Presented by Sergio Lainez Mentored by Dr. Alex Storrs. Reconstruction of Main Belt Asteroids in the Visible Spectrum
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1 Presented by Sergio Lainez Mentored by Dr. Alex Storrs Reconstruction of Main Belt Asteroids in the Visible Spectrum
2 Introduction In 1997 Dr. Storrs used WFPC2 s Planetary Camera to take images of eight main belt asteroids in the visible light spectrum The goal of this project is to produce accurate reconstructions of each asteroid in order to look for signs of surface variation as well as determine their size and shape This presentation features three of these restored asteroids
3 Method Images of each asteroid were taken in five different wavelength filters: F439W (0.439 µm), F673N (0.673 µm), F953N (0.953 µm) and F1042M (1.042 µm) PSFs for each filter were calculated at 4x enhanced resolution using the TinyTim Web Interface Using the maximum entropy routine, we are able to subsample the input image while simultaneously reconstructing it The resulting images are 16x as large as the input image We then find the ratios between select filters in order to study the composition of the surface
4 8 Flora Top 1. Raw image in the F439W filter 2. Reconstructed F439W filter image 3. Red continuum (ratio of F791W and F439W images) Bottom 4. Water of hydration (ratio of Red continuum and F673N images) 5. Width of silicate band (ratio of red continuum and F953N images) 6. Depth of silicate band (ratio of red continuum and F1042M images) The restored diameter of 145 km approximately the diameter of 135 km reported by IRAS Minor Planet Survey V6.0 Observed on 9/29/97
5 10 Hygeia Top 1. Raw image in the F439W filter 2. Reconstructed F439W filter image 3. Red continuum (ratio of F791W and F439W images) Bottom 4. Water of hydration (ratio of Red continuum and F673N images) 5. Width of silicate band (ratio of red continuum and F953N images) 6. Depth of silicate band (ratio of red continuum and F1042M images) The restored diameter of 503 km is slightly larger than the diameter of km reported by IRAS Minor Planet Survey V6.0 Observed on 11/24/97
6 29 Amphitrite Top 1. Raw image in the F439W filter 2. Reconstructed F439W filter image 3. Red continuum (ratio of F791W and F439W images) Bottom 4. Water of hydration (ratio of Red continuum and F673N images) 5. Width of silicate band (ratio of red continuum and F953N images) 6. Depth of silicate band (ratio of red continuum and F1042M images) The restored diameter of 268 km is slightly larger than the diameter of 212 km reported by IRAS Minor Planet Survey V6.0 Observed on 4/11/97
7 Future Work & Acknowledge ments To take our own exposures of these or other asteroids To repeat the process using MISTRAL, a more effective deconvolution algorithm for asteroids To calculate the albedos of each asteroid I would like to thank my mentor Dr. Storrs for his guidance as well as the Maryland Space Grant Consortium for funding my research
8 References D.I. Shestopalov et al./icarus 225 (2013) Optical maturation of asteroid surfaces. Retrieved from H.A. Weaver et al./a&a 518 (2010) A4. Ultraviolet and visible photometry of asteroid 21 Lutetia using the Hubble Space Telescope. Retrieved from B.H. Zellner et al./icarus 128 (1997) Hubble Space Telescope Images of Asteroid 4 Vesta in Retrieved from
9 Interpretation of ratio images C type Younger surface Reflectance silicate feature S type Water of hydration Older surface Wavelength (nm)
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