search.jsp?R=19740026159 2020-02-22T07:19:37+00:00ZAbstract This is the Final Technical Report under NASA Johnson Space Center Contract NAS9-12557 for Low Brightness Image Data Analysis.The

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NASA CONTRACT NAS9- 12557

FINAL TECHNICAL REPORT

APOUO DATA ANALYSIS MPERIMEM: S-211

LOW BRIGHTNESS INAGE DATA ANALYSIS

Prepared for

Lyndon B . Johnson Space Center National Aeronautics and Space Administration

Houston, Texas 77058

Robert D. Mercer Principal Investigator

January 31, 1974

The Dudley Observatory 100 Fuller Road

Albany, New York 12205

Abstract

This is t h e F ina l Technical Report under NASA Johnson Space Center Contract NAS9-12557 f o r Low Brightness Image Data Analysis. The r epor t gives t he background f o r t he cont rac t and technica l progress made over a two year period. The purpose of t h i s work was t h e s c i e n t i f i c analyses of photographic da t a i n astronouy obtained by t h e Apollo Orb i t a l Science Photographic Team during Apollo f l i g h t s 14 through 17, inclusive. P r inc ipa l Inves t iga tor f o r t h i s work was Mr . Robert D. Mercer of t he Dudley Observatory. Co-Investigator was Mr . Lawrence Dunkelman of t h e NASA Goddard Space F l igh t Center. The Johnson Space Center a l s o provided add i t i ona l funds f o r port ions of t h i s work through a companion In t e rcen te r Agreement t o t h e Co-Invest i ga to r .

Elements of ana lys i s of photographic frames provided by NASA a r e described here in and included severa l tasks. Some of these tasks were t h e co l l ec t ion and co r re l a t ion of Quick-Look l i s t i n g s and working p r i n t s f o r fu r the r study and t h e generation of post-mission and p ro j ec t repor t s . Pos t f l i gh t ca l ib ra t ions of t h e f l i g h t photographic systems were ca r r i ed out , and the r e s u l t i n g da t a were used t o co r r ec t l ens v igne t t i ng e f f e c t s i n t h e o r i g i n a l data . The da t a handling flow included photodig i t iza t ion of f l i g h t da t a photographic scenes, ca l ib ra t ed step-wedges and v igne t t ing pa t te rns foflawed by computer program processing of t h e xesu l t i ng a r r ay of f i l m dens i ty readings.

Several f ac to r s kept r e s u l t s from reaching ' h e o r i g i n a l l y a n t i - c ipated l e v e l of accomplishment. Hawever, br ightness , po la r i za t ion and color informaeion on zodiacal l i g h t and br ightness measurements on the lunar l i b r a t i o n region, Lq, were nearing the point of s c i e n t i f i c publica- t i o n a t t he completion of t h e contracted time period.

Background

The requirement f o r P r inc ipa l Inves t iga tors and Teams of Inves t i ga to r s t o assess s c i e n t i f i c and technica l da t a co l l ec t ed on manned lunar f l i g h t s r e su l t ed d i r e c t l y from the a c t i v i t i e s of the Apollo O r b i t a l Science Photographic Team (APST). This group was e s t ab l i shed i n e a r l y 1970 t o improve t h e s c i e n t i f i c value of t h e Apollo lunar missions using photographic techniques and on-board systems c a p a b i l i t i e s in such f i e l d s a s geology, geodesy/cartography, photogrammetry, astronomy and apace photographic instrumentat ion. The APST served through the Apollo Program Direc tor ' s Off ice a t NASA Headquarters and made its d e t a i l e d recommendations d i r e c t l y t o i n t e - g r a t i o n and operat ions groups a t NASA's Johnson Space Center (JSC).

The i r work was ca r r i ed ou t s epa ra t e ly from those experiments formally accepted by NASA f o r s p e c i f i c f l i g h t s . The formal experiments included t h e usual preparat ion, i n t eg ra t i on , operat ion and d a i a analyses phases; whereas, t he APST work included a l l but t h e da t a ana lys i s phase.

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I n a sense, the APST s c i e n t i f i c a c t i v i t i e s were exploratory i n nature and c u t across many d i s c i p l i n e s ; so, no one could be c e r t a i n of r e s u l t s . For t h i s reason, then, it was considered premature t o add d a t a analyses r e s p o n s i b i l i t i e s t o t h e i r c h a r t e r , bu t t he APST members were not pre- cluded from pa r t i c ipa t ing i n such analyses , i f warrented by t h e quan t i t y and q u a l i t y of da ta s o obtained.

The work of t he APST proved q u i t e f r u i t f u l from t h e beginning, and NASA Headquarters issued an Announcement f o r Data Analysis Oppor- t u n i t i e s i n t h e Spring of 1971. Contract NAS9-12557 f o r Low Brightness Image Data Analysis was one of t h r ee proposals accepted i n t he a r ea of astronomy, the o ther two being concerned with s o l a r corona data . A l l used techniques of photographic photometry t o ob ta in abso lu te br igh tness measurements on t h e i r sub j ec t matter. A s i s NASA's custom, these da t a analyses e f f o r t s were given iden t i fy ing numbers associated wi th t h e i r experimental work; i n t he case of Contract NAS9-12557 it became Experi- ment S-211. Proposals had t o include not only known photographic r e s u l t s , bu t a l s o d a t a expected o r poss ib le t o c o l l e c t , because they were submitted t o NASA p r i o r t o t he launch of t h e l a s t t h r ee lunar missions.

The P r inc ipa l Inves t i ga to r (PI) , Mr. Robert D. Mercer of t h e Dudley Observatory, and t h e Co-Investigator (Co-I), Mr. Lawrence Dunkelman of NASA's Goddard Space F l i g h t Center (GSFC), were d i r e c t l y involved i n t h e acqu i s i t i on of these da t a a s the astronomical members of t h e APST. They were a l s o involved i n reversed r o l e s under the formal Apollo Experi- ment S-178, Gegenschein/Moulton Region, where the da ta obtained would be handled i n almost exac t ly t he same manner. I n both cases , t h e work was

planned t o u t i l i z e government f a c i l i t i e s a s much a s possible . While t he bas ic government cont rac t was wi th t he Dudley Observatory, a companion e f fo r t : . l a s funded a t GSFC by JSC through an I n t e r c e n t e r Agreement f o r t he Co-I t o use GSFC'S con t r ac t o r s tudent s e rv i ce personnel a s we l l a s government f a c i l i t i e s and equipments. This agreement is included a s Attachment 1. Advantages and disadvantages i n t h i s j o i n t arrangement w i l l be discussed below.

Technical Pronress

The i n i t i a l t echnica l approach, a s ou t l ined i n t h e proposal, was t o use an automated, Joyce-Loebl double-beam microdensitomcter a t GSFC t o photodig i t ize those frames of t h e o r i g i n a l . F i l m which contained s c i e n t i f i c a l l y valuable information. Stepped l i n e scan readings of f i l m dens i ty would be recorded on magnetic tape f o r l a t e r input t o a d i g i t a l computer a t GSFC. Density readings of ca l i b r a t ed step-wedges contained on t h e f l i g h t f i l m and of a second standard wedge f o r instrument c a l i - b r a t i o n would a l s o be recorded and used i n a computer program t o convert scene d e n s i t i e s t o abso lu te br igh tness measurements. F ina l ly , c a l i b r a t ed readings of t h e f l i g h t l e n t s photometric t r ans f er funct ion, usua l ly r e f e r r ed t o a s its "vignet t ing function", would be appl ied t o br igh tness readings t o a r r i v e a t a c t u a l values of b r igh tness across t h e scene. The computer program t o handle these inputs was in development by another Co-I, D r . Charles Wolff, on Experiment S-178. This , then, was t h e s i t u a t i o n a t t h e beginning of t h e contracted e f f o r t .

D ig i t i za t i on of da t a f o r Experiment S-178 a t GSFC proved t o be much slower than an t i c ipa t ed , on t h e order of hours per f u l l frame. Furthermore, t he number of frames containing important astronomical d a t a obtained on t h e l a s t four Apollo lunar missions ran i n t o t he hundreds wi th ha l f again a s many c a l i b r a t i o n frames. The workload grew w e l l beyond t h a t o r i g i n a l l y an t ic ipa ted . Other means t o ca r ry out t h i s work had t o be sought. Fortunately, s eve ra l vendors were j u s t beginning t o produce more f u l l y automated and much f a s t e r photodig i t iz ing equipments. The f i n a l d i g i t i z i n g method used w i l l be discussed more f u l l y below.

Meanwhile, a f t e r c a r e f u l considerat ion by a l l concerned, it was judged t o o g r e a t a burden t o develop the Experiment S-178 computer program t o meet S-211 requirements. I n s p i t e of t h e much simpler needs f o r S-178, t h e programing had gone very slowly. Besides, t h e S-211 d a t a would r equ i r e a g rea t e r soph i s t i ca t i on t o dea l wi th frame mosaicing and removal of image smear on t h e var ied sub jec t mat ter r e s u l t i n g from success fu l APST e f f o r t s . The S-178 program was only intended t o remove s t a r l i g h t by c l ipp ing sharp grad ien ts i n t h e s p a c i a l values of b r igh tness , smoothing over t h e remaining scene, and, i f required, superimposing

and adding a r rays of values. The l a s t process mentioned required considerable time t o ad j u s t a r r a y s represen t ing l a r g e granula t ion in read ings , anc! then checking frame r e g i s t r a t i o n outputs before t he a d d i t ion process.

Thus, another premise on which the o r i g i n a l proposal had been based had t o be . ~ d i f i e d a f t e r s i x months i n t o t h e cont rac t . Here, aga in , a l t e r n a t i v e techniques were known t o be ava i l ab l e ; however, it had been hoped t h a t t h e simpler S-178 programwould be adequate, because these a l t e r n a t i v e s involved very l a r g e programs wi th many soph i s t i ca t ed processors. A s expected i n t h e case of these l a rge r programs, i t r e - qu i red a longer time t o become f ami l i a r wi th t h e i r use, although t h e q u a l i t y of s c i e n t i f i c r e s u l t s could be correspondingly improved. One of t he se new techniques involved a program running on an IBM computer t o t a l l y dedicated t o image processing work a t t h e V i s i b i l i t y Laboratory i n La J o l l a . However, those i n charge of processing a c t i v i t i e s f e l t t h a t t h e time required t o support t r a i n i n g and use of t h i s system would over tax t h e i r l imi ted s t a f f and resources; so, arrangements f o r i ts use could no t be made.

Another sophis t ica ted system, t h e Video Image Communication and Re t r i eva l (VICAR) Program, developed a t t h e Jet Propulsion Laboratory (JPL) f o r processing t e l ev i sed d a t a from the Ranger, Surveyor and Lunar Orb i t e r spacecraf t , was a l s o s a t i s f a c t o r y f o r S-211 requirements. Further- more, it had a l ready been acquired fromJPL by D r . Dan Klinglesmith of GSFC f o r h i s an t i c ipa t ed needs t o support t he In t e rna t iona l U l t r av io l e t Experiment (WE) S a t e l l i t e Program. I n t h e f a l l of 1972 D r . Klinglesmith, who, l i k e the Co-I, works i n t h e Laboratory f o r Opt ica l Astronomy, was checking ou t t he VICAR Program a t t h e GSFC Computer F a c i l i t y f o r ope ra t i ona l use. He was q u i t e w i l l i n g t o include our requirements i n r e t u r n f o r personnel a s s i s t a n c e wi th t h e checkout of add i t i ona l processors i n t he program a s wel l a s soma f i n a n c i a l support t o acqui re d i sp l ay devices t h a t a r e e spec i a l l y u se fu l f o r presenting VICAR output. These reques t s were met us ing I n t e r - cen t e r Agreement funds f o r graduate s tudent a s s i s t a n t s and f o r a port ion of t h e equipment requirements. I n addi t ion , M r . G. C. Alvord, a consui tan t t o t h e P I i n Albany, made a number of t r i p s and spent many weeks a t GSFC working d i r e c t l y on S-211 d a t a requirements. A more d e t a i l e d desc r ip t i on of VICAR processing is given l a t e r i n t h i s repor t . Af te r a l i t t l e more than one year , then, t h e f i n a l d i r e c t i o n t o proceed on photodig i t iza t ion and computer processing could be s t a r t e d wi th ce r t a in ty .

A be la ted Data Analysis and Handling Plan was then w r i t t e n , and it is included a s Attachment 2. Included wi th it was a d r a f t Exhibi t A f o r t h e GSFC Procurement Division t o use i n i t s Request f o r Proposals (RFP) on photodig i t iz ing se rv ices . D e t a i l s f o r accomplishing a l l port ions of t h e -

work a r e spec i f i ed i n t h i s plan and w i l l not be repeated here. Because of problems noted both above and below and a l s o because many s t eps in t h e processing flow had t o progress in s e r i e s as shown on page 3 of Attachment 2, it was not poss ib le t o increase the r a t e of accomplishment simply by spending more time. For ins tance , f i n a l computer program tests could go only s o f a r without d i g i t i z e d da ta . It took th ree months from d r a f t of t he RFP Exhibi t A t o bid se lec t ion . Only a f t e r t h a t could arrangements be made f o r ob ta in ing t h e f l i g h t f i ln . and t r a v e l i n g t o vendors f a c i l i t i e s . But, computer processing of these da ta could progress no f u r t h e r than the point where v igne t t i ng funct ion cor rec t ions had t o be applied. Vignetting da ta , i n t u rn , was dependent on o p t i c a l t e s t s and access t o f l i g h t camera systems, and s o on.

I d e n t i f i c a t i o n of sub j ec t u t t e r , t h e c e l e s t i a l coordinates of each frame, and times and d u r a t i i o of exposures began immediately, because t h i s was of g r e a t value t o a l l o ther aspects of t h e work. This t a sk always seems r a t h e r mundane, s i n c e it does not usua l ly uncover s i g n i f i c a n t new s c i e n t i f i c i n£ ormat ion, b u t it is very important, never t h e l e s s , because it r equ i r e s t h e co l l ec t i on , a s s imi l a t i on and cross-referencing of a l l support ing da ta . This can permit researchers t o avoid some b l ind a l l e y s a t l a t e r s tages i n t he processing. Resul t s of t h i s work a r e shown i n t h e Quick-Look L i s t s included a s Attachment 3. Since they have only been d i s t r i b u t e d t o a few in t e r e s t ed persons, t he PI and Research Ass i s t an t s , Linda Schwabe and Karen Jacobs, in tzc2 t o publish t he se l i s t s ' s o o n wi th support ing information i n co l labora t ion with t he National Space Science Data Center (NSSDC) fo r much wider d i s t r i b u t i o n a s a Data Users Note.

During the Apollo 17 mission more than a hundred frames of lunar sur face t a r g e t s of opportuni ty were obtained using t h e Nikon system and type 2485 film. Most of these photographs were taken near t h e terminators o r i n ear thsh ine where t he scene br ightnesses were t oo weak f o r color f i l m o r slower lenses . Most of t he se scenes were in te rspersed throughout t he 5-211 da ta . The P I e l ec t ed t o ca ta log these frames a s a pa r t of S-211 work f o r two very p r a c t i c a l reasons, s i n c e it was not a formal requirement on any o ther PI. F i r s t , t h e support ing da t a had a l ready been co l lec ted f o r S-211 work and the PI'S d i r e c t support of t he Apollo 17 mission a s and APST member made it e a s i e r f o r him t o perform t h i s t ask , t5an f o r o the r s not f ami l i a r with t h e c e l e s t i a l scenes o r sources of support ing da ta . Second, t he d e t a i l e d work could be ca r r i ed ou t by Research Ass is tan t Karen Jacobs without s l i g h t i n g o ther on-going work.

I n t h e meantime, photodig i t iz ing se rv ices were procured on a t r i a l b a s i s by GSFC, using t h e i r In t e r cen t e r Agreement funds, from both Photometric Data Systems (PDS) of Perkin-Elmer Corp. i n South Pasadena and from Dicomed Corp. i n Minneapolis. The r e s u l t s from PDS proved b e t t e r f o r experimental

requirements, and s p e c i a l arrangements were made with another P I , D r . Don Von Steen, i n t he Earth Resources Technology S a t e l l i t e (ERTS) Prog,cam a t t h e Dept. of Agricul ture i n Washington, D. C. t o use exac t ly t h e ::am equipment t h a t had been u t i l i z e d under t he s e rv i ce con t r ac t a t PDS. This saved considerable t r a v e l and se rv i ce cos t s on the cont inuing photodig i t iza t ion work. Unfortunately, t h e i n i t i a l s e rv i ce con t r ac t s and subsequent arrangements f o r t he photodig i t iz ing work d id not g e t underway u n t i l t h e l a s t seven months of the two year cont rac t . A t t h e c lo se of t h i s cont rac t photodig i t iza t ion of some c a l i b r a t i o n and v igne t t i ng frames and a l l of t h e Apollo 17 da t a frames remained t o be done.

The d e t a i l s of t h e photodig i t iza t ion process a r e q u i t e simple i n pr inc ip le . A square ape r tu re , t h i r t y - s i x micrometers on a s i d e , of col l imated, white l i g h t is allowed t o pass perpendicular ly through t h e o r i g i n a l negat ive of a s e l ec t ed photographic frame. This beam then impinges upon a ca l i b r a t ed photomult ipl ier tube, and t h e developed g r a i n i n t h e photographic emulsion is put i n t o focus a t i t s photocathode. An output vo l tage of t h e photomult ipl ier is recorded i n terms of dens i ty , t h a t is , i n terms of the logarithm, base 10, of t ransmi t ted beam i n t e n s i t y . The beam is f i r s t stepped ho r i zon ta l l y , t h i r t y - s i x microns per s t e p , completely across t h e frame i n t h e "x-direction", which is p a r a l l e l t o a s i d e of t h e square aper ture . This is done by mechanically moving t h e s t age , t o which the f i l m i s a t tached , using computer cont ro l led servo- motors. A t the end of t h i s l i n e scan, t h e s t age is stepped v e r t i c a l l y downward i n t h e "y-direction" by t h i r t y - s i x microns and scanned back i n t he "negative x-direction". Ind iv idua l readings and information on pos i t ion a r e temporarily s tored by t h e cont ro l computer, then w r i t t e n onto a magnetic tape a s a s t r i x g of values following the frame ident - i f i c a t i o n group loaded by the o ~ e r a t o r . One 35 mm frame scanned s ide- to- s i d e from t h e bottom p a r t of upper sprocket holes t o t h e t op p a r t of lower sprocket ho les r equ i r e s about f o r t y minutes and produces approximately 0.7 mi l l i on s epa ra t e readings. The g ra in s i z e on t h e very high-speed, 2485 type emulsion is a l ready on t h e order of t en microns; so, t he re is very l i t t l e r e s o l u t i o c l o s s using t h e t h i r t y - s i x micrometer beam. The f i l m could e a s i l y be d i g i t i z e d t o a higher r e so lu t ion , but t h a t e f f o r t would prove was te fu l i n terms of t h e add i t i ona l computer s to rage and da t a manipulations required. For instance, i f t h e ape r tu re were reduced t o twelve microns square, the photodig i t iza t ion time, t h e d a t a s torage a r r a y size, and subsequent computer manipulations would each increase by nine times.

Vignet t ing tests had t o be performed with grea t care . These t e s t s were delayed by non-ava i lab i l i ty o f , f i r s t , f l i g h t camera8 from JSC and, second, personnel and laboratory space a t GSFC. The t e s t s were f i n a l l y ca r r i ed out during the l a s t t h r ee months of the cont rac t . The procedure

f o r t h e s e t e s t s r equ i red t h a t photographs be made of a p e r f e c t l y uniform f i e l d of w h i t e l i g h t by each f l i g h t camera system a t t h e same l e n s f - s t o p s e t t i n g and i n t h e same f i l t e r c o n f i g u r a t i o n a s t h a t used f o r t h e d a t a c o l l e c t i o n . The image of t h i s scene recorded on t h e emulsion showed g r e a t e s t exposure a t t h e c e n t e r of t h e frame w i t h response dropping o f f towards t h e edges and l e a s t response a t t h e corners . T h i s f a l l o f f i n apparen t l i g h t l e v e l is very pronounced f o r l a r g e l e n s a p e r t u r e s , t h a t i s , f o r low f - numbers. However, l a r g e a p e r t u r e s e t t i n g s a r e r equ i red f o r c o l l e c t i n g a l l of t h e a v a i l a b l e l i g h t i n low b r i g h t n e s s scenes . Thus, t h e s e s e t t i n g must b e used and t h e d a t a c o r r e c t e d f o r t h e i r e f f e c t s l a t e r .

T e s t photographs of v i g n e t t i n g on c a l i b r a t e d f i l m is t h e means f o r doing t h i s . These t e s t frames a r e d i g i t i z e d j u s t l i k e d a t a frames. From t h e i r step-wedge c a l i b r a t i o n s , e m u l s i o n d e n s i t y can be conver ted t o a b s o l u t e i n t e n s i t y over t h e frame, then normalized t o t h e maximum value . The l o g a r i t h m of t h e s e normalized read ings w i l l be z e r o a t t h e b r i g h t e s t p o i n t on t h e o p t i c a l a x i s near t h e c e n t e r of t h e frame. A t d i s t a n c e s away from t h e o p t i c a l a x i s , t h e l o g w i l l have n e g a t i v e va lues of l a r g e r and l a r g e r magnitude.

T h i s ma t r ix of va lues is a l i g n e d w i t h t h e d i g i t i z e d emulsion d e n s i t i e s conver ted t o l o g i n t e n s i t i e s f o r a p p r o p r i a t e d a t a frames. The v i g n e t t i n g l o g i n t e n s i t i e s a r e then s u b t r a c t e d p o i a t by po in t from t h e d a t a l o g i n t e n s i t i e s , which i n c r e a s e t h e r e s u l t i n g values p r ~ ; ~ r e s s i v e l ~ f u r t h e r away from t h e o p t i c a l a x i s . I n e ssence , t h i s mathemat ica l ly r a i s e s t h e i n t e n s i t i e s away from t h e c e n t e r of t h e frame by t h e i n v e r s e r a t i o of t h e v i g n e t t i n g f a l l o f f , which is e x a c t l y t h e d e s i r e d r e s u l t . T h i s process r e q u i r e s c a r e f u l de te rmina t ion of t h e emulsion response , o r I1H&D" curves , bo th f o r t h e d a t a and f o r t h e v i g n e t t i n g s o t h a t a c c u r a t e a b s o l u t e measurements can b e made and preserved throughout t e d i o u s computer manipula t ions .

T h i s l a s t c o n s i d e r a t i o n cannot b e overemphasized, and i t i s t h i s u s e of t h e VICAR program by S211which is somewhat unique, g i v i n g an e x p l o r a t o r y n a t u r e t o t h i s image process ing technique. On previous programs some of t h e a v a i l a b l e p rocessors of VICAR had been used t o enhance, purposely , t h e scene b r i g h t n e s s e s o r s t r e t c h t h e i r c o n t r a s t s s o t h a t l u n a r s u r f a c e d a t a might y i e l d more d i s c e r n a b l e f e a t u r e s f o r s c i e , ~ t i f i c s tudy . T h i s i s q u i t e v a l u a b l e f o r c r e a t i n g d a t a format ted f o r b e s t i n t e r p r e t a t ion by t h e eye. Unfor tunate ly , it purposely d i s r e g a r d s t h e f i d e l i t y of t r u e scene b r i g h t n e s s e s o r r a t i o s oi b r i g h t n e s s e s . Work performed under t h i s c o n t r a c t had t o use t h e o p p o s i t e emphasis and t a k e g r e a t pa ins t o p rese rve q u i t e a c c u r a t e l y t h e b r i g h t n e s s .

This has kept t he pace slow and d e l i b e r a t e f o r t he i n i t i a l d a t a processing, Qual i ty , in terms of photometric accuracies , is the u l t imate goal of t h i s da ta ana lys i s e f f o r t . Where t he br ightnesees a r e j u s t on t h e threshold of d e t e c t a b i l i t y , t he abso lu te e r r o r ba r s increase rap id ly . Th i s , i n t u rn , has g rea t in f luence on determinating t h e ex t en t of l i m i t s f o r vague, ragged edged phenomena, So f a r , only a few of t h e Apollo 15 d a t a frames have progressed t o t h e s t a g e of corrected br igh tnesses across t h e i r c e l e s t i a l scenes.

Besides the br igh tness computations, computer programing has begun bu t r e s u l t s have not ye t been forthcoming, on two other p a r t s of t he work. The f i r s t of these is the VIEWS Program obtained from JSC. When t h i s program is supplied with an appropr ia te s t a t e vec tor , look angle and f i e l d - of-view s p e c i f i c a t i o n s , it w i l l compute instantaneous c e l e s t i a l coordinates , and it then p l o t s s t a r s , p lane ts and su r f ace f ea tu re s of e a r t h or moon t h a t f a l l i n t o t he f ie ld-of -view. The program i s ac tua l ly a synthes i s of s eve ra l , i n d i v i d ~ a l subprograms i n which each pa r t takes a s i t s input t he output of t he preceding par t . Thus, a given s t a t e vector is in tegra ted forward or backward i n time by a Lunar Tra jec tory Module (LTM) t o the moment of i n t e r e s t where look angle and field-of-view spec i f i ca t i ons a r e supplied. Limit ing coordinates of t h e scene a r e developed s o t h a t a l i b r a r y of s t a r and planet pos i t ions and magnitudes can be searched and those ob j ec t s f a l l i n g wi th in t h e scene a r e converted t o p l o t coordinates . F i n a l l y , i f e i t h e r the e a r t h o r moon is i n view, an or thographic pro jec t ion of vector segments ahowing su r f ace d e t a i l s is added and occul ted s t a r s removed. An opt ion is a v a i l - a b l e t o add c e l e s t i a l , geographic and/or selenographic coordinate l i n e s a s well. The computer program which performs these searches and ca l cu l a - t i o n s f i n a l l y produces a magnetic p lo t t ape f o r use on a Stromberg Carlson 4060 P l o t t e r , D i g i t a l values on t h i s tape d r ive both scan and i n t e n s i t y c i r c u i t s of a cathode ray tube t o produce the f i n a l p l o t s f o r recording on rnicrof i l m .

It was intended t o use t h e VIEWS Program t o make c e l e s t i a l over- l ays t o match important da t a frames. While checkout of the program d id reach the s t a g e where p lo t tapes were produced, the need f o r thLs type of d a t a was considered l e s s important than checkout of the VICAR Program software; so, no overlays had been developed a t t h e completion of t h e cont rac t . The LTM rou t ine was used separa te ly , however, i n an attempt t o compute t he instantaneous pos i t ion of t h e lunar l i b r a t i o n point Lq with s o l a r and planetary per turba t ions included. Resul t s irom 4p0110 15 of one four-minute exposure i n t h e supposed d i r e c t i o n of L4 madv t h i s support ing computation important. But, a f t e r s eve ra l weeks work, i t was c l e a r t h a t the LTM program could not be used i n khis way. b second computer program using a Double-Precision Tra jec tory (DPTr3j) rou t ine

was obtained and checked out f o r t h i s work. Several weeks were needed t o t a i l o r it t o t h e L4 problem, and here again, such work had t o cease s o t h a t t he computer consul tan t , M r . Alvord, could he lp with t he VICAR processing. The ex ten t t o which the e f f o r t had prw? a l s o indicated t h a t it would be b e t t e r t o delay f u r t h e r comput~ii. ; . , A 1 1 the L4 point u n t i l t he da ta frame had been processed and an, ,yzed tu .:ssure t h a t publ ishable da t a was obvious on the fi lm. It u ~ i l l s e w . ' ..s doubtful t h a t t h e Lq region of l i g h t enhancement is present on t h i s frame. Although t h i s frame is one of a dozen t h n t a r e t he f u r t h e s t along i n ana lys i s , add i t i ona l VICAR processing w lll be required p r io r t o publ ica t ion of s c i e n t i f i c r e s u l t s .

There have been many i n t e r r e l a t e d a c t i v i t i e s between t h i s con- t r a c t e d e f f o r t and NASA Centers. Planned use of government teams and f a c i l i t i e s was made, of c o u r s e , . i n the i n t e r e s t of economy. However, i n many instances the scheduling of t h e government's support could not be advantageously timed, and t h i s is p a r t l y t he reason why the con- t r ac t ed e f f o r t has been delayed. Reporting of t echnica l a c t i v i t i e s had always been an important r e s p o n s i b i l i t y put on t he cont rac tor , but i t has not been a companion requirement on government supportirkg groups, and the intermeshing of mileetones has not been c l e a r t o a l l . Verbal communications were good, i n genera l , but t h e lack of posit ive, management techniques including w r i t t e n technica l r epo r t s and published schedules f o r o v e r a l l con t ro l of t h i s work, whether in o r out of government, has caused hards'hips, This point is reported here not a s an excuse f o r de lays , but s o t h a t f u t u r e arrangements of t h i s type can be s t rength- ened. A s smaller budgets put cons t r a in t s on NASA's s c i e n t i f i c work, it could appear prof i t a b l e t o use j o i n t personnel t e a m and f a c i l i t i e s . Whether t he r e s u l t s produced from such arrangements a r e t r u l y economical w i l l depend on the government's giving equal weight t o managemsnt of i t s 4nhouse p a r t i c i p a t i o n a s wel l a s i ts contracted e f f o r t s .

Important Related Matters

A t t h e beginning of the cont rac t , t he P I designed two f i l t e r s f o r use with the f l i g h t Nikon camera system. With dedicated s e rv i ce s from engineer ing, d r a f t i n g and t h e mechanical shop a t Dudley, these f i l t e r s progressed from concept t o acceptance f o r f l i g h t and de l ive ry t o the launch s i t e i n about nine weeks t o ca r ry out an APST requirement on t h e Apollo 16 f l i g h t . One f i l t e r provided a b lue bandpass from 510 nanometers t o t he Cornmand Module window cutoff a t about 420 nanometers; the o ther provided a red bandpass from 610 nanometers t o type 2485 f i l m s e n s i t i v i t y cu tof f a t 700 nanometers. These s p e c i a l f i l t e r s were needed t o photograph suggested emission l i n e s of hydrogen i n the red and s ing ly and doubly ionized oxygen i n t he b lue from the Gum Nebula while suppressing l i g h t from the Milky Way

region beyond. A second set of these t i l t e r s flew on Apollo 17 fo r two, very success fu l photographic series of t he zodiacal l i g h t , another APST requirement.

During the f i r s t year of t h i s cont rac t t he PI and Co-f were a l s o very busy support ing the APST a c t i v i t i e s f o r thc Apollo l b f l i g h t i n Apr i l and the Apollo 17 f l i g h t in December of 1972. Those f l i g h t schedules and r e l a t e d support work necessar i ly d i c t a t ed when and where the i nves t i - ga to r s could apply themselves t o work under t h i s cont rac t . On the one hand, it d id delay e a r l y t r a i n i n g by the PI of h i s two Research Ass is tan ts brought on s p e c i f i c a l l y t o he lp in t h i s work, and i t hampered e a r l y a t - tempts t o follow i n s t i t u t i o n a l management of the con t r ac t , mainly b e c a u ~ e the PI had t o spend considerable time t r ave l ing t o NASA Centers, On the o the r hand, t h i s t r a v e l permitted b e t t e r coordination of t h e PI'S e a r l y da t a reques t s t o NASA, aqd APST t r i p s t o the West Coast were very usefu l i n the f i n a l s e l e c t i o n of t he computer program f o r processing photodigi- t i z ed data . Furthermore, i t was extremely valuable f o r t he P I and Co-I..& t o b i ' a b l e . t o thinksthrough t h e i r photocal ibrat ion and support ing da t a needs p r i o r t o each of these l a s t two f l i g h t s when spec i fy ing experimental requirements a s members of t h e APST. I n r e t ro spec t , t h e wearing of these two h a t s was b e n e f i c i a l ove ra l l , but e a r l y milestones i n t he da ta ana lys i s e f f o r t suf fe red a s a r e s u l t .

A t h i r d r e l a t ed matter regards t h e f i n a n c i a l and adminis t ra t ive support of t h i s con t r ac t by Dudley Observatory management. This support became a negat ive f a c t o r of l a r g e proportion a f f e c t i n g el' phases of the work. The PI and h i s a s s i s t a n t s had t o spend conside- , , time checking and recons t ruc t ing f i n a n c i a l da ta ; t h i s time dimini- . i e i r s c i e n t i f i c and technica l e f f o r t s . The author of t h i s repor t n ieves q u i t e f i rmly t h a t Dudley management does not have the q u a l i f i c a t , experience o r d e s i r e t o dea l with day-to-day a f f a i r s of s c i e n t i f i c ,.fogram adminis t ra t ion , and t h a t management ac t i ons a r e only taken t o dea l wi th c r i s e s .

A t t h e PI'S request t h e government stepped i n t o review the s i t u a - t i o n two-thirds of t h e way through the contract . The i r review and f i n a n c i a l a u d i t r e su l t ed i n Dudley management re turn ing $20,288 t o a $92,541 e f f o r t . A t the c lo se of t h i s con t r ac t , some e i g h t months a f t e r t he s t a r t of t he government's review, t he Observatory is s t i l l in the process of deve!.oping f i n a n c i a l , adminis t ra t ive and personnel po l i c i e s under duress and under continuing sc ru t iny by government monitors. Even though t h e s c i e n t i f i c goa ls sought under t h i s con t r ac t a r e j u s t now nearing publ icat ion s t age , t h e PI has e lec ted t o c lo se out work under the Dudley Observatory a t t he f i r s t convenient opportuni ty s o a s no: t o subjec t the government o r himself and h i s team t o f u r t h e r waste of time and money t o he lp an i n s t i t u t i o n so lve i t s own, i n t e r n a l l y c rea ted problems.

Conclusions

The conclusions a t the c lose of t h i s con t r ac t a r e a s follows:

Resul t s of t h i s da t a ana lys i s work a r e near ing the point of publ ica t ion f o r NASA and the s c i e n t i f i c community. The o v e r a l l e f f o r t i s approximately s i x t o nine months behind the o r i g i n a l schedule, but the q u a l i t y expected i n r e s u l t s has undergone improvement. Brightness measurements w i l l be tnost success fu l fo r (1) t he zodiacal l i g h t i n polar ized and p l a in white l i g h t and i n red and b lue l i g h t from about one t o e tgh ty degrees elongation and fo r (2) t he lunar l i b r a t i o n r eg io r L4 i n white l i g h t .

2. The requirement f o r con t ro l l i ng t echn ica l progress through technica l repor t ing and milestone scheduling is, of course, v i t a l , bu t it must be extended t o i n c l d e inhouse government technica l a c t i v i t i e s supporting outs ide contracted e f f o r t s .

The uncertain na ture of da ta ana lys i s work, particularly when port ions of th2 da t a a r e not y e t co l l ec t ed , r equ i r e s t h a t cont rac tua l goals and schedules undergo per iod ic review t o change emphasis a s needed. This is p a r t i c u l a r l y t r u e f o r work where t he d a t a a n r l y s i s techniques themselves a r e under- going development, and time is needed f o r exploring var ious opt ions. T h i ~ f a c t o r determines the res-arch versus the product ion na ture of t he da ta ana lys i s t asks .

Recommendat ions

Recommendations concerning t h i s work a r e a s follows:

1. This da ta reduct ion and ana lys i s work should be continued, It w i l l ptovide two important r e s u l t s . F i r s t , i t w i l l complete the debalcpment of new techniques f o r accomplishing photographic photometry using sophis t ica ted computer techniques. Second, new s c i e n t i l i c measurements w i l l r e s u l t from completed ana lys i s of t h e zodiacal l i g h t ar.d lunar l i b r a t i o n region, Lq, d a t a n w in processing.

2. Data m a l y s i s work should t e c a r e h l l y assessed fo r t he degree of nev techniques required. The quant i ty o r r a t e of production fo r processed da t a and the tfme involved should be extended ir. proportion t o t he unce r t a in t i e s i n such developmental e f f o r t s .

The author wishes t o express h i s s incere appreciation t o the many NASA and supporting contractor personnel whose help has made the present level of accomplishment possible. Some of these people have been mentioned above, and the author wishes t o include i n h i s thanks Dr. Floyd I. Roberson, Essers. S. Nat Hardee, Tony C. Riggan, James Taylor, and James Ragan of NASA, Mr. Paul Hopkins of the Department of Agriculture, and M r . Joe Dixon and J. Wesley Simpson of Lockheed A i r - c r a f t Corp.

I n addition t o two Research Assistants a t Dudley Observatory, the work benefi t ted grea t ly from the excellent services of M r . Dave Wachtel, photography, his. Gail Chien, draft ing, and Mrs. Gen Pruscop, typing

MSG/GSFC AGREEMENT

APOLLO LOW BRIGHTNESS IMAGE ANALYSIS

The tasks t o be performed by GSFC, i n support o f pol lo Low Brightness Image Analysis and the Dudley Observatory, are speci f ied i n the attached statement o f work. This w i l l apply t o f i l n analy- s i s f o r Apollo Missions 14, 15, 16, and 17. The re la t ions and e f f o r t between the two renters w i l l be conducted according t o t h i s agreement .

Approved :

~anned- Spacecraft Center

fl~i rec t o r Goddard Space F l i ght Center

STATEMENT OF WORK

Number:

Experiment Long T i t l e : Low Brightness Image Analysis

Experiment Short T i tl et Same

Concurrence : Concurrence (MSC) : n

L L r B - H h A Principal Investigator

- Co-Invest1 ga tor (GSFC:

STATEMENT OF WORK

SERVICES REQUIRED OF GODDARD SPACE FLIGHT CENTER IN SUPPORT OF LOW BRIGHTNESS IMAGE ANALYSIS (DUDLEY OBSERVATORY)

1 .O PURPOSE

1 . I The purpose of th is statement of work (SOJ) i s t o define those services which are required of; GSFC in support of the Low Brightness Image Analysis. In addition, these services will pertain to the support of the NASA/MSC Experiment Manager for th is analysis.

2.0 OBJECTIVES

2.1 To furnish the sensitometric equipment and accessories necessary to give the support required to complete the subject analysis.

3.0 TASKS

3.1 Close coordination i s required between the PI, Co-I, GSFC technical personnel, and the MSC Experiment Manager on a l l aspects of GSFC's services in support of the Low Brightness Image Analysis. Mr. L. Dunk1 eman, Co-Investigator, i s completely responsible for the management and imp1 ementation of a1 1 GSFC effort .

3.2 A11 original f i l m applicable to Apollo 14, 15, 16, and 17 D i m L i g h t Photography will be transmitted t o Mr. Dunkleman, Co-I. He will have the responsibility of their transmittal for analysis, safekeeping, and ultimate return t o MSC.

3.3 GSFC will provide the densitometer and related equipment necessary to provide isophotes, isodensitracings, and digital program readouts on magnetic tape.

3.4 GSFC will provide the necessary technical personnel (including computer programner) to secure the data required by the PI, cal ibrate the equipment, and maintain the optimum equipment performance.

4.0 DOCUMENTATION REQUIREMENTS

4.1 Monthly Cost Reports to date

4.2 Quarterly Cost Projections per 533 requirements

5.0 FUNDING REQUIREMENTS

Funding requirements are as follows:

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NASA CONTRACT NAS9- 12557

Apollo Data Analysis

Experiment S-211

LOW BRIGHTNESS IMAGE DATA ANALYSIS

DATA ANALYSIS AND HAIUDLING PLAN

Prepared for

National Aeronautics and Space Administration Johnson Space Center

Houston, Texas 77058

Robert D. Mercer Principal Investigator

March 30, 1973

The Dudley Observatory 100 Fuller Road

Albany, New York 12205

General

This document presents a plan for data handling and analysis of low brightness images from those portions of astronomical photography covered by Experiment S-211 (Contract NAS9-12557). This plan is required from the Principal Investigator (PI) both scientifically and contractually for good reasons. First, it assures that the methods and procedures for accomplishing the final objective have been clearly thought through. This assures that maximum scientific content will be extracted within the time and cost scope of the contract. It also guarantees that original photographic materials will be properly safeguarded by the PI prior to their release to him and his team.

It was originally proposed that individual plans be submitted for each of the Apollo missions covered by this data reduction work. However, the similarity in procedures, particularly with regard to the establishment and utilization of image brightness digitization techniques to be followed by highly sophisticated computer processing, indicated that one overall procedure could be written. This composite plan is presented below and applies equally to photographic images, calibrations, and equipment test data for each miosion covered by this data analysis work, namely Apollo flights 14,15,16 and 17.

Data Processin9 F l o w

An overview of the data handling and analysis process will now be presented. Figure 1 shows this data flow in block diagram format. This will be followed by an elaboration on certain special details such as film handling and the like.

Master positive transparencies and duplicate negatives of each photographic data frame will be scanned visually to ascertain the scientific value, image quality and data reduction priority of each frame. Quick-look identification listings of all frames will be mde. These listings relate frames by their NASA photo numbers to the times made, subject matter, approximate celestial location and orientation, and associated camera donfiguration and settings. These lists, one for each flight from Apollo 14 to 17 inclusive, become interim but finished products that are individually complete enough for use by others. In that sense they will be made available to all NASA personnel associated with this work, including the National Space Science Data Center (NSSDC), outside scientists, and interested laymen lho 'express a specific interest in our early results. Such lists are p.rticu1arly important in this field of work where the phenomena under study are relatively unknown and where there is a very limited number of easily identifiable objects even to the trained eye of most astronomers.

2

. .G:* . I'D,' w APPLY PREFLIGHT CALS . -. - . , ON F L I G H T & BACK-UP FIUl

GROUI'TD BASED PHOTO LUNAR ORBIT PHOTOS ON BACK-UP F I L M ~5- ON FLIGHT I F I I M

RETURN BACK-UP t ,, 1 F I U 4 A

RECOVERY & RETURN OF

I ORIGINAL FLIGHT F I U 4 --.-.-.-.-.-. L I

- I

APPLY PoSTFLIGH!J! CALS

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m s u R E M E M T s , *

ANALYSES & _ INTERPRETATION I COMPATABLE TAPES)

I

VICAR PROGPAM EVAL, ANAL 17mssrro/ l a y (

PRODUCTION OF OVERLClYS r"l

PRODUCE S L I D E S FOR PRESENTATIONS -j/

-

1 FINAL ANALYSES, -1 & IncpImwTIw a' S I G ~ ~ C E - , , .~-h.n,,,i-.l.,., '.,,',. . , - . . , . . I . . . .,, 1, . . . , ,, ,,,, .... .,, .I . . . - 8 . . ..-a,. . . ....-..,.

\t I * * * a

PRODUCE FIGURES PRODUCE SLIDES FOR PUBLICATION FOR PRESENTATIONS

I I I

PUBLICATION * PRESENTATIONS

SCIEi'TCE DATA

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I NASA SCIEWNl?IC 1 [ ASTRONOiYlICAL & SCIENTIFIC 1

Figure

Concurrent with this effort, data technicians will make blow-up prints from the master positives and duplicate negatives. These prints are much easier to handle and to study for more detailed visual analyses. They are absolutely essential for measurements of angles and distances between celestial objects; such data extracted from these working prints will be used as numerical inputs to sophisticatsd computer processing 1::er. In addition, such prints and associated projector slides are used for presentations and publications of preliminary results required by NASA. They are required by the scientific obligations inherently levied on all investigators as reporters to their disciplines within the scientific community at large.

Second and third generation 35mm format film must also be used for some photometry and microdensitometry. Certain frames will undergo unsophisticated measurements to determine approximate values of brightness of key features, ranges of brightness within a frame and base fog levels. From these analyses a first selection of frames will be made for further processing.

This initial group will contain the following information: data frames, brightness calibration frames, and exposures to assess the brightness portion of the optical transfer function for the flight lenses and for the image digitizing equipments used in the data reduction process. Lens calibration photography will be obtained by the Co-Inves;*gator (Co-I) usiny appropriate optical laboratory faciJ.ities and components at NASA's Goddard Space Flight Center (GSFC) . All of these photographic images will be digitized from original flight and ground calibration negatives using the most economical and scientifically qualified technique available. The digitizing services will be obtained by the Co-I through the GSFC Procurement Office using a portion of the funds transferred for this work from the NRSA Johnson Space Center(JSC) to GSFC. A suggested Statement of Work for the first digitizing effort is included as Appendix A. The results of this work will be a set of digitized brightness measurements for each frame recorded on computer-compatable magnetic tapes.

These tapes along with progrqm control statements and other numerical data from earlier processing will become the input to the Video Image Communication and Retrieval (VICAR) Program developed by the Jet Propulsion Laboratory (JYL) and now being made operational at GSFC for a number of image processing applications. The VICAR Program will be used for the many tasks specified below.

1. Eliminate camera lens and digitizing equipment brightness recording (vignetting) effects.

2. Locate and eliminate stzrlight.

3. Smooth unnatural discontinuities in digital readings.

4. Create brightness-versus-position contour (isophote) maps.

5 . Match up and extend isophotc maps over many adjacent frames.

G. Perform spec i a l addi t ions of data where scenes overlap and s igna l s a r e extremely weak.

7. Remove image motion from longer exposures where r a t e s of change i n vehicle a t t i t u d e s could not be avoided.

This VICAR Program processing i s i t e r a t i v e , i . e . the r e s u l t s oE manipulations with any data s e t must be analyzed by both inves t iga to r s and programers t o bes t determine what subsequent VICAR processing must be attempted. Moreover, the same s e t of br ightness measurements may undergo severa l d i f f e r e n t kinds of computer processing depending upon the pa r t i cu l a r s c i e n t i f i c ob jec t ive being sought.

Another computer e f f o r t , using the VIEWS Program Ceveloped a t JSC, will be ca r r i ed out a t Dudley Observatory t o produce s t a r f i e l d and c e l e s t i a l coordinate overlays f o r se lec ted da ta frames. It w i l l be checked out on a Univac computer a t the S t a t e Universi ty of New York i n Albany. Inputs t o t h i s program w i l l include: t ime-related t r a j e c t o r y s t a t e vec tors , telemetered a t t i t u d e and r a t e data f o r t he Command Modules, and the data cameras' l ines- of-s ight and fields-of-view with respect t o the vehicles ' body axes. Output wi l l be computed pointing pos i t ion and a spec i a l computer magnetic tape f o r processing o r i en t a t ion on the SC4060 p l o t t e r a t GSFC. Processing by the p l o t t e r w i l l produce scenes iden t i ca l ly located on the c e l e s t i a l sphere a s the da ta frame made a t the same corresponding time. These microfilms w i l l be enlarged and printed on or tho, clear-backed, f i lm base t o produce ovcrlays f o r working p r i n t s of the datz frames. A copy of the microfilm w i l l a l s o be provided t o NSSDC, s ince i t w i l l be very usefu l f o r o ther researchers who might wish t o ex t r ac t o ther information from the f l i g h t data .

F ina l r e s u l t s of a l l of the above work w i l l be informatiori f o r publ icat ion i n NASA documents and s c i e n t i f i c journals including statements on the in t e rp re t a t ion and s igni f icance of f indings. Accompanying analyses w i l l attempt t o provide mathenatical expressions f o r the br ightness pa t te rns being s tudied. Where possible , information on polar iza t ion and s p e c t r a l parameters w i l l a l s o be included.

The i n i t i a l group of o r i g i n a l data and ca l ib ra t ion frames, containing approximately 20% of a l l frames which might eventually be processed, w i l l be d i g i t i z e d and s t a r t e d through the handling and ana lys is process a s a v e r i f i c a t i o n tha t the procedures a r e adequate and t h a t de t a i l ed problems i n the da t e flow a r e well understood. The suggested Statement of Work i n Appendix A i s meant t o include only t h i s i n i t i a l group. Once t h i s work has progressed t o the point where intermediate r e s u l t s , including computer outputs , a r e ava i lab le f o r inves t iga tor ana lys is , decis ions w i l l be made on which frames and how many of the remainder should a l s o be d ig i t i zed . This a l s o assures tha t a l l f i nanc ia l resources a r e not expended onlv on e a r l y s tages of data reduction without reaching f in i shed conclusions on a t least. some port ion cf the work.

It should be f u r t h e r noted t h a t d e t a from A p o l l ~ ~ Lunar Experiment S178, ~egensch ien /Moul ton Region w i l l a l s o be handled i n a s i m i l a r manner, s i n c e i t is a l s o conta ined on t h e same f l i g h t emulsion and because i t s s u b j e c t m a t t e r i s analogoud t o t h e low b r i g h t n e s s phenomena under t h i s t a s k . I a f a c t , some e a r l y d i g i t a l d a t a read from S178 frames on GSFC Joyce-Loebl m i c r o d e n s i t m e t e r is be ing used a s t z s t i n p ~ f o r e a r l y checkout of VICAR Program process ing rout . ines. One important conclus ion from t h i s t e s t \Jrk h a s been t h a t d i g i t i z a t i o n on t h i s GSFC equipment i s f e r t o o slow and expensive f o r t h e amount o f d a t a y e t t o be d i g i t i z e d . Therefore , i t has been necessa ry t o tieek vendor s e r v i c e s t h a t were not o r g i n a l l y contemplated. It h a s fur the . . been a s c e r t a i n e d t h a t such an approacl: w i l l d e f i n i t e l y be muck f a s t e r and l e s s c o s t l y f o r t h e government, and e t t h e same t ime IL w i l l g r e a t l y reduce t h e amount of f i l m hand l ing necessa ry f o r t h e o r i g i n a l f l i g h t i "qa t ives . Th i s i s t h e on ly subcont .-acted e f f o r t t h a t i s now fo reseen .

Handling of O r i g i n a l F l i g h t Nc , a t i v e s

I n Figure 1 a dash-dot l i n e has b e e . added t o show t h e path fo l lowed by t h e o r i g i n a l f l i g h t f i lm. It ill on ly be r e q u i r e d by t h e P I and h i s team dur ing t h e d i g i t i z a t i o n process a f t e r which i t i s r e t u r n e d t o NASA JSC f o r a to rage . I t is proposed t o a r range i n advance f o r t h e s e uses s f t h e o r i g i n a l photographic m a t e r i a l s . Then t h e P I o r h i s a u t h o r i z e d r e p r e s e n t a t i v e w i l l pe r sona l l ) p ick i t up a t JSC, hand c a r r y i t t o t h e v e n d o r ' s s i t e of d i g i t i z a t i o n , remalr. wi th t h e f i l m and moni tor t h e d i g i t i z i n g prr.:ess, and r e t u r n t h e f i l m t o JSC by hand-carry immediately t h e r e a f t e r .

A s noted p rev ious ly , not a l l frames w i l l be d i g i t i z e d i n i t i a l l y . There fo re , a minimum of two such t r i p a r e necessary , and i t is expected t h a t t h i s would be t h e maximum, a s w e l l . I f problems occur i n s a t e r s t a g e s of t h e d a t a process ing t a s k s f o r t h e i n i t i a l group d i g i t i z e d , i t could r e q u i r e t h a t t h r e e o r , a t t h e ve ry most , f o u r t r i p s m i ~ h t be necessary . I n each i n s t a n c e i t i s expected t h a t t h e o r i g i n a l f l i g h t nega t ives wo*.~ld be away from JSC no longer than one week a t a time.

A t l a t e r s i a g e s i n t h e ana lyses i t might be necessary t , make a few s p a c i a l readings on t h e GSFC m i c r d e n s i t o m e t e r s t o c l a r i f y l e r t a i n read ings i n t h e product ion phase d i g i t i z a t i o n performed prevLously a t t r i e vendor ' s f a c i l i t y . Here, aga in , t h e t ime away from JSC might be a s long a s one month f o r any recheck, and arrangements f o r handl ing and s t o r a g e a t GSFC would be i d e n t i c a l wi th t h o s e a l r e a d y used f o r the S178 f i l m w i t h hand-carry back and f o r t h between NASA c e n t e r s .

A t NASA c e n t e r s and the0vendor t s f a c i l i t y t h e o r i g i n a l f l i g h t f i l m w i l l be mainta ined a t 702 10 F and 50+ ~ 5 % r e l a t i v e humidity normally provided by a i r condi t ioned o f f i c e s and optics? l a b o r a t o r i e p Wheu not i n use o r i n t h e hands of r e spons ib le personnel , i t w i l l be s t o r e d i n locked c o n t a i n e r s l o c a t e d i n a i r cond i t ioned quarters. During t r a n s i t i t w i l l be double-bagged po lye thy lene envelopes s e a l e d a i r - t i g h t t o avoid humidity chavges. The c o ~ r i e r

w i l l i n s u r e t h a t t h e f i l m c o n t a i n e r s do not exper ience excess ive temperatures o r rap id changes i n temperature.

Film w i l l be handled d i r e c t l y only wi th gloved hands on i t s edges o r on i t s base s i d e , and c l o t h mouth-guards v i l l be used when f i l m i s under examination o r when personnel must work i n c l o s e proximity t o t h e f i lm. L igh t t a b l e s and o t h e r s u r f a c e s wi th which f i l m may come i n con tac t w i l l be c leaned by normal o p t i c a l procedures, i . e . g rease and o i l f i l m removers a p p l i e d , wiped d ry wi th a c lean , l i n t - f r e e c l o t h and a f i n a l l e n s t i s s u e rub down. Emulsion s i d e of o r i g i n a l f i l m w i l l always be maintained away from mechanical s u r f a c e s . Emulsion s i d e of f i l m w i l l only come i n con tac t wi th mechanical o r o p t i c a l su r faces a t sprocket ho les o r o u t e r edges dur ing frame by frame t r a n s p o r t o r i f c u r l must be removed using edge clamps.

Requirements f o r Data from NASA

I n i t i a l sources of da ta f o r t h i s d a t a reduc t ion and a n a l y s i s work a r e , of course, NASA JSC. Figure 1 shows t h e types of d a t a t h a t must come t o t h e i n v e s t i g a t o r s f o r t h e i r use. Some of t h e s e requirements a r e a s s p e c i f i e d i n t h e Mission Requirements Document (MRD) and Photographic D i s t r i b u t i o n Plans f o r each miss ion on which t h i s photography was accomplished.

I n genera l , they include:

Best Estimated T r a j e c t o r y d a t a dur ing per iods o f low b r i g h t n e s s photography i n each miss ion. One copy of t h i s da ta i s required on computer compatable magnetic t a p e s o r on microfi lm pr innout accompanied by documents on formats .

Command Module a t t i t u d e s and r a t e s da ta i n Ear th Centered I n e r t i a l (ECI) coord ina tes dur ing these same per iods . One copy of t h i s d a t a i s requ i red e i t h e r on magnetic t apes o r on s t r i p c h a r t recordings wi th formats s p e c i f i e d .

Command Module te lemetry measurement numbers CGOOOl V on Apollo 14, CK 1043 Y on Apollo 15, CK 1040 X and CK 1043 X on Apollg 16, and CK 1043 X on Apollo 17 dur ing t h e s e same per iods on s t r i p c h a r t recordings a t t e n inches per second. Data channels and time channels must be proper ly i d e n t i f i e d , and t ime code format s p e c i f i e d .

Conmand Module a i r - to-ground vo ice t r a n s c r i p t s wi th time r e f e r e n c e s f c r t h o s e comments a p p l i c a b l e t o t h i s photography, One copy i s r ~ q u i r e d , and t h i s must s p e c i f i c a l l y inc lude p e r t i n e n t por t ions of t b DSE Voice Dump Transcr ip t ions .

Crew ~ogbooks conta ining annotated f l i g h t p lans , c h e c k l i s t s and log s h e e t s . One copy i s required f o r each, e n t i r e mission.

S c i e n t i f i c and photographic procedures d e b r i e f i n g s of f l i g h t crews.

One copy of debriefing transcriptions or voice-recorded magnetic tapes is required.

Second and third generation photographic products of all Very High- speed Black and White (VHBW) film. Number of copies must be as specified in the Photographic Distribution Plan for the PI and Co-I for applicable flights.

Original VHBW backup film used for ground based photography by the investigators and developed along with the flight film. In addition, one copy of the H & D curves used to establish control of its photoprocessing at JSC will be required.

Access to and occasional possession of original VHBW flight film under handling conditions specified previously. H & D curves of its photoprocessing will also be required.

Those, then, are the products required by the investigators from the government. The photo products can be supplied by the Photographic Technology Division. Spacecraft telemetry data, air-ground voice and debriefing transcript and logbooks can be supplied from the PIetric Data File. The postflight, Best Estimated Trajectory tapes are created by the Mission Planning and Andlysis Division. Original photographic materials should only be transferred using courier hand-carry by duly authorized representatives of the government or the PI. A11 other data sources can be mailed or shipped with appropriate follow-up communications to assure all items are received by the PI or his team members.

Scientific Disciplines Involved in Analyses

The scientific phenomena on which data are now thought to exist include:

1. Zodiacal light

2. Lunar libration region, L4

3. Diffuse galactic light

4. Large filaments and extended galactic regions

5. Lunar eclipse

6. Contamination particles near vehtcle

7. Solar Corona

The last two subjects f analy~,es will only be accomplished in coordination with Experiment S 2 1 ~ and 52,2 PI'S who have formal responsibilities for these areas of data, because there is some level of overlap between the three

experiments'requirements.

Extent of Data Analyses

The level of data reduction and analyses to be expected caunot be completely specified, as yet. It can be stated that fuil processing and analyses on each data frame and the interrelziionship between frames is a task requiring several years work and, therefore, beyond the scope of time and cost alloted for this work. However, that was not unexpected considering the degree of success in data collection from flight to flight. The major decision for the investigators, therefore, is the priority to be given to the various subjects under study and what level of data reduction to attempt in each case in order to maximize the scientific return.

The pacing item for all of this work will be the amount of output and degree of sophistication that can be achieved by VICAR Program processing. This certainly does not imply that valuable results cannot be realized without it. Indeed, some preliminary results from Apollo's 15 and 17 already reported now provide scientifically valuable information on zodiacal light and solar corona previously unknown.

The major goal of the current work will be to obtain. brightness maps to the best accuracy possible over as large an area of the celestial sphere as data frame coverage permits. Particular areas of interest will be along and close to the ecliptic plane on both sides of the sun, the lunar libration region L4, the Gum nebula, galactic light, and the lunar disk entering and leaving the earth's shadow. Brief analyses of airglow and atmospheric extinction may be attempted using the ground-based data frames made on backup film in conjunction with corresponding flight data frames.

The main goal using the VICAR Program will be the complete development of isophote maps prior to removing image smear for each frame adjudged to have scientific importance. A higher level goal, if it can be achieved within the time and cost limitations of this work, will be to integrate the isophote maps of individual, adjacent frames into a larger isophote map, but again, without consideration for image smear. Finally, if all proceeds extremely well, the goal will be to remove Image smear prior to the creation of individual and composite isophote maps mentioned previously.

Some of the procedures outlined in Figure 1 have been underway for many months. Well over half of the required data has been received from JSC. This has included all of the critical items except some camera lenses needed for calibration tests and the original flight film. Initial access to the latter will be requested in late April or early May 1973 to begin the digitization processing.

Required scientific reporting up through and including the Preliminary Science Reports (PSR) has been completed except for the phot.ographic figure for the Apollo 17 PSR. This will ,e submitted in April

1973. The excellent results from Apollo 15 were reported to the Optical Society of America (OSA) meeting at Ottawa in October 1971 and to the Committee on Space Research (COSPAR) at Madrid in May 1972. Both pa;ers were joint efforts from several investigators including the Comand Module Pilot, A. Worden. The COSPAR Paper will appear shortly in Space Research XI11 which is now in press. Similar papers on A:.ollo 17 results and on the low light level photographic effort for the comi i.ned four missions are planned for the summer of 1973; the latter will be a GSFC Technical 7e;ort. An article for the journal Sky and Telescope is also in the planni-lg .,tagen As more precise information is developed, the investigators inte~., to present papers at scientific meetings-and to submit a&iclt?s to well known journals in the field of optics, astronomy, nhysics and geuerel scl.ence.

Quick-look identification lists for Apollo missions 14,15, and 16 have been pre~sred and distributed to all appropriate parties including NSSDC. A similar list for Apollo 17 has also been made; however, it or.ly contains low brightness astronomy information. It will be completed after coordination with investigators and crew about such subjects as lunar surfacc ieatures and cabin interior scenes, that are interspersed in the VHBW film along with the astronomical data. The abbreviated list on Apollo 17 astroncmical photography has had limited distribution among investigators and among individuals at JSC who are cognizant of this work.

Additional Postmission Information Requirements

The only postmission requirements now foreseen are the use of rlight lenses and filters for transmission and vignetting calibration tests. As noted previously, data from such tests is vital in computing brightness corrections for the data frames. Part of this testing is currently underway at GSFC; however, lenses from Apollo missions 14,15, and 17 will be required by the end of June 1973. A11 flight filters have been received by the PI.

One other possible source of error has already been tested. An unexpected, weak exposure was experienced on the 16mm Data Acquisition Camera film of Apollo 14. In order to verify whether or not this effect might have been caused by a loss in window transmission, the investigators performeti postflight tests on the right-hand rendezvous window at the Rockwell International plant in Downey, California during May 1971. These tests showed negligible transmission losses. This has not been considered a source of error in subsequent flights, and requirements for such additional tests are, therefore, waived.

Conclusions

This concludes the data handling and analysis plans for low brightness image studies. As of this writing on 1April 1973, it provides a best estimate of total planning in this regard. Should additional or modified requirements arise, the investigators will communicate variances in this plan to the Technical Monitor.

1 1

APPENDIX A

STATEMENT OF WORK

Respondents to this RFP must make digital readings of black-and-white,

photographic emulsion densities on roll film to be supplied by the government.

These readings, along with appropriate identification and X-Y positional

information within each frame, must be recorded on compute-. cmpqtable magnetic

tapes. The films provided will include original photographic materials from

Apollo lunar orbital flights. This will require that a government representative

be in attendance during densitmetry operations, and the respondent must provide

safekeepiag of such film at all times when it is in his hands for processing.

Detailed specifications are provided belov:

A. Photographic Materials Input

1. 16mmfilm

a) Uncut reeled motion picture film, 40 frames per foot, 100 feet

in length, PH22. 110 perforation configuration

b) Type 2485 Eastman Kodak emulsion on 4-mil Estar base

c) Base plus fog density approximately 0.70

d) Density range of interest approximately 0.65 to 1.85.

e) Dimensions of interest for each full frame including some portion

of adjacent sprocket holes are 8 mm by 12 mm.

f ) Number of frames approximately ten (10) and they are not

located sequentially on film.

2. 35 mm film

a) Two reels of spliced film, 8 frames per foot, one reel 50 feet

in length and one reel 100 feet in length, PH22.139 perforation

configuration.

b) Type 2485 Eastman Kodak emulsion on 4-mil Estar base

c) Base plus fog density approximately 0.65 for reel #1 and

0.55 for reel #2

d) Density range of interest approximately 0.35 to 1.85 for

reel #1 and 0.35 to 1.85 for reel #2

I e) Dimensions of interest for each data frame including some

portion of adjacent sprocket holes are 38 m by 22 m,

and for partial sections of calibration frames they are

30 mm by 18 mm.

f ) Number of frames approximately thirty (30) full data frames and

ten (10) calibration frames,, with frames not necessarily located

sequentially on film.

3. 7 0 m f i l m

a) One reel of spliced film, 4.8 frames per foot, 50 feet in length,

type 2 perf orations.

b) Type 2485 Eastman Lodak emulsion on 4-mil Estar base

c) Base plus fog density approximately 0.6.

d) Dsnsity range of interest approximately 0.35 to 1.85

e) Dimensions of interest for each full data frame including some

portion of adjacent sprocket holes are 62 rmn by 62 m, and

for partial sections of calibration frames they are 30 mm by 16 mm.

f) Number of frames is approximately six (6) full data frames

and four (4) calibration frames, with frames not necessarily

located sequentially on film.

B. Digital Data Output

1. Number of gray levels to include the ranges specified above

will be sixty four (64) and steps must provide linear change

in density to within? 1% over the entire range.

2. Signal to noise ratio must be better than 20 db.

3. Two additional matrices of values must be provided to determine

A 3

densitometer flatness of field over each density range and

the largest dimension size specified. One matrix must be made

after densitometry equipment warm-up and stabilization but just

prior to reading of data and/or calibration frames; the second

matrix must be made immediately after these readings and

prior to any change in photometric settings of the densitometry

equipment.

4. Output of all digital information must be stored on 9-track, 800

bits-per-inch magnetic, computer compata3le tapes to be supplied

by the government. Storage format on these tapes will require one

value of grey level per character block.

5 . Equipment must be available to reconstruct any image from matrix

of readings on output tapes in order to verify adequacy and complete-

ness of digitization,process.

6. Scanning Specifications

a) Sizes of two dimensional scanning matrices may change from

frame to frame but will include 2048 x 2048, 1024 x 1024,

512 x 512 and 100 x 1024 matrix formats.

b) Densitometered spot size and accuracy in the X-Y centering

for each position exanined must be such that the 1024 x 1024

matrix of positions covers more than 75% of the total area

with less than 10% overlap.

c ) Scanning rates must be rapid enough that the set up and

reading of sixty (60) frames in the fonnats specified can

be accomplished within five (5) normal working days.

Qu

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search.jsp?R=19740026159 2020-02-22T07:19:37+00:00ZAbstract This is the Final Technical Report under NASA Johnson Space Center Contract NAS9-12557 for Low Brightness Image Data Analysis.The