ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O O O O O O O O B-CelestialObject O O O O O O O O O O O O B-Survey O O O O O O O O O O O O O O O O O O B-CelestialObject O O O O B-Mission O O O O O O O O O O O O O O O O B-CelestialObjectRegion O O O O O O O O O O O O O B-CelestialObjectRegion O O O O O O O O O B-Citation I-Citation I-Citation O O B-CelestialObjectRegion O O O O O O O O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O B-CelestialObjectRegion O O O O O O O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O O B-CelestialObject O O O O O O B-Citation I-Citation I-Citation O O O O O O O O O O O O O O B-CelestialObject O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Survey O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O O O O O O O O O O O B-CelestialObject O O O O O O O O O O O O O O O O B-CelestialObject O O B-CelestialObjectRegion O O O O O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O O O O O
tokens: includes several vestoids and inner belt non-vestoids, while the second group includes some inner belt vestoids and non-vestoids, as well as middle/outer belt non-vestoids. It is worth noting that the errors involved in the determination of spectroscopic and polarimetric parameters are usually large. In many cases, the differences observed amongst the samples fall within their 1 uncertainties, making them indistinguishable in practice. In principle, there is no clear relation between these spectroscopic and polarimetric differences and the different dynamical populations. 2.3 Size distribution So far, the clearest evidence that prevents a link between (4)Vesta and (1459)Magnya is the size of the latter, which does not fit within the expected size frequency distribution (SFD) of the ejecta from craterization events (Durda etal. 2007 ; Michel etal. 2015 ) like those that excavated the surface of (4)Vesta. On the other hand, the remaining non-vestoids (from both the spectroscopic and SDSS samples) are all as small as the vestoids and may also have originated from craterization events. Images of Vestas surface taken by the Dawn probe revealed two large basins in the south pole of the asteroid. One of them, named Rheasilvia with 500km of diameter, has been dated 1Gyr ago. The other one, named Veneneia with 400km of diameter, has been dated 23Gyr ago (Marchi etal. 2012 ). While Rheasilvia is the likely source of the current vestoids (Buratti etal. 2013 ; McSween etal. 2013 ), Veneneia could be the source of several non-vestoids (Schenk etal. 2012 ). Pirani Turrini ( 2016 ) studied the formation of large basins on the surface of (4)Vesta during the epoch of the giant planet instability and concluded that any record of such basins would have been erased by the subsequent crater saturation over the age of the Solar system. This is in line with the fact that observed craters on Vestas surface dated less than 4.1Gyr ago (OBrien etal. 2014 ). Therefore, the possibility of a very early craterization event on the surface of (4)Vesta that led to the origin of a Vesta-like family cannot be ruled out. In this context, it is interesting to discuss the SFD of the different dynamical populations of V-type asteroids. This is shown in Fig. 2 for the sample of SDSS V-type candidates, but a similar result was obtained by Nesvorn etal. ( 2008 ) considering the spectroscopic sample. The fugitives population shows a similar SFD to the vestoids, indicating that these two populations may be related and have the same collisional age. On the other hand, the low-inclination population and the middle/outer population show SFDs that differ from the Vesta family, suggesting that these populations have a different origin/age. These populations (excluding (1459)Magnya due to its size) could have been originated by early craterization events on the surface of (4)Vesta, like the Veneneia basin or even older events (Schenk etal. 2012 ; McSween etal. 2013 ). Figure 2. The cumulative