Mars Landing Site Catalog

Home , Ceraunius Fossae, Chasma Boreale, Claritas Fossae, Daedalia Planum, Mensa (geology), Nilosyrtis Mensae

NASA Reference Publication 1238

1990 Mars Landing Site Catalog

Ronald Greeley, Editor Arizona State University Tempe, Arizona

National Aeronautics and Space Administration Office of Management Scientific and Technical Information Division

PREFACE

This catalog was compiled from material provided by the planetary community for areas on Mars that are of potential interest for future exploration. The catalog has been edited for consistency insofar as practical. However, the proposed scientific objectives and characteristics for the sites have not been reviewed. It should be noted that this is a "working" catalog that is being revised, updated, and expanded continually.

Acknowledgments: My thanks to the following persons who helped in the preparation of this document: Katherine Price, Peggy Thomas, Susan Selkirk, Daniel Ball, Sherry-lynn Smith, Maureen Geringer, Loretta McKibben, Ricky Reynolds, Jim Rice, and Kevin Gorman.

R. Greeley 5 December 1989

iii

BRT..CEDLNG PAGE [tl_i P._LL._.INI[N' l|0N_kl BLANK NOT FILMED MARS SITE INDEX 31

WESTERN HEMISPHERE O EASTERN HEMISPHERE C) ;:o -o Table of Contents

°°, Preface ...... 111 iii Acknowledgments ......

Introduction ...... 1 1 Catalog Access ...... Rover/Sample Return Missions ...... 7 7 General Statement ...... Science Issues ...... 7 7 Science Objectives ...... 8 Rover Issues ...... Sampling Strategy and Validation ...... 9 Lander Issues ...... 12 14 Penetrator Missions ...... Science Criteria ...... 14 14 Sampling Objectives ...... Engineering Constraints ...... 14 Meteorological Considerations for Penetrator Sites ...... 14 Balloon Missions ...... 16 16 Initial Site ...... 16 Drift Mission ...... 16 Science ...... 17 Meteorological Stations ...... Landing Site Descriptions 001 Eridania NW ...... 18 002 Parana Valles ...... 20 003 Eridania ...... 22 004 Eridania SE ...... 24 005 Iapygia ...... 26 006 Noachis ...... 28 007 Terra Cimmeria ...... 30 008 Mare Tyrrhenum ...... 32 009 Sinus Sabaeus ...... 34 010 Terra Tyrrhena ...... 36 011 Phaethontis SW ...... 38 012 Samara Valles ...... 40 SITES 013 - 017 HAVE BEEN DELETED ...... 42 018 Alba Patera ...... 43 46 019 Northern Elysium ...... 49 020 Argyre Ph'mitia ...... 51 021 Maja Valles ...... 54 022 Candor Mensa ...... 023 Memnonia ...... 58 024 Mouth of MajaValles ...... 61 025 Maja Valles Canyon Flood Plain ...... 64 026 Upper Maja ...... 66 027 UpperMangalaValles...... 68 028 OlympusMons Southeast...... 71 029 WesternDaedaliaPlanum...... 81 030 North PolarCap...... 87 031 North Pole ...... 88 032 HadriacaPatera...... 89 033 ChasmaBoreale...... 91 034 PlanumAustrale...... 92 035 MemnoniaSulci ...... 94 036 OlympusRupes(Southeast)...... 96 037 KaseiValles...... 98 038 MangalaVallesWest ...... 100 039 MangalaVallesEast...... 102 040 Elysium Mons ...... 104 041 Apollinaris Patera...... 106 042 Nilosyrtis Mensae...... 108 043 CandorChasmaI ...... 110 044 Tharsis-Olympus...... 112 045 ChasmaBoreale...... 114 046 LabeatisNorth ...... 116 047 LabeatisSouth...... 118 048 Solis...... 120 049 Hadriaca...... 122 050 Elysium...... 124 051 MareotisVolcanic Field ...... 126 052 TempeVolcano ...... 128 053 CerauniusFossaeVolcanic Field ...... 130 054 Candor...... 132 055 NorthernCydonia/SEAcidalia...... 134 056 Tharsis-Olympus...... 136 057 Labeatis...... 138 058 ChrysePlanitia/Viking 1...... 140 059 Amenthes Southeast ...... 143 060 Isidis North ...... 145 061 Arabia ...... 147 062 Hadriaca ...... 149 063 Arabia South ...... 151 064 Isidis Planitia ...... 153 065 Utopia ...... 155 066 Elysium Southwest ...... 157 067 Elysium South ...... 159 068 Medusae Fossae ...... 161 069 Olympus South ...... 163 070 Alba West ...... 165 071 Kasei South ...... 167 072 Candor Chasma II ...... 169 073 Lunae Planum East ...... 171

vi 173 074 CapriChasma...... 175 075 Meridiani Southwest...... 177 076 Tempe...... 179 077 Ares .°oH°°._Io.o.I°°°°H.°°,oo°o o,o°o,.°°°o°°,°°o°,,°, o,,,°° °°,.°°°,oo°°oo°°.°oo°*°°°°_-,,°.°,°°°'''o°°°°°*'°° °'°°'''" °*''° 181 078 Tempe Fossae ...... 079 Aeolis Southeast ...... 183 186 O8ODao Vallis ...... 189 081 Acidalia Planitia ...... 191 082 Arcadia Planitia ...... 193 083 Utopia Planitia ......

vii

Introduction

The late 1980s saw a renewed interest in missions 3-1/2" diskettes in PageMaker 3.01 format, Apple to Mars. Studies have been made and are underway Macintosh version. The disk version of the catalog by various United States, Soviet, and European includes scanned copies of all maps and photo- committees to recommend missions ranging from graphs. relatively simple unmanned probes to exploration programs involving humans presence on Mars. A Hard copy or information on diskette versions of key part of most of these programs includes selection the catalog can be obtained from: of sites on Mars for vfirious purposes, including selection of sampling area for detailed analysis either in situ or for return to Earth. Ronald Greeley Department of Geology This catalog is established to provide ready access Arizona State University to information on potential landing sites. It is Tempe, AZ 85287-1404 structured to allow expansion of the data base (both in number of sites, and in information on each site) SPAN address: ASUIPF::GREELEY and to be readily accessible either electronically or via hard copy; input to the catalog is also welcomed. NASAMAIL address: RGREELEY

Catalog Access Input to the catalog should be made by completing As well as being available in printed form, the most the form on the following page. Comments on sites recent version of the catalog may be purchased on in the catalog are also welcomed and will be added. POTENTIAL MARS LANDING SITE

Name Phone Address

Type of landing site: ['-]Rover [-'i Sample return [-']Penetrator ["]Balloon _'] Other (specify)

1. Name of area Location °laL__°long. Map sheet (MTM#) • Elevation km Viking Orbiter images

2. Scientific rationale for site

3. Specific science objectives (list by priority):

Probability of Success Objectives in Meeting Objective a.

4. Targets (keyed to above). Identify by lat. and long. and/or on sketch map. Include xerox of images with frame numbers.

5. Potential problems, mission/spacecraft constraints.

. Estimated trafficability for roving vehicle (Scale 1-5, 1= smooth plain, 5 = fresh lava surface)

7. Estimatedtraversedistance(round-trip) km

8. Other(backof page,additionalsheets;photos,maps,etc.)

Send to: Ronald Greeley, Dept. of Geology, Arizona State University,Tempe, AZ 85287-1404 / Table. Landing site parameters (keyed to index map and catalog site number ).

No. Name Type Contributor Quadrangle Elevation Latitude (') Long. ('W) Geology

1 Eridania NW MRSR S. Squyres MC-29 NW 3.0 to 4.0 36.00 S 228.00 Ancient cratered highlands. 2 Parana Valles MRSR S. Squyres MC-19 SE 1.0 22.00 S 12.00 Old voicanics and channel deposits. 3 Eridania MRSR S. Squyres MC-29 SE, SW 4.0 58.00 S 212.00 Old volcanic plains. 4 Eridania SE MRSR S. Squyres MC-29 SE 5.0 57.00 S 195.00 Inter. age volcanic plains. MC-21 NE 5.0 9.00 S 279.00 Inter. age to old volcanic plains. 5 Iapygia MRSR S. Squyres 6 Noachis MRSR S. Squyres MC-27 SW 5.0 55.00 S 337.00 Inter. age to old volcanic plains. 7 Terra Cimmeria MRSR S. Squyres MC-29 NC 5.0 42.00 S 211.00 lntex, age to old volcanic plains. 8 Mare Tyrrhenum MRSR S. Squyres MC-22 SE 3.0 to 4.0 23.00 S 231.00 Old volcanic plains. 10 Terra Tyrrhena MRSR S. Squyres MC-22 SW 3.0 25.00 S 266.00 Inter. age to old volcanic plains. 11 Phaethontis SW MRSR S. Squyres MC-24 SW 5.5 51.00 S 153.00 Inter. age to old volcanic plains. 12 Samara Valles MRSR S. Squyres MC-19 SE, SW 2.0 23.00 S 21.00 Old volcanic plains and channel deposits. 13 MRSR S. Squyres 14 MRSR S. Squyres 15 MRSR S. Squyres 16 MRSR S. Squyres 17 MRSR S. Squyres 18 Alba Patera MRSR D. Schneeberger MC-2 SE 3.0 47.00 N 116.00 Young volcanics. Young volcanics and channel deposits. 19 Northern Elysium MRSR P. Mouginis-Mark MC-7 SC 0.0 33.00 N 212.00 Ancient crust and layeredplains deposits. 20 Argyre Planilia MRSR T. Parker MC-26 SW 1.0 55.00 S 42.00 MC-10 NE -0.5 18.95 N 53.50 Ancient crust, channel, and lacustrine. 21 Maja Valles MRSR J. Rice 22 Candor Mensa MRSR B. Lucchitta MC- 18 NW 1.0 5.50 S 74.50 Young volcanics and sedimentary deposits. 23 Memnonia MRSR D. Scou MC-16 NW 1.0 11.00 S 173.00 Voicanics and channeldeposits. Channel deposits. 24 Mouth of Maja Valles MRSR R. DeHon MC- 10 NE -0.5 17.90 N 53.80 Channel and lacustrine deposits. 25 Maja VallesCanyon MRSR R. DeHon MC-10 NE -0.5 17.65 N 54.25 Intermediate-age volcanics and lacustrine 26 Upper Maja MRSR R. DeHon MC-10 NE 0.5 18.20 N 57.00 deposits. MC-16 NE 3.0 13.80 S 148.10 Channel deposits. 27 Up. Mangala Valles MRSR J. Zimbeiman MC-9 SW 2.8 14.00 N 131.00 Young-to-intermediate-age volcanics. 28 Olympus Mons SE MRSR R. Greeley Ancient crust and young-to-intermediate- 29 W Daedalia Planum MRSR R. Greeley MC-16 SE 3.0 19.00 S 144.00 age volcanics. Polar-layered deposits. 30 North Polar Cap MRSR C. Leovy MC-IA, B 1.0 80-85 N -- 31 North Pole MRSR C. Leovy MC- IA, B 1.0 90.00 N m Polar-layered deposits. 32 Hadriaca Patera MRSR F. West MC-28 NE 1.5 32.50 S 266.00 Young-to-intermediate-age voicanics and channel deposits. 33 Chasma Boreale MRSR H. Masursky MC-IA, B -0.5 80.80 N 44.00 Polar-layered deposits. H. Masursky MC-30A,B 4.0 82.50 S 60.00 Polar-layered deposits. k34 Planum Australe MRSR J Table. Landing site parameters (keyed to index map and catalog site number ).

No. Name Type Contributor Quadrangle Elevation Latitude (') Long. ('W) Geology

35 Memnonia Sulci MRSR H. Masursky MC -16 NW 2.0 9.70 S 174.20 Young volcanics. 36 Olympus Rupes SE MRSR H. Masursky MC-9 SW 2.0 13.80 N 131.20 Young volcanics. 37 Kasei Valles MRSR H. Masttrsky MC-10 SW, NW 1.0 15.10 N 75.80 Young-to-intermediate-age volcanics and channeldeposits. 38 Mangala Vailes West MRSR H. Mnsursky MC-16 NW 1.0 7.20 S 158.60 Young-to-intermediate-age volcanics and channel deposits. 39 Maagala Valles East MRSR H. Masmsky MC-16 NE 2.5 4.70 S " 147.50 Young-to-intermediate-age volcamcs and channel deposits. 40 Elysium Mons MRSR H. Masursky MC-15 NW 4.0 24.30 N 214.80 Young volcanic plains. 41 Apollinaris Patent MRSR H. Mnsursky MC-23 NE 1.0 7.50 S 187.20 Young-to-intermediate-age volcanics. 42 NilosyrtLs Mensae MRSR H. Mnsursky MC-5 SE 2.5 35.50 N 302.50 Intermediate-age volcanics and ancient cratereduplands. 43 Candor Chnsma MRSR H. Masursky MC-18 NW 2.5 10.50 S 74.50 Young voicanis and sedimentary deposits. 44 Tharsis-Olympns MRSR D. Scott/I(. Tanaka MC-9 SW 4.0 12.00 N 125.00 Young volcanic plains and aureole deposits. 45 Chasma BoriSe MRSR D. Scott/K. Tanaka MC-I A, B 0.0 82.00 N 57.00 Polar layered deposits and grooved plains. 46 Labeafis North MRSR D. Scott/K. Tanaka MC-3 SE 2.5 31.00 N 83.(30 InUmnediate-age volcanic plains. 47 _lis South MRSR D. Scott/I(. Tanaka MC-10 NW 2.0 24.00 N 80.00 Intermediate-age volcanicplains. 48 SoiLs MRSR D. Scott/K. Tanaka MC-17 SE 9.0 27.00 S 100.00 Ancientcrust,intermediate-age volcunics. 49 Hadriaca MRSR D. Scott/K. Tanaka MC-28 NE; MC-22 SW 1.0 29.00 S 269.00 Intermediate-age volcanicplains and ancient crust. 50 Elysium MRSR D. Scott/K. Tanaka MC- 15 NE .0.5 27.00 N 185.00 Young-to-intermediate-age volcanic plains. 51 Mareotis Volcanic MRSR H. Moore MC-3 SE 3.0 36.00 N 88.00 Old-intermediate-age volcanics. 52 Tempe Volcano MRSR H. Moore MC-3 SE 1.8 39.00 N 76.00 Intermediate-age volcanics. 53 Ceraunins Fossae MRSR H. Moore MC-9 NE 5.0 20.00 N 112.00 Young-to-intermediate-age volcanics. 54 Candor MRSR E. Robbins MC-18 NW 2.0 5.50 S 74.50 Sedimentary deposits. 55 No. Cydonia MRSR P. Etzler MC-4 SE -0.5 40.00 N 10.00 Erosional remnants of plateaus on highland- lowland boundary scarp. 56 ThatsLs-Olymlms MRSR D. Scott MC-9 SW 3.5 12.50 N 125.50 Young voicanics. 57 _s MRSR D. Scott MC- 10 NW 2.5 25.00 N 82.00 Intermediate-age volcanic plains. 58 Chyrse Planitia MRSR R. Craddock MC-10 NE -2.2 22.52 N 47.97 Intexmediate-age volcanic plains. 59 Amenthes SE Penettator US/Soviet Group MC-14 SE, SW 1.0 to 2.0 4.00 N 247.00 Ancient highlands. 60 Isidis North Balloon US/Soviet Group MC-6 SE, SW; -1.0 to 2.0 16-36 N 267-282 Intermediate-age voicanics, eolian deposits. 13NE; 14NW 61 Arabia Penetrator US/Soviet Group MC-5 SC; 12NE 1.0 to 2.0 30.00 N 327.00 Old volcanics. 62 l-ladriaca Penetrator US/Soviet Group MC-28 NE, NW 0.0 to 1.0 36.00 S 271.00 Intermediate volcanics. Table. Landing site parameters (keyed to index map and catalog site number ).

No. Name Type Contributor Quadrangle Elevation Latitude (') Long. ('W) Geology

63 Arabia South Penetrator US/Soviet Group MC-12 SE, NE 1.0 to 2.0 15.00 N 333.00 Ancient highlands. 64 Isidis Planitia Penetrator US/Soviet Group MC-13 SE -3.0 to -2.0 10.00 N 275.00 Intermediate-age volcanics. 65 Utopia Penearator US/Soviet Group MC-6 SE -3.0 to -2.0 45.00 N 251.00 Channel deposits and ground ice. 66 Elysium SW Penetrator US/Soviet Group MC-15 NW; 14NE -1.0 to 0.0 17.00 N 224.00 Intermediate-age volcanics. Channel deposits and young voicanics. 67 Elysium South Balloon US/SovietGroup MC-14 SE; 15SW; -1.0 to 2.0 4 S-7 N 205-32 22NE; 23NW 68 Medusae Fossae PenewaXor US/Soviet Group MC-16 NE, NW 1.0 to 2.0 2.00 S 159.00 Young volcanic plains. Young volcanic plains. 69 Olympus South Penetrator US/Soviet Group MC-8 SE; 9SW 1.0 to 2.0 11.00 N 137.00 70 Alba West Penetrator US/Soviet Group MC-2 SE 1.3 45.00 N 126.00 Intermediate-age voicanics. 71 Kasei South Peneuator US/soviet Group MC-10 SW 0.0 to 1.0 10.00 N 80.00 Young voicanics. 72 Candor Chasma Penetrator US/soviet Group MC-18 NW -1.0 to 0.0 6.00 S 73.00 Sedimentary deposits. Intermediate-age volcanics. 73 Lunae Pianum East Penetrator US/soviet Group MC-10 NE, SE 1.0 to 2.0 16.00 N 63.00 Sedimentary deposits. 74 Capri Chasma Penetrator US/Soviet Group MC- 18 NE, SE; -2.0 to - 1.0 14.00 S 46.00 MC-19 NW, SE 75 Meridiani SW Penetrator US/Soviet Group MC-19 NE 1.0 to 2.0 12.00 S 7.00 Ancient highlands. 76 Tempe Balloon US/Soviet Group MC-4 SW; 10NE 0.0 to 1.0 25-52 N 30-60 Ancient plateau and channel deposits. 77 Ares Balloon US/Soviet Group MC-11 SE,SW; -1.0 to 1.0 13 S-10 N 0-25 Ancient highlands and channel deposits. 19 NE, NW Ancient fractured terrain. 78 Tempe Fossae MRSR C. Madras MC-3 SE 2.0 40.00 N 76.50 79 Aeolis SE MRSR N. Cabrol MC-23 SE 0.0 15.50 S 188.50 Ancient cratered highlands. 80 Dao Vallis Balloon F. West MC-28 HE 1.5 30.00 S 262.00 Intermediate-age volcanic and sedimentary deposits. 81 Acidalia Planitia Balloon J. Runavot MC-4 NE, NW, -3.0 to -1.0 40--60 N 10-40 Northern lowland plains. SC, SE 82 Arcadia Planitia Balloon J. Runavot MC-2 NW, SW, SC -3.0 40-60 N 150-180 Northern lowland plains. Northern lowland plains. 83 Utopia Planitia Balloon J. Rmmvot MC-6 NE, SE; -3.0 to -1.0 40-60 N 240-270 7 SW

Rover/Sample-Return Missions

General Statement Premise 5: Candidate sites will be selected initially This document outlines the criteria for selecting using science criteria. Engineering criteria such as landing sites on Mars. It is derived from the MRSR accessibility, trafficability, and landability will be work group subcommittee, chaired by M. Drake. used as disciminants among science sites of Because of the lack of detail concerning the comparable interest. mission(s), it is necessary to state certain premises upon which the criteria are based. Premises in- Science Objectives clude science, lander, and rover issues. The criteria are written in general terms. The criteria will It is important to know the timing and nature of evolve and become more specific as the mission(s) major events on Mars, such as atmospheric becomes better described. Should any of the prem- outgassing, core formation, crust formation, ises prove to be incorrect, the criteria may require erosional episodes, depositional episodes, and reconsideration. organic formation. Such knowledge is critical to a comprehensive understanding of the origin and Science Issues evolution of Mars as a planet and as a possible host for life forms. This chronological and systemic Science Premises knowledge can be gained from an efficient sampling program. Premise 1: There will be a minimumoftwo sample return missions as part of a Mars program. The Studies which will characterize the major geologic second mission will be a backup for a possible units in terms of age, composition, morphology, failure of the first mission. and origin may be grouped into three categories, each of valid scientific importance. Premise 2: At some point the mission will be defined. At present there are several unknowns. It Planetary igneous differentiation and crust is not known whether there will be one or two formation. Samples should include landers per mission, nor are the capabilities of the unweathered volcanic rocks from the maj or landers or the rovers known. These uncertainties terrains (ancient cratered plains, northern may affect site selection criteria when resolved. It resurfaced plains, Tharsis plateau) and is assumed that the mission will meet the science unweatheredplutonic rocks from the ancient objectives as defined in subsequent site selection cratered uplands for determination of criteria (see section 3.2.2). radiometric ages, chemical compositions, and mineralogy. Premise 3: Landing site selection criteria will evolve. Apollo experience on the Moon shows that Effects of water and other volatiles on as scientific and engineering data are obtained, the surface chemistry and morphology, and on mission goals become more ambitious. climate. Samples should include sediments of fluvial, aeolian, or lacustrine origin and Premise 4: Preferable candidate landing sites igneous rock altered by weathering. In selection will occur after Mars Observer (MO) data addition, ground ice and atmospheric gases are available. MO data will enhance the ability to should be sampled. Samples should be determine if a site meets science and engineering taken from regions where accompanying criteria. units provide radiometric age control,

PRECEDING PAGE BLANK NOT FILMED either through stratigraphically interleaved Rover Issues volcanic rocks or through crater-count ages calibrated by radiometric information. The ability to reconcile the conflicting requirements for site safety, acquisition of variety of sample Conditions for and evidence of develop- types, and acquisition of samples of known ment of life. Samples should include sedi- provenance depends to a major degree on rover ments from sites suspected of harboring mobility. Mobility permits acquisition of rocks water and organic material considered even when the landing is on unconsolidated debris; conducive to the development of life and it permits travel from safe, bland, landing sites to likely to have preserved organic chemicals. sites of geologic interest; and it permits movement These materials should come from sites from one geologic unit to another in order to whose ages and sedimentary nature is acquire samples, thereby insuring a variety of understood from sample categories 1 and 2 samples of known provenance. The value of above. mobility is difficult to quantify but the following table indicates qualitatively how range and 'risk' Criteria Derived From Scientific of failure to meet sample objectives are related. Considerations RELATION BETWEEN ROVER RANGE From the preceding scientific objectives the AND SCIENCE RISK following statements are derived for priority in Radial range Science Risk landing site selection: from No Only 1 Landing Point Rock rock type Sites should provide samples of unambiguous provenance(s) and ensure 0.001 km high high 0.I km moderate high sampling of major geologic units. Landing 1 km low high site complexity does not necessarily equate 10 km low moderate to ambiguous provenance. 100 km low low

Sites collectively should address the maximum number of scientific questions. The risk assessment of acquiring no fresh rocks is Individual sites should address areasonable based mainly on Viking experience. The two subset of scientific questions (a trade-off is Viking sites are known from thermal inertia data to recognized between developing an be more rocky than most of Mars. Yet only a few small rocks were within reach of the landers, and extremely capable--and expensive--rover and increasing the number of landing sites). all attempts to pick up and analyze small rocks failed. The 'rocks' analyzed turned out to be clods The ideal site would provide ready access to the of unconsolidated debris, not true rocks. Thus, at following: a typical Mars site there is a high probability that no rocks are within reach of a sampling arm on a 1. Young Igneous Rocks lander. In addition, drifts of poorly consolidated 2. Intermediate Age Igneous Rocks material, several meters across, occur throughout 3. Old Igneous Rocks the Viking 1 site. Again, because the VL-1 site is 4. Water-laid Sediments atypically blocky, we can expect such drifts to be 5. Old Impact Breccias more extensive at other, more typical sites, and 6. Ground Ice mobility of a few to tens of meters may be required 7. Soils - upper level of weathered to acquire rock samples. This problem could be rock profile exacerbated if the lander had some terminal

, "Loess" - windblown dust guidance system to avoid blocks. Therefore, with

8 mobility of 100m thereis still moderatechance the Viking landing sites are probably more blocky that no rocks will be accessible.(Theenormous than most of Mars. Insofar as blocks impede difference betweenMars and the Moon in this movement, therefore, more mobility should be respectneedsre-emphasis.Theloosedebrisonthe possible at a typical site than is suggested by the Moon is composedlargely of rock fragments characteristics of the Viking sites. Movement over comminutedbyimpacts.Mostoftherockfragments extreme terrain (such as talus slopes), fresh lava arechemicallyandmineralogicallyunaltered,and flows (such as aa), and lee slopes of dunes are not so are representativeof the geologic unit from required for science purposes. whichtheyoriginated. Theloosematerialon the Moon wasthereforevery usefulin reconstructing Rover Trafficability Premises theMoon'sgeologichistory.Marsisverydifferent. Premise 1: There will be some sort of rover. Theloosematerialonthemartiansurfaceisalmost certainlyhighly weathered,andsoprovideslittle Criteria Derived From Rover Trafficability information on the chemistryandmineralogyof Considerations primary rocks. The loosematerialis alsofine- grainedanddepositedbythewindsoit will tendto There are three identifiable classes of trafficability hazards: discrete, statistical, and time variable. buryanycoarser,unweatheredimpactdebristhrown into thesite. In addition,no rockfragmentswere Some hazards may fit into more than one class, and presentin fine-grainedandcloddymaterialat the are listed in the class in which they are most likely Viking landersites,basedontheircohesionduring to be detected prior to landing. surfacesampling.Theloosematerialatthemartian surfaceisthusof limitedusefulnessin reconsmactingDiscrete: Includes hazardseparation (e.g., blocks) thegeologichistoryof theplanet). n x turning circle (n>2); and long linear obstacles, such as fractures which would require longer rover Mobility is alsoneededto ensurethat more than range. one rock type is sampledat a given site. The mobility requiredto do thisis difficult toquantify. Statistical: Site does not exceed critical frequency Uncertaintiesin thelocationofgeologicboundaries of untrafficable slopes (critical frequency = ?), are typically a few kilometers. Lava flows are (untrafficable slopes =?); site is smooth at critical typicallyseveralto afewtensof kilometersacross. scale (scale 1/slope), (1 m on horizontal surface), Forsafetyreasons,thelandingellipsewill probably and avoid sites with low beating strength. be placed entirely within one geologic unit, characterizedas'safe'. Unlessthereis landmark Time Variable: Avoid sites of known dust storm tracking,theellipsewill likelybeseveralkilometers generation and avoid sites with temperatures which across,so a severalkilometer traversemay be impair mission operations. For example, if one requiredto gofrom the'safe' landingsitetoamore objective is to use remote sensing instruments to scientificallyinterestingsite.Thus,differentfactors select non-ice samples, then the landing site should suggestthatmovementof severalkilometersfrom not be near polar caps where frost deposition will thelandingpointwill berequiredtoensurethattwo likely occur. geologicunits can be sampled Travel of several tensof kilometersappearsrequiredfor a safesite Sampling Strategy and Validation and in order to samplea diversesetof geologic units andmaterials. Choice of where to sample and what to retain will be made on the basis of the remote sensing Inordertomovetensof kilometers the rover should instruments on-board the rover, the remote sensing have the capability of moving relatively rapidly in instruments on the orbiter, previously acquired bland, hazard-free areas. As previously indicated, remote sensing data, and on analytical data from

9 theroverinstruments.Foracquisitionof mostrock theneedfor complexsamplehandlingcapabilities samples,thespectralandopticalinstrumentswill involving temporary storageon the rover and provide the information on which the choiceis temporarystorageatthelander,suchthatsamples made. Every effort shouldbe madeto acquire areheldpendingdecisionstoberetainedorrejected. samples representative of the spectral and An implication is that the rover should,on any morphologicalvarietythat areaccessible.In some traverse,carryexcesssamplingholdingcapability infrequent cases,acquisition of information in in the eventsomeextraordinaryfind occurs(the addition to remote sensingdata may be needed proverbialdinosaurbone). A possiblealternative beforeadecisionismadeto acquireasample.For tothispolicyisthattherovercarrymultiplemodules thesecases,it is desirableto havethecapabilityof that fit into the samplecannisteron the Ascent placing the Alpha Proton X-ray Spectrometer Vehicle,andadecisioncouldbemadenotto load (APXS)againsttherocksto besampled.While it someof themodulesfor returnto Earth. would be ideal to get APXS dataon all samples acquired,this is thought to be unwise,because After eachrovertraverse,approximatelyonethird increased complexity and increased time of of theremainingspacein theSampleCannisteron operationsin sampleacquisition reducesrover the AscentVehicle will be filled. Sampleswill mobility,therebydecreasingthechancesofreaching neverberemovedfrom theAscentVehicle. The differentgeologicunits,andacquiringavariegated purposeof thispolicyistwofold. Thefirst is tonot sampleset. risk damagingthesamplecannisteron theascent vehicle by repeatedly inserting and removing Trenchingorcoringoftheunconsolidatedmaterials samples.The secondis to ensurethat theascent will bedoneat only afew locationschosenon the vehiclealwayshassampleson-boardin theevent basis of remote sensing information, neutron of forcedearlydeparture. spectrometerdata, and Differential Scanning CalorimetercoupledwithanEvolvedGasAnalyzer A photographicrecord should be made of the (DSC/EGA) analysesof materialat the surface. geologicsettingof all samples,both beforeand Thedecisionto takeandretainsamplesfrom depth aftersampleacquisition,andthelocationsof all in will be basedlargely on the resultsof theDSC! situ analyses. Spectral data should also be acquired EGA analyses.Theseanalyseswill bemadeprior on all samples. toacquisitionof samplesforretentionandreturnto Earth. No analysesneedbe performedon the Samples collected separately should be separately samplesacquiredfor Earthreturn. Analysesof packaged and labelled. nearbysampleswill providesufficientinformation onwhetheror notto retainsamples.Thispolicy is Remote Sensing on Rover invoked to impose simplicity on the sample Remote sensing has two functions. The first is to acquisitionprocess. It implies that "splits" need notbemadeonacquiredsamples,with partsbeing aid in navigation of the rover. The second is to aid in sample acquisition and characterization of the analyzed,and parts being retainedpending the resultsof theanalyses. landing site by identifying chemical and mineralogical differences of materials within view OnceasamplehasbeenacquiredforreturntoEarth of the sampling vehicle, and by characterizing andloadedinto the samplestoragedeviceon the physical processes that might affect the samples. rover,it will beretained,ultimatelyto beloadedon the Ascent Vehicle for Earth return. In other Stereo Imaging with Resolution of about 10 cm at 100 m; 0.1 cm at lm words,thedecisionto acquirea samplefor Earth return is made at the samplesite, not at some (These resolutions are approximate and provided subsequenttime.Thispolicyisintendedtoeliminate as an indication of what might be necessary). The

10 cameraneedstobemountedatleastTBD m above resolution views of nearby materials, ff the cam- the groundfor navigationpurposesand for far- eras have multispectral capabilities then the utility field viewing. This scientificrequirementarises of this capability is greatly enhanced. The objec- from the need to interpret local geology and tive is to characterize accessible materials at the recognizesamplingandscienceopportunities. scale of mineral grains (equivalent to a geologist using a hand lens in the field to identify rocks and Multi-spectraol Sensing Capability with minerals). Wavelength Range of O.3 to 25 microns Analytical Instruments on the Rover Spatial and spectral resolution, number of wavelength channels, and whether an imaging The purpose of the analytical instruments is two- fold. The first is to directly support sample selection. spectrometer or a point spectrometer are required are all TBD. Because only a limited mass of material can be returned to Earth, some capability for discriminati ng

This requirement can be accomplished in different between different types of samples is needed in order to ensure that a variegated sample set is ways as follows roughly in decreasing order of desirability. However, how spatial resolution, collected. With analytical capability on the rover, spectral resolution and imaging capability are traded intelligent choices can be made as to where to go to against each other remains TBD. sample, what to sample, and what to retain in order to maximize variety in the returned set. The second Spectral capability with 100+ channels on one of purpose of analytical instruments is to do in situ the stereo cameras indicated above, coupled with science. A number of measurements, such as those the capability of changing the number of channels sensitive to local conditions, can be made only on as desired (multi-spectral imaging). Mars. In addition, first order interpretations can be made concerning the types of materials avail able at Addition of about 10 spectral channels to one of the the landing site, and the general geologic context, stereo cameras indicated above, coupled with a while the mission is in progress. These point spectrometer with spatial resolution TBD, interpretations could influence the subsequent but comparable to the camera resolution, and with course of the mission, affecting traverse planning, spectral resolution of at least 20 nm (multi-band sampling strategy and so forth. The following imaging plus spectrometer). capabilities are desired to support sample selection and to establish the geologic context in which the No spectral capability on the stereo cameras but mission is conducted. Each analytical procedure independent point spectrometer with spatial resolution comparable to the camera and spectral will have requirements on sample size, sample resolution of at least 20 nm (monochrome imaging preparation, and sample manipulation. Until plus spectrometer). The multispectral capability is specific instruments are selected, the particular needed to identify mineralogic and chemical sampling and preparation requirements remain variations in the surrounding materials, and to TBD. make tentative identification of the case of the General Elemental Analysis variations, primarily in order to support rover traverse planning and sampling strategy. As General elemental analysis with the following previou sly indicated, the decision to acquire samples will be based largely on the spectral data. capability:

High Resolution (0.005 cm) Imaging (1) major elements with a sensitivity of The intent here is to utilize the on-board cameras, 0.1 atom percent and an accuracy of by addition of appropriate optics, to provide high about 3 atom percent,

11 (2) primordialradionuclidesto a sensitiv- The DSC should be capable of measuring solid- ity of TBD, state transitions characteristic of volatile-bearing minerals including major groups of clay minerals, (3) selectedminor andtraceelements hydrous salts, and carbonates, and including (e.g.C, N, F, P, S, C1,Ti) to TBD occurrence of those phases as minor (1-10% sensitivity. abundance) components of bulk samples. The EGA should be able to perform as an independent Thepreferredinstrumentisthealphaproton,X-ray analyzer of the atmosphere or as analyzer of the spectrometer(APXS) because,of the analytical DSC gaseous effluent, with the ability to reliably instruments currently available, it will suffer identify and measure at least molecular water, minimuminterferencefromtheeffectsof theradio- carbon dioxide, carbon monoxide, nitrogen, oxygen, thermal generator. In addition to being able to sulfur dioxide, nitrogen (II and IV) oxides, and analyze acquired and prepared samples,it is organics. desirablethatit can bemanipulatedsoasto place it againstmaterial,such asa rock face, that are The purpose of this instrument is to determine low difficult to sample. temperature mineralogy and the composition of volatile components, including organics. Results Onepurposeof havingan analyticalcapabilityon from the instrument, in conjunction with spectral therover is to chemicallycharacterizeaccessible data, will be used to decide where best to sample for materials as an aid in sample selection. As volatile rich materials. The results are particularly previouslyindicated,thisdoesnot imply that all applicable to sampling the unconsolidated materials samplesacquiredneedto be analyzed,or that at and water-lain sediments. The instrument will also samplesitesnumerousanalysesbe madeof local be used to make measurements on Mars of charac- materialsinordertodecidewhatshouldbesamples. teristics that are unlikely to be preserved, or diffi- Manyof thedecisionsonsampleacquisitioncanbe cult to preserve in returned samples. madeonthebasisofdatafrom spectralinstruments, coupled with a generalknowledgeof how the Other Possibilities spectraldataarerelatedto APXS data. A second function of the on-board chemical analysis Other possibilities include some device for capability is to aid in interpretationof the local measuring hard-rock mineralogy (X-ray geology and thereby supportplanning of rover diffractometer), a stable isotope laser spectrometer operations.Theon-boardanalyticalcapabilitywill (SILS), and some way of measuring the Eh and pH alsohelpcalibratetheremotespectralobservations. of the soil.

Neutron Spectrometer Premise 1: Rover design is predicated on current knowledge of the martian surface. Neutron Spectrometer to distinguish between thermal, epithermal and fast neutrons. The main Premise 2: Rover will have the capability of purpose of this instrument is to determine the H traversing terrains subject to engineering criteria to content and hence the I-I20 content in the materials be developed. within 1 meter of the surface. The instrument will give an indication as to where subsurface sampling Lander Issues might unearth materials more water rich than typical. Landability Premises

Differential Scanning Calorimeter Coupled with Premise 1: Landing sites will be selected based on an Evolved-Gas Analyzer (DSC-EGA) landability and trafficability criteria.

12 Premise 2: Lander design is predicated on current of one successful landing in one attempt is 0.984, for two successful landings in two attempts is 0.97, knowledge of Mars. and for one successful landing in two attempts is Premise 3: A safe landing site means that a lander 0.9997. can touch-down intact, a rover can be deployed, and an ascent vehicle can be launched. Landing Site Criteria Derived From LandingSafety Considerations Premise 4: Landability criteria must be practical, i.e, data must be available to evaluate candidate There are three identifiable classes of landability sites. hazards: discrete, statistical, and time variable. Some hazards may fit into more than one class, and Premise 5: Criteria should permit probability of are listed in the class in which they are most likely safe landing superior to Viking post-mission to be detected prior to landing. Dimensions of the estimates. hazards remain TBD.

Discussion: There is an interaction between landing Discrete: Linear features such as crevasses or site selection criteria and the approach taken to ridges; high mountains along ground track; and lander design to reduce landing hazard. Options maximum landing site altitude. include a robust lander, precision landing, and active hazard detection and avoidance. Each has Statistical: Big rock; steep slopes; and beating implications for the level of information required strength/coefficient of friction must be sufficient to about specific landing sites. For example, if a support lander. lander is built to survive blocky hazards with a zone of influence of 1 m and to survive slopes of up to Time Variable: Avoid sites of known dust storm 14 °, Viking Lander data suggest that the probability generation_

13 PENETRATOR MISSIONS

The following science criteria, sampling objec- 10% below the seasonal mean (equivalent to about tives, and engineering constraints were defined at 1 km). the 25 July 1989 meeting of the joint United S tates/Soviet Landing Site Working Group, held in Wind drift may be a consideration for penetrator Flagstaff, Arizona. entry. Winds are currently very poorly known in general, but may be expected to be much better Science Criteria understood before the mission with the aid of Mars Observer data and improved models. However, • Uniform geology some general statements can be made. Regions of • Potential future sites for lander low regional slope in the northern hemisphere mid- • Inaccessibility by other means latitudes should be relatively safe at this season • Seismic spacing from the point of view of winds. We have specific • Meteorologic spacing evidence of very light winds in the lowest scale • Highest possible latitude height at the Viking lander 2 site in Utopia Planitia. Stronger winds are likely in regions of high regional Sampling Objectives slope in low latitudes. There is evidence of moderately strong slope winds above the boundary • Recent volcanics layer at Viking lander 1 (-20 m/s), and cloud forms in the vicinity of the Tharsis volcanoes and Olympus • Intermediate-age volcanics • Ancient highlands Mons during the early morning hours suggest strong • Ground ice (i.e., high latitude) winds there at those times. There is a possibility of • Waterlaid sediments strong winds associated with storminess at southern mid-latitudes at this season, but we have little data • Explosive (felsic?) volcanics bearing on this. • Polar deposits • Dust and soil and atmosphere (any site) b) Meteorological science considerations for a 3- Engineering Constraints 4 station network: Several grouping strategies could accomplish important science goals for meteorology, as follows: • +45 ° latitude • <2 km high (i) Low latitude string. A string of 3-4 pressure • -150 km error radius measurements, widely separated in longitude, with • Identical payloads high precision pressure measurements would allow • 2 m (2-10 m) (?) penetration detailed study of Kelvin waves, thermal tides, Meteorological Considerations for Pene- normal modes, and if winds are measured, low trator Sites latitude regional topographic winds (e.g., 068,072, 069, 064). (drafted by C. Leovy) a) Site safety considerations: To satisfy the (ii) Southern vs. northern hemisphere winter storms. landing pressure constraint, all sites have been these storms are responsible for considerable dust chosen to have elevations below the 2 km. It should raising and transport in the north. The key site in be noted that the landing season, late northern the list for this purpose is 062. It would be highly summer, is near the seasonal pressure minimum, so desirable to have two sites near 45°S, plus one or the pressure on entry can be expected to be about two sites in the north at about the same latitude.

14 (iii) Regional slope pressure variations and winds. effects from pressure and/or temperature data alone If wind data could be obtained, stations on opposite is questionable. sides of a regional slope would allow a strategy to (iv) Constant longitude string. A string of 3 or 4 determine regional slope winds. For example, 068, stations along a nearly constant longitude stretching 070, 071, and 072, around the Tharsis bulge would from southern to northern mid-latitudes, including form a useful network for this purpose. The poten- at least one in low latitudes could accomplish some tial for deducing regional slope meteorological of the science of both (i) and (ii) above.

15 BALLOON MISSIONS

The following considerations were developed at Drift Mission: the 25 July 1989 meeting of the joint United States/ Elevation: <+2 km over range of approximately Soviet Landing Site Working Group meeting, held 1,000 km in Flagstaff, Arizona. Slope: (wind shear limi0:<1/100 Winds: (10 m/s = 900 kin/Mars day) <4,000 km in 10 days travel; 10 hours/day

Initial Site: Science:

Maximum variety of geology, or unit of great <-2 km elevation interest, especially at landing site and expected at -45 to +55 latitude (1984) first (few) descents.

16 METEOROLOGICAL STATIONS

Meteorological Measurements Pressure required to :L-0.01 hPa.

Temperature required at 1 meter above the ground At each landing site a long-lived meteorological to accuracy and precision of:t2°C, and desired also station should be deployed in such a way that its at 10-20 cm above the ground with the same measurements suffer minimal interference from the lander. The intent is to follow diurnal and accuracy. seasonal variations in the atmosphere in order to Wind speed to accuracy of :1:20%, direction to better model atmospheric dynamics, and to +30 ° . characterize atmospheric processes at the site. Atmospheric variations also influence weathering, Frost point temperature to +7°K for frost points erosion, migration of volatiles in the soil and above 180°K. exchange of volatiles between the soil and the atmosphere. The station should have a long lifetime Two upward-looking broad-band photometers, one (TBD) and make the following measurements over in the UV, one in the visible and near IR, both with at least one annual cycle with at least 20 averaging accuracies of +10% and precisions of +5%. intervals per day.

17 Site 001 - Eridania NW

Site 001 Latitude: 36°S Site Name: Eridania NW Longitude: 228°W Elevation: + 3.0 to + 4.0 km Type of Site: Rover/Sample Return

Maps: MC-29 NW Contact: Steve Squyres Viking Orbiter Images: 420S 16 through Department of Astronomy 420S21; resolution is 90 m/pxl. Space Sciences Building Cornell University Date Entered: 31 October 1989 Ithaca, NY 14853 Date Last Revised: 31 October 1989 (607) 255-3508

Geologic Setting Scientific Rationale

The site lies at a contact between ancient To be determined. cratered terrain and ridged plains materials that are probably flood lavas of intermediate Objectives age. Plains materials lap up against the higher cratered terrain at the contact. A Ancient cratered terrain, recent volcanics. number of well-developed ancient valley systems are present in the cratered terrain and Potential Problems debouch at the contact. The valleys appar- To be determined. ently predate emplacement of the plains materials. The geometry of the valleys is not clearly confluent, so it is not clear that fluvial Trafficability sediments underlie the plains materials. Fresh To be determined. craters up to about 10 km in diameter excavate into the plains materials, and there are a Estimated Traverse Distance few ancient buried craters whose rims pro- trude upward through plains materials. To be determined.

18 NclVEtgOJ.OHcr 3_I.IHM (]NV 3,q.Vd -1VNIL)I_O

saJ/,nbs eAeiS epnl!Buo-I M oSgg 'epnlile7 S o9_ :e;!S 6u!pueq ® MN6_- OV_

uJ_ 001.

I I I I I

MoO£:_

IS3MH/_iON VINV(]IEI3 1.00 oI!S Site 002- Parana Valles

Site 002 Latitude: 22°S Site Name: Parana VaUes Longitude: 12"W Elevation: + 1.0 km Type of Site: Rover/Sample Return

Maps: MC-19 SE Contact. Steve Squyres Viking Orbiter Images: 651A91 through 651A95; resolution is 260 m/pxl. Space Sciences Building Cornell University Date Entered: 31 October 1989 Ithaca, NY 14853 Date Last Revised: 31 October 1989 (607) 255-3508

Geologic Setting Objectives The site lies at the confluence of a number of Ancient cratered terrain, waterlain sediments. valley systems in ancient cratered terrain. The primary feature of the site is a closed Potential Problems topographic depression with many inflow valleys and a single outflow. The depression To be determined. is not clearly filled with volcanic deposits, and hence may contain waterlain sediments Trafficability that are near or at the surface. The deposits filling the depression have an unusual hum- To be determined. mocky texture of unknown origin.

Scientific Rationale Estimated Traverse Distance

To be determined. To be determined.

2O Site 002 PARANA VALLES

10°W 20°S

• i ¸

N \

r,J

• 10°W

CO r-

20oS •

I I I I I I 100 km 33

ASU - 434 (_) Landing Site: 22 ° S Latitude, 12 ° W Longitude Steve Squyres -J

_,L,. Site 003 - Eridania

Site 003 Latitude: 58°S Site Name: Eridania Longitude: 212"W Elevation: + 4.0 km Type of Site: Rover/Sample Return

r Maps: MC-29 SE Contact: Steve Squyres Viking Orbiter Images: 551B27 Department of Astronomy through 551B32; 373S03; resolution is Space Sciences Building 70 m/pxl. Cornell University Ithaca, NY 14853 Date Entered: 31 October 1989 (607) 255-3508 Date Last Revised: 31 October 1989 ,. J

Geologic Setting Scientific Rationale

The site lies at a contact between ancient To be determined. cratered terrain and ridged plains materials that are apparently flood lavas of intermedi- Objectives ate age. The latitude of the site is high enough that ground ice may be present. Lava flows Ancient cratered terrain, intermediate vol- are observed on the plains. These lavas lap up canics, ground ice. against the higher cratered terrain at the contact. Several well-developed ancient valley systems are present in the cratered Potential Problems terrain and debouch at the contact. The To be determined. valleys apparently predate emplacement of the plains materials. The geometry of the valleys is not clearly confluent, so it is not Trafficability clear that fluvial sediments underlie the plains To be determined. materials. Fresh craters up to about 10 km in diameter excavate, into the plains materials. One such crater very close to the site has a Estimated Traverse Distance well-developed double-lobed fluidized ejecta blanket. To be determined.

22 Site 003 ERIDANIA

215°W I

.54°S

54os -

60°S

60oS -

215°W

I I I I I I 100 km

MC -29SE (_) Landing Site" 58 ° S Latitude, 212 ° W Longitude Steve Squyres

23 ORfGT_'!AL P,qGE BLACK Ai',_D V,/di]-E. £_OTOGRAPN Site 004- Eridania SE

Site 004 Latitude: 57°S Site Name: Eridania SE Longitude: 195°W Type of Site: Rover/Sample Return Elevation: + 5 km

f Maps: MC-29 SE Contact: Steve Squyres Viking Orbiter Images: 553B09 through Dept. of Astronomy .... 553B16; 373S25 Space Sciences Bldg.

Date Entered: 22 November 1989 Cornell University Ithaca, NY 14853 Date Last Revised: 22 November 1989 : (607) 255-3508

Geologic Setting to about 7 km in diameter excavate into the plains materials. The site lies at a contact between ancient cratered terrain and ridged plains materials Scientific Rationale that are apparently flood lavas of intermediate age. The latitude of the site is high enough To be determined. that ground ice may be present. Lava flows are observed on the plains. These lavas lap up Objectives against the higher cratered terrain at the Ancient cratered terrain, intermediate vol- contact. Several small ancient valley sys- canics, ground ice. tems are present in the cratered terrain and debouch at the contact. The valleys appar- Potential Problems ently predate emplacement of the plains materials. The lavas seem to fill a closed To be determined. depression into which the valleys drain, so there is a possibility of waterlain sediments Trafficability being present under the lavas (though this To be determined. possibility probably is not high enough for Estimated Traverse Distance this site to be considered as a prime one for sampling such sediments). Fresh craters up To be determined.

24 Site 004 ERIDANIA SOUTHEAST

195°W

55°S .

59oS -

195°W

I I I I I I 100 km

MC -29SE _) Landing Site: 57 ° S Latitude, 195 ° W Longitude Steve Squyres

BLACK Ai',;D ...... Site 005- Iapygia

Site 005 Latitude: 9°S

Site Name: Iapygia Longitude: 279°W Type of Site: Rover/Sample Return Elevation: + 5.0 km

Maps: MC-21 NE Contact: Steve Squyres Viking Orbiter Images: 754A07 through Dept. of Astronomy 754A 11

Date Entered: 22 November 1989 Date Last Revised: 22 November 1989 (607) 255-3508

Geologic Setting Scientific Rationale

The site lies at a contact between ancient To be determined. cratered terrain and a plains unit that may be volcanic material of intermediate age. Within Objectives the ancient terrain very close to the contact, a Ancient cratered terrain, waterlain sediments, well-developed valley system debouches into intermediate volcanics. a very degraded 10-km impact crater. The Potential Problems crater appears to be largely filled, and is likely to contain a significant quantity of To be determined. waterlain sediments. There is no clear evi- Trafficability dence for volcanic material in the crater, though this possibility cannot be excluded. To be determined. There is a fresh 2.5-km crater formed in the Estimated Traverse Distance crater-filling deposits. A single valley flows out of the 10-km crater and onto the plains. To be determined.

26 Site 005 IAPYGIA

280°W I

8os _ .8os

11os - •11°S

° 280°W

I I I I I 100 km

MC -21NE _) Landing Site: 9° S Latitude, 279 ° W Longitude Steve Squyres

2? (3R'IC-.f_!& L p,_,,__ BLACK Ar,;ib WHITE. £HO;O,3riAPN Site 006- Noachis

Site 006 Latitude: 550S Site Name: Noachis Longitude: 337°W Type of Site: Rover/Sample Return Elevation: + 5.0 km

Maps: MC-27 SW Contact: :: " Steve Squyres Viking Orbiter Images: 575B03 through Dept. of Astronomy 575B08 Space Sciences Bldg. C_rnell University Date Entered: 22 November 1989 :Ithaca, NY 14853 Date Last Revised: 22 November 1989 (607) 255-3508 j

Geologic Setting Objectives The site lies at a contact between ancient Ancient cratered terrain, intermediate vol- cratered terrain and plains materials that are canics, ground ice. probably flood lavas of intermediate age. The latitude of the site is high enough that Potential Problems ground ice may be present. A very fresh 15- To be determined. km crater with a well-developed fluidized ejecta blanket lies very near the contact. Trafficability To be determined.

Scientific Rationale Estimated Traverse Distance

To be determined. To be determined.

28 Site 006 NOACHIS

355°W I

55°S _

- 55oS

i 355°W

I I I I I I I00 km

MC -27SW (8) Landing Site: 55 ° S Latitude, 337 ° W Longitude Steve Squyres 29

BLACK AI',J5 '_r,, ,_- HriC;_)"' r_*,",.'..,- F_ Site 007-Terra Cimmeria

Site 007 Latitude: 42"S Site Name: Eridania NC Longitude: 21 I°W Elevation: + 5 km Type of Site: Rover/Sample Return

Maps: MC-29 NC r Contact: Steve Squyres Viking Orbiter Images: 370S50; Department of Astronomy resolution is 230 m/pxl.

Date Entered: 7 November 1989 Ithaca, NY 14853 Date Last Revised: 7 November 1989 (607) 255-3508 J

Geologic Setting Scientific Rationale To be determined. The site lies at a contact between ancient cratered terrain and ridged plains materials that are apparently flood lavas of intermedi- Objectives ate age. These lavas lap up against the higher Ancient cratered terrain, intermediate vol- cratered terrain at the contact. Many well- canics. developed ancient valley systems are present in the cratered terrain and debouch at the Potential Problems contact. The valleys apparently predate To be determined. emplacement of the plains materials. The lavas seem to fill a closed depression into which the valleys drain, so there is a possibil- Trafficability ity of waterlain sediments being present under To be determined. the lavas (though this possibility probably is not high enough for this site to be considered as a prime one for sampling such sediments). Estimated Traverse Distance Fresh craters up to about 12 km in diameter To be determined. excavate into the plains materials.

3O Site 007 TERRA CIMMERIA

41.5°S

210°W

• 210ow

41.5 S

I I I I I I 100 km

V.O. 370S50 _) Landing Site: 42 ° S Latitude, 211 o W Longitude Steve Squyres

._._ACK Al'..,,5 ,'fr,i _. r _,;:., _;,;.,,_.,-N Site 008- Mare Tyrrhenum

Site 008 Latitude: 23°S

Site Name: Mare Tyrrhenum Longitude: 231"W Elevation: + 3.0 to + 4.0 km Type of Site: Rover/Sample Return

f ConlaCt: Maps: MC-22 SE Steve Squyres Department of Astronomy Viking Orbiter Images: 629A10, Space Sciences Building 629A27; resolution is 250 m/pxl. Cornell University Ithaca, NY 14853 Date Entered: 7 November 1989 (607) 255-3508 Date Last Revised: 7 November 1989

Geologic Setting Scientific Rationale

The site lies at a contact between ancient To be determined. cratered terrain and ridged plains materials that are apparently flood lavas of intermediate Objectives age. These lavas lap up against the higher Ancient cratered terrain, intermediate vol- cratered terrain at the contact. Many well- canics. developed ancient valley systems are present in the cratered terrain and debouch at the Potential Problems contact. The valleys apparently predate emplacement of the plains matefiais. The To be determined. lavas seem to fill a closed depression into which the valleys drain, so there is a possibility of waterlain sediments being present under Trafficability the lavas (though this possibility probably is To be determined. not high enough for this site to be considered as a prime one for sampling such sediments). Estimated Traverse Distance Fresh craters up to about 6 km in diameter excavate into the plains materials. To be determined.

32 Site 008 MARE TYRRHENUM

233°W 229°W I i

19°S - -t9os

25,_S _ '29'S

I I 233ow 229°W

1 I I I I I 1O0 km

MC -22SE Landing Site: 23 ° S Latitude, 231 ° W Longitude Steve Squyres

33 C.R!G i i',b"-,L P.,,.s c 6L,.ACK AND WHITE ?u;OTOGRAF'U Site 009 - Sinus Sabaeus

Site 009 Latitude: 6.5°S Site Name: Sinus Sabaeus Longitude: 335.5°W Type of Site: Rover/Sample Return Elevation: + 4.0 km

Maps: MC-20 NE

Viking Orbiter Images: 618A09 through :: Depa_ment of Astronomy 618A11; resolution is 230 m/pxl. ::: : Space:Sciences Building : Cornell University Date Entered: 7 November 1989 Ithaca, NY 14853 Date Last Revised: 7 November 1989 (607) 255-3508

Geologic Setting Scientific Rationale

The site lies in a 25-km impact crater in To be determined. ancient cratered terrain. One well-developed valley system and several smaller valleys Objectives drain into the crater, so it probably was a site Ancient cratered terrain, possible waterlain of ancient aqueous sedimentation. No clear sediments. evidence for subsequent volcanic filling of the crater is seen, but the resolution of the Potential Problems existing image probably is insufficient for detection of many possible volcanic To be determined. landforms. The site lies less than 100 km from "White Rock," an unusual high-albedo Trafficability crater floor deposit that has been guessed by To be determined. some to be a possible carbonate or evaporite deposit. This is potentially quite an interesting site, but a major improvement in data quality Estimated Traverse Distance is required before it could be considered seriously. To be determined.

34 Site 009 SINUS SABAEUS

335"W 337°W I

-5os 5°S -

-8os

8oS -

i 337°W 335'W

I I I I I I 100 km

MC -20NE (_) Landing Site: 6.5 ° S Latitude, 335.5 ° W Longitude Steve Squyres

0 ,?!,?__ !i',!4 !_ ,'--'.*...... _ _£. BLACK At',_D ' ';-- ,..... Site 010- Terra Tyrrhena

Site 010 Latitude: 25"S Site Name: Terra Tyrrhena Longitude: 266"W Type of Site: Rover/Sample Return Elevation: + 3.0 krn

Maps: MC-22 SW

Viking Orbiter Images: 625A31

Date Entered: 28 November 1989 Date Last Revised: 28 November 1989 :_mell University Ithaca, NY 14853 } _ Space Sciences Bldg. 1 _ : (_7)255-3508

Geologic Setting Scientific Rationale

To be determined. The site lies at a contact between ancient cratered terrain and plains materials that may Objectives be flood lavas. However, the resolution is too Ancient cratered terrain, intermediate vol- low to confirm the origin of these plains. canics and/or waterlain sediments. Many well-developed valley systems are present in the cratered terrain and debouch Potential Problems with a confluent geometry at the contact, so a To be determined. sedimentary origin cannot be ruled out. Ifthe plains are volcanic, they are likely to be Trafficability underlain in some locations by waterlain To be determined. sediments. A fresh 35 km crater with a broad Estimated Traverse Distance ejecta blanket excavates into the plains material near the contact. To be determined.

36 ...... q_'_JV

seJ_nbs e^e_S epn],!6uoq M o99;_ 'epnl!lel S o£;_ "e],!S 6u!pue-I ® l.SV£_9 OA

&_ oo I. I I I I I I

MoS9_

So£_,

/ N L

MoS9_'

• So£_

VN=IHI=INA$ Vt=ll=l=l/ 01.0 e:l!S Site 011 - Phaethontis SW

Site Ol l Latitude: 51°S Site Name: Phaethontis SW Longitude: 153°W Type of Site: Rover/Sample Return Elevation: + 5.5 km

Maps: MC-24 SW Contact: Steve Squyres Viking Orbiter Images: 526A50 through 526A52 Dept. of Astronomy Space Sciences Bldg. Comell University Date Entered: 28 November 1989 Ithaca, NY 14853 Date Last Revised: 28 November 1989 (607) 255-3508 K_

Geologic Setting Scientific Rationale The site lies at a contact between ancient To be determined. cratered terrain and ridged plains materials that are apparently flood lavas of intermedi- Objectives ate age. The latitude of the site is high enough Ancient cratered terrain, intermediate vol- that ground ice may be present. Several well- canics, ground ice. developed ancient valley systems are present in the cratered terrain and debouch at the Potential Problems contact. However, the geometry of the valleys is not clearly confluent, and they do not To be determined. clearly flow into a closed depression, so the presence of waterlain sediments, even be- Traffieability neath the lavas of the plains, is uncertain at To be determined. best. The largest craters excavating into the Estimated Traverse Distance plains materials near the contact are smaller than 5 km in diameter. To be determined.

38 Site 011 PHAETHONTIS SOUTHWEST

155°W 152 °W I I

- 49os

49os -

-52.5os

52.5oS -

1s?,ow ls'2ow

I I I I I I 100 km

MC -24SW l_) Landing Site: 51° S Latitude, 153 ° W Longitude Steve Squyres

39 (_:'_:;':_:rT;'_-.:. _. .,,;.. j_, .,._., - 5_.ACK Af',.& ,',_.K;I-E. _-_._",; O,S',W,,:'r., Site 012- Samara Valles

Site 012 Latitude: 23°S Site Name: Samara VaUes Longitude: 21°W Elevation: + 2.0 km Type of Site: Rover/Sample Return

Maps: MC-19 SE, SW Contact:

Viking Orbiter Images: 615A41 through 615A43 Space Sciences Bldg. Cornell University Date Entered: 28 November 1989 Ithaca, NY 14853 Date Last Revised: 28 November 1989 (607) 255-3508 J

Geologic Setting data quality is required before it could be considered seriously. The site lies in the vicinity of two large impact craters in ancient cratered terrain. Scientific Rationale One is about 100 km in diameter, and the other is about 35 km. Many well-developed To be determined. valley systems drain into the larger crater, and at least one well-developed one drains Objectives into the smaller one. Both probably were Ancient cratered terrain, waterlain sediments. sites of ancient aqueous sedimentation. No clear evidence for subsequent volcanic fill- Potential Problems ing of either crater is seen, though the resolution of the existing images is insufficient for To be determined. detection of many possible volcanic landforms. For the larger crater, subdued valley Trafficability renmants are visible over much of the crater To be determined. floor, making deep volcanic burial there Estimated Traverse Distance appear unlikely. This is potentially quite an interesting site, but a major improvement in To be determined.

4O ro c_ o ! L.L

ro i-n

Q. I'0 GO

I-"

Q_ CO (,Q 0 wo CD DO I"0 C.O o

I-- o i,-t- t- 3 - Q.

o I /

I-- r"- 0 i- _Q B. ra c Q.

_ o oo .0 c 2' Sites 013-017- DELETED

Site 000 Latitude: Site Name: Longitude: Type of Site: Elevation:

Maps: Contact:

Viking Orbiter Images:

Date Entered: Date Last Revised:

42 Site 018 - AIba Patera

Site 018 Latitude: 47°N Longitude: 116*W Site Name: Alba Patera Elevation: + 3 km Type of Site: Rover/Sample Return r Contact: Maps: MTM#45117; MC-2 SE Dale Schneeberger Jet Propulsion Laboratory Viking Orbiter Images: 252S32, 252S34 48(KI Oak Grove Drive M/S 183-501 Date Entered: 18 October 1988 Pasadena, CA 91109 Date Last Revised: 18 October 1988 (818) 354-2451

Geologic Setting b) possible pyroclastic materials or deeply weathered material; potential access Alba Patera, a unique volcanic feature, is the problem (success 50-70%); largest central volcano in the solar system. At c) possible older "basal" sheet flows the center lies a 100 km wide caldera. associated with early Alba activity; Extending from the central caldera for uncertainty of stratigraphic nature hundreds of miles are channel-fed flows, (success 50-70%); sheet lavas, and complex tube-fed lavas. The d) tube-fed flow sample; traverse to sample landing site lies in Alba Fossae, a set of location may pose a problem to sample fractures which postdate flows on the acquisition (success 40-60%). Northwest summit region of Alba Patera. Potential Problems

A potential problem associated with the Scientific Rationale proposed sample collecting site lies with the The site provides accessibility to lava flows uncertainty of the surface roughness. The that appear to exhibit a range in rheology as surface appears relatively smooth in the 60- demonstrated by the various flow 80 m/pxl images. However, very high morphologies. Crater numbers suggest that resolution images (9-10 m/pxl) south and three of the units here are not significantly east of the sample site show surfaces marked different in age from each other. The site also by numerous small pits or craters to about 30 offers an opportunity to sample volcanic meters in diameter (limit of resolution). Yet, materials thought to be pyroclastics. all exhibit a similar surface appearance in images of comparable resolution. Therefore, the surface of the proposed sample site may Objectives have a potential roughness characteristic of the very high resolution images. Thus, sur- a) Tabular flow sample; collectionofsample face roughness will have an impact on sample may be hindered by steepness of slope of acquisition. The degree of impact will de- flow lobes (success 70-90%)

43 pendon thecapabilityof therovervehicle,or pyroclasticterrain,maymakesampleacqui- whateversamplemeansare used. If, for sitiondifficult. example,surfaceconditionsaretoorough,a traverseof more thanafew kilometersmay Trafficability beimpossible.Otherproblemssuchassteep To be determined. topographicgradients,like thatfoundneara tabular flow front, or irregular (etched) Estimated Traverse Distance topographyassociatedwith thehypothesized To be determined.

44 Site 018 ALBA PATERA

116° W I

47° N- - 47° N

I 116° W

I I I 20 km

MTM 4511 7 _) Landing Site: 47 ° N Latitude, 116 ° W Longitude D. Schneeberger

t.:',, - . .. i _ 45 Site 019 - Northern Elysium

Site 019 Latitude: 33°N

Site Name: Northern Elysium Longitude: 212"W Elevation: 0 km Type of Site: Rover/Sample Return

r Contact: Maps: MTM#35212; ML-75L Peter Mouginis:Mark

Viking Orbiter Images: 86A35 through 86A40 Hawaii Institute Geophysics 2525 Correa Road Honolulu, HI 96822 Date Entered: 22 September 1988 (808) 948-6488 Date Last Revised: 22 September 1988

Geologic Setting c) identify physical properties of flanks of Hecates Tholus (success high: providing The landing site is located on the northwest rover has sampling arm/trench); flank of Hecatus Tholus. Hecatus Tholus, d) investigate stratigraphy of lowlands/ one of the three Elysium volcanoes, is 180 highlands scarp (success medium: rover km wide, 6 km high, and topped by a complex imaging may not have resolution. Canyon caldera from which several lines of floor topography unknown). depressions and grabens radiate. Small, fluvial-like channels of controversial origin Landing Site: Sample and return selected arise close to the landing site. materials from plains that underlie lobate flows from Elysium Mons. Scientific Rationale Interpretation: Undifferentiated lava flows Age date for lower Amazonian lavas--cali- from Elysium Mons. brate crater chronology; investigate origin of Goal: Age date flows. materials on flank of Hecates Tholus (explo- Station 1: Sample and return material from sive?); study possible volcano/ground ice distal end of lobate flow from Elysium Mons. interactions to constrain martian volatile Interpretation: Relatively young lava flow history. from Elysium Mons (Lower Amazonian; Objectives Greeley and Guest, 1987). Goal: Age date lava flow. Resolve issue of a) Sample and return lava flow on plains why lava flows on Mars travel up to ^500 north of Elysium Mons; calibrate size/ km from source (chemistry vs. effusion frequency crater curves (success high: rate?). but lander-scale topography may make landing interesting); Station 2: Sample and return material from b) resolve stratigraphy of flanks of Hecates edge of subdued flow lobe. Tholus--old or young channels? (success Interpretation: Mud flow produced by vol- medium: I'm not sure rover cameras will cano/ground ice interactions in northern pick up correct morphology); Elysium.

46 Goals: Identify mode of formation of flow boundary between northern plains and lobe. Age date event Elysium lavas.

Station 3: Resolve stratigraphy of deposits Potential Problems associated with channels from Hecates Landing site may be rough at scale of Tholus. spacecraft; long traverse (-170 km)--could Goals: Answer questions of whether channels rover live required time?; physical properties pre-date or post-date plains materials and of flanks o fHecates Tholus unknown--could whether channels were water carved or be too soft for rover (or too steep?). formed by debris flows.

REQUIRED ROVER CAPABILITIES: Station 4: Investigate physical properties of 1) sample return capability (atleast3 selected flanks of Hecates Tholus. rocks). Goals: Determine if flanks comprise ash fall 2) trafficability - A200 km range. deposits, pyroclastic flows, or 3) Rover-to-Earth communications. hydrothermally-altered lava flows. This 4) Science experiments: is of key importance in our attempts to a) cameras (video and multispectral). determine if early martian volcanism was b) gravimeter. explosive in nature and the possible c) trenching ability (^20 cm depth). paleoclimatic effects explosive eruptions d) active seismic experiment. may have had early in martian history. LANDING SITE CONSTRAINTS: Station 5: Investigate physical properties of 1) "hazard-free" landing ellipse (no impact isolated massifs and knobby materials on craters in 10 km diameter target detectable the plains north of Hecates Tholus. on 50 m/pxl images). Goals: Determine if there are morphologic 2) low elevation (< 2 km above 6.1 mb or compositional differences between datum). massifs (assumed to be remnants of earlier,

partially-buried surface) and northern TARGET AREA: -50 km west of Hecates plains. Tholus at 33°N, 213°W.

Station 6: Investigate physical properties of Trafficability eroded scarp along boundary of northern plains and Elysium Mons lava flows. To be determined. Goal: Search for evidence of stratigraphy in Estimated Traverse Distance scarp wall and for evidence of paleo ground- ice. Required Travel Distances

Landing site to station 1: roundtrip 15 km Sites 3-5 Traverse: Conduct gravity and Landing site to station 2: roundtrip 13 km active seismic experiments to determine Landing site to station 3: 81 km Station 3 to station 4: (up-slope) 11 km sub-surface structure to northwest of Station 4 to station 5: (down-slope) 26 km Hecates Tholus. Station 5 to station 6: 18 km Goals: 1) Determine basal diameter of Hecates Tholus, 2) determine thickness of TOTAL ...... 164 km Elysium Mons lavas, and 3) determine

47 Site 019 NORTHERN ELYSIUM 213 ° W I 211°W I

34 ° N -

CO r-- ('3

33 ° N-

._c2

O £b

"-c .'3" I I 213 ° W I I I I I I 211°W 50 km

MTM 35212 (_ Landing Site: 32.5 ° N Latitude, 212.5° W Longitude Pete Mouginis-Mark Site 020- Argyre Planitia

Site 020 Latitude: 55"S Longitude: 42"W Site Name: Argyre Planitia Elevation: + 1 krn Type of Site: Rover/Sample Return Contac. Maps: MTM# -55044; MC-26 SW i Timothy Parker Jet Propulsion Laboratory Viking Orbiter Images: 567B53 Oak Grove Drive

Date Entered: 22 September 1988 Pasadena, CA 91109 Date Last Revised: 22 September 1988 (818) 354-2451

, I I I

Geologic Setting c) massifs (2): possible deep crustal material (success moderate: depends on steep- The landing site lies in Argyrc Planitia, one of ness of approach to"fresh" rock at base of the largest and best preserved ancient impact each massif). basins. Surrounded by rugged massifs which form vague, concentric and radial patterns around the basin. The original basin floor is Potential Problems buried and no inner rings arc visible. Site is at a moderately high southern latitude, Scientific Rationale placing delta vee and communication link constraints on all component vehicles. Sample layered basin-fill material of possible Southern approach for lander and ascent lacustrine origin (search for fossil organic vehicles may require consideration of material), unusual sinuous ridges, and possible avoidance of high south basin rim mountains. deep crustal material in basin rim massifs.

Objectives Trafficability

a) Layered plains material (success high: To be determined. landing site on plains; distance to deflated exposures may be small); b) sinuous ridge material (success high: Estimated Traverse Distance landing site near prominent ridge; traverse to massif crosses ridge); To be determined.

49 Site 020 ARGYRE PLANITIA

42°_W

I"-

55.5 ° S "

r_ r,_ •

-' F.t

3> 42 _ W

I I I 20 km

Viking Orbiter 567B53 _) Landing Site: 5.5 ° S Latitude, 42 ° W Longitude Tim Parker Site 021 - Maja Valles

Site 021 Latitude: 18.95"N Longitude: 53.50"W Site Name: Maja Valles Elevation: - 0.5 km Type of Site: Rover/Sample Return

f • • Maps: MTM#20052; MC-10 NE Contact: Jim Rice Viking Orbiter Images: 825A25, Department of Geology 825A27, 825A46, 825A48 Arizona State University Tempe, Arizona 85287-1404 Date Entered: 22 September 1988 (602) 965-7029 Date Last Revised: 22 September 1988

Geologic Setting c) crater ejecta (small craters) (success excellent); exposed strata along channel Maja Valles are northeast-trending outflow walls I success average); atmospheric channels deeply incised into old cratered sample (success excellent); terrain between Lunae Planum and Chryse d) exobiology (extinct) (success below Planitia. To the south of Maja Valles is average); exobiology (extant) (success Valles Marineris. remote); ground ice (success remote).

Scientific Rationale Potential Problems

To obtain data/samples on channel morphology, outflow dynamics, stratigraphy Obvious malfunction of mechanical compo- of fan-delta complexes at the mouths of Maja, nents, accuracy of landing ellipse, patches of Maumee, and Vedra Valles. Also of interest: very rough terrain, rover traverse distance, origin of streamlined islands and wrinkle and curation of samples containing volatiles ridges; oldest mappable rock unit (Nb) on and any exobiology if present. Mars and the extensive ridged plains unit Trafficability

(I/r) are also contained in this site. To be determined. Objectives

a) Gravels/sediment from channels (suc- Estimated Traverse Distance cess excellent); fan-delta sediments (success excellent); lake deposits (suc- SOLID TRAVERSE is for separate rover/ cess average); sample return vehicles which requires rover b) ancient crustal material (Nb) (success to return to sample return orbital module above average); modified basal unit of (traverse distance = 100 km). Hesperian System (Hr) (success excellent); in situ wrinkle ridge and is- DASHED TRAVERSE is for a combined land (success excellent); rover/sample return vehicle which allows

51 more terrain to be covered and does not distance = 100 km; with touchdown point at require returning to landing site (traverse station 9 on solid). f MAJA VALLES SITE: POSSIBLE SAMPLES (Keyed to map of site)

STATION STATION NUMBER DESCRIPTION NUMBER DESCRIPTION

1 Lake deposits and or Maja Valles 17 Nb material and ejecta from large fan delta sediments crater 2 Streamlined island material near 18 Wrinkle ridge material that may tail be buried crater rim crest 3 Wrinkle ridge material 19 Wrinkle ridge material from 4 Maja fan delta sediments and buried crater rim modified Hr material 20 Lake deposits and/or crater infill 5 Streamlined island material material 6 Margin of Maja and Vedra fan A18 Channel sediments and/or lake delta deposits deposits 7 Vedra fan delta sediments and A 19 Streamlined island material near outflow channel deposits prow and small crater ejecta at 8 Outflow channel deposits and lower left of island possible lake sediments A20 Major outflow material from 9 Margin of Vedra and Maumee fan Maja delta deposits A21 Crater ejecta 10 Maumee fan delta deposits A22 Plunge pool material possibly 11 Crater ejecta from small impact scouredbedrock and Vedra sediments A23 Crater ejecta and channel material 12 Ancient crustal material (Nb) and A24 Maja fan delta sediment and crater lake outflow sediments channel margin material 13 Margin of Maja and Maumee fan A25 Subsequent secondary channel delta deposits material 14 Nb Material A26 Streamlined island material 15 Crater ejecta of small impact (immature) and channel plains 16 Nb material and ejecta from large material crater ,)

52 Site 021 MAJA VALLES

54° W I

19° N- •19° N

18° N- .18ON

54°W I I I 10 km

MTM 20052 _) Landing Site: 18.95 ° N Latitude, 53.50 ° W Longitude Jim Rice

53 _?;LACK fJ"_D Wr;;_-E. i-_-.:',::_OC,:,_FI-_ Site 022 - Candor Mensa

Site 022 Latitude: 5.5"S Site Name: Candor Mensa Longitude: 74.5"W Elevation: + 1 km Type of Site: Rover/Sample Return

r N Maps: MTM#-5072 Contact: Baerbel Lucchitta Viking Orbiter Images: 915A12 U.S. Geological Survey 2255 N. Gemini Dr. Date Entered: 6 September 1988 Flagstaff, AZ 86001 Date Last Revised: 6 September 1988 (602) 527-7176

Geologic Setting d) cap rock ofLunae Planum Plateau; basaltic? sedimentary? (success marginal; The landing site is located on Candor Mensa, reworked in landslide); a mesa in Candor Chasma, which is an east- e) landslide processes: dry? contained water west trending trough associated with Valles or ice? important for wall-rock Marineris. Valles Marineris, known as composition (success marginal). canyonlands, is made up of grabens, canyons, pit craters and channels. The canyon walls exhibit horizontal layering. VALLES MARINERIS, MARS: AN OPTIMUM SCIENCE-SAMPLE SITE Scientific Rationale B.K. Lucchitta, U.S. Geological Survey, Nearby rocks have range of ages and Flagstaff, Ariz. 86001 compositions, from very old to very young. Potential to find lake beds (carbonates?) in The Valles Marineris troughs offer a layered interior deposits. Potential to find unique sampling opportunity because they very young volcanic deposits. Exciting site expose a thickness of upper crustal rocks as for human exploration. great as 7 km. Also, because of their long and varied history, the troughs give insights into Objectives a number of processes that are critical to a) Nature of crustal composition up to 6 km deciphering the history of Mars. below surface; ancient rocks (success Ideal sample sites on Mars would yield good; reworked in landslide; outcrop of information on rocks in close proximity more difficult access); having a range of ages and compositions. b) nature of layered deposits; volcanic? The Valles Marineris fulfill these sedimentary? fossils? (success good; requirements. Very old units of Noachian rocks in place; accessible); age (Scott and Tanaka, in press) are exposed c) youngrocks(post-landsliding);volcanic? in the lower walls that would give us data on ashflow tuffs? felsic? (success good; rocks compositions and ages of rocks that are deep in place; accessible); below the surface at most other places. The

54 mostcommonlyacceptedhypothesisis that Mass-wastingprocessesresulted in talus theserocksarelunarhighlands-typebreccia slopesand landslides. Whether the land- (Carr, 1979). The landslidesof the Valles slideswerewetordryisnotentirelyresolved; Marineris, also, furnish excellent sites to thisquestioncouldbeaddressedbysampling sampletheseancientrocks,becausetheslides the matrix of landslide deposits. Further- fell from troughwallsandthusincorporated more,alargechannelappearstohaveemerged wall rock. Additionally, most landslide from one of the slides and causeda cata- materialscontainsomecaprock of thepla- strophicflood(Lucchitta,in press);sampling teau,thusoffering anopportunityto sample of thechannel-floormaterialmight confirm materialofintermediateage(EarlyHesperian) thisorigin. Thecompositionof thechannel (1). Thecaprockiscommonlyinterpretedas materialmayalsoestablishwhetherice was floodbasalts(ScottandCarr,1978),butother involvedin theflooding. Wateror ice in the compositionscannotbeexcluded. Younger channelmust havecome from the trough intermediate-agerocks (Later Hesperian) walls,andthediscoverythateitherwaspres- (ScottandTanaka,in press)form partof the entwould confirmtheexistenceof thehypo- layered interior deposits. Their origin is theticalground-icereservoiron Mars. uncertain;they havebeenconsideredto be Winddepositsareabundantonthechannel volcanic flows, fluvial deposits(Lucchitta, floors. Dark barchan dunes consist of 1982),or wind drifts trappedin ice-covered reworkeddark materialthatappearsto have lakes(Nedellet al., 1987).Samplesof these come from volcanic vents in the troughs; rocks would illuminate an important seg- samples of this material would give mentof martianmid-historyandshedlight compositionsandages,andthustheymight notonly on thecompositionof thesemateri- confirm the existence of such vents. alsbutalsoon theprocessesthatoperatedat Establishinggrainsizesof thedunematerial thattime. would also shedlight on the mechanismof A secondsuiteof interiordepositsoccurs emplacementand,by analogy,on theorigin on the Valles Marineris floors, resting of many similar duneselsewhereon Mars, unconformablyonallotherunitsandreaching particularly those trapped inside craters. thicknessesof asmuchas3,000min western Light-colored,reddishdustfromatmospheric CandorChasma(Lucchitta, 1985). These fallout is alsoabundantin the troughsand rocksareyoung,of LateAmazonianage,and might be sampledto obtainits composition, aremostlikely of volcanicorigin. Theyare thus resolving the controversyof whether locally composedof verydarkmaterialsthat dust-stormmaterialiscomposedof smectite are easily reworked by the wind and may clay (Clark, 1978) or palagonite (Singer, havecomefrom youngvolcanicvents(Luc- 1982). chitta,1987).Elsewherethesedepositsareof Overall, the Valles Marineris offer an variedalbedoandrugged,andtheymaybe opportunity to sample rocks that reflect composedof volcanic rock of unknown variousagesandcompositions,givinginsight composition. Samplingtheserocksandob- into importantprocesseson Mars. Most of taining their precisecompositionsandages the samples would be located within wouldbeanimportantcontributionto unrav- reasonableproximity and could be easily eling thethermalevolutionof Mars. reachedby rovers or balloons. Although SamplesfromtheVallesMarineriswould landingaspacecraftonthefloor of theValles alsogive insightsinto a numberof martian Marinerismaybe toodangerousfor thefirst processes.Theeffectsof tectonismcouldbe sample-returnmissionto Mars,thescientific assessedbysamplingmaterialsonbothsides rewardswouldbesogreatthatsuchalanding of theyoungfaultsthatcutthetroughfloors. shouldbeconsideredfor later flights. 55 REFERENCES: Scott, D.H. and M.H. Carr 1978. Geologic map of Mars: U.S. Geol. Survey Misc. Inv. Series Map Cart, M.H. 1979. Formation of martian flood features Series 1-1083, scale 1:25,000,000. by release of water form confined aquifers. J. Scott, D.H. and K.L. Tanaka (in press). Geologic map Geophys. Res., 84, no. B6, 2995-3007. of the western equatorial region of Mars: U.S. Clark, B.C. 1978. Implications of abundant hygro- Geol. Survey Misc. Inv. Series Map 1-1802A, scopic minerals in the martian regolith. Icarus, scale 1:15,000,000. 34,645-665. Singer, R.B. 1982. Spectral evidence for the mineral- Lucchitta, B.K. 1982. Lakes or playas in Valles Mar- ogy of high-albedo soils and dust on Mars. J. ineris (abs.), in Repts. Planetary Geology Geophys. Res., 87, no. B12, 10159-10168. Program---1982: NASA TM-85127, 233- 234. Potential Problems Lucchitta, B.K. 1985. Young volcanic deposits in the Valles Mafineris, Mars (abs.), in Lunar Planet. Steep cliffs to north and east; sampled rocks Sci. 16. The Lunar and Planetary Institute, cannot be tied to cratering chronology. Houston, Texas, 503-504. Lucchitta, B.K. 1987. Recent mafic volcanism on Trafficability Mars. Science, 235, 565-567. Lucchitta, B.K. (in press). VaUes Marineris, Mars: To be determined. Wet debris flows and ground ice. Icarus. Nedell, S.S., S.W. Squyres, and D.W. Anderson 1987. Estimated Traverse Distance Origin and evolution of the layered deposits in the Valles Marineris. Icarus, 70, 409-441. To be determined.

56 Site 022 CANDOR MENSA 73 ° W I

-4 ° S

75o'W 73 ° W I I I i ! I 50 km

MTM -05072 Landing Site: 5.5 ° S Latitude, 74.5 ° W Longitude Baerbel Lucchitta

_"LL. J ",. Site 023 - Memnonia

Site 023 Latitude: 1 I°S Site Name: Memnonia Longitude: 173°W Type of Site: Rover/Sample Return Elevation: + 1 km

Maps: MTM# -10172; MC-16 NW Contact: (I-1188) David Scott .... U.S. Geological Survey Viking Orbiter Images: 599A95, 2255 N. Gemini Drive 599A97, 440S05 Flagstaff, AZ 86001 (602) 527-7188 Date Entered: 6 September 1988 K_ Date Last Revised: 6 September 1988

Geologic Setting mining the absolute age of the bend in the martian cratering rate curve where the rap- The Memnonia site is in a valley between the idly decaying early flux changes to a nearly northern lowland plains and southern constant rate (Neukum, 1987). Together highlands. The landing area is on ridged with Amazonian and Noachian rock samples plains lava flows, a globally extensive rock they would provide data on the composition unit of intermediate (Hesperian) age. The and radiometric ages for major rock units on ridged plains are overlain to the north by very Mars. young (Amazonian) rocks postulated to be ash-flow tufts (Scott andTanaka, 1982, 1986) Objectives or paleopolar deposits (Schultz and Lutz, 1988). On the south side of the valley the Primary sample locations (fig. 1) are ridged plains embay ancient (Noachian) numbered in table 1; targets of opportunity cratered highlands. A small young channel that might be sampled enroute are indicated of unknown origin is close (6 km) to the by letters. The landing and ascent sites are landing site. Viking images (-50 rn/pxl) assumed to be the same or close together. indicate the area is relatively smooth and free of obstacles. Summary of objectives:

Scientific Rationale a) Rocks of intermediate age (Hesperian) at landing site (success excellent); In situ rock outcrops of young (Amazonian), b) possible pyroclastic rocks of very young intermediate (Hesperian), and ancient age (Amazonian) near (-15 km) landing (Noachian) ages occur within about 0-15 km site (success very good); from the landing site. Young stream channel c) ancient rocks (Noachian) near (5-15 km) deposits and layered material in the channel landing site (success very good); gorge could also be sampled. Ridged plains d) fluvial materials and young outflow lava flows of Hesperian age are considered to channel near (6 km) landing site (success be the most important rock units for deter- excellent).

58 REFERENCES Potential Problems

Stream channel and floodplain deposits Neukum, G. 1987. Absolute ages from crater sta- including large rocks may be more extensive tistics: Using radiometric ages of martian samples than presently apparent--need much higher for determining the martian cratering chronology resolution images than 40 m/pxl. (abs.), in Workshop on Mars Sample Return Science, LPI Tech. Rept. 88-07, pp. 128-129. Schultz, P.H., and A.B. Lutz, 1988. Polar wandering Trafficability on Mars: Icarus, 73, 91-141. Scott, D.H., and K.L. Tanaka 1982. Ignimbrites of the Appears good at image resolution. Amazonis Planitia region of Mars: J. Geophys. Res., 87, no. B2, 1179-1190. Estimated Traverse Distance Scott, D.H., and K.L. Tanaka 1986. Geologic map of the western equatorial region of Mars. U.S. Geol. 1) 35 km Survey Miscellaneous Investigation Series Map 2) 40 km 1-1802A. Total ...... 75 km

"-Table 1. Materials to be sampled on proposed landing site traverses at primary sample stations (numbers) and secondary targets of opportunity (letters). Landing site (LS) and traverses shown in the site figure. Estimated minimum traverse distance Station/Target from LS (kin) Sample description and geologic significance 1 (LS) 0 Basalt flows of intermediate age (unit Hr); widespread occurrences; globally correlative geologically and by crater counts. A 6 Channel material (unit Ach) in bar or island remnant; TV scan for layering, sorting, size distribution. B 13 Knobby material (unit Nk). 2 16 Member 2 (unit Am 2) of Medusae Fossae Formation (young ash flow?); TV scan to determine nature of contact with adjacent basalt flows (unit Hr) and knobby material (unit Nk). 3 21 Channel gorge cutting possible layered basalt flows (unit Hr) and older rocks. C 26 Samples and TV scan along channel from station 3 to C to observe possible layering of basalt flows in channel wall. 4 32 Ejecta and rim material around 500-m-diameter crater in ridged plains unit. 1 (Ls) 35 Completion of first traverse. D 5 Ejecta and rim material around 600-m-diameter crater in ridged plains unit. 5 14 Rim of Noachian (c_) crater. E 16 Ridged plains/c_ contact from station 5 to E. 6 23 Wrinkle ridge in ridged plains unit; TV observation of ridge structure. 7 25 Ejecta and rim material from young crater (1,500 m in diameter) in ridged plains unit. 8 29 Fresh crater (300 m in diameter) superposed on channel material and on basalt of ridged plains unit. F 31 Channel material. 1 (is) 40 Completion of second traverse.

75 km Total distance of two traverses. J

59 -l_.<

_0 8-

® o r"-

o.. 2D O0 m.

(o 0 Ix.)

r,a

o ,..¢._,-2-. 3 e" m Q. z ",,I _o © o z "-,t.., 7, ,,*- r"" > o x_

_----d t" Q. -, ;L7

dr"

L ' i L t2 _D <

(-.) _t o

o Site 024 - Mouth of Maja VaUes

Site 024 Latitude: 17.9°N Longitude: 53.8°W Site Name: Mouth of Maja Valles Elevation: - 0.5 km Type of Site: Rover/Sample Return

f Maps: MTM#20052; MC-10 NE Contact: Rene DeHon Viking Orbiter Images: 825A27, Department of Geology 825A29, 825A46, 825A48 Northeast Louisiana University Monroe, LA 71203 Date Entered: 6 September 1988 (318) 342-2188 J Date Last Revised: 6 September 1988

the local vicinity for fan dissection. The Geologic Setting possibility exists that this region is a wind gap The surface characteristics vary from smooth of higher wind velocity and that the area is to rough at meter scale. The material at swept cle_tr of eolian debris. Bedding in the landing site consists of alluvial materials fan could reveal part of the flow history in with possible eolian cover. Landing site is on Maja. Sampling of fan sediments would the head of an alluvial fan at mouth of a gorge. provide materials for analysis from the canyon The basement material is Noachian material section of Maja. It is doubtful that material of the Xanthe Terra highlands and ridged from beyond Xanthe Terra would be present. plains of Chryse Planitia. Once a site of pronounced erosion, the site was later 5 km traverse: Would place a rover at the subjected to deposition by waning flood nearest edge of the gorge with the possibility waters. The local relief is probably dominated of sampling the oldest rocks (Noachian by late stage gullying in alluvial materials; basement materials) either in place or as hence, it may be both a bouldery and colluvial material not far removed from its channelled surface. It may be blanketed with source. later eolian material. Ridged plains materials are probably not exposed in the immediate I0 km traverse: To the west would allow vicinity. inspection of the north wall of the gorge and dissected Noachian materials. A traverse to Scientific Rationale the southern wall would allow inspection of the tributary/distributary gorge on the south To be determined. wall.

Objectives 25 km traverse: Up the canyon (west) would 1 km traverse: Would allow sampling mate- allow inspection of the wall of the canyon rials of the fan. If an eolian cover is not (Noachian materials), sediments in smooth present, a traverse would be able to examine deposits of the floor, and possible bedrock

61 materialsin hummockyfloor material. Al- a fan/delta type deposit. An on-board seismic ternately, the traversecould proceedeast- experiment could investigate the Xanthe wardonto thefan proper. Terra/Chryse Planitia boundary and/or the fan configuration. 50 km traverse: Covering a larger area would offer little new. Iftherover moved westward, Potential Problems it would essentially be trapped within the To be determined. canyon and not be able to explore the plains on either side. If the rover moved eastward, the most common terrain would be materials Trafficability of the alluvial fan/delta. To be determined.

Comments: Ambitious in terms of safety, Estimated Traverse Distance with all the good and bad points of working 1-50 km

62 Site 024 MOUTH OF MAJA VALLES

53.5° W 55 ° W ! I

-18.5 ° N 18.5 ° N -

'3",

f--

17.5 ° N- -17.5 o N

I'Q

i I 55 ° W 53.5 ° W eD I I I I I I 50 km

Rene De Hon MTM -20052 Landing Site: 17.9 ° N Latitude, 53.8 ° W Longitude Site 025-Maja Valles Canyon Flood Plain

Site 025 Latitude: 17.65"N Site Name: Maja Valles Canyon Flood Longitude: 54.2 - 54.3°W Plain Elevation: - 0.5 km Type of Site: Rover/Sample Return

Contact: Maps: MTM#20052; MC-10 NE Rene DeHon

Viking Orbiter Images: 825A25, Department of Geology ..... 825A27, 825A46, 825A48 Northeast Louisiana University Monroe, LA 71203 (318) 342-2188 Date Entered: 6 September 1988 Date Last Revised: 6 September 1988

Geologic Setting valley, materials on the floor of Maja proper, and colluvium from the high wall on the Lacustrine materials (possible eolian cover). northern side of Maja. Relatively flat plain on the south side of Maja Valles. The site was a region of deposition Potential Problems during ponding of Maja waters prior to cutting through the highland barrier. To be determined.

Scientific Rationale Trafficability

This site offers a potentially safer landing To be determined. site, but traverses would have to be a greater distance to areas of interest. Estimated Traverse Distance Objectives For minimum potential the rover would have The primary traverse would be eastward to to be capable of at least a 10 km traverse, and the secondary channel that leads into the a 30-50 km capability would be most Maja proper. The sampling route would desirable. Safer than the primary site (site traverse probable lake sediments, crater ejecta, .024), the alternate site requires more stringent colluvium from the walls of the secondary mobility requirements.

64 Site 025 MAJA VALLES CANYON FLOOD PLAIN

55° W 53.5 ° W I !

18° N - -18° N

r- C_. 17.5 ° N - "17.5 ° N

' r_

'_,

! 55° W 53.'5° W I I t I I i 50 km

MTM 20052 ® Landing Site: 17.65 ° N Latitude, 54.25 ° W Longitude Rene De Hon Site 026 - Upper Maja

Site 026 Latitude: 18.2°N Longitude: 57°W Site Name: Upper Maja Elevation: + 0.5 krn Type of Site: Rover/Sample Return

Maps: MTM# 20057; MC-10 NE Contact. Rene DeHon Viking Orbiter Images: 825A26 Department of Geology Northeast Louisiana University Date Entered: 6 September 1988 Monroe, LA 71203 Date Last Revised: 6 September 1988 (318) 342-2188

Geologic Setting ejecta to sample materials beneath the ridged plains materials; the Lunae Planurn--Xanthe Surface of Lunae Planum. This area was Terra boundary to sample Noachian cratered awash by the Maja outflow and probably held plateau material and/or Noachian basement ponded waters. The area of the landing site is materials; and the head of a channel entering an undetermined thickness (but probably a Xanthe Terra to inspect channel materials thin cover) of alluvial and lacustrine sedi- and channel walls. ment overlying ridged plains materials. Comment: I would rate this as one of the Scientific Rationale safer landing sites--but not particularly inter- Smooth plain, high density of small pits; esting. Probability of eolian cover is high. A smooth to moderately rough at meter scale; seismic experiment could investigate the thickness of eolian/lacustrine sediments and sampling of possible eolian cover; probable lacustrine sediments; basalts exposed as ejecta the thickness of ridged plains materials. With from small craters in the area. maximum range, and on-board seismics, the rover could enter one of the canyons and Objectives investigate the Lunae Planum/Xanthe Terra boundary structure. 1-10 km traverse: A short traverse from a safe landing site will not provide much more Potential Problems than sampling of the plains materials and underlying Hesperian volcanics exposed as To be determined. crater ejecta. Below the eolian cover, the sediments are derived from the full 1000 km Trafficability

reach of the upper Maja Valles section. To be determined.

20-50 km traverse: Longer traverses allow Estimated Traverse Distance the possibility of a greater diversity of materials. Traverses could reach fresh crater To be determined.

66 UOH eC] auel=l epnl!6uo-1/V_ oL£ 'epnl.!l.e-1 N o88 I. :e1.!S 6u!pue-1 _) LgO0_ IAI.LIAI

('7

ua_OL

I I ! 17"/. M ogg M oZg I I • . t'J

l C

N o81.- - Nogl.

kC)

N o61.- -N o6L

1 M ;9s M oLg vrvw 1::13ddR 9_0 el!$ Site 027 - Upper Mangala Valles

Site027 Latitude: 13.8"S; alternate 13.7"S

Site Name: Upper Mangala Valles Longitude: 148. I'W; alternate 148.7°W Elevation: + 3 km Type of Site: Rover/Sample Return

Maps: MTM# - 15147; MC-16 NE Contact: (I-1185) James Zimbelman NASM 3166. Viking Orbiter Images: 639A12, Smithsonian :Institution 447S35

Date Entered: 6 September 1988 j Date Last Revised: 3 July 1989

Geologic Setting b) Noachian-age materials exposed along scarp at west base of prominent ridge Mangala Valles is an outflow channel which (oldest material exposed in landing area) originates in a graben associated with (success high. Location is -18 km from Memnonia Fossae just south of the landing landing site; trafficability should be good); site. Landing site 027 is located west of the c) Noachian-age cratered plains exposed Tharsis Mountains and south of the highland- northwest of landing site. Note: plains lowland border. are superposed on Target 2 materials Scientific Rationale (north of site) (success high. Location is ~26 km from landing site; trafficability Sample an extensive plains unit intimately should be good); related to flooding events in Mangala VaUes, d) fresh-appearing craterejecta. Target 4 is while providing access to other major geo- a rampart at distal edge of ejecta (related logic materials along relatively short trav- to volatiles?); Target 4' is lunar-like cra- erses. The suite of samples could span much ter (success moderate. Crater ejecta may of the geologic history of the planet. Note: be very blocky, making travel difficult. An extended roving mission could traverse However, the rampart may be very im- down Mangala Valles. portant for volatile-related questions). Objectives Potential Problems a) Sample Hesperian-age plains that were either emplaced by floods in Mangala Lack of high resolution Viking images of Valles, or modified by the floods (suc- proposed site (639A 12 has 244 m/pxl resolu- cess very high. Target site is on this tion). 45 m/pxl images are available for plains unit. 447S35 frame shows large adjacent areas (e.g. 447S35) so that an alter- areas that are featureless at 45 m/pxl native site could be selected within the cov- (safe?); erage of these images; unfortunately, a site

68 further west would lengthen the traverse Estimated Traverse Distance -50 distanceto the Noachianmaterials(to Prime site: <100 km total, two separate km one way). Note: Good Earth-basedradar traverses (see figure). data are available at latitude 14.46°S. Alternate site: ~100 km for all but Target 2 Trafficability (Noachian) materials. Good to excellent around landing site, mod- ~160 km for all target sites in erate on Noachian materials, moderate to one long traverse. poor on crater ejecta.

69 Site 027 UPPER MANGALA VALLES

148° W

Hm I

--4 O

-14°S Nplh

148° W

I I I I I I 50 km

MTM -15147 ® Landing Site: 13.8 ° S Latitude, 148.1 ° W Longitude James Zimbelman (_ Alternate Landing Site: 13.7°S Latitude, 148.7° W Longitude Site 028 - Olympus Mons Southeast

Site 028 Latitude: 14°N; alternate 13°N Longitude: 131"W; alternate 125°W Site Name: Olympus Mons Southeast Elevation: + 2.8 km Type of Site: Rover/Sample Return

Maps: a) MC-9 SW (I-1259) Contact: and MC-9 NW (I-1261) Ronald Greeley b) Controlled photomosaic of the Department of Geology Olympus Mons region of Mars Arizona State University (I-1379) Tempe, AZ 85287-1404 c) Geologic Maps: MC-9 SW (602) 965-7045 (I- 1268) and MC-9 NW (I-1266)

Viking Orbiter Images: Date Entered: March 1989 044B27 (resolution: 147 m/pxl) Date Last Revised: March 1989 045B61-68 (resolution: 146 m/pxl) 046B34-40 (resolution: 135 m/pxl) 890A34 (resolution: 162 m/pxl)

Geologic Setting flows (Amazonian age) possibly derived from fissures east of Olympus Mons. Youngest lava flows in region (and per- This site lies on young lava (basaltic?) plains haps on Mars). Age determinations will on the southeastern margin of the shield provide calibration for young magmatic volcano, Olympus Mons. It includes a vari- activity on Mars. Some flows exhibit ety of geologic units such as old fractured mare ridges. There is controversy over terrain, aureole deposits, and lava flows origi- the origin and age of these features nating from Olympus Mons as well as flows (younger or same age as flows). Long- from possible local fissures and vents. range transect crosses one set of mare ridges and possible source area. Scientific Rationale Crater calibration: Total area of con- tiguous unit--420,000 km2; although it is Principal sampling objective(s): Intermedi- composed of multiple flows probably ate and young volcanic units, aureole depos- erupted from multiple vents, it is a homo- its of Olympus Mons, terra material (frac- geneous unit at regional scale. tured rough and smooth terrain), aeolian deposits. b) Olympus Mons post-scarp flows (unit Aorn_): Youngest lava flows that were Sampling rationale: derived from flanks of Olympus Mons after formation of basal scarp. Agedeter- a) Plains material (unit Aop): Young lava minations will provide data for some of

71 the most recent volcanic activity on Mars. mation on contemporary geologic proc- Crater calibration: Total surface area of esses on Mars. the shield represented by this sample site=376,000 km 2. Potential Problems c) Aureole deposits (units AHoa I and Hazard Assessment AHoa2): Highly fractured and dissected hilly terrain that is embayed by plains Principal hazards: Possible lava flow lobes (lava?) material. Very extensive to north on the plains; blocks and rubble downslope and west of Olympus Mons. Two units of from or at the base of areas of high relief (e.g., apparently different ages mapped in area. aureole outcrops, the Olympus Mons scarp); Origins controversial, but may be de- fractures on the smooth lava flow surface; rived from gravity spreading from older, ridges on smooth lava flow surface. "precursor" volcano to Olympus Mons, or from ash-flow deposits. Composi- The site is on a lava flow surface which tional determinations from samples will appears to be generally flat and of intermedi- help to assign origin to these extensive ate-to-young age. Lavas are inferred to have units. erupted from vents on ESE base of Olympus Crater calibration: AHoaa= 144,000 km 2, Mons scarp (Scott and Tanaka, 1986) and AHoa2=62,000 km2; may be very diffi- flowed from there northward and southward cult to obtain meaningful crater statistics around the base of the Olympus scarp to for these units because they are highly embay surrounding aureole deposits and to fractured. truncate flows from the Olympus summit which have flowed over the scarp. Flow d) Terramaterial (HNht): Mapped as single features are found near the inferred vent area unit, but two units evident in area. Unit (ESE side), and include ridges and apparent (a) consists of fractured and slumped tensional fractures, possible collapsed tubes blocks along eastern scarp of Olympus or fractures, flow lobes, and possible glassy Mons; probably represents early shield- remnants of gaseous lavas (e.g. cavernous, building materials. Unit (b) consists of "shelly" pahoehoe). Aeolian mantling is extensive fissured and fractured plains evident in many areas. material. Compositional data and age determinations will provide information Objectives on origins of these two units. In particu- Landing Sites lar, determination of the age, origin, and

composition of these units and compari- Option A: Short range (Lander and Rover son with the various aureole deposits at same site) 100 km traverse. may enable the controversy of the aureole material to be resolved. Location: 14 ° 10' N; 131 ° 50' W. Crater calibration: HNht=159,000 km2; also occurs as extensive unit to the east Geologic units: near Valles Marineris. Olympus Plains material (Aop): overlapping e) Surficial materials, incluch'ng debris flows smooth lava flows. on marginal escarpment, and wind streaks Olympus Mons post-scarp flows (Aom2): on plains material: Samples from these multiple lava flows of Olympus Mons materials will provide important infor- shield volcano.

72 Presumedterm material(early-stageshield- with younger flows. Good probability building material exposedin scarps): of sampling success. Rover returns Unit a,slumpedblocksfrom marginal samples to Lander. escarpmentof OlympusMons(HNht,). Option B: Long Range: Traverse by Rover Sequence of operations: from Lander (L) to Ascent vehicle (A). Approximate traverse length is 500 km.

. Lander (L) and Rover (R) land on plains close to base of Olympus Mons scarp. Geologic Units: Obtain samples of"fresh" younger lava Aureole members 1 and 2 (AHoal_): dis- flows with source away from Olympus sected material of uncertain origins. Mons (sample S-1) for radiometric age Possible landslide material or ash flow determinations and correlation with tuff. crater count ages; also sample weath- Plains material (Aop): overlapping smooth ered flow surfaces (S-2); and soil (S-3) lava flows. at lander site. Excellent probability of Shield member (Aos): multiple lava flows of sampling success. Olympus Mons shield volcano. Includes pre-scarp flows (Aom,) and post-scarp

. Traverse A: Deploy Rover to obtain flows (Aorrh). samples of fresh (sample S-4) and Older fractured material: embayed and frac- weathered (sample S-5) basalts from tured materials (HNht ,b). lava flows that originate on Olympus Aeolian material (bright streaks). Mons shield and flow across marginal escarpment. Good probability of sam- Sequence of operations: piing success at flow margins. Rover

returns samples to Lander. . Ascent vehicle (A) lands on plains close to margin of Olympus Mons shield.

. Traverse B: Deploy Rover to obtain Obtains sample of fresh (sample L-l) samples of in situ material (sample S-6) and weathered basalt (sample L-2) at and talus material (sample S-7) from landing site for radiometric age deter- scarp zone on southeast margin of minations and correlation with crater shield; will provide samples of older count ages of plains member (Aop). term material. Good probability of High probability of sampling success. sampling terra material. As in other localities along the scarp zone, it may . Rover (R) lands 450 km to east-south- be difficult to assign a context to talus east on plains material (Aop) close to material, which could have been de- contact with terra material. Rover is rived from the Olympus Mons shield, deployed and collects sample of fresh the term material of the scarp zone, or and weathered plains material (samples post-scarp flows or plains material at L-3,4). High probability of sampling the base of the scarp. Rover returns success. samples to Lander.

. Rover moves northeast across plains

° Traverse C: Deploy Rover to obtain unit to terra material. Samples this unit samples of lava flows on plains adja- (sample L-5). Samples required for cent to shield (sample S-8). Additional radiometric age determinations and samples of plains unit for comparison correlation with crater count ages. As

73 this material is old and heavily cratered, parisons between geographically sepa- it may have a thick regolith; thus, ob- rated outcrops of the aureole unit. taining a fresh sample may be difficult. However, it may be difficult to obtain a The probability of obtaining a good fresh sample of aureole materials. These sample will be enhanced by sampling a materials may be weathered, and their graben wail. dissected nature suggests that talus may

. Rover turns to move west-northwest, be abundant. If the aureole materials recrosses plains material to aureole are ash flows, then obtaining radiomet- material. Crosses low aibedo zone ric ages may be difficult. Adjacent to where aeolian or weathered material aureole deposits, Rover samples the may be absent. Samples plains mate- bright aeolian material to south of out- rial (sample L-6). The probability of crops (samples L-12,13). If high al- successfully sampling this material is bedo materials on Mars are dust, then enhanced by the probable absence of there is an excellent opportunity to surficiai materials. Collects samples of sample windblown material at this aureole material (AHoal) from outliers location. of aureole deposits (sample L-7) for 7. Rover travels southwest across plains compositional and possible radiomet- material (sample L- 15) to base of scarp ric age determinations. It may be diffi- of Olympus Mons shield. Good proba- cult to obtain a fresh sample of aureole bility of sampling success from plains materials. These materials may be material. Roverobtains sampleoflobate weathered, and their dissected nature unit at base of scarp. This unit is a suggests that talus may be abundant. If possible post-scarp lava flow (sample the aureole materials are ash flows, L-16). Good possibility of sampling then obtaining radiometric ages may be success at flow margin. Rover then difficult. obtains samples of in situ material

. Rover proceeds northwest across plains (sample L- 17) and talus (sample L- 18) unit. Samples fresh and weathered from fractured terra material (HNht) plains member at three locations exposed in scarp on southeast margin (samples L-8,11) to determine com- of shield. However, the presence of positional and possible age differences post-scarp lava flows in this area may between basalt flows of plains mem- prevent access to in situ terra material. ber. High probability of successfully Also samples lobate material that may sampling plains material. Samples L- be debris cone or post-scarp lava flow 9,10 from fractured area; flow lobes are (sample L-19). Good probability of visible. Possible local sources of lavas sampling this unit, the origin of which of plains member. Near-vent location is uncertain. As in other localities may give rise to occurrence of shelly along the scarp, it may be difficult to pahoehoe, with attendant trafficability assign a context to talus material, which hazards. In addition, lavas extruded could have been derived from the may be glassy in texture, leading to Olympus Mons shield, the terra mate- problems with age and compositional rial of the scarp zone, or post-scarp determinations. flows or plains material at the base of

. Rover proceeds to sample outliers of the scarp. aureole unit (AHoa_) (sample L-14). 8. Rover continues south along base of Information from these samples will scarp on lava plains. Rover samples in facilitate age and compositional com- situ material (sample L-20) and talus

74 (sample L-21) from fractured terra flows, Aon%). Excellent probability of material(HNht,) exposedin scarpon sampling success at flow margins. southeast margin of shield. Good proba- Rover returns samples to ascent ve- bility of sampling terra material. As in hicle. other localities along the scarp, it may be difficult to assign a context to talus 13. Ascent vehicle returns samples to Earth. material, which could have been derived from the Olympus Mons shield, DESCRIPTION OF UNITS ON the terra material of the scarp zone, or ACCOMPANYING GEOLOGIC MAP post-scarp flows or plains material at the base of the scarp. Aop Olympus Plains Flows - Embays ba.ml scarp of Olympus Mons and overlaps post-scarp flows, mottled albedo. 9. Rover diverges to southeast across lava plains. Additional sample obtained of Interpretation: Lava flows from most re- this unit (sample L-22). Good probabil- cent fissure eruptions southeast of Olympus Mons. ity of sampling success. Rover reaches ridge that may be fissure vent and col- Olympus Mons Post-scarp Flows - Lava lects sample from end of ridge (sample A°m2 flows form complex, finely textured, in- L-23). It may be very difficult to obtain terfingering tongues and lobes, mottled a good sample of the ridge material, as albedo. talus mantling the end of the ridge may Interpretation: Lava flows from crest and restrict access to fresh samples. flanks of Olympus Mons, after formation of 10. Rover continues southwest along base basal scarp. of scarp. Collects samples of talus (sample L-24), and resamples fractured AHoa 2 Olympus Mons Aureole, Unit 2 - Islands of hilly material embayed with Aop. material at southwest end of exposure (samples L-25,26). Good probability Interpretation: formed by gravity spread- of sampling terra material. As in other ing of materials from an earlier, larger localities along the scarp zone, it may Olympus Mons; alternatively, ash or lava be difficult to assign a context to talus flows. material, which could have been de- Olympus Mons Aureole, Unit 1 - Hilly rived from the Olympus Mons shield, AHoa_ material with corrugated surface cut by the terra material of the scarp zone, or numerous faults and fractures. Embayed post-scarp flows or plains material at with Aop. the base of the scarp. Interpretation: Similar to AHoa 2, but 11. Rover reaches site of ascent vehicle formed at an earlier time.

(L)and unloads samples collected. HNht Terra Material, Undivided - both rough 12. Rover proceeds on loop traverse to and smooth; fractured, faulted, and cratered obtain samples of fresh (sample L-27) material, numerous blocks and slump fea- and weathered (L-28) basalts from lava tures along base of Olympus Mons. flows that originate on Olympus Mons Interpretation: Gravity slides along base shield and flow across scarp (post-scarp of Olympus Mons.

75 Appendix: Science Rationale for study remnants are the present day aureoles. Ac- of aureole deposits cording to this model, one would expect to sample shield volcano material such as ha- Among the more enigmatic features salts which would be old compared to observed on the surface of Mars are the Olympus Mons. It also may be possible to aureole deposits concentrated around the base sample the ancient shield at the base of the of Olympus Mons. These features consist of scarp of Olympus Mons. large patches of rough, irregular terrain, pre- Blasius (1976) suggested that plu- senting in many cases a lobate boundary. The tonic activity related to the formation of terrain is characterized by numerous mounds Olympus Mons may have been responsible of material, dissected in radial and circumfer- for the formation of the aureoles. Shallow ential patterns by narrow ridges and grooves. plutons would have been unroofed and eroded, The origin(s) of these features are not known, again by wind. The erosional remnants of although numerous theories and models have this process represents the aureoles. Samples been proposed. These theories can be broadly in this case would be various plutonic rocks. categorized into two groups, magmatic and A very different type of model has tectonic/mass-wasting. We first review the been proposed by Hodges and Moore (1979). magmatic models. They envision a thick ice layer under which King and Riehle (1974) envision a Olympus Mons erupted and eventually period of pyroclastic volcanism at Olympus reached the surface, analogous to an Ice- Mons, during which ash deposits are carded landic table mountain. Continuing eruptions long distances from the shield and emplaced then formed the shield. Around Olympus as nuees ardentes. This friable ash is eroded Mons, basaltic magma erupted from vents by wind and compacted. The aureoles are the and intruded the ice layer, similar to the mode erosional remnants of these deposits. Samples of formation of Icelandic mobergs. The of aureole material formed by this mecha- aureoles are the surface expressions of this nism would be composed of tuff and com- intruded basalt, and would be composed of pacted ash. palagotonized tufts, breccias, and pillow A similar model of aureoles resulting lavas. directly from volcanic emplacement is pre- Williams (1988) proposed that the sented by Morris (1979, 1982). Volcanic area was covered with aeolian deposits prior vents around the shield are presumed to have to magmatic activity. Sills intruding below erupted pyroclastic materials which were these deposits caused them to be uplifted and deposited in huge sheets away from the shield. fractured, and were subsequently eroded by These were then eroded by wind. The aure- wind. The aureoles represent the vestiges of oles represent the weathered remnant of the these aeolian deposits. Samples therefore ash sheets. Ignimbrites, tufts, and other would be expected to consist of ancient aeo- pyroclastic materials would be the expected lian material. samples in this case. The second type of model of aureole The existence of a large volcanic formation invokes tectonic and mass wasting construct which pre-dates Olympus Mons is processes rather than magmatic activity. proposed by both McCauley et al. (1972) and Harris (1977) proposed that Olympus Mons Carr (1973). After its formation, a long was formed on top of a thick sequence of period of weathering and erosion occurred, frozen bedded volcanic and aeolian sedi- followed by the growth of the Olympus Mons ments. The weight of Olympus Mons shield. The outskirts of this large structure squeezed these beds out, in the form of grav- exceeded the size of Olympus Mons, and the ity-assisted thrust sheets. The aureoles repre-

76 sent the distal edges of these sheets, which REFERENCES have ridden over one another. Sample 5 in Blasius, K.R., (1976). Topical studies of the geology this case would be taken from old bedded ash of the Tharsis region of Mars, Ph.D. dissertation, Calif. Inst. Tech. and lava flows. Carr, M.H. (1973). Volcanism on Mars, J. Geophys. A similar model is envisioned by Res., 78, 4049-4062. Francis and Wadge (1983) in which thrust Francis, P.W., and G. Wadge (1983). The Olympus sheets originally spread under gravity from Mons aureole: Formation by gravity spreading, J. Geophys Res., 88, 8333-8344. an ancestral Olympus Mons structure. Again, Harris, S.A. (1977). The aureole of Olympus Mons, the aureoles would be the edges of the thrust Mars, J. Geophys. Res., 82, 3099-3107. sheets and would be composed of lavas and Hodges, C.A., and H.J. Moore (1979). The subglacial pyroclastic and erosional deposits. birth of Olympus Mons and its aureoles, J. Geo- Thrusting of a thin ductile layer over- phys. Res., 84, 8061-8074. King, J.S., and J.R. Riehle (1974). A proposed origin lain by a thicker brittle layer is modeled by oftheOlympusMonsescarpment, Icarus,23,300- Tanaka (1985). Interstitial ice comprising 317. 10% of the volume of the layers is proposed Lopes, R.M., J.E. Guest, and C.J. Wilson (1980). to allow the thrusting to extend to the large Origin of the Olympus Mons aureole and the distances observed. The aureoles are frac- perimeter scarp, Moon Planets, 22, 221-234. tured erosional remnants of the thick brittle Lopes, R.M., J.E. Guest, K. Hiller, and G. Neukum (1982). Further evidence for a mass movement layer, consisting of aeolian deposits of lava origin of the Olympus Mons aureole, J. Geophys. flows. Presumably the lower layer may be Res., 87, 9917-9928. exposed as well, allowing ancient materials McCauley J.F., M.H. Cart, J.A. Cutts, W.K. Hart- mann, H. Masursky, D.J. Milton R.P. Sharp, and such as pyroclastic s and impact breccias to be D.E. Wil helms (1972). Preliminary Mariner 9 report sampled in addition to the surface lava and on the geology of Mars, Icarus, 17, 289-327. aeolian material. Morris, E.C. (1979). A pyroclastic origin for the Lopes et al. (1980, 1982) envision aureole deposits of Olympus Mons, NASA Tech. large scale landslides on the scarps of Memo., 82385, 252-254. Morris, E.C. (1982). Aureole deposits of the martian Olympus Mons. These landslides deposit volcano Olympus Mons, J. Geophys. Res., 87, material around Olympus Mons, as well as 1164-1178. forcing thrust sheets to develop further out Scott, D.H. and K.L. Tanaka (198). Geologic Map of from the base of the shield. The aureoles are the Western Equatorial Region of Mars: Map 1- the result of these landslides and thrust sheets. 1802-A, scale 1:15,000,000. Scott, D.H, G.G. Schaber, K.C. Horstman, A.L. Dial, For this case samples would be ancient crus- Jr., and K.L. Tanaka (1981a). Map showing lava tal material, possibly remnants of a shield flows in the northwest part of the Tharsis Quad- pre-dating Olympus Mons. rangle (MC-9 NW) of Mars. U.S. Geological Careful study of material gathered on Survey Miscellaneous lnvestigation Series Map 1- a sample-return mission could distinguish 1266, scale 1:2,000,000. Scott, D.H, G.G. Schaber, K.C. Horstman, A.L. Dial, between many of these models. Some, such Jr., and K.L. Tanaka (1981a). Map showing lava as those of Hodges and Moore (1979), and flows in the southwest part of the Tharsis Quad- Blasius (1976), could be determined uniquely rangle (MC-9 SW) of Mars. U.S. Geological based on the data. Possible uncertainties may Survey Miscellaneous lnvestigation Series Map 1- exist distinguishing between certain of the 1268, scale 1:2,000,000. Tanaka, K.I_. (1985). Ice-lubricated gravity spreading other models based on the samples alone, but of the Olympus Mons aureole deposits, Icarus, 62, combining this data with high resolution 191-206. spacecraft pictures and rover images should Williams, S.H. (1988). Tharsis aureole deposits: An enable a distinction to be made between any alternative origin (abstr.),Lunar Planet. Sci. Conf., of these models. 19, 1279-1280.

77 Estimated Traverse Distance

Table 1: Summary of sample locations at Olympus Mons Southeast site.

Option A: Traverse by Rover from Lander

Station Loop Distance Cumulative Prime Objective (On) Distance (kin)

S-1,3 0.0 0.0 Plains material

Traverse A S-4,5 27.0 27.0 Post-scarp flow

Traverse B S-6,7 51.0 78.0 Fractured terra material Traverse C S-8 22.0 100.0 Plains material

Option B: Long range traverse

Station Distance from Cumulative Prime Objective last station (kin) Distance (km)*

L-3,4 0.00 0.00 Plains material L-5 15.00 15.00 Terra material L-6 22.50 37.50 Plains material L-7 42.75 80.25 Aureole deposits L-8 45.75 126.00 Plains material L-9,10 40.50 166.50 Plains material (near source) L-11 37.50 204.00 Plains material L-12 9.00 213.00 Bright streak L-13 11.25 224.25 Bright streak L-14 7.50 231.75 Aureole deposits L-15 36.75 268.50 Plains material L-16,18 57.00 325.50 Possible post-scarp flow, fractured terra material L-19 21.75 347.25 Lobate debris flow or post-scarp flow L-20,21 26.25 373.50 Fractured terra material L-22 16.50 390.00 Plains material L-23 17.25 407.25 Ridge in plains material L -24,26 72.00 479.25 Fractured terra material L-l,2 8.25 487.50 Plains material L-27,28 27.00 514.50 Post-scarp flow * from Rover landing site J

78 Site 028 OLYMPUS MONS SOUTHEAST

t \ ¢

OO "n :O I o__ O_

,0 "_ c31> :_ I"- I"1'1 i_o¸ w

Ronald Greeley ASU 465 (_) Landing Site: 14 ° N Latitude, 131 ° W Longitude (_ Landing Site: 13 ° N Latitude, 125 ° W Longitude Site 028 OLYMPUS MONS SOUTHEAST 130 ° W t 125 ° W

15 ° N -"

''t "

t":_ ' .

C) 130 ° w I I I I I I "t. 50 km 7: ASU 465 (_) Landing Site" 14 ° N Latitude, 131 ° W Longitude Ronald Greeley (_ Landing Site: 13 ° N Latitude, 125 ° W Longitude Site 029 - Western Daedalia Planum

Latitude: 19°S; alternate 18.5°S Site 029 Longitude: 144°W; alternate 147°W Site Name: Western Daedalia Planum Elevation: + 3 km Type of Site: Rover/Sample Return

r Maps: MC-16 SE Contact: Ronald Greeley Viking Orbiter Images: 637A 81, 83 Department of Geology (resolution 130-300 m/pxl); Arizona State University 639A 11-14, 16, 35, 37 Tempe, AZ 85287-1404 (602) 965-7045 Date Entered: February 1989 Date Last Revised: February 1989

volcanics (represents unit(s) of 724,000 Geologic Setting km0. High probability of sampling This site is in western Daedalia Planum SUCC_;SS. where lava flows of the Tharsis province C° Central peak material: Landing site embay cratered terrain of the martian high- adjacent to central peak for a 120 km lands. The specific site is located on lava impact crater. Lavas "flood" the cen- flows which lap against the base of the central tral peak and provide access to either peak for a large (120 km diameter) nearly- outcrop or to debris shed from the peak. buried impact crater. The regional structure Peak material probably derived from a is dominated by fractures which trend east- northeast and are related to the Tharsis Rise. depth of 10 km or more and would enable sampling of deep crust and/or Scientific Rationale upper mantle. Good probability of sampling success; samples may be a. Young volcanics: Amazonian-agelava weathered. flows derived from Tharsis (probably Arsia Mons); provides samples of late- Additional Consideration: stage igneous activity and allows cra- The central peak rises about 3 km ter-count calibration (represents unit(s) above the surrounding lava plains. The of 603,000 kin2). High probability of slope on the eastern flank of the peak is sampling success. estimated to be -7.6 °. If the rover were b. Intermediate-age volcanics: Landing capable of negotiating this slope and site on a unit mapped as Amazonian- the inferred blocky surface, there may Hesperian age (Scott and Tanaka, 1986). be the opportunity to sample a rela- May be younger (Greeley and Crad- tively undisturbed cross section of the dock, 1988) and from a local eruptive crust. source; provides potential for sam- It must be noted that the impact occurred in an area surfaced with early- pling from a different igneous province and crater-count calibration than young stage volcanics. Consequently, there is

81 a possibility that the central peak is OPTION A: "veneered" with lavas. In addition, the Site Within Lava-flooded Impact Crater western side of the central peak may be (19°S, 144"W) Short-range (Lander, Rover veneered with ejecta from a younger same site) Traverse (100 km) crater superposed on the primary crater. A critical measurement via Mars Geologic units: Observer would be remote sensing "young" lava flow (AHlp2, basalt) for compositional information on the Tharsis lava flow (At, basalt) central peak. central peak (Nplcp, deep crustal material) d. Surficial materials: Wind streaks in western Daedalia indicate the presence large crater rim material (Nplcr, crustal material) of aeolian material. Moderate proba- small crater ejecta (basalt or excavated bility of sampling windblown material. crust) weathered material/alluvium (basalts or Gullies on the eastern side of the crust) central peak suggest erosion by fluvial processes. Cannot determine if similar Stations: gullies are accessible from landing site for "fluvial" sample. 1. Lander (X) androver (R) landon"young" lava flow within floor of large flooded crater e.Crater rim material: Ancient crustal rocks near Tharsis lava flow lobe; obtain samples exposed in rim of the 120 km impact of "fresh" basalt (sample S l-l), weathered crater; would represent less-deep crust basalt (sample S 1-2), and soil (sample S 1-3) than the central peak. Weathered and at landing site for radiometric age determina- possibly fresh rocks available, either as tion of "fresh" basaltic surface and correla- outcrop or as slope debris. tion with crater-counting ages.

f° Ancient cratered uplands: Exposed 135 2. Deploy rover to obtain samples of fresh km due west of the landing site; mapped (sample $2-1) and weathered (sample $2-2) as the oldest and most widespread crus- basalts and soils (sample $2-3) from Tharsis tal material on Mars (Scott and Tanaka, lava flow lobe (10 km, traverse A) for studies 1986); would provide compositional of basalts of different age and perhaps com- data on this key unit and opportunity to position. Rover returns samples to lander. obtain radiometric dates for crater-count 3. Deploy rover to obtain: fresh central calibration (represents unit of 315,000 peak (sample S3-1) sample for compositional km2). The unit does not appear to have analysis of deep crustal material; weathered been excessively modified by fluvial or material from central peak for evaluation of aeolian materials, increasing the proba- weathering processes (sample $3-2); ejecta bility of obtaining valid samples for the from small crater (sample $3-3) adjacent to unit. central peak for analysis of less weathered subsurface basalt and]or shocked materials Objectives (30 km, traverse B). Roverreturns samples to Intermediate age and young volcanic lander. rocks, ancient cratered terrain, central peak material from a 120 km crater (to obtain a 4. Deploy rover to obtain sample of: fresh deep crustal sample). large crater rim (sample $4-1) for analysis of

82 "fresh" crustalhighlandmaterial;weathered 3. Rover moves to southwest to obtain talusfrom largecraterrim for evaluationof samples of crater ejecta (sample L3-1), weatheringprocessesand effects (sample mantled "young" lava flow surface (sample $4-2);ejectafromsmallcrater(sample$4-3) L3-2) and soil (sample L3-3). for samplingof subsurfacematerial("fresh" basalts,underlyingcrust?);possiblebright- 4. Rover moves to southwest to obtain fresh streakmaterialfrom smallcrater(sample$4- sample of large crater rim material (sample 4)for analysisof aeoliandustand/orsand(60 IA-1) and weathered material (alluvial? flu- km, traverseC). Rover returnssamplesto vial?) at/near base of slope (sample L4-2, 12 lander. km traverse).

OPTION B: Long-range (Lander, Rover 5. Roverturnseastsoutheast toobtain sample separate sites) Traverse (500 of crustal highland material at promontory km) (sample L5-1), weathered crustal material (sample L5-2) and soil (sample L5-3, 83 km Geologic units: traverse). dark-streak material (AHIP2, unmantled basalt?) 6. Rover traverses plain to crater, obtaining large crater rim material (Nplcr, crustal samples of crater ejecta (sample L6-1, basal- material) tic material from different depths, possibly crustal material (NPI_) shocked materials), soils (sample L6-2), and "young" lava flow (AHlP2 ' basalt) bright streak (aeolian dust and/or sand) mate- Tharsis lava flow (At) rial (sample L6-3, 70 km traverse). central peak (Nplcp, deep crustal material) 7. Rover continues east to sample fresh crater rim material (Nplcr, crustal mate- (sample L7-1) and weathered (sample L7-2) rial) crustal material of large crater rim, and soil small crater ejecta (sample L7-3, 45 km traverse). Rover returns weathered material/alluvium to lander, deposits samples (50 km traverse).

Stations: 8. Rover moves north to obtain samples of: 1. Lander (X) lands (19°S, 144°W) on fresh (sample L8-1) and weathered (sample "young" lava flow within floor of large L8-2) basalt from Tharsis lava flow lobe (8 flooded crater, obtain samples of fresh (sample km traverse); fresh (sample L9-1) and weath- LI-1) and weathered basalt (sample L1-2), ered (sample L9-2) deep crustal material of and soil (sample L1-3) at landing site for central peak (28 km traverse); small crater radiometric age determination of "young" ejecta (sample L10-1) and soil (sample L10- basaltic surface and correlation with crater- 2, 10 km traverse); returns to Lander. counting ages. Potential Problems 2. Rover(R)lands-300km(18.5°S, 147 °w) The site is on lava flow surfaces inferred to be to westnorthwest of the lander, within dark relatively flat and of intermediate-to-young streak of small crater located on "young" lava age. Flows are inferred to be of"flood" style, flow surface; obtains sample of unmantled i.e., very fluid, spread as flat sheets; do not lava flow (sample L2-1, "fresh" basalt?) at appear to have local flow features such as landing site.

83 channelsorcollapsedlavatubeswhichwould Blocks shed from the central peak and crater posehazardsandobstacles. May be thinly rim may prevent travel on slopes of those mantled with aeolian deposits which would features. Such blocks would provide alterna- reduce local relief. Principal hazards are fives to samples obtained from outcrops of possible blocks weathered free from the tops the central peak and crater rim. of lava flows and possible local flow scarps.

Estimated Traverse Distance

Mars Landing Site: Western Daedalia Planum

Option A: Short-range Traverse

Station Loop Cumulative Prime Sampling Objective Distance (km) Distance (km)

S1-1,2,3 0 0 Tharsis lava; soil

$2-1,2,3 10 10 Tharsis lava; soil

$3-1,2,3 30 40 Central peak material; small crater ejecta

$4-1,2,3,4 60 100 Crater rim material; small crater ejecta; high albedo patch

Option B: Long-range Traverse

Station Distance from Cumulative Prime Sampling Ob- jective Last Station (km) Distance (km)

L2-1 0 0 Unmantled lava flow

L3-1,2,3 10 10 Crater ejecta; young lava flow; soil

LA-1,2 12 22 Crater rim material

L5-1,2,3 83 105 Plateau unit; soil

L6-1,2,3 70 175 Crater ejecta, soil, high albedo material

84 Site 029 WESTERN DAEDALIA PLANUM

AHIp I / °

CO "J_t

At /. o

_-,.j I 147"W 143" W Ronald Greeley ASU 3381-H (_) Landing Site: 19° S Latitude,144 ° W Longitude C'3 (_ Landing Site: 185 oS Latitude, 147° W Longitude Site 029 WESTERN DAEDALIA PLANUM

147 ° W 143 ° W i I

!!.

-17 ° S

_J I-" c) - 20 ° S

r,'l

•-, r.t

| 147 ° W , i , _ I , 143°W 50 km

ASU 3381-H @ Landing Site: 19° S Latitude,144 ° W Longitude Ronald Greeley @ Landing Site: 18.5 ° S Latitude, 147 ° W Longitude Site 030 - North Polar Cap

Latitude: 80- 85"N Site 030 Longitude: Any Site Name: North Polar Cap Elevation: + 1 to - 2 km Type of Site: Rover/Sample Return f Contact: Maps: MC-1, A and B Alan Howard Department of Environmental Viking Orbiter Images: 816A41-42, Sciences .... 840A12, 768A05, 765A26+28, Brooks Hall 714A07, 750A25, 801A42, 798A42 University of Virginia Charlottesville, VA 22903 Date Entered: March, 1989 (804) 924-0563

Date Last Revised: J

Geologic Setting b) controls on layering: do variations in ice/ dust content control layering? Is there Polar ice and polar layered deposits com- layering at a scale of millimeters to centi- posed of water-ice and dust surround the meters? (success: if conditions permit North Pole. roving, prospects are excellent); c) surface processes on ice: ablation, dust- Scientific Rationale ice deposits, wind action. Micro-relief Polar layered deposits have most complete features (success excellent). record of modern climatic evolution. They Potential Problems may also control cycling of volatiles and dust High latitude: landing, temperatures, sea- Objectives sonal winds, uncertain surface roughness. Sampling: Core sample desirable. What is a) Compositions of ice/dust in polar depos- the hardness of the ice-dust mixture? its: questions include relative amount of ice/dust, grain size of dust, weathering of Trafficability dust, dust aggregates (success depends To be determined. upon how sampling is conducted - re- Estimated Traverse Distance quires a strategy different from other areas of Mars, e.g. coring, melting, etc.); (round trip) 10-20 km

87 Site 031 - North Pole

Site 031 Latitude: 90"N Site Name: North Pole Longitude: Elevation: + 1 km Type of Site: Rover/Sample Return

Maps: MC-1, A and B Cnnf_ef: Conway Leovy, Viking Orbiter Images: 765A26, Department of Geophysics 768A05, 768A06 University of Washington Seattle, WA 98195 Date Entered: March 1989 (206) 543-1812 Date Last Revised: March 1989 J

Geologic Setting c) EM sounding for depth and layer structure of polar caps (success high); Polar ice and polar layered deposits com- d) seasonal and interannual variations con- posed of water-ice and dust surround the trolling condensation regime (success North Pole. high). Scientific Rationale Potential Problems Communications and orbit transfer problems Center of a unique repository of volatiles. require study. Maintenance through cold and Opportunity to investigate properties of sea- dark season requires study. Effects of CO 2 sonally varying cap materials - key to current ice deposition on spacecraft require study. climate. History of volatile deposition over precessional cycle. Dust storm history. Trafficability To be determined.

Objectives Estimated Traverse Distance a) Seasonal composition of volatile depos- (round trip) (a):0, (b) 1000 km; (a) No its (success very high); traverse needed for primary mission, (b) Long b) drill to obtain 2 meter core for preces- traverse capability would allow determina- sional cycle composition variations; dust tion of spatial deposition history across the vs. water, etc. (success moderate); cap.

88 Site 032 - Hadriaca Patera

Site 032 Latitude: 32.5°S Site Name: Hadriaca Patera Longitude: 266"W Type of Site: Rover/Sample Return Elevation: + 1.5 km

f Maps: MC-28 NE Contact: Frederick R. West Viking Orbiter Images: 62S 18-20, 519 Monroe Circle 32A529 Glen Burnie, MD 21061

Date Entered: 6 September 1989 Date Last Revised: 6 September 1989

Geologic Setting Objectives

Mid-Hesperian central vent volcano, Hadri- Land on the south slope of Hadriaca Patera. aca Patera (AHh), and the older channel From there the vehicle is to move south, material of Harmakhis Vallis (Hch) leading going into the graben-like start of Harmakhis down into Hellas Planitia's modified eolian, Vallis. From there the vehicle is to move fluvial, and lava flow material (Hh3). through the Harmakhis Vallis, taking pictures and making measurements. If range Scientific Rationale permits, the vehicle should follow Harmakhis Vallis into Hellas Planitia. Investigation of the slopes of Hadriaca Patera and nearby volcanoes and ancient cratered Potential Problems terrain. Investigation of a channel, Har- To be determined. makhis Vallis and possible investigation of the junction area of Harmakhis Vallis with Trafficability Hellas Planitia. This may give the opportu- To be determined. nity to investigate some of the floor of Hellas Planitia, possible investigation of frosts, Estimated Traverse Distance clouds, and dust storms in Hellas Planitia. To be determined.

89 Site 032 HADRIACA PATERA - DAO VALLES

270°W 265°W

35oS - - 35°S

! 270°W 265°W

I I I ' ' ' 50 km

ASU -71 3 (_ Landing Site: 33 ° S Latitude, 266 ° W Longitude Frederick R. West 90

6LACK AKb ...... _n,]-_._- rr-.,_...... ;'-,..,___c-,,-,.,''.... ' ' "_-_._' Site 033 - Chasma Boreale

Site 033 Latitude: 80.8°N Site Name: Chasma Boreale Longitude: 44.0°W Elevation: - 0.5 km Type of Site: Rover/Sample Return

f Maps: MC-1, A and B Contact: Harold Masursky Viking Orbiter Images: 058B34, U.S. Geological Survey 4261B22 2255 N. Gemini Drive Flagstaff, AZ 86001 Date Entered: March 1989 (602) 527-7003 Date Last Revised: March 1989

Geologic Setting Objectives

Chasma Boreale is a large swirl pattern trough Rocks available: water ice cap, layered deposits, northern plains material. originating in Planum Boreum. Planum Boreum is composed of poha" ice and polar Potential Problems layered deposits surrounded by thick, smooth To be determined. to hummocky eolian deposits. Trafficability To be determined. Scientific Rationale

To be determined. Estimated Traverse Distance To be determined.

91 Site 034 - Planum Australe

Site 034 Latitude: 82.50S Site Name: Planum Australe Longitude: 60.0ow Elevation: + 4 km Type of Site: Rover/Sample Return

Maps: MC-30, A and B Contact: Harold Masursky Viking Orbiter Images: 319B52 U.S. Geological Survey 2255 N. Gemini Drive Date Entered: March 1989 Flagstaff, AZ 86001 Date Last Revised: March 1989 (602) 527-7003

., J

Geologic Setting Objectives Rocks available: carbon dioxide ice cap, Planum Australe consists of polar ice depos- layered deposits, southern plains material. its covered by CO 2 frost (because of colder temperatures relative to the North Pole), and Potential Problems polar layered deposits. These are adjacent to To be determined. Dorsa Argenta polar plains materials. Trafficability To be determined. Scientific Rationale Estimated Traverse Distance To be determined. To be determined.

\ Site 034 PLANUM AUSTRALE

65° W 60° W I I

- 82.5 ° S

-84 ° S

| ! 65° W 60° W

I I I 10 km

MTM -85080 _) Landing Site: 82.5 ° S Latitude, 60 ¢ W Longitude Harold Masursky

93 Cr,,r. ;r..,,,_w p_\(_ BLACK AND WHITE Pr_uAOGr,,_PH Site 035 - Memnonia Sulci

Site 035 Latitude: 9.7°S Site Name: Memnonia Sulci Longitude: 174.20W Type of Site: Rover/Sample Return Elevation: + 2 km

r Maps: MC-16 NW 0-1186) Contact: Harold Masursky Viking Orbiter Images: 599A55 U.S. Geological Survey 2255 N. Gemini Drive Date Entered: March 1989 Flagstaff, AZ 86001 Date Last Revised: March 1989 (602) 527-7003 K._

Geologic Setting Objectives Ancient cratered deposits (possible norites), Memnonia Sulci is southwest of the Tharsis intercrater plains, basaltic lava flows, rhy- Bulge and just north of the highland-lowland olitic volcaniclastic deposits. boundary scarp. The Medusae Fossae For- Potential Problems mation consists of smooth to rolling hills, and To be determined. in places is ridged and deeply eroded. Trafficability To be determined. Scientific Rationale Estimated Traverse Distance To be determined. To be determined.

94 Site 035 MEMNONIA SULCI

174" W /

8 ° S_,

° °

"'8 ° S

10 ° S.

4/ !

/ 174 ° W

"10 ° S

¢ 172 ° W

I I I I I I 50 km

Viking Orbiter (_ Landing Site: 9.7 ° S Latitude, 174.2 ° W Longitude Harold Masursky 599A55 95

lk'" I " i [_ t ; r'_,_ F"" _.

_'T ACK /',r,[] '_'Vc;:T__ _"i:"_ -_"'-'"_'J Site 036 - Olympus Rupes (Southeast)

Site 036 Latitude: 13.8"N

Site Name: Olympus Rupes (Southeast) Longitude: 131.2"W Elevation: + 2 km Type of Site: Rover/Sample Return

"N Maps: MC-9 SW 'Contact:

Viking Orbiter Images: 045B44 U.S. Geological Survey 2255 N. Gemini Drive Date Entered: March 1989 Flagstaff, AZ 86001 Date Last Revised: March 1989 (602) 527-7003

Geologic Setting Objectives

Olympus Rupes is the scarp on the southeast Basaltic lava flows of three ages. flank of Olympus Mons. The plains and shield members of the Olympus Mons For- Potential Problems mation consist of smooth lava flows. Highly To be determined. deformed terrain materials occur along the scarp. Trafficability To be determined.

Scientific Rationale Estimated Traverse Distance To be determined. To be determined.

96 Site 036 OLYMPUS RUPES

131°_W

,.0 --4

-14 ° N

CO 14 ° N - r-- c)

--4

i-i r__._ 1"9 | 131ow

l I I I l l

'j_) 50 km G) (_ Landing Site:13.8 ° N Latitude, 131.2 ° W Longitude Harold Masursky "D Viking Orbiter 045B44 I Site 037 - Kasei Valles

Site 037 Latitude: 15.1"N Site Name: Kasei Valles Longitude: 75.8"W Type of Site: Rover/Sample Return Elevation: + 1 km

Maps: MC-10 SW and MC-10 NW; Contact: MTM# 15077 Harold Masursky U.S. Geological Survey Viking Orbiter Images: 858A34 2255 N. Gemini Drive Flagstaff, AZ 86001 Date Entered: March 1989 (602) 527-7003 Date Last Revised: March 1989

Geologic Setting Objectives Intermediate age basalt flows into which Kasei Valles originates in the Tharsis Montes channels are incised, and young flows that Formation lava flows which are of two differ- overlie channels. ent ages; an earlier flow has been dissected Potential Problems and partially covered by a younger flow. To be determined.

Trafficability Scientific Rationale To be determined. To be determined. Estimated Traverse Distance To be determined.

98 66

X_sJnselAI PlOJeH epni[6uo-I M o8"£/_ 'epni[ieq N o L£ L :ells Bu[pue-I ® ZZO£1. IAIII,N

tu_ OL

I I M o£/. M ogZ I

N oSL- -No£L

N o9L- -N o91.

I I M oSL M o9L S3q-IVA 13SV_I /_g0 el!s Site 038 - Mangala Valles West

Site 038 Latitude: 7.2°S

Site Name: Mangala Valles West Longitude: 158.6°W Elevation: + 1 km Type of Site: Rover/Sample Return

Maps: MC-16 NW (I-1186); MTM# 05157 Harold Masursky U.S. Geological Survey Viking Orbiter Images: 637A75 2255 N. Gemini Drive Flagstaff, AZ 86001 Date Entered: March 1989 (602) 527-7003 Date Last Revised: March 1989

Geologic Setting diate-composition lava flows, young basaltic Mangala Valles is west of Tharsis Montes. flows, and younger rhyolitic volcaniclastic rocks. Mangala Valles West is the western distributary channel which cuts through Noachian cratered unit of the Plateau Sequence. The Potential Problems Medusa Fossae Formation north of the landing site consists of smooth lava flows of To be determined. different ages. Scientific Rationale Trafficability To be determined. To be determined.

Objectives Estimated Traverse Distance Ancient cratered terrain (possible norites, anorthosites), intermediate-age and interme- To be determined.

100 Site 038 MANGALA VALLES 159° W 158° W

6.5°S - - 6.5° S

N \

r Cb

7.5 ° S - - 7.5: S

r_ ..% _ 159 _W ! I I 158° W o 10 km (") MTM 05157 _) Landing Site 7.2 ° S Latitude, 158.6 ° W Longitude Harold Masursky "O ! Site 039 - Mangala Valles East

Site 039 Latitude: 4.7°S Site Name: Mangala Valles East Longitude: 147.5°W Type of Site: Rover/Sample Return Elevation: + 2.5 km

Maps: MC-16 NE (I-1185); MTM# 05147

Harold Masursky Viking Orbiter Images: 639A29+31 U.S. Geological Survey 2255 N. Gemini Drive Date Entered: March 1989 Date Last Revised: March 1989 Flagstaff, AZ 86001 (602) 527-7003

Geologic Setting diate-composition lava flows, young basaltic flows, and younger rhyolitic volcaniclastic Mangala Valles is west of the Tharsis Montes rocks. and cuts through the Noachian cratered unit of the Plateau Sequence. The Medusae Fos- Potential Problems sae and Tharsis Montes lava flows are near the landing site. To be determined.

Scientific Rationale Trafficability To be determined. To be determined. Objectives Ancient cratered terrain (possible norites, Estimated Traverse Distance anorthosites) intermediate-age and interme- To be determined.

102 Site 039 MANGALA VALLES EAST 148 ° W 147 ° W ! !

_ 4os 4 ° S-

o L_,a

T'" ,'-,

5 ° S -

I C, I I I I C_ 148 ° W 147 ° W >, 10 km

-( ,2 MTM 05147 ® Landing Site: 4.7 ° S Latitude, 147.5 ° W Longitude Harold Masursky Site 040 - Elysium Mons

Site 040 Latitude: 24.3"N Site Name: Elysium Mons Longitude: 214.8"W Type of Site: Rover/Sample Return Elevation: + 4 km

"N Maps: MC-15 NW; MTM# 25212 Contact: Harold Masursky Viking Orbiter Images: 541A44 U.S. Geological Survey 2255 N. Gemini Drive Date Entered: March 1989 Date Last Revised: March 1989 Flagstaff, AZ 86001

Geologic Setting Objectives The site lies on the western flank of Elysium Two ages of basaltic flows. Mons. The main edifice of Elysium Mons Potential Problems consists of filled lobate deposits. Radiating To be determined. away from the edifice are lobate plains deposits that overlie and embay neighboring Trafficability volcanoes Albor Tholus and Hecates Tholus. To be determined.

Scientific Rationale Estimated Traverse Distance To be determined. To be determined.

104 I'O t'o

o z Z ! I'o Po

® F-

-3 O0 _o U)

ct) 0 t_ 0 7", 0 FI'I Z r'- r-- o m. Or) f- Q. C

r.,,-, p_ r- co © 0

,.--. Z 03 r-- o

w+ t--

--r S Q_

r'.)

I c f'o .., J t.ll

Z _e Z Site 041 - Apollinaris Patera

Site 041 Latitude: 7.5°S

Site Name: Apollinaris Patera Longitude: 187.2"W Type of Site: Rover/Sample Return Elevation: + 1 km

Maps: MC-23 NE

Viking Orbiter Images: 635A55+57, U.S. Geological Survey 596A36 2255 N. Gemini Drive Flagstaff, AZ 86001 Date Entered: March 1989 (602) 527-7003 Date Last Revised: March 1989

Geologic Setting Objectives

Apollinaris Patera is a shield volcano located Two ages of basaltic flows. just north of the highland-lowland border, Potential Problems and southeast of Elysium Mons. Apollinaris To be determined. Patera consists of several members including deposits dissected by channels. Trafficability To be determined. Scientific Rationale Estimated Traverse Distance To be determined. To be determined.

106 Site 041 APOLLINARIS PATERA

7.5 ° S 188°W t

7.5 ° S

10° S.,

185°W /

J "10 ° S 188 ° W

i , J l I I 50 km

Viking Orbiter (_) Landing Site: 7.5 ° S Latitude, 187.2 o W Longitude Harold Masursky 635A57 107 f->.'..;)e_r._tl p&,_-_'

uLA_,<"t r,I AKD VTHIIE P_r;O=I ....k.)'_ FCAPM Site 042 - Nilosyrtis Mensae

Site 042 Latitude: 35.5°N

Site Name: Nilosyrtis Mensae Longitude: 302.5°W Type of Site: Rover/Sample Return Elevation: + 2.5 km

Maps: MC-5 SE f Contact: Harold Masursky Viking Orbiter Images: 569A20 U.S. Geological Survey 2255 N. Gemini Drive Date Entered: March 1989 Flagstaff, AZ 86001 Date Last Revised: March 1989 (602) 527-7003

Geologic Setting Objectives Basaltic intermediate age plains, and ancient The Nilosyrtis Mensae area is situated on the heavily cratered uplands. highland-lowland border. The ridged unit Potential Problems and undivided unit of the Plateau Sequence are extensive in this area. To be determined.

Trafficability Scientific Rationale To be determined. To be determined. Estimated Traverse Distance To be determined.

108 Site 042 NILOSYRTIS MENSAE

301 ° W 303 ° W I I

36° N- -36 N

34 ° N-

303 _ W 301.0 W

I I I I I I 50 km

Viking Orbiter (_ Landing Site: 35.5 ° N Latitude, 302.5 ° W Longitude Harold Masursky 569A20

109 ORIGINAL Pt-,u_ _,LACK AND WHITE_ PblOTOGRAPH Site 043 - Candor Chasma I

Site 043 Latitude: 10.5°S Site Name: Candor Chasma I Longitude: 74.5°W Type of Site: Rover/Sample Return Elevation: + 2.5 km

Maps: MC-18 NW Contact: Harold Masursky Viking Orbiter Images: 608A70+72 U.S. Geological Survey 2255 N. Gemini Drive Date Entered: March 1989 Flagstaff, AZ 86001 Date Last Revised: March 1989 (602) 527-7003

Geologic Setting Objectives

Candor Chasma and Melas Chasma are east- Layered rocks in canyon. west trending troughs associated with Valles Potential Problems Marineris. Valles Marineris, known as can- To be determined. yonlands, is made up of grabens, canyons, pit craters and channels. The canyon walls exhibit horizontal layering. Trafficability To be determined. Scientific Rationale Estimated Traverse Distance To be determined. To be determined.

110 Ill

A_sJnselAl PlOJeH epnl!6uo-i M ogt,L 'epnl!le-I £ og'0L"el!s 6u!puel _) _L00 L- V_J.W

M o_L M ogL I I

SoLL - -Soll

SoOL- -So0l

! I M o_L M oSL I VIAISVHO EtOONVO 8170oi!S Site 044 - Tharsis-Oiympus

Site 044 Latitude: 12ON

Site Name: Tharsis-Olympus Longitude: 125°W Elevation: + 4 km Type of Site: Rover/Sample Return

Maps: MC-9 SW CO ntact.• D.H. Scott and K.L. Tanaka Viking Orbiter Images: 045B68 U.S. Geological Survey 2255 N. Gemini Drive Date Entered: March 1989 Flagstaff, AZ 86001 Date Last Revised: March 1989 (602) 527-7188 ,. j

Geologic Setting Objectives

The site lies between Tharsis Montes and Aop, flows of Olympus plains (Aoa_), lower- Olympus Mons. Smooth lava flows of the most aureole of Olympus Mons (Hf), frac- Olympus Mons plains member intersect the tured flows of Ulysses Fossae. older Olympus Mons aureole deposit which is smooth and degraded by wind. The younger Potential Problems fractured material of the highly deformed To be determined. terrain material (Ulysses Fossae) forms relatively smooth raised surfaces of moderate Trafficability relief with fractures, grabens, and collapse depressions. To be determined.

Scientific Rationale Estimated Traverse Distance

To be determined. To be determined.

112 Site 044 THARSIS-OLYMPUS

.UZo

! I ! 20 km

D. Scott and K.L. Tanaka Viking Orbiter Landing Site: 12° N Latitude, 125 ° W Longitude 045B68

lL3 BLACK AND WHITE PriOiOGRAPh Site 045 - Chasma Boreale

Site 045 Latitude: 82"N Site Name: Chasma Boreale Longitude: 57"W Elevation: 0 km Type of Site: Rover/Sample Return

Maps: MC-1, A and B; MTM# 80050 Contact. D.H. Scott and K. L. Tanaka Viking Orbiter Images: 790A25 U.S. Geolo_cal Survey 2255 N. Gemini Drive Date Entered: March 1989 Flagstaff, AZ 86001 Date Last Revised: March 1989 (602) 527_7188 J

Geologic Setting Objectives

Chasma Boreale is a large swirl pattern trough Polar layered material (Apl); grooved plains originating in Planum Boreum. Planum material (Hvg); crater material (c). Boreum is composed of polar ice and polar layered deposits surrounded by thick, smooth Potential Problems to hummocky eolian deposits. The grooved To be determined. member of the Vastitas Borealis Formation subpolar plains deposits exhibits a polygonal Trafficability pattern in the mouth of Chasma Boreale. To be determined.

Scientific Rationale Estimated Traverse Distance To be determined. To be determined.

114 Site 045 CHASMA BOREALE

55° W 50'' W I I

82° N- 82° N

80° N - 80° N

I 55 ° W 50 ° W

I I I I I 50 km

MTM -80050 _) Landing Site: 82 ° N Latitude, 57 o W Longitude D.H. Scott and K.L. Tanaka

115

.... ; ' )C,. BLACI{, Af:.D _,c;,l c. r r_'.., I_J,..r,,_PH Site 046 - Labeatis North

Site 046 Latitude: 31°N Site Name: Labeatis North Longitude: 83°W Elevation: + 2.5 km Type of Site: Rover/Sample Return

top --¸ Maps: MC-3 SE Contact: D.H. Scott and K.L. Tanaka Viking Orbiter Images: 858A03 U.S?Geological Survey 2255 N. Gemini Drive Date Entered: March 1989 Flagstaff, AZ 86001 Date Last Revised: March 1989 (602) 527-7188

Geologic Setting Objectives The site is northeast of the Tharsis Montes Member 2 of Tharsis Montes Fm (Ht2); ridged plains material (Hr); highly deformed near Tempe Fossae. Faults trending north- (faulted) material (Nf). east, which are part of the system of faults radiating from Tharsis Montes, run through Potential Problems this area. Three formations, Tharsis Montes To be determined. formation, ridged plains material, and highly deformed material, are near the landing site. Trafficability To be determined.

Scientific Rationale Estimated Traverse Distance To be determined. To be determined.

116 Site 046 LABEATIS NORTH

84:W 82_.W I I

31ON - -31oN

29 '_N- -29 N

J ! 84 ° W 82 '_W

I I I I I I 50 km

Viking Orbiter _) Landing Site: 31° N Latitude, 83 o W Longitude D.H. Scott and K.L. Tanaka 858A03 ]17 (;:7:',t._ :&t. i:/..__U Site 047 - Labeatis South

Site 047 Latitude: 24°N Site Name: Labeatis South Longitude: 80"W Elevation: + 2.0 km Type of Site: Rover/Sample Return

f Maps: MC-10 NW; MTM# 25077 Contact: D.H. Scott and K.L. Tanaka Viking Orbiter Images: 555A26 U.S. Geological Survey 2255 N. Gemini Drive Date Entered: March 1989 Flagstaff, AZ 86001 Date Last Revised: March 1989 (602) 527-7188 J

Geologic Setting Objectives The site is northeast of Tharsis Montes near Member 4 of Tharsis Montes Fm (At,); member 2 of Tharsis Montes Fm (Ht_); ridged Tempe Fossae. Three formations are close to plains material (Hr). the landing site: smooth flows of member 2 of Tharsis Montes Formation, light flows Potential Problems with dark wind streaks of member 4 of That- To be determined. sis Montes Formation, and ridged plains materials. Trafficability To be determined.

Scientific Rationale Estimated Traverse Distance To be determined. To be determined.

118 e_eUe_L -1>1 pue J4o::)SH(] epnl!6uoq AA o08 'epn;!leq N ot,_ e;!s Bu!pueq _) LLOg_ _IV_

Lu:,t0£

I I l I I (J M °08

, , i, J

.-g r23

N o17_- C, t

I M oog HZnOS SI/V3E]V7 Z#O ells Site 048 - Solis

Site 048 Latitude: 27°S Site Name: Solis Longitude: 100*W Elevation: + 9.0 km Type of Site: Rover/Sample Return

f Maps: MC-17 SE (I-1190)

D.H. Scott and K.L. Tanaka Viking Orbiter Images: 606A14 U.S. Geological Survey 2255 N. Gemini Drive Date Entered: March 1989 Flagstaff, AZ 86001 Date Last Revised: March 1989 (602) 527-7188

Geologic Setting Objectives

Solis Planum, a highly cratered and faulted Lower member of Syria Planum Fm (Hsl); plain, lies to the east of the landing site and older fractured flows (HI'); basement mate- Claritas Fossae runs through the site. Clari- rial (Nb). tas Fossae is an intense fracture zone south of Tharsis, part of the extensive array of roughly Potential Problems radiant fractures surrounding the Tharsis Bulge. These formations intersect at the To be determined. landing site: highly cratered and faulted plains of the lower member of the Syria Planum Formation, a highly deformed ter- Trafficability rain material, and younger fractured mate- To be determined. rial.

Scientific Rationale Estimated Traverse Distance To be determined. To be determined.

120 %

r,g c 0 I-- _i ,d b.. "[3 • L',LJ _J

"- "lZ 0 rJ3 r: 0

0 5

::3

,[Z 03 0 --.I _1 0 o rd3 o E o 00 ,,,¢ 0 o -1 o_ r,./) _1 ruO o I"- 04

0 0 ¢- .-I

E ®

O_ /

"-- ¢,,,0 -4_o ;>co Site 049 - Hadriaca

Site 049 Latitude: 29°S Site Name: Hadriaca Longitude: 269°W Elevation: + 1 km Type of Site: Rover/Sample Return

Maps: MC-28 NE, MC-22 SW, Contact: MC-28 NE D.H. Scott and K.L. Tanaka U.S. Geological Survey Viking Orbiter Images: 629A13, 2255 N. Gemini Drive 629A 16, 629A 18, 106A08 Flagstaff, AZ 86001 (602) 527-7188 Date Entered: March 1989 Date Last Revised: March 1989

Geologic Setting plains material (Hr); mountains of Hellas rim Hadriaca Patera is a central vent volcano material (Nm). northeast of Hellas Planifia, with radial ridges, a low profile, and a smooth floored caldera in Potential Problems the center. The landing site lies on the north- western flank of Hadriaca Patera and inter- To be determined. sects with four formations listed below.

Scientific Rationale Trafficability To be determined. To be determined.

Objectives Estimated Traverse Distance Shield material of Hadriaca Patera (Hhp); smooth unit of plateau sequence (Hpl,); ridged To be determined.

122 C_ --- c_

o oCO co O / 8-

I'O

"-'1

69 D.

co o OO GO

O ___+" C- Q.

1,o I > cO o

o > 0 ]> c- O..

C_ q.- -I _ 09 C_ O ro

o O_

--t O I ro

o 69 Site 050 - Elysium

Site 050 Latitude: 270N

Site Name: Elysium Longitude: 185"W Elevation: - 0.5 km Type of Site: Rover/Sample Return

-N Maps: MC-15 NE Contact: D.H. Scott and K.L. Tanaka Viking Orbiter Images: 545A08, 545A29

2255 N. Gemini Drive Date Entered: March 1989 Flagstaff, AZ 86001 Date Last Revised: March 1989 (602) 527-7188 J

Geologic Setting Objectives The main edifice of Elysium Mons consists Plains flows of Elysium Mons (Aelt); ridged plains material (Hr); knobby remnants of of rilled lobate deposits. Radiating away plateau materials (HNu). from the edifice are lobate plains deposits. The site is located on the far eastern flank of Potential Problems Elysium Mons amid plains, flows, ridged To be determined. plains material and knobby remnants of plateau material. Trafficability To be determined. Scientific Rationale Estimated Traverse Distance To be determined. To be determined.

124 Site 050 ELYSIUM

186° W 185° W I

28° N- - 28° N

26° N- - 26° N

I ! 186o W 185o W

I I I I I .--1 50 km

MC - 15NE (_) Landing Site: 27 ° N Latitude, 185 o W Longitude D.H. Scott and K.L. Tanaka

125 ORiO I;"._AL PAGE 6L,kCK AND WH;iE P;-_OTOGRAPN Site 051- Mareotis Volcanic Field

Site 051 Latitude: 36°N Site Name: Mareotis Volcanic Field Longitude: 88"W Elevation: + 3 km Type of Site: Rover/Sample Return

_r Maps: MTM# 35087:MC-3 SE Contact:

Viking Orbiter Images: 627A45, 857A27

Branch of Astrogeology MS 946 Date Entered: 3 April 1989 345 Middlefield Road Date Last Revised: 3 April 1989 Menlo Park, CA 94025 (415) 329-5175 J

Geologic Setting c) not yet evaluated; Mareotis volcanic field, part of Mareotis d) not yet evaluated. Fossae, is northeast of the Tharsis Bulge. The Tharsis fractures trend northeast through the Potential Problems volcanic field. The site is in Mareotis Fossae andis among rough hilly material and smooth, Unknown at this time. light-colored, partly mottled material.

Scientific Rationale Trafficability Establish relations between volcanism, tec- To be determined. tonism, and fractured terrain.

Objectives Estimated Traverse Distance a) Sample volcanic materials; b) sample old fractured terrain materials; To be determined.

126 Site 051 MAREOTIS VOLCANIC FIELD

90 ° W 88 ° W I I

37 ° N -

tO _j

Cb ;:;q

_.o

_'2_ ;_:

r,J [- 35 ° N- =- _ | ! r_, 90 ° W 88 ° W O I I I I I I c,) _3 50 km ):,

Viking Orbiter 857A27 _ Landing Site: 36 ° N Latitude, 88 ° W Longitude Henry J. Moore Site 052- Tempe Volcano

Site 052 Latitude: 39"N Longitude: 760W Site Name: Tempe Volcano Elevation: + 1.8 km Type of Site: Rover/Sample Return

Maps: MTM# 40077:MC-3 SE Contact:

Viking Orbiter Images: 704B52 Branch of Astrogeology MS 946 Date Entered: 3 April 1989 345 Middlefield Road Date Last Revised: 3 April 1989 Menlo Park, CA 94025 (415) 329-5175

Geologic Setting b) sample volcanic flow materials (0.98 success rate); The Tempe volcano is in Tempe Fossae, c) not yet evaluated; northeast of Tharsis Montes. The landing d) not yet evaluated. site lies in highly deformed material with complexly oriented faults, fractures, and Potential Problems collapse depressions. Unknown at this time. Scientific Rationale

Establish relations between volcanism, tec- Trafficability tonism, and fractured terrain. To be determined.

Objectives Estimated Traverse Distance a) Sampleoldfractured terrain material (0.99 To be determined. success rate);

128 Site 052 TEMPE VOLCANO

76° W 74 ° W I I

39° N - -39ON

37 ° N - -37°N

I I 76° W 74° W

I I I I I I 50 km

Viking Orbiter _) Landing Site: 39 ° N Latitude, 76 o W Longitude Henry J. Moore 704B52

129 ORIGINAL PAISE BLACK AND WHITE F'H_, i L)GRAP_ Site 053- Ceraunius Fossae Volcanic Field

Site 053 Latitude: 20°N Site Name: Ceraunius Fossae Volcanic Longitude: 112ow Elevation: + 5 km Field Type of Site: Rover/Sample Return f Contact: .... Maps: MTM# 20112:MC-9 NE Henry J. Moore U.S. Geological Survey Viking Orbiter Images: 516A34 Branch of Astrogeology MS 946 345 Middlefield Road Date Entered: 3 April 1989 Menlo Park, CA 94025 Date Last Revised: 3 April 1989 (415) 329-5175 J

Geologic Setting b) sample old fractured terrain materials (0.98 success rate); Ceraunius Fossae Volcanic Field, south of c) not yet evaluated; Alba Patera, consists of a series of overlap- d) not yet evaluated. ping flows whose surfaces are relatively smooth and even-toned to mottled and Potential Problems streaked. Ceraunius Fossae, highly deformed terrain material, lies east of :he landing site. Unknown at this time.

Scientific Rationale Trafficability

Establish relations between volcanism, tec- To be determined. tonism, and fractured terrain. Estimated Traverse Distance

Objectives To be determined. a) Sample volcanic materials (0.99 success rate);

130 Site 053 CERAUNIUS FOSSAE VOLCANIC FIELD

114ow 112°W

21° N....

-21 ° N

19 ° N-

419° N

I ! 114°W 112°W

I I I | I I 50 km

Viking Orbiter 516A34 ® Landing Site: 20 ° N Longitude, 112°W Latitude Henry J. Moore

131

p i--_ c.-

BLACK Ai'_D Wri,i-E=" i-'_ilb.... J_,_-,APH'-".... '_' Site 054- Candor

Site 054 Latitude: 5.5°S Site Name: Candor Longitude: 74.5°W Elevation: + 2 km Type of Site: Rover/Sample Return

Maps: MTM# 05072; MC- 18 NW Contact: Eleanora I, Robbins Viking Orbiter Images: 561A26, 561A27 U.S. Geological Survey 927 National Center MS 956 Date Entered: May, 1989 Reston; VA 22092 Date Last Revised: May, 1989 (703) 648-6527 J

Geologic Setting for morphologically distinct Fe and Mn ox- Candor Chasma is an east-west trending ide minerals that might have been precipi- trough associated with Valles Marineris. tated by ancient iron bacteria. (Success is Valles Marineris, known as Canyonlands, is unknown regarding presence of bacteria. made up of grabens, canyons, pit craters and Location easily reached.) channels. The canyon walls exhibit horizontal layering. Potential Problems Scientific Rationale Landing inside Valles Marineris troughs. If site was locus of ground water discharge in the past, then microbial minerals precipitated by ancient iron bacteria might be concen- Trafficability trated at heads of channels, at sapping sites, lto2. and along base of valley wall scarps.

Objectives Estimated Traverse Distance To collect weakly indurated iron ore at red and black patches to scan with microscope 50 km.

132 Site 054 CANDOR 75 ° W 74°_W !

-5 ° S S° S -

L,o

r-- 3_ C)

-6 ° S 6 ° S ° 3: Z

"o ''¢j

C. rq --I C_3 57 75 ° W 74 ° W :::o

I "O I I I I I 50 km

MTM 05072 Landing Site: 5.5 ° S Latitude, 74.5 ° W Longitude Eleanora I. Robbins Site 055- Northern Cydonia/SE Acidalia

Site 055 Latitude: 40°N

Site Name: Northern CydoniaJSE Longitude: 10"W Acidalia Elevation: - 0.5 km Type of Site: Rover/Sample Return

r Contact: Maps: MC-4 SE Paul Etzler Geospectra Corp. Viking Orbiter Images: 561A07, P.O. Box 1387 561A24, 561A26, 637B54, 637B56 Ann Arbor, MI 48106 (313) 994-3450 Date Entered: May, 1989 Date Last Revised: May, 1989

Geologic Setting Potential Problems

The site is on the southeast margin of Acidalia Sampling area consists of smooth plains. Planitia and on the northern edge of the Debris from erosional remnants may cause highland-lowland boundary. Nearby materi- some problems. Fractured terrain may be als include the Vastitas Borealis grooved difficult to traverse, but need only be sampled member, hummocky undivided material, at edges. Erosional remnants may cause Plateau Sequence cratered unit, and Arcadia some problems when landing, but should be Formation flows with lobate margins. avoidable. Sampling operations should be Scientific Rationale simple. Contact between northern plains and southern cratered highlands. Trafficability

Objectives mostly 1; maybe some 5. Sample northern plains, fractured terrain, base of cratered highland remnants (may measure Estimated Traverse Distance time sequence of debris aprons), volcanic cons.tructs, and pseudocraters. 100 km.

134 Site 055 NORTHERN CYDONIA/SOUTHEAST ACIDALIA

10 ° W I

40 ° N- - 40 ° N

I 10°W

! I I I l J 50 km

MC - 4SE (_ Landing Site: 40 ° N Latitude, 10 ° W Longitude Paul Etzler 135

O_;G', ?"At. _/f ,__'.3r,:_"I-- BLACK AND V,/r-i,1_-'-.,- t-;IqGTOS;-_APt4 Site 056- Tharsis-Olympus

Site 056 Latitude: 12.5°N

Site Name: Tharsis-Olympus Longitude: 125.5°W Elevation: + 3.5 km Type of Site: Rover/Sample Return

Maps: MC-9 SW

Viking Orbiter Images: 890A41, 045B68

2255 N. Gemini Drive Date Entered: July, 1989 Flagstaff, AZ 86001 Date Last Revised: July, 1989 (602) 527-7188

Geologic Setting b) Highly deformed terrain materials (unit I/f) consisting of fractured crustal rocks Landing site lies between Olympus Mons, an (success excellent; appear to be acces- enormous shield volcano, and Tharsis Mon- sible within about 15 km from landing tes, the three large shield volcanoes of the site); Tharsis bulge. The site is on the edge of an c) Aureole deposits, lower member (unit aureole lobe southeast of Olympus Mons, Aoa_) of Olympus Mons (success excel- one of several lobes of ridged terrain that lent; within 15 km or less range from extend several hundred kilometers out from landing site). the base of Olympus Mons.

Potential Problems Scientific Rationale Lack of high-resolution (<50 rn/pxl) images To obtain samples of very young (Upper to better assess smoothness of landing area Amazonian) lava flows and intermediate age and mobility of rover to other location objec- (Hesperian) rocks together with materials tives. forming aureole deposits of Olympus Mons.

Trafficability Objectives 2. a) Lava flows of upper member (unit Aopl ) of Olympus Mons Formation (success Estimated Traverse Distance excellent; landing site smooth-appearing plains); 30-1- km.

136 Site 056 THARSIS OLYMPUS

125°W !

-12_N

t4 12ON -

i 125°W

I I I I -J 50 km

David Scott Viking Orbiter (_ Landing Site: 12.5 ° N Latitude, 125 ° W Longitude 890A41

137 ORIGINAL F,,,.___ BLACK AND WHITE PHO_FOGRAPH Site 057- Labeatis

Site 057 Latitude: 25-30°N Site Name: Labeatis Longitude: 81-83"W Type of Site: Rover/Sample Return Elevation: + 2.5 km

f Maps: MC-10 NW Contact: David Scott Viking Orbiter Images: 858A05, U.S. Geological Survey 858A03, 555A28 2255 N. Gemini Drive Flagstaff, AZ 86001 Date Entered: July, 1989 (602) 527-7188 Date Last Revised: July, 1989

Geologic Setting Planum (success excellent; terrain appears featureless and flat); Landing site consists of several possible sites Lava flows (unit Hr) of Lunae Planum; along the linear contact between flows from b) Tharsis and flows from Lunae Planum. The most widespread plains type of lava flows on Mars. Age very important for Mars area is cut by faults radiating outward from chronology (success excellent; same as the Tharsis bulge. above with more faulting and small crater density). Scientific Rationale

Nearly linear contact extending for 300+ km Potential Problems between young Hesperian (unit Ht2) lava flows from Tharsis (probably Ascraeus Mons) None envisioned, but high resolution images not available. and early Hesperian lava flows (unit Hr) of Lunae Planum. Trafficability

Objectives 2. a) Lava flows (unit Ht2) from Tharsis Mon- tes; these flows overlap (unconformably) Estimated Traverse Distance the ridged plains (unit Hr) flows of Lunae <30 km.

138 Site 057 LABEATIS

84ow 81 °W U I

29ON -- -29:N

26oN- "26':'N

| I 84ow 81 °W

l I I I I I 50 km

Viking Orbiter _) Landing Site: 25 °- 30 ° N Latitude, 81°- 83° W Longitude David Scott 858A05 ]39

CT, T_._:i,', I-'_,'.t.f F _,t,'."_k]_; ,'zL,- I:_LA,_._*l f_: t AND ,,t , r,,,_ -" _.r- PHL; i OGRAPH Site 058- Chryse Planitia/Viking 1

Site 058 Latitude: 22.52°N

Site Name: Chryse Planitia/Viking 1 Longitude: 47.97°W Elevation: - 2.2 km Type of Site: Rover/Sample Return

f Maps: MTM# 20047, 25047 Contact: Robert A. Craddock Viking Orbiter Images: 20A44 through CEPS/NASM 3101 20A53; 20A66 through 20A75; 452B10, Smithsonian Institution 452B 11 Washington, D.C. 20560 (202) 357-1457 Date Entered: July, 1989

Date Last Revised: July, 1989 J

Geologic Setting materials will influence the age of all other martian geologic units (success: This site is dominated by Hesperian ridged very high; depends on successful landing plains material with wrinkle ridges (Xanthe of rover and return vehicle, which is Dorsa) that trend north-south. The Hesperian aided by surface photographs obtained ridged plains are one of the most extensive by Viking 1); units mapped on Mars. b) target B; obtain ejecta sample from crater Scientific Rationale formed by jettisoned Viking aeroshell located approximately 1 km south of the Obtain sample of Hesperian ridged plains, proposed landing site (or approximately one of the most extensive units on the martian 1 km north of the Viking 1 landing site). surface, and to conduct further scientific Collected samples would represent mate- investigations in the vicinity of the Viking 1 rial to a depth of about 2 m, eliminating lander. Design of the spacecraft is aided by the need for a drill aboard the rover "ground truth" observations made by the (success: high; depends on targeting abil- Viking lander, elevation of landing site, and ity before and after landing); latitude (i.e., line-of-site communication). c) target C; obtain sample of the Viking 1 lander (e.g., sampler shroud) to deter- Objectives mine weathering rates on Mars, obtain a) Target A; land 2 km north of the Viking soil/rock samples from Viking landing 1 landing site at 22.52 °, 47.97 °. Obtain site, conduct range of complementary contingency sample of Hesperian-age science experiments in the vicinity of the ridged plains, which compose one of the lander, photograph the lander, and send most extensive geologic units on Mars. radio commands to turn lander antennae Geologic mapping indicates that the age back towards Earth (success: high; de- of the ridged plains represents the end of pends on ability to direct rover to Viking the period of heavy bombardment on 1 position. Trafficability will be poor Mars, so that an absolute age of these based on Viking photographs, but rover

140 will probablybe designedto copewith volatiles in target material). Observe this typeof terrain). Returnto landing distribution of coarse/finematerialdur- site(targetA) beforebeginningthesec- ing traversetodeterminepossibleChryse ond phaseof themission; channel-formingmechanism(s)(success: d) targetD; obtainsamplesofXantheDorsa high to moderate;dependson durability ridge from proposedlandingsiteto San of rover). Returnto landing site(target Juancrater. Photographsof theridgein A) to completesecondphaseof themis- variousplacesmayaidin theunderstand- sion. ing of ridge formation. Ejectamaterial from SanJuanwould representmaterial Potential Problems

to a depthof approximately50 m (suc- To be determined. cess:high; dependson theperformance of the roving vehicle in rocky terrain. Navigationshouldbe aidedby thepres- Trafficability enceof thewrinkle ridge); 3. e) targetE; obtainejectasamplesfrom the rampartcrater,Yorktown, to determine Estimated Traverse Distance possible ejecta flow mechanism(e.g., 100 km.

141 Site 058 CHRYSE PLANITIA/VIKING 48o'w

-23 ° N

.3: _

_.i_. r _ - 22 ° N CJ

48JW

I I I I 30 km

MTM 20047 and MTM 25047 (_ Landing Site 22.52 ° N Latitude, 47.97 ° W Longitude Robert A. Craddock Site 059- Amenthes Southeast

Site 059 Latitude: 4°N Longitude: 247"W Site Name: Amenthes Southeast Elevation: + 1 to + 2 km Type of Site: Penetrator Contact: Maps:MC-14 SE, SW US/Soviet Landing Site Working Grp. Michael Carr Viking Orbiter Images: U.S. Geological Survey, MS 946 Branch of Astrogeological Studies Date Entered: 25 July 1989 345 Middlefield Road Date Last Revised: 25 July 1989 Menlo Park, CA 94025 (415) 323-8111

Geologic Setting global in conjunction with other penetrators), meteorology, and photogeology. Heavily cratered terrain southwest of Nepen- thes Mensae with old degraded craters and Potential Problems rough intercrater surface resulting from eolian and fluvial erosion. Old highland mate- To be determined. rial with fluvial and eolian material inside the craters. Trafficability Not applicable. Scientific Rationale

Ancient highlands. Estimated Traverse Distance Not applicable. Objectives

Obtain composition of ancient highlands Other material, local seismic information (possibly Landing circle size is 150 km radius.

143 Site 059 AMENTHES SOUTHEAST

250 ° W 245 ° W

.5ON

S°N -

7" "- r,.:: --

..... j .... _ ;_

| i 250 ° W i I _ I I I 245 ° W 100 km

MC - 14 SE and SW (_ Landing Site" 4° N Latitude, 247 ° W Longitude U.S./Soviet Group Site 060- Isidis North

Site 060 Latitude: 36"N to 16°N Site Name: Isidis North Longitude 282"W to 267"W Elevation: - 1 km to + 2 krn Type of Site: Balloon

Contact: Maps: MC-6 SE, SW; MC-13 NE; US/Soviet Landing Site Working Grp. MC-14 NW; l:15M (I-1321) Michael Carr U.S. Geological Survey, MS 946 Viking Orbiter Images: Numerous Branch of Astrogeological Studies images 345 Middlefield Road Menlo Park, CA 94025 Date Entered: 25 July 1989 (415) 323-8111 Date Last Revised: 25 July 1989

Geologic Setting plains, grooved member of Vastitas Borealis Formation (lava flows, alluvium which have The area is located northeast of Syrtis Major, undergone compaction or periglacial proc- a low relief volcano. The area is cut by esses). graben (Nili Fossae) which trend southwest- northeast. To the southeast is Isidis Planitia, Potential Problems an ancient impact basin. To be determined. Scientific Rationale

Geologic and meteorologic assessment of Trafficability the Isidis basin. To be determined.

Objectives Estimated Traverse Distance

Obtain composition of ancient plateau se- To be determined. quence, knobby plains (volcanic?), smooth

145 Site 060 ISIDIS NORTH

280ow 270°W i !

30°N . -30ON

20ON • - 20ON

i 280'°W 270ow

I I I I I 200 km

1:15 M USGS 1-1321 Site: 16°N-36°N Latitude, 267°W-282 ° W Longitude U.S./Soviet Group

146 Site 061- Arabia

Site 061 Latitude: 30°N Longitude: 327°W Site Name: Arabia Elevation: + 1 to + 2 km Type of Site: Penetrator

Contact: Maps: MC-5 SC, MC-12 NE US/Soviet Landing Site Working Grp. Michael Carr Viking Orbiter Images: U.S. Geological Survey, MS 946 Branch of Astrogeological Studies Date Entered: 25 July 1989 345 Middlefield Road Date Last Revised: 25 July 1989 Menlo Park, CA 94025 (415) 323-8111

Geologic Setting (possibly global in conjunction with other Site lies on ancient ridged plains,just north of penetrators), meteorology, and photogeol- the large crater Cassini. Ridged plains mate- ogy. rial is interpreted to be of volcanic origin. Impact crater density is high and implies Potential Problems Noachian age. If the volcanic interpretation is correct, these are some of the oldest vol- To be determined. canic materials on the planet. Because of the substantial age of the region, geologic modi- Trafficability fication may have been quite significant; in particular, crater-filling sediments and crater Not applicable. ejecta deposits excavated from below the ridged plains material may be common. Estimated Traverse Distance Scientific Rationale Not applicable. Ancient volcanics, ridged plains.

Objectives Other Obtain composition of ancient volcanics, Landing circle size is 150 km radius. ridged plains, local seismic information

147 Site 061 ARABIA

329°W 325ow I I

32°N. -32ON

28oN - -28ON

329°W 325°W

I I i I I I 100 km

MC -12NE and 5SC _) Landing Site: 30 ° N Latitude, 327 ° W Longitude U.S./Soviet Group 148 Site 062- Hadriaca

Site 062 Latitude: 36"S Site Name: Hadriaca Longitude: 271"W Elevation: 0 to + 1 km Type of Site: Penetrator

Contact: Maps: MC-28 NW, NE US/Soviet Landing Site Working Grp. Michael Carr Viking Orbiter Images: U,S. Geological Survey, MS 946 Branch of Astrogeological Studies Date Entered: 25 July 1989 345 Middlefield Road Date Last Revised: 25 July 1989 Menlo Park, CA 94025 (415) 323-8111

Geologic Setting in conjunction with other penetrators), mete- Northeast margin of Hellas basin composed orology, and photogeology. ofvolcanics ofHadriaca Patera. The smooth- ened plain-like surface tilted to southeast is Potential Problems complicated by southwest-northeast grooves. At southeast the plain is dissected by Dao To be determined. Vallis, at northwest the relic of highly cratered terrain. Volcanic material (possibly pyro- Trafficability clastic) of intermediate age, material of cratered highland, lahar deposits. Not applicable.

Scientific Rationale Estimated Traverse Distance Intermediate volcanics. Not applicable. Objectives Other Obtain composition of intermediate volcanics, local seismic information (possibly global Landing circle size is 150 km radius.

149 Site 062 HADRIACA 272.5 ° W 267.5 ° W !

- 32.5oS

tJi O

I;0

3L" ;':"

C; i/: 0 -37.5, S C,)

| i 272.5 ° W 267.5 ° W I I I I I I 100 km

ASU - IPF 710 _) Landing Site: 36 ° S Latitude, 271 ° W Longitude U.S./Soviet Group Site 063- Arabia South

Site 063 Latitude: 15°N Site Name: Arabia South Longitude: 3330W Elevation: ÷ 1 to + 2 km Type of Site: Penetrator

f • Contact: Maps: MC- 12 SE, NE US/Soviet Landing Site Working Grp. Michael Cart Viking Orbiter Images: U.S. Geological Survey, MS 946 Branch of Astrogeological Studies Date Entered: 25 July 1989 345 Middlefield Road Date Last Revised: 25 July 1989 Menlo Park, CA 94025 (415) 323-8111

Geologic Setting global in conjunction with other penetrators), The site is located within the ancient cratered meteorology, and photogeology. highlands. This is one of the few areas of the cratered highlands that lies below the +2 km Potential Problems contour. The area is dissected by numerous finely branching river valleys and the area To be determined. between the large craters is gently roiling, thereby indicating that younger intercraters Trafficability plains are largely absent, and that the old highland surface is exposed. Not applicable.

Scientific Rationale Estimated Traverse Distance Ancient highlands. Not applicable.

Objectives Other Obtain composition of ancient highland material, local seismic information (possibly Landing circle size is 150 km radius.

151 Site 063 ARABIA SOUTH

335°W 330°W

•18°N 18ON .

.12°N 12°N"

.....i-';_ :

! i 335°W 330°W

I I I I I I 100 km

MC -12NE and SE _) Landing Site: 15 ° N Latitude, 333 ° W Longitude Steve Squyres

]52 ORIO-_NAL P,_,:,:- BLACK AND WHITE PHOTOGRAPh Site 064- Isidis Planitia

Site 064 Latitude: 10°N Site Name: Isidis Planitia Longitude: 275°W Elevation: - 2 to - 3 km Type of Site: Penetrator

r Contact: "_ Maps: MC-13 SE US/Soviet Landing Site Working Grp.[ Michael Cart l Viking Orbiter Images: U.S. Geological Survey, MS 946 l Branch of Astrogeological Studies l Date Entered: 25 July 1989 345 Middlefield Road l Date Last Revised: 25 July 1989 Menlo Park, CA 94025 l (415) 323-8111 )

Geologic Setting conjunction with other penetrators), meteor- Site lies on the floor of the Isidis basin on ology, and photogeology. volcanic plains of intermediate age. Distinct lava flows are not observed. The area is Potential Problems dominated by numerous small cones, presumed to be volcanic in origin, aligned in To be determined. chains as if above curvilinem" fissure vents. Cones frequently have elongate pits at their Trafficability summits. Post-volcanic mantling in this region appears minor. Not applicable.

Scientific Rationale Estimated Traverse Distance Small volcanic cones. Not applicable.

Objectives Other Obtain composition of volcanic materials, local seismic information (possibly global in Landing circle size is 150 km radius.

153 Site 064 ISIDIS PLANITIA

275°W

10°N. -10ON

5ON - - 5ON

i 275°W

I I i t I I 100 km

MC -13SE (_ Landing Site: 10 ° N Latitude, 275 ° W Longitude U.S./Soviet Group

]54

BLACK AND '¢VHtTE '; .... " "_-_,'.-, Site 065- Utopia

Site 065 Latitude: 45°N Longitude: 251°W Site Name: Utopia Elevation: - 2 to - 3 km Type of Site: Pcnetrator r Contact: Maps: MC-6 SE US/Soviet Landing Site Working Grp. Michael Cart Viking Orbiter Images: U.S. Geological Survey, MS 946 Branch of Astrogeological Studies Date Entered: 25 July 1989 345 Middlefield Road Date Last Revised: 25 July 1989 Menlo Park, CA 94025 (415) 323-8111

Geologic Setting Objectives Site lies at a low elevation on Utopia Planitia. Obtain composition of sediments (aqueous, volcanic, aeolian?), determine if ground ice This region is believed to be the primary site is present, local seismic information (possi- of deposition for water and mud flows that bly global in conjunction with other penetra- were produced by volcano-ground ice inter- tors), meteorology, and photogeology. actions in the Elysium region to the southeast. Waterlain sediments may be the domi- Potential Problems nant materials at the site. In addition, the high To be determined. latitude of the site substantially improves the possibility that ground ice could be preserved. Trafficability Post-fluvial modification of the area of various sorts has probably taken place, and vol- Not applicable. canic and eolian materials may also be present along with aqueous sediments. Estimated Traverse Distance Not applicable. Scientific Rationale Other Sediments, ground ice, lahars(?) from Ely- sium. Landing circle size is 150 km radius.

155 0 C_ :7 I I 6_ 0O m

7 O_

7 ro

O0 __° CD O0 O1 m. o Z CD r-" 0 C7_ 0 0 On

cD 3 C _J DO -H

o 0

o 7

,.-e. _L .- • c Q_ CD

CD r _,7 •

0 . C on

Go c)

CD © 3 c

z Site 066- Elysium Southwest

Site 066 Latitude: 17°N Longitude: 224°W Site Name: Elysium Southwest Elevation: - 1 to 0 km Type of Site: Penetrator f Contact: Maps: MC-15 NW, MC-14 NE US/Soviet Landing Site Working Grp. Michael Cart Viking Orbiter Images: U.S. Geological Survey, MS 946 Branch of Astrogeological Studies Date Entered: 25 July 1989 345 Middlefield Road Date Last Revised: 25 July 1989 Menlo Park, CA 94025 (415) 323-8111 ./ !

Geologic Setting bly global in conjunction with other penetrators), meteorology, and photogeology. 700 km southwest of summit of Elysium Mons on Member 1 (oldest unit) of the Ely- sium Formation. Consists of lobate, plains- Potential Problems forming deposits that overlie and embay units from Albor Tholus and Hecates Tholus. To be determined. Ellipse includes relatively fresh impact craters, some as large as 50 km. Wind streaks Trafficability indicate presence of aeolian material. Bright Not applicable. streaks show winds predominantly from the east. Estimated Traverse Distance Scientific Rationale Not applicable. Flows, intermediate volcanic.

Objectives Other Obtain composition of intermediate volcanic materials, local seismic information (possi- Landing circle size is 150 km radius.

157 Site 066 ELYSIUM SOUTHWEST

227°W 221°W I I

20ON _ 20°N

16°N - -16°N

I i 227°W 221 °W I I I I I I 100 km

MC -14NE and 15NW (_ Landing Site: 17 ° N Latitude, 224 ° W Longitude U.S./Soviet Group

158

6L.A,CK A,r',.;5 ''_/VUqi ...... i ,,-. t" J _ i *.,"'J _p-,_"l'i Site 067- Elysium South

Site 067 Latitude: 7"N to 4"S Site Name: Elysium South Longitude: 232"W to 205"W Elevation: - 1 km to + 2 km Type of Site: Balloon r Contact: Maps: MC-14 SE, MC-15 SW, US/Soviet Landing Site Working Grp. MC-22 NE, MC-23 NW; l:15M (I-1321) Michael Carr U.S. Geological Survey, MS 946 Viking Orbiter Images: Numerous Branch of Astrogeological Studies images 345 Middlefield Road Menlo Park, CA 94025 Date Entered: 25 July 1989 K. (415) 323-8111 Date Last Revised: 25 July 1989

Geologic Setting and pyroclastics, and fluvial deposits, mete- The area is located southwest of Elysium orology, and photogeology. Mons, a large shield volcano. The area is predominantly smooth plains with young Potential Problems channels and flood plains located to the east. To be determined. Scientific Rationale Geologic and meteorologic assessment of Trafficability northern plains and its boundary with the To be determined. southern cratered uplands.

Objectives Estimated Traverse Distance Obtain composition of smooth plains, an- To be determined. cient plateau sequence possible lava flows

159 Site 067 ELYSIUM SOUTH

230°W 220°W e t 210,°W

TO ! I 230°W 220'ow 21 O°W

:.q:_ rq F- I i J I I 200 km C._ r_t -ff O 63

"13 1:15 M USGS 1-1321 Site: 4°S-7°N Latitude, 205°W-232 ° W Longitude U.S./Soviet Group Z Site 068- Medusae Fossae

Site 068 Latitude: 2"S Longitude: 159"W Site Name: Medusae Fossae Elevation: + 1 to + 2 km Type of Site: Penetrator f Contact: Maps: MC-16 NW, NE US/Soviet Landing Site Working Grp. Michael Cart Viking Orbiter Images: U.S. Geological Survey, MS 946 Branch of Astrogeological Studies Date Entered: 25 July 1989 345 Middlefield Road Date Last Revised: 25 July 1989 Menlo Park, CA 94025 (415) 323-8111

Geologic Setting terrain?), local seismic information (possibly The site is located entirely within a thick, global in conjunction with other penetrators), easily erodible sedimentary deposit that meteorology, and photogeology. overlies volcanic plains and highlands in the area. The origin of these deposits is contro- Potential Problems versial. One possibility is that the deposits are thick sequences of pyroclastic deposits of To be determined. ignimbrites. Another hypothesis is that they are analogous to the present polar layered Trafficability terrain and formed when one of the poles was at this location. If ignimbrites, the deposits Not applicable. may have formed as a result of more silicic volcanism than the lava plains. Estimated Traverse Distance Scientific Rationale Not applicable. Volcanics (silicic?).

Objectives Other Obtain composition of volcanics (silicic?) Landing circle size is 150 km radius. and composition of sediments (polar layered

161 Site 068 MEDUSAE FOSSAE 162 ° W i 155 ° W i

3os - -3os

r-- ¢'b

r.2 _] 6oS -

-f : --., -6os

U] I-" "t.,..:_'J

| "0 162 ° W i t I t I I • 155 ° W 100 km

MC - 16NE and NW (_ Landing Site 2 ° S Latitude, 159 ° W Longitude U.S./Soviet Group Site 069- Olympus South

Site 069 Latitude: 1 I°N Longitude: 137°W Site Name: Olympus South Elevation: + 1 to + 2 km Type of Site: Penetrator Contact: Maps: MC-8 SE, MC-9 SW US/Soviet Landing Site Working Grp. Michael Carr Viking Orbiter Images: U.S. Geological Survey, MS 946 Branch of Astrogeological Studies Date Entered: 25 July 1989 345 Middlefield Road Date Last Revised: 25 July 1989 Menlo Park, CA 94025 (415) 323-8111 ,, J

Geologic Setting conjunction with other penetrators), meteor- 300 krn south-southwest of Olympus Mons ology, and photogeology. scarp. Consists of young volcanic plains member of the Olympus Mons Formation; Potential Problems includes lobate to smooth lava flows possibly erupted from fissure vents. Bright wind To be determined. streaks indicate presence of windblown material and winds predominantly from the Trafficability east. Relatively few superposed impact craters. Not applicable.

Scientific Rationale Estimated Traverse Distance

Young volcanics. Not applicable.

Objectives Other Obtain composition of volcanic materials, Landing circle size is 150 km radius. local seismic information (possibly global in

163 Site 069 OLYMPUS SOUTH

140°W 135°W I I

14°N -14ON

-9oN 9oN

140°W 135°W

i I i I I I 100 km

MC - 8SE and 9SW _) Landing Site: 11 ° N Latitude, 137 ° W Longitude U.S./Soviet Group

164

BLACK Ai',;D ''¥,l_-ii ":i t...... i" ti J i o__',,._1"_1ii"1"l Site 070- Alba West

Site 07O Latitude: 45"N Site Name: Alba West Longitude: 1260W Elevation: + 1 km Type of Site: Penetrator r Contact: Maps: MC-2 SE US/Soviet Landing Site Working Grp. Michael Cart Viking Orbiter Images: U.S. Geological Survey, MS 946 Branch of Astrogeological Studies Date Entered: 25 July 1989 345 MiddlefieldRoad Date Last Revised: 25 July 1989 Menlo Park, CA 94025 (415)323-8111

Geologic Setting information (possibly global in conjunction with other penetrators), meteorology, and Site lies on volcanic plains of intermediate photogeology. age, west of Alba Patera. Volcanic flow fronts are observed, but are less distinct than Potential Problems on younger Alba volcanic materials. Low To be determined. ridges may indicate that flows were tube-fed. Some eolian mantling of the flows is likely, and the high latitude suggests that ground ice Trafficability could be present. Not applicable.

Scientific Rationale Estimated Traverse Distance Intermediate volcanics. Not applicable.

Objectives Other

Obtain composition of volcanic material, Landing circle size is 150 km radius. detect ground ice if present, local seismic

165 Site 070 ALBA WEST 125 ° W

-45ON

O',

'LT,J t'-"

7 L: _-/: -40ON

f',)

3, t

125 ° W I 1 I I I I 100 km

MC - 2SE (_ Landing Site: 45 ° N Latitude, 126 ° W Longitude U.S./Soviet Group Site 071- Kasei South (Euchus Chasma)

Site 071 Latitude: 10"N Site Name: Kasei South (Euchus Chasma) Longitude: 80"W Elevation: + 1 km to 0 km Type of Site: Penetrator

Contact: Maps: MC-10 SW US/Soviet Landing Site Working Grp. Michael Cart Viking Orbiter Images: U.S. Geological Survey, MS 946 Branch of Astrogeological Studies Date Entered: 25 July 1989 345 Middlefield Road Date Last Revised: 25 July 1989 Menlo Park, CA 94025 (415) 323-8111

Geologic Setting formation (possibly global in conjunction with other penetrators), meteorology, and Young volcanic plains of Tharsis; consists of photogeology. Member At5 of the Tharsis Montes Forma- tion; smooth to lobate flows from the west Potential Problems (some of the youngest of the Tharsis area). Bright wind streaks suggest aeolian deposits To be determined. and winds predominantly from the west- southwest. Eastern third of landing ellipse is Trafficability in the channel of Euchus Chasma. Not applicable.

Scientific Rationale Estimated Traverse Distance

Young volcanics. Not applicable.

Objectives Other

Obtain composition of volcanic material and Landing circle size is 150 km radius. possibly fluvial sediments, local seismic in-

167 Site 071 KASEI SOUTH (EUCHUS CHASMA)

82oW 75oW I I

13ON -

7oN -

i 82°W 75 W

I I I I I I

1 O0 km

MC -10SW {_) Landing Site: 10° N Latitude, 80 ° W Longitude U.S./Soviet Group ]68 Site 072- Candor Chasma II

Site 072 Latitude: 6°S Site Name: Candor Chasma II Longitude: 73°W Elevation: 0 km to - 1 km Type of Site: Penetrator

Contact: Maps: MC- 18 NW US/Soviet Landing Site Working Grp. Michael Carr Viking Orbiter Images: U.S. Geological Survey, MS 946 Branch of Astrogeological Studies Date Entered: 25 July 1989 345 Middlefield Road Date Last Revised: 25 July 1989 Menlo Park, CA 94025 (415) 323-8111 ,. J

Geologic Setting conjunction with other penetrators), meteorology, and photogeology. The site straddles both Ophir and Candor Chasmas. The areas covered have several kilometers of relief from the floors of the Potential Problems canyons to the volcanic plateau in which the To be determined. canyons are cut. Within the canyons is a thick sequence of sediments that is believed to be waterlain. The main interest of the site is the Trafficability waterlain sediments of intermediate age. Not applicable.

Scientific Rationale Estimated Traverse Distance Sediments, igneous rocks(?). Not applicable.

Objectives Other Obtain composition of sediments (aqueous?), local seismic information (possibly global in Landing circle size is 150 km radius.

169 Site 072 CANDOR CHASMA TI-

75°W 70:W I I

-5os 5oS

.lO_S 10'S -

I I I I I I IO0 km

MC -18NW _) Landing Site: 6 ° S Latitude, 73 ° W Longitude U.S./Soviet Group

170

6LACK AND WHITE Fr_ _O_r_AP_ Site 073- Lunae Planum East

Site 073 Latitude: 16°N Site Name: Lunae Planum East Longitude: 63°W Elevation: + 1 km to + 2 km Type of Site: Penetrator Contact: Maps: MC-10 SE, NE US/Soviet Landing Site Working Grp. Michael Carr Viking Orbiter Images: U.S. Geological Survey, MS 946 Branch of Astrogeological Studies Date Entered: 25 July 1989 345 Middlefield Road Date Last Revised: 25 July 1989 Menlo Park, CA 94025 (415) 323-8111

..... J

Geologic Setting penetrators), meteorology, and photogeology. Site is 450 krn west-southwest of boundary with Chryse Planitia. Ridged plains of pre- Potential Problems sumed volcanic origin (lunar mare-type; flood lavas?). Ridges trend north-south; fresh To be determined. impact craters to 30 km in diameter occur within the ellipse. Trafficability Not applicable. Scientific Rationale

Ridge plains, intermediate volcanics. Estimated Traverse Distance Not applicable. Objectives

Obtain composition of ridged plains, vol- Other canic material, local seismic information Landing circle size is 150 km radius. (possibly global in conjunction with other

171 Site 073 LUNAE PLANUM EAST

65ow 57ow

20ON - - 20oN

11ON - -llON

i 65°W 57°W

I I 1 I I I 100 km

MC -10NE and SE (_ Landing Site: 16 ° N Latitude, 63 ° W Longitude U.S./Soviet Group

]72

[..) :b.'_ix _,_. i * _ BLACK A[,_D '_,'i-;17L_ _-_;,..:, C&'iJ,i--t, Site 074- Capri Chasma

Site 074 Latitude: 14°S Longitude: 46°W Site Name: Capri Chasma Elevation: - 1 km to - 2 km Type of Site: Penetrator r Contact: Maps: MC-18 NE, SE; MC-19 NW, SE US/Soviet Landing Site Working Grp. Michael Carr Viking Orbiter Images: U.S. Geological Survey, MS 946 Branch of Astrogeological Studies Date Entered: 25 July 1989 345 Middlefield Road Date Last Revised: 25 July 1989 Menlo Park, CA 94025 (415) 323-8111

Geologic Setting tion (possibly global in conjunction with other penetrators), meteorology, and photo- The site lies almost wholly within Capri Chasma at the eastern end of Valles Marin- geology. eris. Waterlain sediments and erosional remnants of the pre-canyon surface covers Potential Problems most of the site. The main interest of the site is the sediments, which could give an indica- To be determined. tion of whether the canyon did at one time contain standing water. A secondary objec- Trafficability tive at the site is to sample the ancient volcanoes and highland into which the canyons are Not applicable. cut. Estimated Traverse Distance Scientific Rationale Not applicable. Sediments, igneous rocks(?).

Objectives Other Obtain composition of sediments (aqueous?), Landing circle size is 150 km radius. and ancient volcanics, local seismic informa-

173 Site 074 CAPRI CHASMA 50 ° W 40ow I

11°S. -1 l°S

"--4

'3-.} t"- C_

r-i "

-19°S 19°S -

.-7. i ! 50°W I I I I I I 40°W 100 km

MC - 18NE, SE; 19NW, SW ® Landing Site: 14 ° S Latitude, 46 ° W Longitude U.S./Soviet Group Site 075- Meridiani Southwest (Margaritifer Terra) Site 075 Latitude: 12"S Site Name: Meridiani Southwest (Margar- Longitude: 7"W itifer Terra) Elevation: + 1 km to + 2 km Type of Site: Penetrator r Contact: US/Soviet Landing Site Working Grp. Maps: MC-19 NE Michael Carr U.S. Geological Survey, MS 946 Viking Orbiter Images: Branch of Astrogeological Studies 345 Middlefield Road Date Entered: 25 July 1989 Menlo Park, CA 94025 Date Last Revised: 25 July 1989 (415) 323-8111

Geologic Setting global in conjunction with other penetrators), meteorology, and photogeology. Ancient heavily cratered terrain carved by fluvial and eolian processes. Ancient high- Potential Problems land material and remnants of sedimentary mantle. To be determined.

Scientific Rationale Trafficability Not applicable. Ancient highlands. Estimated Traverse Distance Objectives Not applicable. Obtain composition of ancient highland material and sedimentary mantle (aeolian, Other fluvial?), local seismic information (possibly Landing circle size is 150 km radius.

175 Site 075 MERIDIANI SOUTHWEST (MARGARITIFER TERRA)

1I°W 3oW I I

7_S _ - 7oS

14°S - -14os

1l°W 3ow

I I ' i i i 100 km

MC -19NE Landing Site: 12 ° S Latitude, 7 ° W Longitude U.S./Soviet Group

176

BLACK /J,,_ ...... _; _ _"i ;:.L.. r' .....t3i. i L'_j,C,,_...... _:" I;i Site 076- Tempe

Site 076 Latitude: 17"N to 40°N

Site Name: Tempe Longitude: 60"W to 61"W Elevation: 0 km to + i km Type of Site: Balloon rContact: Maps: MC-4 SW, MC-10 NE; l'15M US/Soviet Landing Site Working Grp. (I-1320) Michael Can" U.S. Geological Survey, MS 946 Viking Orbiter Images: Numerous Branch of Astrogeological Studies images 345 Middlefield Road Menlo Park, CA 94025 Date Entered: 25 July 1989 (415) 323-8111 Date Last Revised: 25 July 1989

Geologic Setting ground ice, fluvial processes, ridged plains, and channel material. The area is located northeast of the Tharsis Bulge and north of Kasei Vallis, a major Potential Problems outflow channel. To be determined. Scientific Rationale Trafficability Geologic and meteorologic assessment of Tempe Terra Plateau. To be determined.

Objectives Estimated Traverse Distance

Obtain composition of ancient plateau se- To be determined. quence subsequently eroded by decay of

177 Site 076 TEMPE

50°W 40°W t I

50ON • - 50ON

40ON - -40ON

30°N_ .30ON

50;'W 40;W

I l I I I 200 km

1:15 M USGS 1-1320 Site: 25°N-52°N Latitude, 30°W-60 ° W Longitude U.S./Soviet Group

t78

!. , h • Site 077- Ares

Site 077 Latitude: 10°N to 13°S Longitude: 0°W to 25°W Site Name: Ares Elevation: - 1 km to + 1 km Type of Site: Balloon fContact: Maps: MC-11 SE, SW; MC-19 NE, NW; US/Soviet Landing Site Working Grp. l:15M (I-1320) Michael Can" U.S. Geological Survey, MS 946 Viking Orbiter Images: Numerous Branch of Astrogeological Studies images 345 Middlefield Road Menlo Park, CA 94025 Date Entered: 25 July 1989 (415) 323-8111 Date Last Revised: 25 July 1989

terrain. There are also some local patches of Geologic Setting ridged plains material. The area is located near Ares Valles, a major outflow channel with its source area (chaotic Potential Problems terrain) amidst ancient highlands. To be determined.

Scientific Rationale Trafficability Geologic and meteorologic assessment of the Ares Valles outflow channel region. To be determined.

Objectives Estimated Traverse Distance

Obtain composition of ancient highland as- To be determined. semblages, channel material, and chaotic

179 Site 077 ARES

20oW lO°W

0o... "°° N

).. 10oS - -10os

.,,,_

! ! 20°W 10°W I I I I I 200 km

1:15 M USGS 1-1320 Site: 13°S -10°N Latitude, 0°W-25 ° W Longitude U.S./Soviet Group Site 078- Tempe Fossae

Site 078 Latitude: 40"N Longitude: 76.50W Site Name: Tempe Fossae Elevation: + 2 km Type of Site: Rover/Sample Return

f Maps: MC-3 SE Contact: Claudine Madras Viking Orbiter Images: 704B49 through c/o Richard P, Binzel 704B54; 857A29 through 857A31 M.I.T., Bldg. 54-418 Cambridge, MA 02139 Date Entered: August 1989 (617) 253-6486 Date Last Revised: August 1989

Geologic Setting b) Utilization experiments: ability to har- vest by a potential manned mission (suc- Noachian and Hesperian age uplands north- cess high); east of the Tharsis volcanic province; con- c) Study the surface chemistry as a follow- sists predominantly of volcanic materials that up to the Viking experiments (success have been fractured by Tharsis-related tec- high); tonism. d) Search for evidence of life (success medium). Scientific Rationale Potential Problems Investigation of subsurface water for potential use by manned landing mission. Constraints include range of the rover.

Trafficability Objectives 5 a) Measure the characteristics of the perma- frost layer: composition depth and local Estimated Traverse Distance variability (success high); 50 kin.

181 Site 078 TEMPE FOSSAE

80ow i 75;'w

- 42oN

-375_N

80o'W i 75ow

I I I I I I 1O0km

MC -3SE (_ Landing Site: 40 ° N Latitude, 76.5 ° W Longitude C. Madras

182

SLACK AF,JD Wb,;;TE. ': ',_-- ...... 4 r_,._j L,',:,r',,:\b'bt Site 079- Aeolis Southeast

Site 079 Latitude: 15.5"S Site Name: Aeolis Southeast Longitude: 188.5"W Type of Site: Rover/Sample Return Elevation: 0 km

r Contact: Maps: MC-23 SE N.A. Cabrol Ministere De L'Education Nationale Viking Orbiter Images: 596A53 through Observatoire de Paris 596A56, 88A68, 211-5760 Section d'Astrophy_ique 5.Place Jules Janssen Date Entered: 1 November 1989 92195 - Meudon Principal Cedex Date Last Revised: 1 December 1989 Tel.: (1) 45.07.75.30 Telex: 270912 OBSASTR - 201571 LAM

Geologic Setting d) Contribution to the geological layers by rock sampling. The landing site includes a wide impact basin e) Opportunity for biological experiments (150 km diam.) in the Elysium Planitia, and in a past water-rich terrain. a large valley between AI' Qahira and Ma'adim Valles. The landing site is south- Landing site and point a: Collection west ofApollinaris Patera, at 15.5°S, 190°W. of lava samples in the Elysium volcanic re- The average slope does not exceed 1.5%. gion. Erection of seismic stations. Collec- The terrain is open and allows a good margin tion of eolian deposits. Erection of meteoro- for landing operations. Few obstacles are logical stations to analyse possible cathabatic visible according to available data. The site winds at the plateau/plain margin. shows few major impact craters or linear hazards. Traverse 1 and point b: At valley- plain margin, collection of eolian deposits, Scientific Rationale channel material, lava, plateau material (down Non-ambiguous geological diversity includ- the valley slopes) on a small area. Proceed ing volcanic material, possible tectonic ac- with corings at shallow depth to characterize tivity, impact crater material, plain material, different levels of deposits. Possible evi- eolian deposits, plateau material, and chan- dence of water transport. Core may reveal a nel material. succession of eolian and channel deposits. Possible wind deflated lava coming from the Objectives upper plateau and some gravity accumula- tions of plateau materials down the slopes. a) Definition of martian volcanism system by lava sampling. Traverse 2 and point c: Collection of b) Definition of atmospheric model by eo- sediment samples upstream of point b. lian deposit samples. Comparison with point b samples may indi- c) Contribution to martian waterhypothesis cate the transport capacity of a supposed by channel investigations.

183 martianrunoff. Imagesof slopesto docu- for landing operations. Few obstacles are mentpossibleexistenceofterracesin orderto visible according to available data. The se- understandtheflow variations. lected landing site shows few major impact basins or linear hazards. Traverse3andpointd: Collection of slope accumulation samples along traverse. Estimated Traverse Distance Collection of crater ejecta material at point d. Total traverse distance 105 km. Traverse 4 and return to lander: Prepa- ration of samples for Earth return mission. TRAVERSE: Potential Problems 1. Rover traverse from site a to b 30 km To be determined. 2. Rover traverse from site b to c 15 km 3. Rover traverse from site c to d 45 km Trafficability 4. Rover traverse from site d to a 18 km The average slope does not exceed 1.5%. The terrain is open and allows a good margin 5 month mission time.

184 Site 079 AEOLIS SOUTHEAST

189°W 186 °W I I

15°S - -15°S

• - 20"S

i i 189°W 186 °W

I I I I I I 100 km

MC -23SE ® Landing Site: 15.5 ° S Latitude, 188.5° W Longitude N. Cabrol

185 ORtG_NAL F;\_:' ;:" i,_LA,C....KAND WHITE Pr_u-' ....i u"_'_ R,_,ptt- ,' Site 080- Dao Vallis

Site 080 Latitude: 30"S Site Name: Dao Vallis Longitude: 262"W Elevation: + 1.5 km Type of Site: Balloon

Maps: MC-28 NE Contact: Frederick R. West Viking Orbiter Images: 625A 18, 519 Monroe Circle 625A20, 329S29, ASU IPF-710 Glen Burnie, MD 21061

Date Entered: 6 September 1989 Date Last Revised: 1 October 1989 J

Geologic Setting Hesperian Plains, Dao Vallis, and Hellas Planitia. Detection of water vapor. The landing site lies on the upper end of the spatulate depression where Dao Vallis origi- Terrain Units: nates on the slope of Hadriaca Patera. Had- AHh- Hadriaca Patera Formation: Floor riaca is a Mid-Hesperian central vent volcano material of central caldera and of northeast ofHeUas Planitia, with radial ridges, surrounding volcanic eruption mate- a low profile and a smooth floored caldera at rial. its center. Dao Vallis, an apparent outflow Ah5 - Channeled Plains Rim Unit: On east channel, drops 5 km in elevation as it de- rim of Hellas Planitia basin. scends across the southwestern flank of Hch - Older Channel Material: Floors of Hadriaca to its terminus in Hellas Planitia. At Dao and Harmakhis Valles. least 6 different types of terrain units are Hpl3 - Smooth Hesperian Plains: Flat, rela- found either in Dao VaUis or within several tively featureless plains in southern hundred kilometers of it. material. Nhl - Basin-Rim Unit: Material of Hellas Scientific Rationale Planitia basin rim. Nm- Noachian Mountainous Material: Area contains six types of terrain units, volcanics, channel material, basin material, Large, very rugged, isolated blocks scattered around Hellas Planitia Ba- mountainous terrain, plains material. Poten- sin. tial to detect water vapor. Possible frosts, clouds, and dust storms in Hellas Planitia. TENTATIVE TRAVERSE ROUTE: 1. The aerial traverse should start at the Objectives region of Noachian mountainous'terrain An overall survey (incl. closeup images and at about 30"S, 262"W. infrared mapping) of Noachian mountainous 2. After surveying this formation the bal- terrain, Hadriaca Patera caldera and slope, loon should then proceed nearly due west

186 ata heightof 5 km acrosstheHesperian surveyasfar into HellasPlanitia aspos- plainsandtheHadriacaPateraformation sible. totheHadriacacalderaat30.8°S,267°W. Departuresfrom this traverseroute At a height of 5km, the radiusof the canandshouldbemadefor acloserinvesti- sectorof visible martiansurfaceis 183 gation of interesting featuresas they are km. spottedon theimagesproducedby thispro- 3. After surveyingthecalderatheballoon posedaerialsurveyandtraverse. shouldproceedatazimuth100"toaposi- In addition to a television imaging tion abovethe Hesperianplains terrain system,theballoonpayloadshouldat least about31.5°S,263"Wwhich is about30 contain infrared mappingspectrometerfor km north of the apparentstart of the thedetectionof water vaporand aradaror southernbranchof Dao Vallis. laseraltimeterto determineheightabovethe 4. The balloon should then proceeddue martiansurface. southuntil it isdirectly abovethestartof this branchof DaoVallis, andthenpro- Potential Problems

ceed aboveit at azimuth 220°, which To be determined. shouldkeep this branchof Dao Vallis within view of theimagingsystem. 5. When the balloon reaches33.5°Slati- Trafficability tude, it should then turn in a westerly To be determined. direction until it is over the Hesperian plains materialwhich separatesthetwo Estimated Traverse Distance branchesof Dao Vallis. To be determined. 6. At 33.6°S,266.5°W,proceedat azimuth 223*.Thisflight pathwill roughlyfollow Other the courseof Dao Vallis almostto its terminus in Hellas Planitia. Then the Some desired characteristics of the balloon balloon should be able to keep both are: branchesof Dao Vallis underobserva- a) It is powered so that it can follow a pre- tion if it canmaintainanelevationof5km planned route above the Martian surface; abovethe Martian surface. The flight b) it can fly at altitudes of a few meters to path hould takethe balloonnearlyover five kilometers or higher; and thejunction of thetwo branchesof Dao c) it can land payloads (preferably mobile) Vallis at 37°S,270°W. at interesting sites it picks out on the 7. From there,theballoon will follow the Martian surface. lowerDaoVallistoitslargebendat40°S, The balloon might operate (at least partially) 273.8"W not far from its terminus in in a joint traverse with a more advanced Mars HellasPlanitia. Theballoonshouldthen Rover/Sample Return mission on the sur- continueitsaerialsurveyof DaoVallisto face. its terminus,andthencontinueits aerial

187 Site 080 DAO VALLIS

265°W !

30os - -30os

35os -

i 265°W

I I I I I I 1 O0 km

ASU-IPF710 (_) Landing Site: 30 ° S Latitude, 262 ° W Longitude F. West

188

64,.ACK AND WH/]E Pr",OTOGF_APH Site 081- Acidalia Pianitia

Site 081 Latitude: 40" to 60"N Site Name: Acidalia Planitia Longitude: 10 ° to 40°W Type of Site: Balloon Elevation: - 1 km to - 3 km Contact: Maps: MC-4 NE, NW, SE, SC; l:15M Josette Runavot, Chair (I-1320) Internl. Mars Environ. Working Grp Centre National D'Etudes Spatiales Viking Orbiter Images: Numerous Centre Spatiales de Toulouse images 18, Ave. Edouard-Belin 31055 Toulouse Cedex FRANCE Date Entered: 22 November 1989 (by R. Phone: 61.27.37.49 Greeley) Telex: CNES 531 081 F Date Last Revised: 22 November 1989 Fax. 61.28.14.08

Geologic Setting members), fresh lava flows of Arcadia For- Northern lowland plains; plains of volcanic mation and some isolated patches of ancient and/or sedimentary origin; have been exten- highland material. sively modified by aeolian and periglacial processes.

Scientific Rationale Assumptions Site selected to meet engineering constraints. First balloon would be injected October, 1995 at L 170 ° to 175°; second balloon would be Objectives Obtain composition of Vastitas Borealis injected 2 to 4 weeks later. Formation (mottled, grooved, and knobby

189

{. ' I Site 081 ACIDALIA PLANITIA 30°W 20°W 10°W I I

N 50ON- - 50ON

,Ld .| _-.,. I":_ 14

I J I i i l I ! | I I I t, rT_ 40oN _ i , * i I a Is ' i l , , . ..^o_ -I I |, % C_J 30"W 20_'W 10'oW

I I I I I "0 200 km

1:1 5 M USGS 1-1320 Site: 40°N -60°N Latitude, 10°W-40 ° W Longitude J. Runavot Site 082- Arcadia Planitia

Site 082 Latitude: 40* to 60*N Site Name: Arcadia Planitia Longitude: 150 ° to 180*W Elevation: - 3 km Type of Site: Balloon Contact: Maps: MC-2 NW, SW, SC; l:15M Josette Runavot, Chair (1-1320) Inteml. Mars Environ. Working Grp Centre National D'Etudes Spatiales Viking Orbiter Images: Numerous Centre Spatiales de Toulouse images 18, Ave. Edouard-Belin 31055 Toulouse Cedex FRANCE Date Entered: 22 November 1989 (by R. Phone: 61.27.37.49 Greeley) Telex: CNES 531 081 F Date Last Revised: 22 November 1989 Fax: 61.28.14.08 J

Geologic Setting Objectives

Northern lowland plains; covers principally Obtain composition of grooved, knobby, and the Amazonian-age Arcadia Formation (lava mottled members of Vastitas Borealis For- flows, small cinder cones; terrain modified mation, and volcanic materials of Arcadia by aeolian periglacial processes). Toward Formation. the east merges with volcanics from Alba Patera. Assumptions

First balloon would be injected October, 1995 Scientific Rationale at L 170" to 175°; second balloon would be Site selected to meet engineering constraints. injected 2 to 4 weeks later.

191 Site 082 ARCADIA PLANITIA

170°W 160°W 150°W I I I

N 50ON. -50°N

l'J

';3

7, C_ ¢

? -.{ ;;,.

- 40ON

I ! 160°W 150°W J i I I I I I 200 km

1:15 M USGS 1-1320 Site: 40°-60 ° N Latitude, 150°-180 ° W Longitude J. Runavot Site 083- Utopia Planitia

Site 083 Latitude: 40" to 60"N

Site Name: Utopia Planitia Longitude: 240" to 270"W Elevation: - 1 km to - 3 km Type of Site: BaLloon r Contact: Maps: MC-6 SE, NE; MC-7 SW; l:15M Josette Runavot, Chair (I-1321) Inteml. Mars Environ. Working Grp Centre National D'Etudes Spatiales Viking Orbiter Images: Numerous Centre Spatiales de Toulouse images 18, Ave. Edouard-Belin 31055 Toulouse Cedex FRANCE Date Entered: 22 November 1989 (by R. Phone: 61.27.37.49 Greeley) Telex: CNES 531 081 F Date Last Revised: 22 November 1989 Fax: 61.28.14.08

Geologic Setting Objectives

Northern lowland plains; includes subpolar Obtain composition of Vastitas Borealis plains of Vastitas Borealis, plus mottled ter- Formation (mottled, grooved, and knobby rain interpreted to be wind-deflated, and members), channel material, and volcanic grooved terrain (periglacially modified?) of plains modified by fluvial, periglacial, and or Hesperian age; also includes part of the Ely- aeolian processes. sium formation (lava flows and/or lahars from the Elysium volcanics). Assumptions

First balloon would be injected October, 1995 Scientific Rationale at L 170 ° to 175°; second balloon would be Site selected to meet engineering constraints. injected 2 to 4 weeks later.

193 Site 083 UTOPIA PLANITIA

260_W 250°W,

N 50ON- - 50ON

_o 4_

, , J

| .... _°|

i I 260°W 250°W

! I I I I 200 km

1:15 M USGS 1-1321 Site: 40o-60 ° N Latitude, 240o-270 ° W Longitude J. Runavot Report Documentation Page N,alO_]l/:_¢Or_ul_s ac_3 _[l_Ce A_lmtc.shahcx7 3. Recipient's Catalog No. 1. Report No. 2. Government Accession Ne.

NASA RP-1238

4. Title and Subtitle 5. Report Date

Mars Landing Site Catalog August 1(,)90 6. Performing Organization Code

7. Author(s) 8. Performing Organization Report No.

Ronald Greeley, Edit:or

10. Work Unit No.

9. Performing Organization NameandAddre_ 11. Contract or Grant No. Arizona State University Tempe, AZ 85287 NAGW-1306 13. Ty_ ofReportandPeriodCovered

12. Spon_ring AgencyNameandAddre_ Reference Publication Office of Space Science and Applications 14. Sponsoring Agency Code National Aeronautics and Space Administration SL Washington, DC 20546

15. Supplementary Notes

16. Abstract

This catalog wa_; compiled from material provided by the planetary community for areas on Mars that are of potential interest for future exploration. The catalog has been edited for consistency insofar as practical. However. the proposed scientific objectives and characteristics have not been reviewed. This is a "working' catalog that is being revised, updated, and expanded continually.

17. Key Words(SuggestedbyAuthor(s)) 18. Distribution Statement Mars Unclassified - Unlimited planetary exploration

Subject Category 91

19. S_uriW Cla_if.(ofthisreport) _. SecurityCla_if.(ofthispage) 21. No. of pages 22. Price

Unclassified Unclassified 204 AIO

NASA FORM 1626OCT _ Available from the National Technical Information Service, Springfield, VA 22161 NAS*-I._a_ey.1990