APOLLO MANNED LUNAR LANDING

SCIENTIFIC EXPERIMENT PROPOSAL

GEOLOGICAL FIELD INVESTIGATION IN EARLY

APOLLO MANNED LUNAR LANDING MISSIONS

Abstract

and

Techi~ ica l Section

E. M.Shoemaker, U. S. Geological Survey

Principal Illvestigator

E. N. Goddard, Uiliversity of Michigan

Co- investigator

J. H. Mackin, Univers i ty of Texas

Co- investigator

H. M. Schrnitt, National Aeroilautics

and Space Adrninis t ra t ion

Co- investigator

A. C.Waters , Uiliversity of California

a t Sa i~ t aBarbara

Co- investigator

November 1965

APOLLO MANNED 1,UNAR I,ANDING

SCIENTIFIC EXPERIMENT PROPOSAL

GEOLOGICAL FIETAD INiTESTXGATTON IN EARLY

APOELO MANNED LUNAR LANDING MISSIONS

Sponsor

U. S. Geological Survey

GSA Building

Washington, D. C. 20242

Harold L. James

Chief Geologist

U. S. Geological Survey

GSA Building

Washington, D. C. 20242

202-343-2125

Investigators

Eugene M. Shoemaker Center of Astrogeology 602-774-5261 Principal Iilvestigator U. S. Geological Survey

601 East Cedar Avenue Flagstaff, Arizona 86001

Edwirl N. Coddard Department of Geology 313-764- 1444 Co- investigator University of Michigan

Ann Arbor, Michigall

J. I-Ioover Mackiil Department of Geology 512-471 -3055 Co- investigator University of Texas

Austin, Texas

1Iarrisoi? 1-1. Schmitt P. 0 . BOX 276 602-969-8933 Co- investigator Williams Air Force Base

Arizona

Aaron C. Watcrs Department of Geology 805 -968- 151 1 Co-investigator University of California

at Salzta narbara Santa Barbara, California

Page

Abstract 1

1. Purpose and objectives of geologic iilvestigatioils in ea r ly Apollo luilar landing missions 3

A. Scie~ltific objectives 3 B . Fine s t ruc ture of the plains sur faces 4 C . Chemical and physical sur face alteration 8

2. State of present developmeilt of Apollo geologic field i~lvestigatioil 12

3. Charac ter i s t ics of the geologic field instrumellts 15

Stereometr ic film c a m e r a

Staff

G11om011

Televisioil c a m e r a

Sampling trowel

Sampling tubes

Sampliilg hammer

Sample sc r ibe r /b rush

Field sample bags

Special sample containers

Tool and sample c a r r i e r

Hand magnifying g lass

Hand- held flashlight N. Audio communicatioils equipment 19

ABSTRACT

The principal geological objectives of --Early Apollo missions

will be study of the fine s t ruc ture of the lunar surface, mainly

in the plains a r e a s favorable for ear ly lauding, and study of the

ilature of the plains mater ials . Plains a r e a s of interest include

not only the mar ia , but a l so the plains of cer tain upland regions.

These plains a r e depositional surfaces, modified by post-

depositional processes of several The pr imary questions

to be answered a r e 1)the lithologic composition, s t ructure, a t ~ d

thicklless of the superficial layer of fragmental mater ia l believed

to cover most par t s of the plains and other a r e a s on the moon

and 2) the composition and origin of the mater ia l underlying the

plains.

Allswers to these questions will be obtained from the geo-

logical observations of the a s t ro~ lau t s , fronl photographs, and

from sarnp1.e~ taken along a se r i e s of foot t r a v e r s e s from the

lunar excursion module. The geological instruments to be used

by the astronauts a r e light, simple hand tools and cameras . The

topographic and geologic relations observed along the t r ave r ses

of the astronauts will be determined primari ly from numerous

stereoscopic photographs supplemented by the astronautsq

descriptions alld by data obtai~led from returned samples. The

photographs provide a detailed record of the surface features,

which can la ter be analyzed quantitatively, and will provide the

geologic context a t the s i te of each sample locality. The orien-

tation of the cameras during exposure of each photograph will

be automatically recorded for use in later photogrammetric and

photometric data reduction.

TECHNICAL SECnON

A. Scientific objectives

The ea r ly Apollo lullar landing s i t e s will probably be on

mar ia floors or other lunar plains, r emote from rugged topo-

graphy. These plains a r e depositional sur faces , modified by

post-depositio~lal processes of seve ra l kinds. The pr imary

geological questions to be answered by e a r l y Apollo l u ~ l a r

lailding missions a r e I ) the nature and origill of the mater ial

underlying these plains, and 2) the nature and r a t e s of the

processes that have taken place on the lunar surfa.ce. Were the

plains ma te r i a l s formed as flows of liquid lava that now range

from solid rock to rock froth, or were they deposited a s a s h o r

granular mater ia l , and now range f rom unconsolidated to solid

depending on the degree of heat o r vacuum welding? The r a t e s

of processes modifyillg the sur faces of the plains a r e exceed-

ingly slow; these processes call best be approached by study of

their long-term effects 011 mater ia l s and topographic forms of

the plains.

The most immediate question will be the composition, fine

s t ruc ture , and thickness of a superficial layer of fragmental

mater ial believed by many studellts of the moo11 to have been

formed by the impact of objects of var ious s i zes over a very

loilg period of t ime. Closely related t o the origin of this

http:surfa.ce

mater ia l , is the distribution and range in size and shape of

craters which pockmark the surface, as seen in the Railger VII,

VIII and IX photographs.

B. Fine s t ruc ture of the plains surfaces

Models of the local fine s t ruc tu re of the plains can be

derived f rom physical studies of the moon's surface, by means

of telescopic photometry, radiometry and reflected microwave

signals, and observations of the lunar c r a t e r distribution in

combination with empir ical knowledge of the phenomenology of

c ra te r ing , c ra te r ing theory, curreil t data 011 the flux of meteor-

oids in the vicinity of the ear th, and es t imates of the effects of

other processes acting on the lunar sur face , such a s sputtering

produced by so la r wind bombardment. P rom such stuclies we already

know that the lunar c r u s t i s demoilstrably heterogeneous in com-

position. The fine s t ruc ture of the sur face a l so may be expected

to be heterogeneous.

On the basis of the available data , i t appears highly probable

that most par t s of the moon's sur face a r e covered with a layer of

finely broke11 rock fragmeilts, the upper surface of which i s

pitted with c r a t e r s . The thicklless of the layer , the s i z e d is t r i -

bution of the rock fragments, and the s i ze and spacing of super-

imposed c r a t e r s probably a l l v a r y abruptly from place to place.

Employiilg the data available from the photographs acquired from

the Iiailger missions, in addition t o the illformation obtained a t

the telescope, a reasonable model of the fine s t ruc ture of a

typical local area on a plains su r face can be described in the

following way:

1. A layer of shattered and pulverized rock probably

covers m o r e than 95 percent of the plains. It is of var iable

thickness and r e s t s with i r r egu la r contact on the uilderlying

substailce of the plains.

2. The fragments in this layer o r blanket of shattered

rock have been derived by ejectioil f rom c r a t e r s , most of

thcrn nearby, but some lying g rea t dis tances away. About

50 percent o r m o r e of the fragments have come from within

one kilometer of the s i te , but t he re is a fiilite probability,

decreasii lg with the distance t o the source , of findiilg a rock

fragmeilt derived from any place on the moon. Except alollg

the margins of a plain, therefore, the pieces of debris will

be composed predomi~lantly of plaiils mater ial . Those frag-

ments that have come from beymd the plains will probably

represell t highly d iverse geologic environments. In addition,

a smal l admixture of meteorit ic mater ia l will probably be

represell ted among the rock debris .

3. F r a g m e ~ l t s occurring a t the base of the debris layer

will, on the average , have been t ransported on ballistic

t ra jec tor ies a sma l l e r ilumber of t imes than pieces near the

middle o r top of the layer . Progressing upward from the

base, the layer has been s t i r r e d o r recoilstituted an

increasing number of times by smaller and smaller and

more and more numerous cratering events. The uppermost

millimeter of the debris layer is probably completely

reorganized once every 10 to 100 years by the formatioil and

filling of minute craters.

4. The average grain size tellds to decrease from base

to top of the debris layer because fragments in the upper

part, oil the average, have been shocked and broken a

greater llumber of times and have been ejected, on the

average, from smaller craters. Near the base, fragments

as large as several centimeters in diameter will be common,

whereas the material of the uppermost few millimeters more

likely will be fillely pulverized. Throughout the debris

layer, the bulk of the rock fragments will probably average

less than a millimeter in grain size, but heaps of coarse

blocky rock from the larger craters may be expected at

many places.

5. Beneath this blanket of shattered rock, the plains sub-

stance, i f originally solid, will in many places show evidence

of having been broken to greater depths by shocks of varying

strength produced during developmellt of the larger craters.

6. The contact between the uilderlying material and the

pulverized surface blanket has collsiderabl e local relief,

collsisting chefly of the intersecting segments of the ori-

ginal floors and walls of nuillcrous old craters that

range from a meter to a few tens of meters across. Most

of these are now buried belleath younger impact debris.

7 . The upper surface of the debris layer is pockmarked

by craters ranging from less than a millimeter to several

tens of meters across (or larger dependingonthe local area).

Craters larger thall one meter in diameter occupy about

50 percent of the surface; smaller craters occupy the rest

of the surface and are also superimposed on the large craters.

Millute craters, with dimensions of the order of a millimeter

or less, probably cover nearly all of the surface and are

superimposed on nearly all other features.

8. The debris layer typically varies in thickness from

a few tens of meters to less $hall a millimeter, It is

thickest where it covers the floors of some of the oldest

and largest craters, and is thin or even absent along the walls

of very young craters that cut through the debris layer into

the underlying plains material.

A similar layer of pulverized rock probably covers nearly

all parts of the moon's surface. It can be expected to vary in

average thickness as a direct functioil of the age of the rocks or

terrain 011 which it is formed. Terrain older than the maria

will have a thicker blallket of debris than the typical mare

surface, and the blanket will be thinner, on the average, on

younger terrain. The average crater size on the surface of the

debris layer will be larger on older terrain and smaller on the

younger terrain.

Examiilatioil of the surf ic ial layer , possible alteration pro-

f i les , and the underlyiilg lunar plains mater ia l s , preseilt a

challengiilg problem for the astronauts , but one that can be

attacked by straight -forward field procedures. Direct visual

examination and sampliilg of the sur face will answer many of the

c r i t ica l questions. A systematic study over an extended period

of t ime will be necessary , however, if the surface s t ruc tu re i s

to be fully understood. Such a study requ i re s that as complete

a r eco rd a s possible be obtained of the shape, s i ze , and spatial

dis t r ibut ioi~ of sur face features a i ~ d mater ia l s . I11 o r d e r t o

analyze the fine s t ruc ture of ally par t of the moon's surface, i t

must be possible to reduce this observational information to

a geometr ic a r r a y , commonly portrayed by geologic maps and

c r o s s sections. Such a r r a y s o r maps contain, in a reduced

fo rm, the illformation derived f rom visual observations, samples ,

photography, and physical measurements r emrned from the moon.

If the astronauts have been fully trailled in the techniques of

accura te aild thorough observation and reporting, descriptions of

the i r visual observatioils of the lailding s i te , recorded on tape

and by rad io commul~ica t io i~ to the ea r th , will be an important

element of the scieiltific record . Abundant high- resolution

photography by film will provide an equally important form of

r eco rd from which much of the on-s i te descriptioil and analysis

call be amplified and verified, and f rom which topographic and

geologic maps of the landii-tg s i t e call be constructed. The

returned samples provide the third major source of geologic

information. The hand specimen descr ipt ions, mineralogy,

petrography, chemis t ry , and nuclear composition of the samples ,

when evaluated together with the field geologic information, will

complete the geologic data required t o in te rpre t the nature and

origin of the lunar plains.

The immediate objectives of the Apallo geologic field inves-

tigations may be described concisely a s the deterrninntio~~ of t h e

local structure and character of the luilar surface n~atericcils and

the processes and sequeilce of events by which these materials

and the structure have originated. Structure, used here in its

broadest sense, refers to the threedimensioi~al array of the

different types of material present in the area studied, aild the

physical and temporal relationships of each type of material to

the others,

To determine structure, it is necessary first to be able to

discriminate or recognize differences in the materials present

and the11 to be able to locate materials with observed differences

within a three-dimensioilal array or coordinate system. The

scientific iilstrurnents proposed here a r e chosen to provide a

detailed permanent record of the visual illformation needed to

discrimillate and correlate differem lui-nar surface materials, the

data necessary to order this information in a geometric array,

and equipment to obtain samples that a r e correlated with the

visual data.

The principal record of the geologic details of the lunar

surface will be provided by photographs. From th? photographs

the morphological details of the surface, railging from the near

microscopic textures to the major topographic elemeuts of the

landiilg s i te , can be reconstructed. Measurements obtained from

the photographs are used to construct maps, profiles, and three-

dime~lsional models, which serve a s a bases on which to plot

geologic information. In addition to morphology, information on

photometric propert ies and color of the sur face mater ia l s can be

accurately recorded in the photographs. These a r e the chief

killds of information used by the geologist t o discr iminate differ-

ent rock mater ia l s and t o decipher geologic s t ruc tu re in the field. .

A s tereometr ic film camera , ca r r i ed by the astronaut and

moullted on a11 instrument holder configured as a walking o r

surveying staff, is the principal geological instrument. With the

aid of a gnomon placed on the surface, the location, shape, and

orientation of fea tures on the lunar surface may be extracted

f rom the photographs by the methods of photogrammetry. These

features will include objects well beyond the t r a v e r s e of the

astroiclaut.

11-1 addition to the s te reometr ic film c a m e r a , the hand- held

levis is ion c a m e r a to be taken to the lunar sur face should a l so be

used to fullest extent practicable a s a scientific instrument. The

abundai~t video images obtained with the high-resolution mode

can be reduced in much the same way as the photographs from

the film camera . The television camera should be used to provide

a highly detailed r eco rd of the t e r r a in and geology in the imme-

diate v i c i ~ ~ i t y of the LEM.

Sarnpliilg tools, sample containers , a tool and sample c a r r i e r ,

a hancl magnifyiilg g lass , a hand- held flash light, and audio

communicatioi~ and recording equipment complete the l is t of

instruments required for the Apollo geological field investigation.

The c a m e r a s and field tools proposed a r e specialized adapta-

tions of coilventional c a m e r a s and geological field equipment.

Design studies are current ly in progress for most of the proposed

instruments. h program of field t e s t s has been initiated to study

the field procedures most suited t o the constraints of the luilar

missions, particularly the constraints imposed by the spacesuits,

the portable life support sys tems, and the charac ter i s t ics of the

LEM.

3. Charac ter i s t ics of the geologic field iilstruments

A. Stereometr ic film c a m e r a

The scielltific requiremellts of the Apallo geologic field

illvestigatiolls will be met by a c a m e r a which can produce s te reo-

scopic images 011 film that is sensit ive throughout the visible

spectrum, to objects rangillg in luminance from 25 to 2500 foot

lamberts . The images should 1) have a resolution of 100 lines

per mil l imeter ; 2) be focused sufficiently well that the maximum

diameter of any circle of confusion is . 02 mm; 3) have a field of

view of approximately 60'; a i ~ d4) be of sufficient photogrammetric

quality that maximum distance measuring e r r o r to objects 5 me te r s

distant i s + 1 percent when the images a r e properly oriented in v

existiilg f i r s t -o rde r plotters. Expasure should be uiliform a c r o s s

the image within 2 percent and the spec t ra l t ransmission of the

color f i l ters should be calibrated t o the response of the film in

o rde r to closely ~ n a t c h the CIE color matchillg functions.

B, Staff

A simple lightweight staff with a bracket t o mount the s te reo-

met r ic film c a m e r a is required t o hold the c a m e r a for taking

pictures. Ail easi ly read cliilometer and sun compass can be

incorporated into the head of the staff for estimating the orienta-

tion of the camera in the field. If it should prove feasible t o

incorporate a n R F trackiilg system into the LEM, the staff will

a l so se rve a s a base oil which to mount the transponder.

C. Ci~omon

A self - righting, tr ipedall y supported ver t ica l rod gimbled

to the support legs , s o as t o allow the automatic ver t ica l posi-

tioiliilg of the rod, is required to recover accura te orientation of

the s t e reomet r i c photographs. This device, when placed on the

ground and photographed, will give a t r u e ver t ica l orientation in

s t e reo models, and the t r a c e of its shadow on the ground will

provide accura te field orientation of the s t e r e o model recovered

from the photographs af te r the mission.

D. Televis ioi~c a m e r a

The Apollo Block II television c a m e r a should be used for the

collection of an extensive image r ecord of geologic features nea r

the LEM. The specifications required f o r scientific u s e of this

c a m e r a are:

(1) The c a m e r a is small , lightweight, and connected to the

t r ansmi t t e r by a co-axial cable about 30 m e t e r s long.

(2) C a m e r a charac ter i s t ics a re : 500 kc bandwidth; 0.625

f r a m e s per second; 1280 lines pe r f rame; 5-2500 foot

l amber t s illumination sensitivity; 3', 30' and 80' fields

of view, and minimum discrimination of 8 gray levels a t

J2 intervals.

(3) Simple c a m e r a orientation subsystems should be provided

to acquire data essent ial t o the interpretation of photo-

me t r i c data.

E. Sampling trowel

Samples of fine-grained surficial debris can be obtained by

a specially designed trowel having the following character is t ics:

(1) tough, chisel blade-front with a dis tal width l e s s than

the width of sample bag openings.

(2) flat bottom with slopiilg flanges on ei ther side.

(3) handle with malleable butt and overall balance compatible

with use a s a hammered chisel, Haiidle should be extei~d-

able to meet sterile sample requirements for biological

samples.

I;. Sampling tubes

The sampliilg of soi l profiles in fine debr is call be accom-

plished in many c a s e s by use of driven o r punched samplillg tubes.

Although telescopic data indicate there is a ve ry fine-grained,

porous surface layer on the moon, it is not cer tain how thick o r

coherent this layer is o r if it coiitaills coa r se fragments in

sufficieiit quantities to ser iously impair the use of sampling tubes.

G. Sampliiig hammer

Chipping of samples from large blocks of rock will require a

sarnpliiqg hammer. A modified geologist 's hammer will best meet

the requiremelits.

II. Sample scr iber /brush

The collection of oriented samples for s t ruc tura l , paleo-

magn?tic, and geochemical purposes requi res a rock sc r ibe r

which, for example, could be used to sc r ibe a shadow line on the

sample pr ior to photographing the sample in place. A sma l l

brush, which can be mouiited 011 the s a m e holder, will be needed

for removing dust f rom rock sur faces t o permit the i r c lose

examillat ioiz.

I. Field sample bags

The pr ime requirements for general geological sample

containers are that they can be eas i ly filled, rapidly sealed

against mixing, conveniently ca r r i ed , and capable of compact

packagillg in LEM/CM sample spaces.

J. Special sample con ta i~ le r s

I11 addition to the sample bags, the field geologic investigations

requi re special sample containers with the following character is t ics :

(1) Oile sample coiltainer should be capable of maintaining the

lunar atmosphere until samples are returned to the

receiving laboratory.

(2) One con ta i i~e r should be designed t o s t o r e the sampling

tubes taken on ally given mission.

(3) Opeiiings of contaiilers should be a s la rge a s possible for

e a s e of packing.

K. Tool and sample c a r r i e r

Efficient operations oil the lunar surface will requi re the

t ransport and ready accessibil i ty of the field tools and sample

containers and c a m e r a s . Studies and field t r i a l s conducted by

the U . S. Geological Survey and Maniled Spacecraft Center

indicate that a t r ipedal f r a m e with a long horizontal bar handle

described in a la te r section best meets the needs of lunar geo-

logical t r ave r ses .

L. Halld magnifyillg g l a s s

To 3id the astronaut in the discrimination and interpretat iol~

of undisturbed smal l fea tures of lunar mater ia l s , a hand magni-

fying glass should be developed having the following general

character is t ics :

(1) 5 to 10 power magnificatio~l

(2) optics and shape compatible with visibility and mobility

colzstraints on the astronaut,

M. Hand- held flashlight

A halld- held, bat tery powered flashlight to be ca r r i ed by the

astrollaut i s needed fo r the examination and photography of objects

partly o r wholly in shadow.

N. Audio communications equipment

Scientific evaluation of lunar surface operations in part

depellds on recovery of the astronaut 's descriptions of the surface.

Real t ime, mutual 2-way a l ~ d i ocommunication between the a s t ro -

lzaut on the surface, the astronaut in the LEM, and the mission

co~ l t ro l ceilter will be required for mission operations. These

commu~lications should be recorded in the i r e ~ l t i r e t y and t ime

coded for correlat ion with O T ~ G Y "scientific data. It is understood

that these requirements a r e met by the communication sys tems

current ly l-eing developed for Project A p ~ l l o .

19

4. Methods of analysis of the data

The images taken by the stereometric film camera will

permit photogrammetric, colorimetric and photometric analysis

of small parts of the moon's surface determined by the astronaut

to be of special interest. Detailed physical dimensions, color

and photometric properties of selected features and surficial

materials within about 5 meters of the astronaut will be obtained

from the images. 11-1addition, large scale topographic and geologic

maps of the landing s i tes and geologic t r averse paths can be com-

piled from the photogrammetric and photometric data obtained by

the s tereo film camera. The astroilaut t r averses with the s tereo-

metr ic camera will provide data comparable to a large number of

close- spaced Sunreyor landings.

A. Photogrammetry

Photogrammetric reductioil of the film camera data a s well

a s s tereo TV camera images will be accomplished by means of a

direct viewing coln puter controlled ailaly-tical stereoplotter.

The staff mouilted vertical base s t e reo camera requires a

f i rs t -order plotter to accommodate the following characteristics:

(1) Two matched lenses with s tereometric model capability

out to 5 m with + 1 percent measurement e r ro r . -(2) Direct viewing plotter capable of working at a base to

d is ta i~ce ra t io of . O l e

(3) Must be able to work with a vertical o r horizontal hase.

(4) Output will be in form of contour lines o r X Y Z

coordinates,

(5) Must be able to work with oblique photography with optical

axis ranging from horizontal to vertical.

(6) F i r s t -order stereoplotter precision in adjustment of

effective focal length from 25 mm through a range of

100 mm.

B. Photometry

Lumi l~a l~ce of ir~dividual resolu"ro11 elemelats of the lulaar

surface will be computed with referellce t o calibration charts on

the sampling hammer and the tool and sample ca r r i e r . Tne data

will be extracted from the photographs by microphotometric

measurement of the pr imary film records. Topagraphic mapping

beyotld the range of photogrammetric capabilities of the s tereo-

metr ic film camera will be extended by photocl i~~ometric methods

and by illterpolation of available orbital photographic data.

C. Colorimetry

Colorimetric measurements will be made by comparison of

the c o r r e s p ~ ~ d i n g luminance of individual image elements which

has been computed from pictures taken with a se r i es of color

fil ters. The method of data extraction will be the same a s for

photometry. Colorimetric measurements fo r each identifiable

element of the lunar scene will be transformed, where possible,

to CIE color coordinates.

D. Polarimetry

Polarimetric measurements will be accomplished by compari-

soil of luminance of iildividual image elemeilts which has been

computed from pictures taken with polarizing f i l te rs a t a series

of positions of the plane of polarization. Both the plane and amount

of polarizatioil of the scat tered sunlight can be obtained in this way.

The polarimetric properties of the lunar surface will be compared

with the color and other photometric properties in analysis of the

geology.

E. Geology

Analysis of the geology of each Early Apollo landing s i te

will be based 011 a syilthesis of the topographic, photometric,

colorimetr ic , polarimetric, textural and structural data extracted

from the photographs and television images, the field descriptioils

of the astronauts, and the lithologic, mineralogic, chemical, and

isotopic data extracted from the returned lunar samples.

5. Experimental procedures

A. Traverse operations

Ranger VIII photograph 570 shown in Fig. la illustrates a

part of Mare Tranquillitatis that is of the size accessible to foot

traverses by astronauts from a landed Lunar Excursion Module

(LEM) of the Apollo spacecraft or from any stationary vehicle on

the lunar surface. The geologic features and units shown in

Fig. l a and b are probably typical of this and other maria surfaces.

A11 example of several hypothetical traverses from the LEM,

arranged to examine features of special geologic interest are

shown in Fig. la. Such traverses should be planned in

advance, on the basis of photointerpretation, essentially to field

check the geology. The field-checking procedure is highly flexible,

and, if time becomes a limiting factor, the amount of detail

examined can be reduced from that shown to only a few of the

most critical features. If the landing is not precisely on the intended

site, a geologic map prepared from pre-flight illformation may

not be available. Even if the lailding takes place on a pre-chosen

site, many of the features seen on photographs may be incon-

spicuous and difficult to identify on the ground. In these latter

cases, the astronaut will have to solve as many of the geologic

relations as he can as he proceeds along his traverse and plan the

traverses as he goes along.

The representative traverses plotted 011 Fig. l a allow sys-

tematic sampling, photography, and description of each major

F i ~ ~ w e1a &o~P$Q,$~ GI_" area CI-~~LZ: 0x1 b %TO8Ranger 7x11I i^LIastra%irig+:p ~a:%r3-.*>:$8top8pPP fost tsavorcjels 'xsor?. h;,oii,esicd 1 ~ r d t x?02-aPi af A p d L s i urrm Exetnasfon Wule a

2.66 :; rruxq. 2k.75 i3 2% %heein+&rmtiele, G e 0 3 ~by Ye::* &l1~ttp G t m pa%se

c iatcr ram MU r i a l sharp ism iratets

Uahiiri m raised rtrns d &rp ~ i r i u b rc r r u r - A h & tacloer ro &r 6mare eurfacc m a t e r i a l li(urpholq3~01 a i l low t i r i i crater% i ruwd by h lgh-angl t i ccomldiy impails

f a u l t i d i i a i i i r i m or w a l l macer ia l

1-1 < rater mate, i a i undifferentiated Lrsrer bench rnster ra l

C O ~ Y ~ X ionvex r x m craceiir t m crarers

M a t r i m i s in subdued craters with h m c a 5 C Edb ralsed rims canvex wvard r lbedo of rims i s dle same as mat of the mare surface mereriai Crater

v a l i ~are catcave inward wtm s l c e b

of appro~tmateiy IFa and lese Rtm

'rests are w r l y defined Probably

ex iensrve iy e r a Bherp i rm

funnel and dlmpic craters

i o. i i t i r tm rnas i r ia l , Crater w a i l rnarerlai, Crater i b r m a t e r i a l , Crater bem h i i ia rcr ta l Ihiw - r n i v a i e r s iow rhm craters I~YWlow r i m c i e l c i S r , m .rat- isin c i s r c r s

I Z ~ W r i m crater w a l i maierxdi mat i i cov n

M s r c surface m r t c r i r l

M r c c i t a ! mak,ng up rhr hulk of Ih m a r e eurlaac Plobably a Nre iqew

type of geologic ullit o r feature presellt within walking distance of

an a rb i t r a r i l y chose11 lailding point. In addition t o study of the

local fea tures , i t i s expected that, alollg each t r a v e r s e , samples

call be ohtailled of ma te r i a l derived f rom impact events in rocks

f a r removed f rom the landing site. Descriptions of topographic

and geologic re la t ions along the traverse l ines should be supple-

mented by abundant s tereoscopic photographs. Good photographs

a r e preferable t o ve rba l descr ip t io~ls of many field re la t ions, such

a s shapes, s i ze range, patterns of alignment o r distributio12 of

rock c l a s t s , and a l l types of topographic fea tures , f rom la rge

c r a t e r s t o detai ls of the fil.ne s t ruc tu re of the surface. Because

interpretation of the geologic s i g ~ ~ i f i c a n c e of samples , a f te r

cornpletioll of the mission, may depeild a s much 01-1 the i r field

re la t ions a s on the physical and chemical propert ies of the

samples themselves , documentary photographs at each sample

station will be llearly a s essent ia l as the samples.

h cr i t ica l ques t io~l is 1 7 0 ~ ~much of the as t ronaut ' s t ime should

be spend in mapping, that i s , in p~sit ion-determinil-tg operations

along the t r a v e r s e l ines. ' ~ h kco l~ t ro l l i~ lgfactor may be the

relatively ralldom distribution of impact c r a t e r s withill reach of

the I X M . Details of the shape, t rends of lillear features , and

orher patter11 relatioils , which a r e essent ia l elements in any study

of structurecl bedrock, a r e not a s c r i t i ca l in e a r l y Apollo recon-

naissance 011 tile lunar plains. Most lineations and other pattern

relations that may occur in the viciility of the LEM should he

evident on photographs taken before o r a f te r the landing. 111

general , t r a v e r s e s should be controlled a s accurately a s practi-

cable, pr imari ly s o that observatiolls and sample locatiolls along

the t r a v e r s e s can be t ied t o these photographs.

Positioning operations should be accomplished insofar as

possible by a tracking device 011 the LEM, o r by shots of the LEM

with the s te reometr ic film c a m e r a from points along the t raverses .

Where it is necessary for the astronaut to dea l with directional

t rends , these call be descr ibed with re ference t o the d i r ec t io i~ of

shadows, which will change l e s s than 2 degrees during most

t r ave r ses .

B. Sampling

One of the principal problems presented by a sur face covered

by a fragmental layer of the kind described above will be to select

appropriate sampIes fo r re turn t o Earth. With a wide variety of

rock fragments to choose f rom, the astronaut will be faced with

the difficult t ask of deciding what specimens best represent the

mater ia l a t hand. He will need t o est imate the relat ive abundai1ce

of different rock types in o r d e r t o select representat ive samples,

and, in addition, he will want to collect a s many of the iilfreque~ltly

occurriilg rock types a s possible, a s these will provide information

on the more distant, and possibly deeper, par t s of the moon.

111 cer tain respec ts the ]nodel described for the fine s t ruc ture

of the plains surfaces i s s imi l a r to t e r r a in on Ear th which has been

covered by deposits left by meltillg of a continental glacier. Like

glacial drift, the debris layer on the moon obscures the "bedrocky' I

in most places, is heterogeneous in character and irremlar in I

thickness, and contaills rock fragments of widely diverse illdividual

histories. Thorough study of such a layer in a local area either on the

moon or 011 the Earth can provide a great amount of information about

the geology and history of a broad segmellt of the planetary crust,

provided that the origill of the fragmeiltal layer is understood.

Failure to understand the nature and origin of the fine structure of

the moon, on the other hand, can lead to serious scientific misinter-

pretation and confusion. For this reason we regard the field geo-

logical investigatiol~ and the role of the astronaut as a trained field

observer to be fulldame~ltal to most of the lunar scientific illvestigations Y

to be performed in Project Apollo, and of paramouilt importance to the

success of later lullar missiol-ns,

Arrangement of materials arouild a fresh crater. --The----

problems of sampling in a typical landing site 012. the lullar plaii~s

can be illustrated with a hypothetical cross sectioil such as that

show11in Fig. 2. The oldest part of the surface in Fig. 2 is the

relatively level arca A; the youngest elemellt of the surface is the

fresh crater C,and crater B, subdued by erosion, is ii~termediate

i n age. The fresh crater may be collsidered to be a few meters to

a few tens of meters in diameter, in the size railge shown on the

/

be within t r a v e r s e distailce of the Ea r ly Apallo landing sites. The

crater is a l so l a rge enough s o that t he re is a good passibility that

the depth of the c r a t e r lnaybe g rea te r than the thickness of the impact-

shat tered blanket. Smaller f r e s h craters will provide informntlon

that is useful but l e s s c r i t ica l for geologic interpretation; l a rge r

fresh c r a t e r s should provide critical illformation but are fewer in

number and hence less apt t o be available fo r study.

Ideally the wall of the f r e sh crater might show, f rom the base

upwards, (1)the ma te r i a l which underlies the lunar plain; (2) the

full thickness of the impact -shat tered mantle, perhaps showing a

compositional profile and/or an alteration profile; and (3) a section

of the ejected mater ial . The Boor of the crater is apt to be under-

lain by breccia , and the l aye r i~ lg of the walls may be co~lcealed o r

obscured in part by slumping and creep. Moreover, the walls may

be s o s teep a s to be difficult of access ; the astronaut should sample

them if he can, but it is likely that he will be able only to photograph

and descr ibe chenl.

If the ru le holds t r u e that mater ia l s in the ejecta blanket a r e

deposited in r e v e r s e s t rat igraphic o r d e r , the upper surface of the

blanket will provide samples derived from deep within the c ra t e r .

Fo r example, if the sur face of the blanket is l i t tered with blocks of

rock differing in s ize , lithology, o r degree of alteration from rock

fragmei-its on the surrounding plaiil, the implication is that the plain

is underlain a t depth a t that place by that rock. 011 the other hand,

a deposit of a s h o r dust , s imi lar ly limited to the upper surface

and dis tal margills of the ejecta blanket, and differillg in composi-

tion, degree of alteration, o r o ther p r o p r t i e s f rom the impact-

shat tered blanket of the surrounding plain, would suggest that the

plain is the re underlain by granular mater ials , r a t h e r than rock.

I f the charac ter of the ma te r i a l s beneath the impact-shattered

blanket could be established in only one place, it would be a grea t

gain; with some luck the e a r l y Apollo m i s s i o l ~ s may establ ish it in

seve ra l places, on plaills of different ages. Samples of the mater ial

subjaceilt to the blanket, whether rock o r granular , a r e the most

meaniilgful that may be available on the lunar plains.

Profile sampling of ma t r ix mater ial . - - Even if no accessible

f r e s h craters penetrate to the base of the impact-shat tered layer ,

valuable evidence bearing ii-tdirectly on the nature of the subjacent

mater ia l , and direct ly on the origin of the fine s t ruc tu re of the

surf ic ial layer , can be obtained by study of sur face profiles. Walls

of f r e s h craters may provide such profiles. If they do not, sampling

the walls of t renches 10-50 c m deep, dug with the specially designed

trowel may be a method which has a good chailce of success in

surf ic ial mater ial with a wide range of g r a i i ~ s i ze and degree of

indurat ioi~, If the wall of such a t rench shows zoilal differeilces iia

co lor , texture, composition, o r other propert ies , the relat io~lships

should be described, photographed, and documeilted by samples cut

with the trowel s o a s to be representat ive of each zone. If there i s

no visible zonation, samples should be cut a t s ta ted intervals from

base to top of the t rench wall with equal c a r e for cornparisoil with

profiles of other ages and composition. The absence of zones

may be a s significant a s their presence.

Depending on the physical properties of the superficial

material , drive-tube samples may be e a s i e r o r more difficult to

obtain than samples cut with a trowel. I11 some mater ia ls the

drive-tube sampling method may not work, but under favorable

conditions the method provides ( I ) a suite of undisturbed o r little-

distorted samples representing the ent ire profile; (2) samples to

a grea ter depth than any reasonable dug trench, and (3) samples

that a r e ui~coi~tamiizated o r have a rniizirnum of contamii1ates

iiltroduced in the collection process, and (4) samples that can be

mailltailled in lunar eilvironmental coi~ditions by addition of gas -

tight jackets around the coring tubes. These advantages a r e s o

great that we recommend that three -drive tube sample devices be

ca r r i ed for t r i a l on the f i r s t Apollo missioi~. The apparatus i s

simple, and can be modified ear ly and quickly fo r use 011 la ter

Rock samples. - -Fragments of rock that l i t ter the surface

beyond the distal margins of the f resh ejecta blankets may be of

two origins- -(l)those that represent the local bedrock, and (2)

those foreign to the s i te , from extra- lunar sources o r other

places on the 1770011. The importance of obtaii1ing adequate

samples of the local rock, if any, has been s t r e ssed above. While

less cr i t ical , the foreign fragments may provide valuable preliminary

information about the composition of more distant parts of the moon.

If t he re i s a var iety of lithologic types, o r fo re ig l~ rocks,

the astronaut should es t imate the relat ive abundai~ce of each

type, and collect one o r a few smal l samples of each. A s the

lithologic var iety inc reases , the difficulty of estimatillg the

percelltage of each rock type inc reases , but the es t imates must

be made. If a la rge number of rock types are present , the

l imited sample re turn will make i t difficult t o bring back a

representat ive sample. Random sampling is justified only if

the fragmellts are s o a l te red o r coated that lithologic differences

are not readily apparent.

Fragments a few cellt imeters in diameter are adequate for

petrographic study and many o ther types of analysis. Fragments

5 t o 10 c m a c r o s s a r e i~eeded for special purpose analyses;

fragmellts l a r g e r than 10 c m probably must be broken fo r

packaging. Depending on the hardness o r toughness of the rock,

it may be possible to break chips f rom large blocks. It is v e r y

difficult, however, eve12 with the gravitational force on Ear th , to

break hard fragments in the 10-50 crn s i z e range embedded in

yielding granular mater ial ; such fragments will probably have to

be c a r r i e d t o a l a rge r block, if any, for use a s an anvil, o r taken

ent i re , o r not taken. a t all . I11 this , a s in eve ry other aspect of

the sampling process , the astrollaut must u s e judgment based 011

a full ul1derstanding of the problem.

Other things being equal, smal l fragments which may be

reaililp available aloilg t r a v e r s e l ines a r e preferable to chips of the

same rock broken from blocks, because of the saviilg in the

astronaut 's time. Similarly, there is no point in digging a

trench to expose a profile if the same profile is exposed in a

c r a t e r wall, o r in the depression, i f any, produced by the blast

of the LEM.

However they may be obtained, the most esseiltial samples

a t each site a r e those that bear directly on the major problems

of the lunar plains, namely, the charac ter and origin of the

material beneath the superficial blanket, and the processes

responsible for the fine s tructure of the surface. If only two

matrix samples can be obtained, they should include (1) a profile

from the oldest surface in the vicinity--probably the flatest,

darkest -colored surface, with the most strongly zoned profile- -

and (2) a profile from the youngest surface, which in most but

not al l cases , will be the outer slopes of the f reshes t c ra ter .

Other types of samples will have grea ter o r less value depending

on how closely they are ideiltified with geologic units, the relative

ages of which a r e known. The fact that the collecting t ime and

weight of samples will be fixed, places a premium on the

discrimination of the astronaut; this depends 011 his experience in

geologic field work in general, and the depth of his understanding

of the particular problems of the Apollo sites.

C. Exploratio~l t ime and astronaut mobility

The fundamel~tal constraints on achieviilg the goals of the

Apollo geologic field investigation a r e the limited number of man

hours available for scientific tasks and the limited mobility of the

astronaut in a spacesuit. The current est imates of the t ime

available for surface activities during ea r ly Apollo landing

average about 15 mail hours divided among 3 excursions of no

m o r e than 3 hours dura t io l~ each. These figures a r e largely a

fuilction of the capacities of the Lunar Excursion Module and

astronaut life-support systems. Such a division of t ime could

include one extravehicular excursion by one man and two excur-

sions by two men working together on the surface.

The mobility of the astronaut outside the spacecraft will be

governed by the mechanical propert ies of the surface, the

charac ter i s t ics of the spacesuit and the life-support sys tem, and

the charac ter i s t ics of the scientific gear that must be transported.

The distances that an astronaut can t r a v e r s e under various c o ~ ~ d i -

tions have not been determined with any degree of certainty,

although some est imates can be made. Allowing 0.5 hours for

e g r e s s , equipment checkout, aild ingress , the maximum useful

t ime for surface exploration duriilg an excursion would be about

2 . 5 hours. Tests conducted by the Manned Spacecraft Center of

the Natio~lal Aeronautics and Space Administration and by the

U. S. Geological Survey suggest that average geologic traverse

speeds (including t ime for description and other activities) over

rolling, loosely aggregated terrai l l may be 01-1. the o r d e r of 10 rn

per minute. Thus, maximum t r a v e r s e lengths on the o rde r of

1500 rn can probably be anticipated during any given excursion,

provided that sampling, photographic, and dc.;cr nprivc: uper,itio!lz,

can be carried out efficiently.

6. Astroilaut t ime requiremeilt synupsis.--

A. Pre-flight time

Pre-flight requirements on the t ime of the astronauts include

t ime for 1) training in geological field methods and 2) practice of

the geological field i~west igat ion in simulated Ear ly Apollo scien-

tific missions. T o date, individual astronauts have spent f rom

9 to 43 days training in geological field methods. About half of

the astrollauts have completed 34 days of training. Approximately

12 days additiollal training in geological field methods is planned.

An average of 12 days of practice of the geological field investi-

gation in simulated Early Apollo scientific missions is planned.

13. In-flight time

In- flight ( lunar surface) t ime required for the geological

field illvestigation is 2.5 to 15 man hours, depending on the i tnigh

of stay on the lullar surface alld the t ime require~nenrsof other

experiments. The maximum t ime that could be usefully employed

in the geologic field investigations great ly exceeds the t ime that

will be available in Early Apollo miss io i~s .

C. Post-flight t ime

Post-flight t ime of the astroilauts will be required for sci.en-

tific debriefing and for participation ill geologic alqalysis of the

returned data. I t i s expected that there wil l be a large range in

the extellt of participation of the astronauts in the post-flight

scientific al~alysis. To the extent that i t is possible for them to

participate, the astronauts should be considered co-investigators

in the geological field investigation. Up to several months of

astronauts' time would be appropriate and desirable for partici-

pation in the post-flight analyses. At a minimum, several days of

debriefiilg spread over a period of several months of data ailalysis

will be required.

The pre-flight requiremenro on the astronauts occur in two

phases, 1) training in geological field methods and 2) practice

of t h e lunar field geological operatioj~si n simulated

missions. In phase one, two-day field exercises about once

every three months are planned for the astronauts. These will

be selaeduled far the c&rn.lvenienceof individual astronauts or small

groups of astronauts. In part, the field exercises will be carried

out at localities where the geologic features correspond to features

that may be e~~countesed Other exercises will on the moon.

coilsist of brief participation in selected Geological Survey mapping

projects,

Phase two of the pre-flight requirements 012 the astronauts

i s divided into two periods. In the first period, prior to assign-

ment to a fligl~tcrew, the astrollauts should participate in field

tr ials and tests of the geologic instruments and contribute to the

evaluation sf the field use of these instruments. 117. the secoi~d

period, following assignmellt of crews to particular Early Apollo

missions, the crews should participate in full-scale simulations

and a dress rehearsal of the lullar geologic field investigatio~~ so

as to attain complete familiarity with all the scientific operations

and maximuln proficiency in carryi l~gout the mission.

B. Post - flight requirements

The post-flight participatioll of the astronauts in the field

geological investigatio~l will begin shortly a f te r the mission with

a thorough summary description and illterpretation of the geo-

logical features seen on the lunar surface. La te r , as s t e r e o

models, mosaics and topographic maps are developed f rom the

returned pictures, the astronauts will be requested to give a s

thorough an i l~ terpre ta t ionof the visual data as they can, in light

of the i r field experience a t each c a m e r a station. Those astroilauts

that participate fully a s co-investigators will probably wish to

participate in the preparation of geologic maps f rom the s t e reo

models and ill the analysis of the geologic history f rom the i r ow11

recorded field descriptions, the photographic data, and the resu l t s

ohtailled from the lunar samples . Some of the as t ronauts should

participate in thorough hand specimen description of the returned

lunar samples in o r d e r to co r re l a t e this data with the i r field

jmpressions and the photographic data.

As Pi-e-f'?j;;;it f i i : * i j i t ic~

13re-flight facilities a r e required for simulation of the l u l ~ a r

surface operatiolls of the geological field investigation. Field

test sites and a data receiving facility for the simulated l u n a r

surface scielltific operations will be supplied by the U. S. Geo-

logical Survey at i t s Center of Astrogeology, Flagstaff. Arizona.

In acidition co the field test sites a room i s needed at the

Manned Spacecraft Center where the 7'V pictures, t l~eastronauts

descriptio~~sof the geology, and rrackillg illformatian giving the

position of the asrronrlut with rcxpcect to :he1.,13M,cnl; be

reccjvetl aatl t i t i l i j i c : t i by the i i3vrL7ti,rt~toiD:-. tliis irrc-onling.!!.:jng

data, the investigntjors will make a prclir~inarganal3jsisof tlie

gt:olc~gyil l real tirile, PiYhi;: r o r j r n , with ilrt: nuc;ctciiltr S c l rec'i~rtiini?;

aquiplxel3t i s needed in p ~ e -f i lgbt time in order. tci c:(-,ild~crdress

rehearsals of the s c i e ~ ~ t i f i cparts of the missions.

B. Recovery facilities

Recovery facil i t ies required for the geological f ie ld investi-

gation illclude the following:

1) Video tape recorders at each of the receivillg statiolls of

the Deep Space Net that will be used in the Early Apollo

Missioi ls alld at the Mission Control Center at the Manl~ed

Spacecraft Center.

2) Kinescope or other film recorders at the Missioil Control

Center and the investigators' room.

3) Video monitors at all stations listed in 1) and 2) above.

4) Audio recorders and monitors at stations listed in I),

2), and 3 ) above.

5) A photographic laboratory for processing, under carefully

coi~trolledconditions, the film returned from the stereo-

metric camera. Special control of processing will be

required for photometric calibration.

6) A sample receiving laboratory where certain preliminary

analyses and thorough hand specimen description of the

returned lullar samples can be carried out under carefully

controlled collditions. It is understood that specifications

for this laboratory already have been prepared.

7) An investigators' plotting room where the incoming video

signal and audio signal call be monitored and recorded.

This room should also contain an X-Yplotter driven by

computer which will record the position of the astronaut

in real time as calculated from telemetry received from

an RP tracking system 011 the LEM.

C. Data handling procedures

The investigators will require release of the data in the

fallowi~~gform from the Manned Spacecraft Center:

I ) One set of duplicate magnetic tapes of all video tele-

lnerry obtained from the lunar surface.

2) One se t of prime negatives obtained from one of the video

film recorders for al l video images obtained on the lunar

surface. The film record should be t ime coded. Six

copies of duplicate negatives prepared from the same

prime film negative will a l so be needed for distribution to

the iwest iga tors .

3) One complete se t of diapositive plates of a l l exposed f rames

prepared directly from the film negative obtained from the

s tereometr ic film camera .

4) Six high-quality f i r s t -generation duplicate negatives pre-

pared with s tep wedge photometric control from the primary

s tereometr ic camera negative.

5) Six copies of the audio te lemetry with a time code for a l l

descriptions of the lunar surface by the astronauts.

6) Detailed descriptions and photographs of each sample

obtained in the sample receiving facility during unpacking

and catalogiilg of the samples. Members of the i i~vest igator

team should participate in the hand specimen description

of these samples at the sample receiving facility.

APQLLB MANNED LUNAR LANDING

SCIENTIFIC EXPERIMENT PROPOSAL,

GEOLOGICAL FIELD INVESrklGATllON IN EARLY

APOLLO MANNED LUNAR LANDING MISSIONS

Part HII

Management Plan

E.M.Shoemaker, U. S. Geological Survey

Principal Investigator

E. N. Coddard, University of Michigan

Co-investigator

J. H. Mackin, University of Texas

Co-investigator

H. H. Schmitt, National Aeronautics and Space Administration

Co-investigator A. C. Waters, University of California

a t Santa Barbara Co-investigator

APOLLO MANNED LUNAR LANDING

SCIENTIFIC EXPERIMENT PROPOSAL

GEOLOGICAL FIEIdD TN\rESTIGATTON IN EARLY

APOLLO MANNED LUNAR LANDING MISSIONS

Sponsor

U. S. Geological Survey

CSA Building

Washington, D. C. 20242

Principal Administrator

Harold L. James

Chief Geologist

U. S. Geological Sumey

GSA Building

Washington, D. C. 20242

202-343-2125

Eugene M. Shoemaker Center of Astrogeology 602 -774- 5261 Principal Investigator U. S. Geological Survey

601 Eas t Cedar Avelzue Flagstaff, Arizona 86001

Edwin N. Goddard Department of Geology 313-764- 1444 Co- investigator University of Michigan

Ann Arbor , Michigan

J. t loover Mackin Departmelzt of Geology 512-471 - 3055 Co- investigator University of Texas

Austin, Texas

FIarr isol~If. Schmitt P. 0. Box 276 602-969-8933 C o - investigator Williams Air Force Base

Arizona

Aaron C. Waters Department of Geology 805 -968- 151 1 Co- investigator Ulliversity of California

at Santa Barbara Sailta Barbara, California

Contents

Management plan

Page

1

1. Responsibilities of the investigators 1

2. Operating budget 3

Resumes

MANAGEMENT PLANS

1. Responsibilities of the investiga tors

E. M. Shoemaker, a s principal investigator, will carry

overall responsibility for the geological field investigatioil in

the early Apollo maniled lunar lai~ding missions and will be

specifically respoilsible for the stereometric film camera, the

staff, and the gnomon. I-le i s also administratively responsible

for the development work and field testing of instruments to be

carried out uilder the Manned Lunar Exploration Studies section

of the Branch of As trogeology of the Geological Survey.

E. N. Goddard , as co- investigator, will be responsible for

the tool and sample carr ier , the hand magnifying glass and the

hand- held flashlight.

J. 13. Mack in, as co- investigator, will be responsible for

the samplillg tools, specifically the samplillg trowel, sampliilg

tubes, sampling hammer, and the sample scriber/brush. This

responsibility will iilclude liasoll with other investigators concerned

with sampling tools, particularly biologists collcerned with sterile

sampling.

H. H. Schmitt, as co-investigator, will be responsible for

the geologic al requirements and field use of the television

camera and the audio communications equipment.

A. C. Waters, as co-investigator, will be responsible for

the geological field requiremellts for the field sample bags and

special sample contaiilers. This responsibility will include liasoll

with other investigators concerned with the sample contaiilers,

particu l a d y geochemists.

The investigators will share equally i n the geologic

interpretation of the data each accordillg to his own special

fields of interest. E. M. Shoemaker will be respollsihle for

photogrammetric, photometric, colorimetric, and polarimetric

reductioll of the photographs and television images and will

supply maps and models portrayiilg this data to the other in-

ves tigators for geological analysis.

2. Operatillg budget

Funds required by the Geological Survey for development

work and field testing of the geological field instruments a re

available through existing contracts with the National Aeronautics

and Space Administration and through expected extellsions of

these contracts. 'The techrzical moizitors of these col~tracts are:

Doilald A. Beattie - Code MTL National Aeronautics and Space

Admillis tration Washington, D. C. 20546

Edward M. Bavii~- Code SNI Natioilal Aeronautics alld Space

Admi12istratioi~ Washington, D. C. 20540

John E.Dorllbach - Lunar Surface Technology Branch Space Environmellt Division Manned Spacecraft Center National Aerol~autics alld Space

Administration Houstolz, Texas 77058

I11 addition to the developmellt work and field testing of the

ii~struments, funds will be required for participatio~~ of the co-

investigators and for acquisition of special instruments for post-

flight analysis of the photographs and television images. Requests

for funds will be submitted by the co- investigators through their

respective institutions.

Funds are needed in fiscal year 1966 for purchase of the

direct viewing computer col1trolled analytical stereo plotter.

This illstrument will be required to verify the photogrammetric

use of the prototype stereometric film camera and to develop

the field procedures for optimum use of this camera.

Approximately twelve months is required for delivery of the

analytical plotter after the purchase coiltract has been negotiated.

The plotter should be ready early in fiscal year 1967 for use in

reduction of photographs obtained from field trials with the

prototype film stereometric camera.

Summary budget estimate for Geological field investigation

i l l earlv A~ol lo maimed lul~ar landing mi ss ioi~s

Fiscal year 1966

Cost Direct viewing, computer coiltrolled

f i r s t order analytical stereoplotter. . . . . . . . $230,000

Edwin N. Goddard, Professor of Geology

Born Oskosh , Wisconsin, October 22, 1904

Attended University of Michigan, 1923-1927, A. B. ; l928,M. S. ; 1936, Ph. D.

Career

Investigat igation of relationships of o r e sits to tertiary intrusives in Front Range of Colorado, 1930- Study of o re deposits in Montana and Colorado, 1937- 1946. Investigation of f luor spar deposits in Colorado and New Mexico, 1942- 1946. Exploration for Manganese deposits in Haiti, 1947. Edited geologic maps and prepared new list of map symbols simplifying and sta~ldardizingU. S. Geological Survey geologic maps, 1948- 1949. Taught Economic Geology and directed geological field training at University of Michigan, 1949. Chairman of the Department of Geo logy, 1952- 1956.

Principal professional activities

Instructor in Geology, University of Michigan 1928- 1930.

Jullior Geologist to Principal Geologist, U. S. Geological Survey,

19 30- 19 49. Geologic map editor, U. S. Geological Survey, 1948- 1949. Professor of Geology and Director of geolog ical field work at

the University of Michigan, 1949- -Chairmall of the Department of Geology, University of Michigan,

1952- 1956. Member of the Field Geology Team, NASA; member of the

geology group of the Falmouth, Massachusetts, conference, NASA

Honors

Chairman of North American Geologic Map Committee, Geological Society of America 1951- 1965

Member and Chairman of Publications Committee,Geological Society of America.

Member of Education Committee, American Geological Institute. Panel Chairman of the Fellowship Program of the National Science

Foua~dation. M ~ m b e r of the Field Geology Team, NASA

Memberships

Geological Society of America, American Association of Petroleum Geologists, Mineralogical Society of America, American Association for the Advallcement of Science, Geochemical Society, Seismological Societyof America, Society of EconomicGeologists, AmericanGeo-

physical Ullion, Geological Society of Washington, Michigall Basin Geologcal Society, Societ6 geologig de France, Royal Netherlands Geological and Mining Society, Geological Society, Sigma Xi.

J. Hoover Mackin, Professor of Geology

Born Oswego, New York, November 16, 1905

Atteilded New York University, B. S. 1930; Columbia University, M. A , , 1932, Ph. D. 1934.

Career

Taught geomorphology and subjects related to geology of igneous rocks, 1934- - . Investigation of geomorphology in Pennsylvania, Colorado, and the northwestern United States, 1933- - . Engineering ology of dam sites and urban areas, 1939- 1941, 19 60, glacial geo y in the state of Washington, 1940-1941. Exploration for ironore deposits in the Iron Springs district, Utah, 1945-1955. Determined the relations of the o re deposits and the igneous rocks. Investigation of uranium- and thorium- beari~lg mineral deposits in Idaho, 1952- 1954. Investigation of the characteristics and origin of widespread ash flow deposits in southwestern United States and northwestern Mexico, 1955--.

Principal professional activities

Professor of Geology, University of Washit~gton, 1934- 1962- - . University of Texas, Farish Chair in Geology, 1962--. U. S. Geological Survey, WAE, 1943- 1952. Geologist, Atomic Energy Commission, 1952- 1954.

Hoizors

Member of National Acadamy of Science, 1963- - . Chairman, Division of Earth Sciences, National Research

Council, 19 65- - . Memberships

Geological Society of America, Chairman of Cordilleran Section, 1952, Counselor, 1953- 1955. American Ge Union. Society of Economic Geologists. American of Petroleum Geologists. American Institute of Professional Geologists. American Association for Advancement of Science. Society of Sigma Xi.

Harrison H. Schmitt, Astronaut

Born Santa Rita, New Mexico, July 3, 1935.

Attended California Institute of Technology 1953- 1957; B. S. 1957, Uiliversity of Oslo (Norway), 1957- 1958; Harvard University, 1958-1964; Ph. D. 1964.

Career

Geological field mapping of layered ultramafic illtrusive and associated iglleous and metamorphic rocks in southeastern Alaska, 1955- 1956. Geological field mappiilg of high- grade meta- morphic gneisses, mafic, and ultramafic rocks in Norway, 19 60. Project Chief of Lunar Field Geological Methods for Manned Lunar Exploration Investigations of the Geological Survey, 1964- 19 65. Astronaut for NASA, 1965.- -Principal professional activities

Geologist with J. A. Noble, Geological Consultant 1955- 1956.

Geologist, U. S. Geological Survey, 1959.

Geologist, Norwe an Geological Survey, Oslo, Norway, June

19 60- November Geologist, U. S. Geological Survey, Branch of Astrogeology,

19 64- 19 65. Astronaut, NASA, 1965--.

Memberships

Geological Society of America Society of Sigma Xi

Iiugene M. Shoemaker, Geologist

Roril I,os Angeles, California, April 28, 1928

Attended Cdifornia iilstitute of Technology, 1944- 1948; B. S. 1947, M. S. 1948, Priilceton University, 1950- 1951, 1953- 1954, M. A. 1954, 1'11. D.1960.

Career

Iixploration for uranium deposits alld investigation of salt structures i1-i Colorado and Utah, 1948-1950. Regional investigations of the geo- chemistry, volcanology, and structure of the Colorado Plateau, 1951 - 1956. Ilesearch 01-1 structure and mechanics of meteorite impact and nuclear explosion craters, 1957-1960; discovered coesite (high pressure form of silica) at Meteor Crater, Arizona, with E. C . T. Chao, 1960. Tnvesti-gatioil of structure and history of the Moon, 1960--. Established a lunar geological time scale and developed methods of geological mapping of the MOOLI, 1960 Applicatioil of television systems to investigation of extraterrestrial geology, 1961 - -. Organized the Branch of Astrogeology of the U. S. Geological Survey, 1961. Organized the Manned Space Sciences I3ivi.ioi-i of the National leronautics and Space Administration, 1963. Developed methods of topographic mapping of the Moon by photometry, 1964. Estab-li shed U. S. Geological Survey Obsenratory for geological investigation of the Moon and planets at Flagstaff, Arizona, 1963.

Pril~cipal Professional Activities -

Geologist, U. S. Geological Survey, 1948- 1960.

Chief, Ilranch of Astrogeology, 1961 - - .

Visiting Professor, California Institute of Techi~ology, 1962.

Researcll Issociate, California Iilstitute of Technology, 1964- - .

Acting Director, Manned Space Sciences Division, National Aeroilautics

and Space Administration, 1963. Co- lllvestigator, Television experiment, Project Ranger, 1961- 1965. Principal investigator, Television experiment, Project Surveyor, 1963- - .

Doc torate of Science, Arizoila State College, 1965.

Wetherill Medal of the Fra~lklin Institute, co- recipient with E. C. T. Chaol 1965.

Memberships

Geological Society of America, Mineralogical Society of America, Society

of 13cono1nic Geologists, Geochemical Society, American 4ssociatioll of

I'et roleum Geologists, America11 Geophysical Ui~io~l , Seismological Society of America, Astrollomical Society of the Pacific, International Astronomical CJniciii

01

Q) .*-I w P-4

3 0 r-i4-J

0

cr;

i=-i tft

C

0

* r4 cn

XI Q)

9-4 0

k a

4 cct

%L.r-i 0

g:

.r-i

k 0-r

GFI_AMLLM_Abstract_11_1995.pdfGFI_AMLLM_Cover_Abstract.tifGFI_AMLLM_Ab_11_1965.tif

GFI_AMLLM_PartIII_11_1965.pdfGFI_AMLLM_PtIII_Cover.tifGFI_AMLLM_PtIII_11_1965.tif