1. LABORATORY SPECTROSCOPY OF RELEVANCE TO CASSINI UVIS AND ISS
JOSEPH AJELLO
ALEX AGUILAR
RAO MANGINA
PAUL JOHNSON
CHARLES MALONE
DAREK DZICZEK
JPL
H. ABGRALL
MEUDON
MICHAEL STEVENS
NRL
XIANMING LIU
SET
Ian Stewart
Kris Larsen
LASP

2. H2 (UVIS, ISS SATURN, JUPITER)
ELECTRON IMPACT INDUCED UV & NEAR IR FLUORESCENCE LAB STUDIES ( nm)
N2 (UVIS TITAN)
MATCH LAB & UVIS AND ID UVIS TITAN EUV SPECTRA
TRANSITION MOMENT STUDIES OF Liu et al., 2007 FOR TITAN UVIS MODELS
H2 (UVIS, ISS SATURN, JUPITER)
MEASURE VOIR SPECTRA ( nm) AND CROSS SECTIONS 100 eV of EF,GK,HH 1Sg+,I 1Pg ,J 1Dg  B,B’ 1Su+, C 1Pg FOR ISS
PROVIDE UV CASCADE CROSS SECTION TO LYMAN & WERNER BANDS FOR UVIS
20 eV SPECTRA GIVE 3p 3Pu, 4p 3Pu – a 3Sg+, FULCHER-a , BETA BAND CROSS SECTION
COMPARE TO MEUDON MODEL
SO2 (ISS IO)
MEASURE VOIR SPECTRA AND CROSS SECTIONS 25 AND 100 eV
APPLY RESULTS TO ISS IO FILTER IMAGE INTENSITIES

3. UVIS EUV IMAGE ON 13 DEC2004 BRIGHT LIMB ALTITUDE DEPENDENCE AT 03h 43’
TARGET DISTANCE: 160k&16 deg phase
Data(60,26,555)
& records of 240”
PEAK EMISSION KM (hvert~ cm-2) VS PEAK PRODUCTION AT 900KM (hvert ~1018 cm-2)

4. LOW RESOLUTION-OPTICALLY THICK 20 eV LAB SPECTRUM WITH ID COMPARED TO UVIS TITAN 13DEC04

5. VOYAGER BASED* MODEL INTENSITIES AND IDENTIFICATIONS OF EUV UVIS AIRGLOW FEATURES
# wavelength(A) UVIS disk rayleighs Theory (AURIC component Rayleighs-IDs)* identity+
c5(0,0),c6(0,0)
c'(6,0),NI,c(0,0)
c'(4,0),c'(6,2),b'(11,0),NI
c'(3,0),c'(4,1),b'(16,2),b'(12,1)
b'(11,1),NII
(c'64),0.2(b'91)
0.2b'(16-3),0.1(c'31) c'(3,1),c'(6,4),b'(9,1),b'(8,1)
(NI953),0.8(c'4,3),0.6(c'3,2)
0.1(b'9,2)0.1(b'16-4),0.5(c'65) c'(4,3),c'(3,2),NI,b'(16,4),b'(9,2),c'(6,5)
(NI964),0.4c'(4,4),0.2(c'66)
0.1(b'93),0.3(c'del v=0) NI,c' delta v=0)
(c'0,1),0.6(c'4,5),0.5c'(34),
0.3c'(6,7),0.3(b'94),0.1(b'16-6) c'(0,1),c'(4,5),b(1,0),c'(6,7),
(c'0,2),0.6(b1,1),0.3(b'16-7)
0.1(b'95),0.3(c'del v=2),0.1(c'46) c'(delta v=2),b'(9,5),b(1,1)
H L(beta),c'(6,9),b(1,2)
c'(delta v=4),NI,b(1,3),b'(3,5)
NI,b'(11,8),c'(delta v=5)
NII
NI,b'(1,6),b'(9,9),b'(6,8),b'(3,7)
b'(2,7),b'(1,7) NI
NI,b'(1,8)
NI,b'(0,8),b'(1,8)
total(29.2R) total(36.8R)
+Ajello et al.,1989;James et al., 1990
*Stevens(2001) F10.7=256(VI,II SOLAR MAX) VS F10.7=90 DEC13, 2004

6. HIGH RESOLUTION LAB WITH ID SPECTRUM COMPARED TO UVIS TITAN 13 DEC2004

7. Lab Study of Pressure Effects of the N2 EUV Spectrum by Electron Impact at 20 eV

8. Geissler et al., 2004

9. VOIR APPARATUS Vis-Optical-near IR (200-1200 nm)

10. CASSINI ANALYSIS WITH SO2 LABORATORY SPECTRUM
CASSINI ISS FILTERS
Filter Center FWHM    nm UV1     255    40
UV2     300    60
UV3     340    70
BL1     445   105
BL2     440    30
GRN     562   145 IR IR
ISS OBSERVATIONS
Filter eV 18 eV 98 eV ISS
UV < 1.0 UV UV BL
GRN

11. CASSINI ISS LAB STUDIES

12. DIRECT MEASUREMENT OF H2 GERADE STATE CASCADE CROSS SECTION TO UV RYDBERG STATES

13. VOIR EF-B CASCADE SPECTRUM IN CROSS SECTION UNITS

14. DISCREPANCY BETWEEN MODEL AND DATA FOR HIGHER LYING GERADE STATES

15. COMPARISON OF CROSS SECTIONS TO UNIVERSITY OF ARKANSAS GROUP

16. MAJOR 100 eV CROSS SECTION RESULTS IN THE VOIR
TABLE 1
                 e + H2  VOIR process   CROSS SECTION
EXP  MODEL PREVIOUS
      (10-19 cm2)      (10-19cm2)    (10-19cm2)                                                                                                                                                  total VOIR cross section  (singlets +triplets+ H-lines)…………63       
total triplet cross section  …………………….…………………… ……..1.2               -       total ungerade    singlet  cascade cross section…………………..51               50*          total H lines  *** EF-state          ? GK+HH+IJ ?               Too large
                                                              e+H2 UV Process                                             total UV direct +cascade ungerade states   (B+C+B'+D+...)……………………………… 460** *Dziczek et al; 2000 (UV Technique)
**Jonin et al; 2000
*** Karolis and Harting;1978 and Vroom and de Heer;1969

17. CONCLUSIONS EARTH AND TITAN PRESENT SIMILAR EUV SPECTRA
OVER 100 N AND N2 FEATURES CONTRIBUTE TO TITAN EUV CHANNEL UVIS SPECTRA
EXCEPT FOR N2(c’[0,0]) BAND UVIS SPECTRUM IS WELL-MATCHED BY eV OPTICALLY THICK LAB SPECTRA OF e + N2
e + H2 VOIR EF-B SPECTRA GERADE-UNGERADE ARE MODELED A AND DISCREPANCIES A
HIGH LYING GERADE STATE MODELS ARE TOO STRONG(J-B,C)
H2 VOIR TRIPLET STATES ARE STRONG AT 20 eV
GROUND-BASED AND HUBBLE IO SO2 EMISSIONS ARE SUGGESTED AT 777,845 NM FOR OI AND 922 NM FOR SI.

18. OPTICALLY THICK LAB SPECTRUM AT 0. 6 AND 0
OPTICALLY THICK LAB SPECTRUM AT 0.6 AND 0.2 A FWHM COMPARED TO CASSINI 4A FWHM

19. GEOMETRY OF 13 DEC2004 TWO LIMB AND DISK OBSERVATIONS
TARGET DISTANCE: 160k and 125k km
Data(60,26,555) AND Data(60,32,555)
records of 240” each
Solar incidence angle=78 deg and 90 deg
Target phase angle=16 deg
Solar emission angle=90 deg limb
Peak emission 1200 km
Temp=150k , H(N2)=70 km, Nhvert (N2)=7x1015 cm-2
Number density N2=109 cm-3
CHAPMAN FACTOR=22 SLANT/VERTICAL
Low Res. EUV slit =2mR (0.1deg) x 59 mR (3.6 deg)

20. STUDY OF FULCHER-a BANDS (d 3Pu -a 3Sg+) OF H2

21. TITAN EUV AIRGLOW DISK SPECTRUM