Jun 30, 1982 - observations of the Earth atmosphere from Skylab or Salyut stations have sho~m that even a plain camera may be useful for atmospheric ...
Adv. SFacC ~cs. V o l . 5, No. 3, pp. 2 7 - 3 0 , Prin[ed
tn Great B r i t a i n .
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1985 reserved.
0 2 7 3 - 1 1 7 7 / 8 5 SO.O0 + .5C Cop,, r i g h t '~ COSP~R
ASTROPHYSICAL A N D GEOPHYSICAL OBSERVATIONS WITH PIRAMIG/SALYUT 7 EXPERIMENT A. C Levasseur-Regourd, 1 G. Courtes, 2 M. Herse, l S Koutchmy. 3 P. Lamy, 2 T. M_ Muharchik, 4 B. R o c c a - V o l m e r a n g e ) S. A. S a v c h e n k o , a B Secher: and H. M. Tovmasslan 5. Crew m e m b e r s A. N Beresovoy, 6 J. L. Chretlen, 7 A. S Ivanchenkov, 6 V. A D j a n i b e k o v . 6 V V. Lebedev, 6 L. I. Popov, 6 S E. S a v l t s k a y a 6 a n d A. A. S e r e b r o ~ ~ tSer~tce d A#ronotme dzt CNRS, BP 3, 91370, Verlt~re~. Fiance 2Lttbotatotre d'Astronomte Spattale, Marsetlle_ France ~hl~tmtt d'Astroph)stque Parrs, France 41KI ~,loscon, U S S R ~B~lual, an Astroph3stcal Observatory. Armema. U_S S_R. ~C:emel of Framing of Cosmonauts. Moscow, U S S R 7C,VES Parts [lance ABSTRACT
The f a c i l i t y o f f e r e d by t h e S a l y u t 7 v e h l c l e has allowed teams of scientists o f 3 CNRS french laboratories to d e v e l o p en I n s t r u m e n t o p t i m i z e d f o r s e v e r a l d i s c i p l i n e s in astrop h y s i c s and g e o p h y s i c s . P . I . R . A . M . I . G . (Photography Infra-Red Atmosphere, Interplanetary Medium, G a l a x i e s ) is a wide f i e l d ( l O * and 60 ° ) camera d e v o t e d ro h i g h s e n s i t i v i t y photog r a p h i c p h o t o m e t r y . The s p e c t r a l range I s l t m l t e d to the v i s i b l e and n e a r - I n f r a r e d (400850 nm), t h e main a d v a n t a g e b e i n g to o b s e r v e a b o v e t h e a b s o r b i n g and e m t t t l n g layers of the a t m o s p h e r e . I~TRUMENTATION When the e x p e r i m e n t s f o r the f r a n c o - s o v i e t manned s p a c e f l i g h t were d i s c u s s e d In 1979, i t appeared t h a t l a r g e scale p h o t o g r a p h y o f a s t r o p h y s i c a l and geophysical o b j e c t s w i t h a h i g h sensitivity camera would g i v e new and i n t e r e s t i n g r e s u l t s a l m o s t I m p o s s i b l e to o b t a i n from the g r o u n d . The a t m o s p h e r i c b r i g h t n e s s , m a i n l y due to OH m o l e c u l e a i r g l o w a f f e c t s any g r o u n d based astronomical o b s e r v a t i o n s In the n e a r I n f r a r e d ; spatial observations eliminate this contribution and a l l o w the s t e l l a r d e t e c t i o n t o be improved by 4 t o 5 m a g n i t u d e s . A l s o , o b s e r v a t i o n s o f the E a r t h atmosphere from S k y l a b o r S a l y u t s t a t i o n s have sho~m t h a t even a p l a i n camera may be u s e f u l f o r a t m o s p h e r i c r e s e a r c h / 1 / 2 / 3 / ; a high sensitivity camera a11ows rhe s t u d y o f f a i n t a t m o s p h e r i c s o u r c e s , w i t h b l u r r i n g due t o the o r b i t a l v e l o c i t y o f a low o r b i t i n g s p a c e c r a f t reduced to an a c c e p r a b l e l e v e l by u s i n g e x p o s u r e t i m e s o f the o r d e r o f 1 second. B e s i d e s , the I n f o r m a t i o n s u p p o r t , such as a c a l i b r a t e d film, can he b r o u g h t dow~ the E a r t h by a v i s i t o r crew, w h i l e the a v a i l a b i l i t y o f the s t a t i o n w i t h the main crew d u r i n g more than 6 months may a l l o w s e a s o n a l d e p e n d a n t phenomena t o be s t u d i e d . INTRODUCTION The a s t r o n o m i c a l o b j e c t i v e s were f i r s t l y the b u l g e and the c e n t e r o f o u r G a l a x y , and then the e x t e r n a l extended g a l a x i e s ( ) 1 0 ' ) such as the H a g e l l a n l c C l o u d s , Andromeda, e t a . . . V a r i o u s c o l o u r s and t h e i r g r a d i e n t s c o u l d a p r i o r i g i v e t n f o r m a c i o n e a b o u t the e m i s s i v i t y and a b s o r p t i o n o f these e x t e n d e d s o u r c e s , w i t h o u t the OH m o l e c u l e a i r g l o w e f f e c t . The purpose of Interplanetary rhodium o b s e r v a t i o n s was m a i n l y to o b t a i n a c a r t o g r a p h y o f the whole z o d i a c a l l i g h t b r t g t h n e s s and p o l a r i z a t i o n I n the n e a r i n f r a r e d . O b s e r v a t i o n s made In s p e c i f i c r e g i o n s (C,e g e n a c h e | n , s ~ e t r y p l a n e o f the z o d i a c a l c l o u d , l l b r a t l o n a points o f the E a r t h - M o o n system, l a r g e s c a l e c o m e t a r y s t r u c t u r e s ) c o u l d h e l p s o l v e some q u e s t i o n s a b o u t the dynamics o f the I n t e r p l a n e t a r y d u s t c l o u d . The a t m o s p h e r i c o b j e c t i v e s were mainly Faint subauroral emissions of forbidden oxygen lines, s m a l l s c a l e structure of aerosol layers and, last but not least, global structure o f OH m a s o s p h e r t c e m t s s l v e w a v e s , w h i c h main c o n t r i b u t i o n appears at wavelengths greater t h a n 724 rim.
PIRAHIG h a s o p e r a t e d s u c c e s s f u l l y during the french "spattonaute" m i s s i o n t n J u n e 1982 and during later missions. The p r e l i m i n a r y enalysle of a b o u t 600 p i c t u r e s obtained I n 1982 demonstrates that various scientific objectives have been r e a c h e d . Of m a l n I n t e r e s t are the d e t e c t i o n o f c o l d s t e l l a r p o p u l a t i o n from n e a r I n f r a r e d p h o t o m e t r y o f G a l a c r f c C e n t e r , q m a l l M a g e l l a n t c C l o u d , M 31 and H 33, the p a r t i a l infrared cartography of zodiacal light w i t h an e s t i m a t i o n o f l i e p o l a r t a a t t o n , as w e l l as the o b s e r v a t i o n o f OH m e s o s p h e r t c waves and o f the f i n e s t r u c t u r e o f a t m o s p h e r i c e m t s s l v e l a y e r s , o r the d e t e c t i o n o f a t m o s p h e r i c aerosols. -'7
28
The
A
(
I. a s ~ u r - R e g o u r d
: .
of PIRAMIG is of the o r d e r of Io-ION cm-2sr-l~a-i The instrumen~ (Fig. a t CNRS L a b o r a t o i r e d ' A s c r o n o m i e S p a t l a l e in 1980/1981 has been d e s c r i b e d / 4 / . Two d i f f e r e n t objectives, 180 =-I f / 2 . 8 and 58 ~=a f / l . 2 (aspherlc lens)
sensitivity
i), built previously
stopped down at f/4 to reduce the vignetting effect, determine fields of view respectively of I0 ° and 40 ° • A set of 15 filters/ polarizers determines the spectral range from the blue to the n e a r - l n f r a r e d (Fig. 2) , c h r o m a t i c d i s p l a c e m e n t o f the f o c u s i s c o r r e c t e d by giving the filters an appropriate thickness. The information is collected on a 70 ~m/lO0 e x p o s u r e s film from a multichannel array Image amplifier. The deletion system allows the m o m e n t / d u r a t i o n of exposure and code letter of the filter to be s i m u l t a n e o u s l y recorded. Callbratlons and ground based tests performed at CNRS Haute Provence Observatory during the winter 1981/1982 gave the following typ,cal values : resolving power i to 4 arc min ( depending on the l e n s e s u s e d ) , slope o f the c h a r a c t e r i s t i c cu rve y = 1.8, optimal exposure times in a 0.3-10 s range. On board relative calibration is provided through a e e n s l t o m e t e r built at CNRS Institut d'Astrophysique. Its 6 x 6 d e n s i t y matrix allowing a 1-3OOO luminance range is illuminated by a low voltage tungsten ribbon lamp ; the sensltom e t e r is used at the beginning or at the end of each film with the set of filters used for t h a t film.
-_-
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o : / \ 10-2
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• 00
500
60; ~,V.'-_.Z_\~~,
=
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=c _ = - :
10
\ 1.
S c h e m a t i c view of PIRAMIC, t . n s t r u ~ e n t Mass
~ 18 kg ; size
\
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~ 70 dm-*
\
I 400
2.
I BOO
1
, 60
~ -
7OC
1 800
Spectral response o[ (a) the filters and of (b) the polaroids, taking into account photocathode spectrum. The response Is given in logarithm of the emission current. EXPERIMENTAL
937
the
CONDitIONS
The instrument was launched by Progress at the end of May 1982 and the f11ms were brought up end down by the crews through Soyuz. The orbital parameters of Salyut 7 during the French spatlonaute mission at the end of June were : apogee ~ 310 km , perigee ~ 290 k~ , inclination ~ 51.6 °. The conditions of observation were orbital night, no moont/ghc, and subsatelllte point located above the sea. In the case of astronomical observations, the i n e r t i a l stsbiltsacion a l l o w e d the o p t i c a l a x i s o f PIRAMIG t o be d i r e c t e d c o n s t a n t l y on the s e l e c t e d s o u r c e . In the case of g e o p h y s i c a l o b s e r v a t i o n s , the o r b i t a l o r i e n t a t i o n a l l o w e d the o p t i c a l a x i s to be d i r e c t e d on the h o r i z o n of the E a r t h . In June 1982, 5 orbital n i g h t s were devoted to g a l a x i e s , 2 ones to interplanetary medium, and 3 o t h e r s ones co the atmosphere. Complementary o b s e r v a t i o n s were performed in J u l y , August , N o v e m b e r and December 1982. This led to a total amount of about 6OO exposures, i n c l u d i n g about 60 ones f o r s e n s t t o m e t r y . The I n s t r u m e n t has been o p e r a t i n g again s i n c e F e b r u a r y 1984. PRELIMINARY
RESULTS - GALAXIES
The C,alactlc Center and the north part of the bulge of our Galaxy have been observed with a 40* field from the blue to the near-lnfrared wavelengths (Fig. 3). From previous observations / 5 / 6 / 7 / , i t appears t h a t the blue e m i s s i v i t y o f the g a l a c t i c c e n t e r I s most d i f f i c u l t to d e t e c t due to a severe a b s o r p t i o n by dust which can reach 30 meg / 8 / , whzle the near-infrared emissivity p r e s e n t s a most e v i d e n t I n t e r e s t f o r v a r i o u s reasons ( a b s o r p t i o n component, c o o l g i a n t p o p u l a t i o n , g a l a c t i c s t r u c t u r e ) . Our o b s e r v a t i o n s c o n f i r m the
Ob~rvatzons
wzth PIR~HIG/SaIyut
7
29
existence of a predominant spheroidal component, possibly flcced wlth a galactic structure model /9/. Moreover the corresponding lO ° ~teld exposures a l l o w t h e a n a l y s i s of the h i g h l y d e n s e p o p u lation o~ t h e M s u p e r g l a n t s . Both s t u d i e s are intimately correlated to an a b s o r p t i o n model and a dust distribution estimation.
From t h e e x t e r n a l g a l a x i e s , most i n t e r e s t is given to the M a g e l l a n l c c l o u d s , Andromeda (M 31) and t h e T r i a n g l e g a l a x y (M 3 3 ) , a l l o b s e r v e d a t 10 ° f i e l d i n varlous colours. One noclces ( F i g . 4) in the near i n f r a r e d the a s s y m e c r i c s t e l l a r reparCltion of the small MageUanlc Cloud, with a steep d e c r e a s e of b r i g h t n e s s t o w a r d s w~sc and a smo~h d e c r e a s e cowards e a s t , in the d i r e c t i o n of the ~rge M a g e l l a n i c Cloud ; c a l i b r a t e d i s o p h o t e s of the Magetlanic clouds can be compared to previous ones in the R band /I0/. Descriptive remarks about t h e m a j o r a x i s of Andromeda may be done : the p o s i t i o n angle ts c o n t i n u o u s l y changing w i t h the wavelength. In all t h e s e galaxies, t h e stellar e m i s I i V i t i e s in blue and near-lnfrared are determined. In particular, the stellar emission at 850 nm Is essentially due to red s u p e r g l a n c s and c o l d g i a n t s and g i v e information about the old stellar population of the galaxy. From such integrated DW and visible photometry, the past star formation race in the Magellantc clouds is about constant from lO Gyr /II/. Similar analysis .~y be done from the nearinfrared photometry of the PIRAMIG experiment, even If the stellar evolutionary parameters are more uncercaln in thls wavelength band than in UV. At last a comparison of the fast scar formation rates from the irregular galaxies (Magellanlc clouds) to the evolved spiral galaxies (St and Sb) will be of most tnterest.
3,
June 30, 1982 ; 15h42m36s UT June 30, 1982 17h26ma6s UT 40 ° f a. IR fzlcers, 10.6 exp.
Survey zn the near ~nfrared of the Galactzc Center, becveen galactzc long~tudes 34¢': and ~5 ° , galactic latitudes - 20" and * 20 ° An~arc~ ~s ~,n the upper left.
.:..
"
-,,..
,::, P
4.
July l, 1982 ; 12h58m09s UT ; I0 ° f/2.8 ; IR filter ; lO.5s exposure Small , ~ g e t l a n i c Clo,~ and I t s I s o p h o t e s . The sky background c o r r e s p o n d s
per sq,]are arc second ; the f i r s t PREI.IMINARY RESULTS
-
"
.
to mag, 23.6
I s o p h o t e i s a t meg. 2 5 . 5 .
INTERPLANETARY
MEDIUM
From the 7 s e t s of e x p o s u r e s o b t a i n e d i n 1982 from t h e b l u e to the n e a r - i n f r a r e d wavelengths, c o l o r i m e C r y and p a r t i a l c a r t o g r a p h y of t h e z o d i a c a l c l o u d can be o b t a i n e d . The most s i g n i f i c a n t r e s u l t s from m i c r o d e n s l t o m e c e r a n a l y s i s a r e t h e f o l l o w i n g . The p o s i t i o n of the p h o t o m e t r i c c e n t e r o f t h e G e g e n s c h e i n h a s been m e a s u r e d in A u g u s t 1982. Our r e s u l t s c o n f i r m Chat, e v e n when o b s e r v e d a b o v e t h e e a r t h ' s a t m o s p h e r e , the Cegenschein is slightly d e v i a t e d from t h e a n t t s o l e r direction /12/13/14/. T h i s c o u l d be due co the f a c t c h a t , a t l a r g e s o l a r e l o n g a t i o n s , t h e s y m m e t r y p l a n e of t h e z o d i a c a l c l o u d is close to t h e l n v a r l a n C p l a n e o f t h e s o l a r s y s t e m . Continuous m o n i t o r i n g of the G e g e n s c b e l n from S a l y u t s h o u l d a l l o w a s e a s o n a l e f f e c t to be d e t e r m i n e d .
t
A. (.
30
L~*vasse ur-Re g¢)urd
The linear polarization of the zodiacal light has been determined for flve fields of view (ecliptic plane aC IO0", 140" and 180 = from the Sun, north ecliptic pole, and 45 ° south of the ecliptic st 180" from the Sun). In the visible, the results are found to be consistent wlth Frevloos observations I151. In the near-lnfrared, one single measurement of polarization [tad been done previously, in the ecliptic at 30 ° from the Sun /16/17/. The values obtained in the v a r i o u s f i e l d s demonstrate that the degree of polarlzatlon may be a few p e r c e n t h i g h e r in the i n f r a r e d than In the v i s i b l e . This r e s u l t should a l l o w c h o i c e s to be made between v a r i o u s m o d e l s o~ interplanetary g r a i n s . PRELIMINARY
RESULTS - ATMOSPHERE
The atmospheric emlsaive layers were observed mainly above the Pacific Ocean, with green, red and near-infrared filters t o study the structure of the oxygen lines and to separate OH mesoepberlc clouds frol tropospheric clouds. Under tangential viewing conditions from Selyut 7, the 40" fleld of view allows a monitoring over more than 15OO km to be made on each exposure. Various structures can be observe on the large set of pictures taken accordlngly to the geophysics progra~n. The most significant ones can be interpreted as explalnea below. On the frames taken with the near-lnfrared filter, elongated structures are clearly visible, even In cloud free areas. Their measured altitude is approxlmatively 85 km and they a~,e due to OR m s o s p h e r l c eaves. Due to some geometric effects /18/, the observed structures are separated by larger distances than those observed from the ground /19/20/21/. The spatial range of observation Is more extended than for ground based observations end PIRAn~G has peffor~med the f i r s t d e t e c t i o n o f OH waves a t low l a t i t u d e s . On the plccure taken at the limb, the emlsslve layer Is seen tangentially, leading to an enhanceIOnt of brlshCaeoe and allowing an accurate determination of the altitude of the layer. 1"-~ altltu~e of the layer and the relative intensities of the peaks In green and red are variable, as c o n ~ t l r m ~ by preliminary results of the PCN experiment on the same mlsslon122/. On some frames, the F region luminosity at 630 nm can be measured in directions almost tanfentlel to the emisslve layer, so that vertical drif velocity effects can sometimes be o b s e r v e d . On all the frames taken in red colour on December 8th 1982, including the low latitude areas, the F region is extremely enhanced, due to the effect of an intense s o l a r activity. On some June and August 1982 pictures, a noticeable absorption both of the emlaslve layers and of the starlight can be detected. This Is due co enhanced aerosols extinction over the Pacific Ocean, as an effect of the eruption of E1 Chlchon volcano in Mexico. ACKNOWLEDGEMENTS This work was supported under CNES contract 205 1980/1982 under a CNES/Intercosmos cooperation. The authors are greatful to A. Magnan, A. Verlhac and many colleagues whose efficient cooperation allowed the rapid achievement of the instrument. We are indebted to J. Blamont, G. Galperln and R. Dumont for commenting the preliminary results. REFERENCES I. GARRIOTT O.K. J. tOpt. Soc. Am., 69, 8, 1064 (1979). 2 GRETCHKO G.M., NIKOL..~ A.N., ROMANENKO Y.N., SAVCHENKO S.A., SIHONOV A.I, ~ , 242 (4), 796 (1978) 3. ( ~ O G.M., R O M ~ E N K O Y.N., SAVCHENKO S.~., SIMONOV S.W. sp.ce ~ r c h ,
Doklady 19, 244,
( 1981 ) 4, LEVASSEUR-KEGOURD A . C . , MAGNAN A . , KOUTCHMY S . , LAMY P. Nouveaux d~;vetoppements dans la ~ o ~ I s n e n c e du Syst&=" solaire, INAG, Paris, 202 (1982). 5. S T ~ # ~ J., ~ i T ~ O ~ A'E. As~roPhys. J., tO6, 235 (1947) 6. KALIMIAK A.A., KRASSOVSK¥ N.J., K~OKONOV W.B. Izvestia Krym, Astrofyz. 5, 119 (1951) 7. DUFAY 3. Ann. AstroDh. 23, 451 (1960) 8. BECKLIN E.g., NEUGE~Ab'ER G. Astroph~s. J., 151, 145 (1968) 9. HAIHARA T., ODA N., SUGIYAMA T., OKUDA H. Pub1. Astron. Soc. Jpn., 30, 1 (1978) IO. VAUCOULEURS G. de Astron. J., 62, 69 (1957) II. ROCCA-VOLMERANGE g., LEQUEUX J., MAUCHERAT M. AsCron. Astroph~s., 104, 177 (1981) 12. ROBLEY R. Ann. GeoDh. , 18, 341 (1962) i3. ROOSEN R.G. Icarus, 9, 429 (1968) 14. SU~'AI~IA S. A a t r o n . A s t r o p h : y s . , 52, 145 (1976) 15. IxrNoNT R., S A ~ E Z F. A~tron. Amczophys., 52, 145 (1976) 16. FREY A., HOPMAN W., L E ~ D.. THUM C. Astron. AacroFhL~a., 36, 447, (1974). 17. PITZ E., LEINKRT C., SCHULZ A., LINK H. Astron. AsCr~q?bys., 74, 15 (1979) 18. H R U E H., MOREELS G., CLAIRBMIDI J. Appl. Opt., ~9, 3, 355 (1980) 19. FLrTERSON A.W., KIEFPABER L.M. Nature, 257, 649 (1975) 20. CRA..U~D J., ROTHWELL P., WELLS ~. Nature, 257, 650 (1975) 21. K ~ S O V S K Y V.I., POTAPOV B.P., SEMENOV A.I. Ann. Geo~h., 33, 3, 347 (1977) 22. KOUTCHHY S., NIKOLSKY G.M., Sky and Tel., 65, 25 ( i ~ 3 )
