Pallas From The NUV To IR: A 4-Telescope Campaign

Details Pallas From The NUV To IR: A 4-Telescope Campaign Pallas From The NUV To IR: A 4-Telescope Campaign

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.2204s&link_type=abstract

American Astronomical Society, DPS meeting #40, #22.04; Bulletin of the American Astronomical Society, Vol. 40, p.426

Astronomy and Astrophysics

Astrophysics

Scientific paper

In July through September of 2007, we observed the third largest asteroid 2 Pallas from NUV-IR with Hubble Space Telescope, Palomar Observatory's 200-inch Hale Telescope, IRTF and Table Mountain Observatory.
Using WFPC2/PC on HST, we determined Pallas’ size, shape and rotation pole: 291 x 278 x 250 km(±9), RA= 42o, Dec=-12o, (±10o). Employing the mass estimate of 1.17x10-10 +/- 0.03 Msun [1], Pallas’ density then becomes 2747 +/- 290 kg/m3, intermediate between basaltic Vesta and icy Ceres. This size is larger than most previous measurements that range from 287 x 262 x 250.5 km, ±10; km [2] to 275±3; x 252.5±2; x 234±9; km [3], with densities from 2.95-3.44 g/cm3. We explore the implications of Pallas' size and density.
Pallas’ surface from the UV to the IR was characterized using HST, TMO, IRTF and Palomar. We observed Pallas with WFPC2 in 5 filters from 336 to 814nm in September 2007, and include the 2001 WFPC2 data of Storrs from 439-1042nm. We combined these with observations from TMO and will present Pallas’ colors, reflectance and phase curve. We observe surface variation of 6% in the NUV-visible light curve amplitudes, greater than previous limits from ground based AO. We will also present photometry and a phase curve from Palomar in the near-IR. Pallas’ spectrum has long been known to contain hydrated minerals[4], and we obtained new spectra from IRTF in the 3-micron region centered at different sub-Earth latitudes and longitudes. The spectra are consistent with one another within uncertainties, suggesting similar amounts of hydrated minerals across Pallas' surface on regional and hemispheric scales.
[1] Goffin, B. (2001) Astronomy & Astrophysics 365, 627-630. [2] Dunham et al. (1990) Astronomical Journal 99, 1636-1652. [3] Drummond, J. D., personal communication. [4] Larson, H.P., et al. (1979) Icarus 39, 257-271.

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