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@ARTICLE{,
    author = {Hanu{\v s}, J. and Marsset, M. and Vernazza, P. and Viikinkoski, M. and Drouard, A. and Brož, M. and Carry, B. and Fetick, R. and Marchis, F. and Jorda, L. and Fusco, T. and Birlan, M. and Santana-Ros, T. and Podlewska-Gaca, E. and Jehin, E. and Ferrais, M. and Grice, J. and Bartczak, P. and Berthier, J. and Castillo-Rogez, J. and Cipriani, F. and Colas, F. and Dudzi{\'{n}}ski, G. and Dumas, C. and Ďurech, J. and Kaasalainen, M. and Kryszczynska, A. and Lamy, P. and Le Coroller, H. and Marciniak, A. and Michalowski, T. and Michel, P. and Pajuelo, M. and Tanga, P. and Vachier, F. and Vigan, A. and Witasse, O. and Yang, B.},
  keywords = {asteroids: individual: 7 Iris, Astrophysics - Earth and Planetary Astrophysics, methods: numerical, methods: observational, minor planets},
     month = {apr},
     title = {The shape of (7) Iris as evidence of an ancient large impact?},
   journal = {Astronomy and Astrophysics},
    volume = {624},
      year = {2019},
     pages = {A121},
      issn = {0004-6361},
       url = {https://ui.adsabs.harvard.edu/abs/2019A&A...624A.121H},
  abstract = {Context. Asteroid (7) Iris is an ideal target for disk-resolved imaging},
={owing to its brightness (V 7-8) and large angular size of 0.33'' during, its apparitions. Iris is believed to belong to the category of large, unfragmented asteroids that avoided internal differentiation, implying, that its current shape and topography may record the first few 100 Myr, of the solar system's collisional evolution. <BR /> Aims: We recovered, information about the shape and surface topography of Iris from disk-, resolved VLT/SPHERE/ZIMPOL images acquired in the frame of our ESO large, program. <BR /> Methods: We used the All-Data Asteroid Modeling (ADAM), shape reconstruction algorithm to model the 3D shape of Iris, using, optical disk-integrated data and disk-resolved images from SPHERE and, earlier AO systems as inputs. We analyzed the SPHERE images and our, model to infer the asteroid's global shape and the morphology of its, main craters. <BR /> Results: We present the 3D shape, volume-equivalent, diameter D<SUB>eq</SUB> = 214 ± 5 km, and bulk density ρ = 2.7 ± 0.3 g, cm<SUP>-3</SUP> of Iris. Its shape appears to be consistent with that of, an oblate spheroid with a large equatorial excavation. We identified, eight putative surface features 20-40 km in diameter detected at several, epochs, which we interpret as impact craters, and several additional, crater candidates. Craters on Iris have depth-to-diameter ratios that, are similar to those of analogous 10 km craters on Vesta. <BR />, Conclusions: The bulk density of Iris is consistent with that of its, meteoritic analog based on spectroscopic observations, namely LL, ordinary chondrites. Considering the absence of a collisional family, related to Iris and the number of large craters on its surface, we, suggest that its equatorial depression may be the remnant of an ancient, (at least 3 Gyr) impact. Iris's shape further opens the possibility that, large planetesimals formed as almost perfect oblate spheroids. Finally,, we attribute the difference in crater morphology between Iris and Vesta, to their different surface gravities, and the absence of a substantial, impact-induced regolith on Iris. <P />The reduced images are only, available at the CDS via anonymous ftp to <A, href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>, (ftp://130.79.128.5) or via <A href="http://cdsarc.u-strasbg.fr/viz-, bin/qcat?J/A+A/624/A121">http://cdsarc.u-strasbg.fr/viz-, bin/qcat?J/A+A/624/A121</A>Based on observations made with ESO, Telescopes at the Paranal Observatory under programme ID 199.C-0074 (PI:, P. Vernazza) and 086.C-0785 (PI: B. Carry)., 10.1051/0004-6361/201834541, eprint: arXiv:1902.09242},
}