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(name, orcid, 
  • Migliorini A. (IAPS-INAF, orcid: 0000-0001-7386-9215)
  • De Sanctis M.C. (IAPS-INAF)
  • Michtchenko T. (IAG, Universidade de San Paulo, Brazil)
  • Lazzaro D. (Observatorio Nacional, COAA, Rio De Janeiro, Brazil , orcid : 0000-0002-4470-6043 )
  • Barbieri M. (Instituto de Astronomia y Ciencias planetarias de Atacama, University of Atacama, Chile)
  • Mesa D. (OAPD, INAF)
  • Lazzarin M. (Dipartimento di Fisica e Astronomia 'G.Galilei', Università di Padova)
  • La Forgia F. (Dipartimento di Fisica e Astronomia 'G.Galilei', Università di Padova, orcid : 0000-0003-3924-1867 )
Titles  Characterisation of V-type asteroids orbiting in the middle and outer main belt
Publisher  INAF - IAPS
Associated Paper  
Publication 2020
Resource type DataSet
Version 1.0
File .zip
Dimension 5.7 MB

We present new spectral observations using ground-based telescopes of 23 putative V-type asteroids, selected according to colour surveys in the visible from the Moving Objects Catalogue of the Sloan Digital Sky Survey and near-infrared from the Moving Objects VISTA catalogue. Ten asteroids are orbiting in the middle main belt, while five in the outer part of the main asteroid belt. For the observed asteroids we assign a taxonomical classification and confirm
the basaltic nature for sixteen of them. The high-quality spectra in the UV range, obtained
with the X-Shooter spectrograph at ESO, allowed the identification of the Fe2+ forbidden transition of pyroxene for ten asteroids. This band is centred at 506.5 nm, and it is diagnostic of the Ca-content in the pyroxene form. We determined a  low Fe-content composition for asteroids (2452)~Lyot, (5758)~Brunini, (7675)~Gorizia, (9197)~Endo, (22308)~1990~UO4, (36118)~1999~RE135, (66905)~1999~VC160, and (189597)~2000~WG119,  and a composition more rich in Fe  for asteroids (75661)~2000~AB79 and (93620)~2000~UQ70.

We also present a dynamical investigation of  V-type asteroids in the middle and outer main belt. The principal finding of these simulations is that the middle and outer V-types are more likely to be associated with some families, which were considered as possibly originated from the break-up of a partially or totally differentiated parent body by diverse studies.  This reinforces the hypothesis that the identified V-type in the region were not originated from (4) Vesta and that the number of differentiated objects in the middle and outer main belt must have been much larger than previously assumed. 




Characterisation of V-type asteroids orbiting in the middle and outer main belt