1. PHEBUS Probing of Hermean Exosphere By Ultraviolet Spectroscopy PHEBUS Science Performance International Mercury Watch GroupObservatoire de Paris 5-6 April 2008 1 PHEBUS SCIENCE PERFORMANCE Mea WEDLUND PhD PHEBUS Project CNRS/Sérvice d’Aéronomie

2. PHEBUS Probing of Hermean Exosphere By Ultraviolet Spectroscopy PHEBUS Science Performance International Mercury Watch GroupObservatoire de Paris 5-6 April 2008 2 PHEBUS PLACEMENT AND DESIGN PHEBUS Probing of Hermean Exosphere By Ultraviolet Spectroscopy Signal-to-noise ratio of 3 is achieved in the radiometric modelling for most important species (depends on integration time) EUV = 55 - 155 nm FUV = 145 - 315 nm NUV = 404.7 nm (K) and 422.8 nm (Ca) EUV: FWHM ~0.48 FW1% ~0.80 FUV: FWHM ~0.94 FW1% ~1.48 Ingenious rotating mechanism with attached baffle - impact parameter from 0 to 1500 km With current configuration and 3600 s integration time sensitivity to lines as weak as 0.1 Rayleigh is achieved in the radiometric model

3. PHEBUS Probing of Hermean Exosphere By Ultraviolet Spectroscopy PHEBUS Science Performance International Mercury Watch GroupObservatoire de Paris 5-6 April 2008 3 PHEBUS DESIGN S

4. PHEBUS Probing of Hermean Exosphere By Ultraviolet Spectroscopy PHEBUS Science Performance International Mercury Watch GroupObservatoire de Paris 5-6 April 2008 4 PHEBUS DESIGN Baffle Mirror Slith EUV FUV NUV Grating

5. PHEBUS Probing of Hermean Exosphere By Ultraviolet Spectroscopy PHEBUS Science Performance International Mercury Watch GroupObservatoire de Paris 5-6 April 2008 5 PHEBUS MISSION OBJECTIVES 1.To measure the exosphere (constituents, species densities, vertical structure, seasonal-, local- and temporal variations) 2.To measure the coupling of the surface-exosphere- magnetosphere system 3.Measuring the escape rates of species from the surface and the composition of the eroding regolith 4.Search for surface ice in the polar regions 5.Low priority: Stellar- and interplanetary physics Magneto- sphereSurface Exosphere

6. PHEBUS Probing of Hermean Exosphere By Ultraviolet Spectroscopy PHEBUS Science Performance International Mercury Watch GroupObservatoire de Paris 5-6 April 2008 6 1.Twilight Mode 2.Vertical Scan Mode 3.Fixed LOS Mode 4.Feature Tracking Mode 5.Nadir Mode 6.Star Mode 7.??? PHEBUS OBSERVATIONS

7. PHEBUS Probing of Hermean Exosphere By Ultraviolet Spectroscopy PHEBUS Science Performance International Mercury Watch GroupObservatoire de Paris 5-6 April 2008 7 PHEBUS MODES Twilight Mode Allows search for trace species near surface and studies of the exosphere’s source and dynamics. Observations when in the shadow of Mercury. The line of sight is as low as possible with no bright emission from the surface is in the field of view Vertical scan Mode Give information on the vertical distribution and its variation with solar zenith angle Fixed LOS Mode A fixed line of sight respective to the spacecraft. A slow vertical scan is obtained from the altitude variation of the spacecraft. Gives information about local density of observed species along the orbit

8. PHEBUS Probing of Hermean Exosphere By Ultraviolet Spectroscopy PHEBUS Science Performance International Mercury Watch GroupObservatoire de Paris 5-6 April 2008 8 PHEBUS MODES Line of sight Feature tracking Mode The LOS moves slightly as in Twilight Mode to follow a feature (or altitude range) along the orbit Nadir Mode The LOS is pointed towards the Nadir on the nightside of the orbit and at high latitude which records the reflectivity of the surface by interplanetry glow (water, sulphur…) Star Mode The aim of the star mode is to follow the ageing of the instrument. Observation of some hot stars within the spectral range 100-300 nm. The number of available stars within the Phebus field of view is TBD (by me!).

9. PHEBUS Probing of Hermean Exosphere By Ultraviolet Spectroscopy PHEBUS Science Performance International Mercury Watch GroupObservatoire de Paris 5-6 April 2008 9 PHEBUS MODES ? Tail mode (under construction)

10. PHEBUS Probing of Hermean Exosphere By Ultraviolet Spectroscopy PHEBUS Science Performance International Mercury Watch GroupObservatoire de Paris 5-6 April 2008 10 PHEBUS MODELING: Radiometric Model Emissions from Mercury (theoretical values) Collecting: Detectors Gathering: Entrance Pupil and Baffle Reflecting: Entrance mirror Gratings Different reactions due to different photocathodes Constraints of field of view and stray light Depends on the separation of the two gratings and the reflectance of coating Not perfectly reflective Instrument Response

11. PHEBUS Probing of Hermean Exosphere By Ultraviolet Spectroscopy PHEBUS Science Performance International Mercury Watch GroupObservatoire de Paris 5-6 April 2008 11 RADIOMETRIC MODEL: Instrument Response and spectra generation 1.Raw list of species with their assumed intensities (preliminary since Mercury’s exosphere is virtually unexplored) 2.List of species subjected to the instrument response 3.‘Spectrum’ of the species list after addition of noise – 1 s integration time 1. 2.3. blue arrow is oxygen at 130,4 nm – ‘easily’ detectable red arrow is clorine at 133,6 nm – ‘difficult’ to detect

12. PHEBUS Probing of Hermean Exosphere By Ultraviolet Spectroscopy PHEBUS Science Performance International Mercury Watch GroupObservatoire de Paris 5-6 April 2008 12 RADIOMETRIC MODEL: Instrument Response 10 seconds 60 seconds 600 seconds 3600 seconds With increasing time the dark current will overtake some lines and change line-ratios

13. PHEBUS Probing of Hermean Exosphere By Ultraviolet Spectroscopy PHEBUS Science Performance International Mercury Watch GroupObservatoire de Paris 5-6 April 2008 13 RADIOMETRIC MODEL: Signal-to-Noise Ratio Species detectable: < 60 s (to make thorough investigations) EUV: He I, CO, O I, H I, C I, N I FUV: Mg I, Si I, Na I, C I, Fe I, S I, Al I, CO, Ni I, Mg II, OH, Ca I, Fe II, H2 >> 3600 s (to confirm that the species exist) EUV: Kr I, Ar I, Cl I and Si II FUV: Al II and Si II Numbers in the tables are integration time in seconds

14. PHEBUS Probing of Hermean Exosphere By Ultraviolet Spectroscopy PHEBUS Science Performance International Mercury Watch GroupObservatoire de Paris 5-6 April 2008 14 RADIOMETRIC MODEL: Detection limit The lowest (integration time of 3600 s) mean detection limit can thus be estimated to: EUV range: ~ 0.1 Rayleigh FUV range: ~ 0.2 Rayleigh red dotted line marks the limit of 0.1 R red area marks most common utilised integration time 1-10 s int. time gives lower limit of 10 R 1-10 s int. time gives lower limit of 5 R 1-10 s int. time gives lower limit of 20 R

15. PHEBUS Probing of Hermean Exosphere By Ultraviolet Spectroscopy PHEBUS Science Performance International Mercury Watch GroupObservatoire de Paris 5-6 April 2008 15 PHEBUS DESIGN ACHIEVEMENTS Signal-to-noise ratio of 3 Spectral range of 55 - 315 nm and the NUV of 404 nm and 422 nm Spectral resolution: FWHM < 1 nm for EUV, < 1.5 nm for FUV. FW1% < 2 nm for EUV and < 3 nm for FUV A vertical scanning range equivalent to an impact parameter from 0 to 1500 km Vertical resolution of ~ 1/2 scale height on most species(~ 20 km). From apoherm this gives spatial resolution ≥ 0.37° Sensitivity to lines as weak as 0.1 Rayleigh Is achieved in the radiometric modelling for most important species (depends on integration time) EUV = 55 - 155 nm, FUV = 145 - 315 nm, NUV = 404.7 nm and 422.8 nm EUV: FWHM ~0.48 FW1% ~0.80 FUV: FWHM ~0.94 FW1% ~1.48 Ingenious rotating mechanism with attached baffle With margin the spatial resolution is ~0.4° in the current evaluation of the geometric performance With current configuration and 3600 s integration time this is achieved in the radiometric model for EUV ~0.1 R (FUV ~0.2 R)