Techniques d'observation spectroscopique d'astéroïdes

CHAPTER 7. SPECTRAL PROPERTIES OF MAIN BELT ASTEROIDS 121
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components of comparable size. Unfortunately, no physical ephemerides of Frostia are known
to have a precise timing of possible mutual phenomena of this system. Nevertheless there is
little chance for a geometry allowing mutual phenomena at the time of our observations.
Based on a physical model of a double system, Behrend et al. [2006] calculated a bulk
density of 750 - 1,020 kg/m 3 . They explain such a low density value by a possible C-type
asteroid with a high macro-porosity of about 45 %.
Sloan Digital Sky Survey (SDSS) colors (Ivezić et al. [2001]) 5 of this object were also reported.
These data show large variations in color. It is important to note that the v−i color is
greater than the v−z one 6 , which suggest the presence of absorption band around 1 µm.
Visible spectroscopy of Frostia was reported by Alvarez-Candal et al. [2006]. These results
are in agreement with SDSS colors and the authors classified this asteroid in the V-taxonomic
class.
NIR spectrum of (854) Frostia was obtained on March 13, 2007. The total integration time
of 40 min allows an accurate spectrum with the S/N of 120. I joined the visible spectrum from
Behrend et al. [2006] with our data in NIR region (Fig. 7.2a). The analysis was made on the
composite V+NIR spectrum. This spectrum likely represents the asteroid globally, being a first
characterization of the asteroid’s mineralogy.
The spectrum of (854) Frostia reveals large and deep absorption bands around 1 and 2 µm.
In Bus-DeMeo taxonomy the V+NIR spectrum is typical of V -type asteroids [DeMeo et al.,
2009], similar to the asteroid (4) Vesta. The next two matches returned by M4AST are Sv and
Sr types but these types have larger matching error (Fig 7.2b).
(854) Frostia was not included in the family of (4) Vesta by Zappala et al. [1995]. The location
of (854) Frostia inside the Main-Belt is very similar to that of Vesta family in semi-major
axis and inclination and may justify its membership to the same clan. Frostia’s eccentricity of
0.17 is slightly over the greater boundary (of 0.12) of Vesta family. This case is not particular
while other V-type asteroids were already reported in the inner part of the Main Belt, relatively
close to the Vesta family [Duffard et al., 2004].
In the assumption of (854) Frostia as a fragment of Vesta’s crust, a value of its density around
3,000 kg/m 3 seems to be reasonable. The value calculated by Behrend et al. [2006] (around
1,000 kg/m 3 ) is very difficult to explain even if an unrealistic porosities of 75% in a rubblepile
structure is assumed. In fact, large porosities for small fragments of large differentiated
bodies are not realistic while the self-gravitation tendency is to decrease the volume of empty
space inside the object. Behrend et al. [2006] inferred a C-type asteroid by analogy with the
asteroid (90) Antiope. It is difficult to reconcile the C and V taxonomic classes while the objects
experienced different temperatures in their history.
Descamps [2010] published recently a refined study of binary systems by accounting in-
5 http://sbn.psi.edu/ferret/
6 Sloan Digital Sky Survey was obtained using five broad band filters, namely u,g,r,i,z centered to 3,551, 4,686, 6,165, 7,481, and 8,931