1. Disk-Integrated Polarization of the Moon in the Ultraviolet from SOLSTICE M. Snow, G. Holsclaw, W. McClintock, T. Woods University of Colorado/LASP snow@lasp.colorado.edu

2. Outline SOLSTICE Instrument Lunar observing campaign Observing geometry Polarization observations

3. SOLSTICE Lunar Irradiance3 SOLar STellar Irradiance Comparison Experiment (SOLSTICE) Measures irradiance in ultraviolet –115-180 nm Far Ultraviolet (FUV) –180-300 nm Middle Ultraviolet (MUV) Measures stellar irradiance for tracking long term degradation. On board SORCE: –Low Earth Orbit

4. SOLSTICE Lunar Irradiance4 Solar-Stellar Ratio Need a large dynamic range to measure both sun and stars with same optics and detectors

5. SOLSTICE Lunar Irradiance5 SOLSTICE Layout Change entrance aperture 2x10^4 Widen exit slit 10 or 20 Lengthen integration 10^3

6. SOLSTICE Lunar Irradiance6 Lunar Observing Campaign June 2006 to December 2010 Added the Moon to the schedule of eclipse calibration activities On average, we observed one disk- integrated spectrum per day in each channel NASA Grant: LASP Lunar Albedo Measurement and Analysis from SOLSTICE (LLAMAS)

7. Overview of Observations ROLO GOME SSBUV (MESSENGER) (Galileo) (SNOE) (Cassini) (Mariner 10) NOZOMI (HUT) (Apollo 17) SOLSTICE

8. Lunar Irradiance Spectra Phase angle 2 degrees

9. SOLSTICE Lunar Irradiance9 Phase Angle

10. Phase Curve (282 nm)

11. UV Disk-integrated Albedo Phase angle 10 degrees

12. Instrument Sensitivity to Polarization Measured at SURF before launch for both channels. Very little sensitivity to polarization in FUV channel.

13. Instrument Roll Angle

14. Calculating Polarization Fraction Using Mueller Matrices, we can express the measured signal in terms of the spacecraft roll angle, θ The polarization of the lunar irradiance is then given by:

15. Extracting P m For each wavelength and phase angle, we can find A and B using least-squares fitting algorithm.

16. Polarization vs Phase

17. Polarization vs Wavelength

18. Summary SOLSTICE has observed the disk integrated albedo of the Moon from -170 to 170 degrees phase 130-300 nm Instrument is sensitive to polarization above 250 nm Reasonable signal-to-noise measurement of polarization from -90 to 90 degrees phase Consistent with WUPPE measurements and trends from visible region of the spectrum Analysis of systematic errors in data processing continues!

19. Acknowledgements & References This work was supported by NASA grant NNX09AQ60G (LLAMAS) and NASA contract NAS5-97045 (SORCE) at the University of Colorado. Snow, M., Holsclaw, G., McClintock, W. E., and Woods T. N. (2012) Absolute ultraviolet irradiance of the Moon from the LASP Lunar Albedo Measurement and Analysis from SOLSTICE (LLAMAS) project. In: Cross-calibration of Past and Present Far UV Spectra of Solar System Objects and the Heliosphere, E. Quemerais, M. Snow, and R. M. Bonnet (eds), ISSI Scientific Report No. 12 (in press) Snow, M., Holsclaw, G., McClintock W. E., and Woods, T. N. (2007) Absolute ultraviolet irradiance of the Moon from SORCE SOLSTICE. Proc. SPIE 6677:66770D

20. Questions?