurel, MD, USA; 4NASA JPL, California Institute of Technology, Pasadena, California, USA; 5University of California, Los Angeles, CA, USA. ([email protected]) Introduction: NASA’s spacecraft Dawn reached its target the dwarf planet Ceres in 2015 [1]. For our measurements we use a Low Altitude Mapping Orbit (LAMO) mosaic with a resolution of 35 m/px supplemented with a Digital Terrain Model (DTM) based on the High Altitude Mapping Orbit (HAMO) [2, 3] to investigate Ceres’ surface features. Images reveal a number of Floor-Fractured Craters (FFC) on Ceres’ surface. Fractures in these craters are linear and/or concentric. Occator e.g. exhibits both kinds of fractures that were likely formed by upwelling material [4, 5], while Kupalo on the other hand only shows concentric fractures, an indication for tear-off edges from slumps or cooling melting processes. Figure 1 Frequency vs. length of 1670 fractures within the In this work we present the parameters length and Floor-Fractured Craters on Ceres. Average length lies be- width of the linear features located on Ceres’ crater tween 1 and 3 km. floors in dependency of their frequency and distribu- tion.
    [Show full text]
  • Ceres: Astrobiological Target and Possible Ocean World
    ASTROBIOLOGY Volume 20 Number 2, 2020 Research Article ª Mary Ann Liebert, Inc. DOI: 10.1089/ast.2018.1999 Ceres: Astrobiological Target and Possible Ocean World Julie C. Castillo-Rogez,1 Marc Neveu,2,3 Jennifer E.C. Scully,1 Christopher H. House,4 Lynnae C. Quick,2 Alexis Bouquet,5 Kelly Miller,6 Michael Bland,7 Maria Cristina De Sanctis,8 Anton Ermakov,1 Amanda R. Hendrix,9 Thomas H. Prettyman,9 Carol A. Raymond,1 Christopher T. Russell,10 Brent E. Sherwood,11 and Edward Young10 Abstract Ceres, the most water-rich body in the inner solar system after Earth, has recently been recognized to have astrobiological importance. Chemical and physical measurements obtained by the Dawn mission enabled the quantification of key parameters, which helped to constrain the habitability of the inner solar system’s only dwarf planet. The surface chemistry and internal structure of Ceres testify to a protracted history of reactions between liquid water, rock, and likely organic compounds. We review the clues on chemical composition, temperature, and prospects for long-term occurrence of liquid and chemical gradients. Comparisons with giant planet satellites indicate similarities both from a chemical evolution standpoint and in the physical mechanisms driving Ceres’ internal evolution. Key Words: Ceres—Ocean world—Astrobiology—Dawn mission. Astro- biology 20, xxx–xxx. 1. Introduction these bodies, that is, their potential to produce and maintain an environment favorable to life. The purpose of this article arge water-rich bodies, such as the icy moons, are is to assess Ceres’ habitability potential along the same lines Lbelieved to have hosted deep oceans for at least part of and use observational constraints returned by the Dawn their histories and possibly until present (e.g., Consolmagno mission and theoretical considerations.
    [Show full text]