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@ARTICLE{Marsset2020,
    author = {Marsset, Micha{\"{e}}l and Brož, Miroslav and Vernazza, Pierre and Drouard, Alexis and Castillo-Rogez, Julie and Hanu{\v s}, Josef and Viikinkoski, Matti and Rambaux, Nicolas and Carry, Beno{\^{\i}}t and Jorda, Laurent and {\v S}eve{\v c}ek, Pavel and Birlan, Mirel and Marchis, Franck and Podlewska-Gaca, Edyta and Asphaug, Erik and Bartczak, Przemyslaw and Berthier, J{\'{e}}r{\^{o}}me and Cipriani, Fabrice and Colas, Fran{\c c}ois and Dudzi{\'{n}}ski, Grzegorz and Dumas, Christophe and Durech, Josef and Ferrais, Marin and F{\'{e}}tick, Romain and Fusco, Thierry and Jehin, Emmanuel and Kaasalainen, Mikko and Kryszczynska, Agnieszka and Lamy, Philippe and Le Coroller, Herv{\'{e}} and Marciniak, Anna and Michalowski, Tadeusz and Michel, Patrick and Richardson, Derek C. and Santana-Ros, Toni and Tanga, Paolo and Vachier, Fr{\'{e}}d{\'{e}}ric and Vigan, Arthur and Witasse, Olivier and Yang, Bin},
     month = {feb},
     title = {The violent collisional history of aqueously evolved (2) Pallas},
   journal = {Nature Astronomy},
    volume = {4},
      year = {2020},
     pages = {569--576},
   address = {AA(Department of Earth, Atmospheric and Planetary Sciences, MIT, Cambridge, MA, USA; Astrophysics Research Centre, Queen's University Belfast, Belfast, UK), AB(Institute of Astronomy, Charles University, Prague, Czech Republic), AC(Aix Marseille Univ, CNR},
      issn = {2397-3366},
       url = {https://ui.adsabs.harvard.edu/abs/2020NatAs...4..569M},
  abstract = {Asteroid (2) Pallas is the largest main-belt object not yet visited by a spacecraft, making its surface geology largely unknown and limiting our understanding of its origin and collisional evolution. Previous ground-based observational campaigns returned different estimates of its bulk density that are inconsistent with one another, one measurement<SUP>1</SUP> being compatible within error bars with the icy Ceres (2.16 ± 0.01 g cm<SUP>-3</SUP>)<SUP>2</SUP> and the other<SUP>3</SUP> compatible within error bars with the rocky Vesta (3.46 ± 0.03 g cm<SUP>-3</SUP>)<SUP>4</SUP>. Here we report high-angular-resolution observations of Pallas performed with the extreme adaptive optics-fed SPHERE imager<SUP>5</SUP> on the Very Large Telescope. Pallas records a violent collisional history, with numerous craters larger than 30 km in diameter populating its surface and two large impact basins that could be related to a family-forming impact. Monte Carlo simulations of the collisional evolution of the main belt correlate this cratering record to the high average impact velocity of ~11.5 km s<SUP>-1</SUP> on Pallas—compared with an average of ~5.8 km s<SUP>-1</SUP> for the asteroid belt—induced by Pallas's high orbital inclination (i = 34.8°) and orbital eccentricity (e = 0.23). Compositionally, Pallas's derived bulk density of 2.89 ± 0.08 g cm<SUP>-3</SUP> (1σ uncertainty) is fully compatible with a CM chondrite-like body, as suggested by its spectral reflectance in the 3 μm wavelength region<SUP>6</SUP>. A bright spot observed on its surface may indicate an enrichment in salts during an early phase of aqueous alteration, compatible with Pallas's relatively high albedo of 12-17\% (refs. <SUP>7,8</SUP>), although alternative origins are conceivable.},
={10.1038/s41550-019-1007-5},
}