Two new basaltic asteroids in the Outer Main Belt?
Two new V-type asteroids in the outer Main Belt?1
R. Du�ard∗2
Instituto de Astrofísica de Andalucía, C/ Bajo de Huetor, 50. 18008. Granada, Spain, and
Max Planck Institute for Solar System Research, Max Planck Str. 2, Katlenburg-Lindau,
Germany
duffard@iaa.es
F. Roig
Observatório Nacional, Brazil
froig@on.br
ABSTRACT
The identi�cation of basaltic asteroids in the asteroid Main Belt and the de-
scription of their surface mineralogy is necessary to understand the diversity in
the collection of basaltic meteorites. Basaltic asteroids can be identi�ed from
their visible re�ectance spectra and are classi�ed as V-type in the usual tax-
onomies. In this work, we report visible spectroscopic observations of two candi-
date V-type asteroids, (7472) Kumakiri and (10537) 1991 RY16, located in the
outer Main Belt (a > 2.85 UA). These candidate have been previously identi�ed
by Roig and Gil-Hutton (2006, Icarus 183, 411) using the Sloan Digital Sky Sur-
vey colors. The spectroscopic observations have been obtained at the Calar Alto
Observatory, Spain, during observational runs in November and December 2006.
The spectra of these two asteroids show the steep slope shortwards of 0.70 µm
and the deep absorption feature longwards of 0.75 µm that are characteristic of
V-type asteroids. However, the presence of a shallow but conspicuous absorption
band around 0.65 µm opens some questions about the actual mineralogy of these
1Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto,
operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía
(CSIC).
2corresponding author
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two asteroids. Such band has never been observed before in basaltic asteroids
with the intensity we detected it. We discuss the possibility for this shallow
absorption feature to be caused by the presence of chromium on the asteroid sur-
face. Our results indicate that, together with (1459) Magnya, asteroids (7472)
Kumakiri and (10537) 1991 RY16 may be the only traces of basaltic material
found up to now in the outer Main Belt.
Subject headings: Asteroids, composition
1. Introduction
Basaltic asteroids are small bodies connected to the processes of heating and melting
that may have led to the mineralogical di�erentiation in the interiors of the largest asteroids.
Therefore, a precise knowledge of the inventory of basaltic asteroids may help to estimate
how many di�erentiated bodies actually formed in the asteroid Main Belt, and this in turn
may provide important constraints to the primordial conditions of the solar nebula.
In the visible wavelengths range, the re�ectance spectrum of basaltic asteroids is char-
acterized by a steep slope shortwards of 0.70 µm and a deep absorption band longwards of
0.75 µm. Asteroids showing this spectrum are classi�ed as V-type in the usual taxonomies
(e.g. Bus & Binzel, 2002).
A few years ago, most of the known V-type asteroids were members of the Vesta dy-
namical family, located in the inner asteroid belt �semi-major axis a < 2.5 AU�. This family
formed by the excavation of a large crater (Thomas et al., 1997; Asphaug, 1997) on the
surface of asteroid (4) Vesta, which is the only known large asteroid �diameter D ∼ 500 km�
to show a basaltic crust (McCord et al., 1970).
Nowadays, however, several V-type asteroids have been identi�ed in the inner belt but
outside the Vesta dynamical family (Burbine et al., 2001; Florczak et al., 2002; Alvarez-
Candal et al., 2006). Basaltic asteroids have also been found in the middle Main Belt
�2.5 < a < 2.8 AU� (Binzel et al., 2006; Roig et al., 2007), as well as among the Near
Earth Asteroids (NEA) population (McFadden et al., 1985; Cruikshank et al., 1991; Binzel
et al., 2004; Du�ard et al., 2006). Recent works (Carruba et al., 2005, 2007; Nesvorný
et al., 2007; Roig et al., 2007) provide evidence that many of these V-type asteroids may
be former members of the Vesta family, that reached their present orbits due to long term
dynamical evolution. The exception is asteroid (1459) Magnya, the only basaltic object so
far discovered in the outer belt �a > 2.8 AU� (Lazzaro et al., 2000). This asteroid is too far
away from the Vesta family and it is also too big �D = 20-30 km� to have a real probability
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of being a fragment from the Vesta's crust (Michtchenko et al., 2002).
Beyond the existence of (4) Vesta and the V-type asteroids related to the Vesta dy-
namical family, the paucity of intact di�erentiated asteroids and of their fragments observed
today in the main belt is an strong constraint to the formation scenario of basaltic mate-
rial. The sample of iron meteorites collected in the Earth indicates that they would come
from the iron core of dozens of di�erentiated parent bodies. However, there are very few
olivine-rich asteroids (classi�ed as A-type) which are assumed to come from the mantle of
di�erentiated bodies, and only one asteroid, (1459) Magnya, is known to sample the basaltic
crust of a di�erentiated parent body other than (4) Vesta. Finally, the other Main Belt
asteroid families, which formed from the disruption of over �fty 10 < D < 400 km asteroids,
show little spectroscopic evidence that their parent bodies were heated enough to produce a
distinct core, mantle and crust (Cellino, 2003).
Aiming to establish if other V-type asteroids might be found together with (1459) Mag-
nya in the outer belt, thus giving support to the existence of a di�erentiated parent body
in that part of the belt, Roig & Gil-Hutton (2006) used the �ve band photometry from the
3rd release of the Sloan Digital Sky Survey Moving Objects Catalog (SDSS-MOC; Ivezi¢ et
al., 2001; Juri¢ et al., 2002) to identify candidate V-type asteroids. Among 263 candidates
that are not members of the Vesta dynamical family, Roig & Gil-Hutton found �ve possible
V-type asteroids in the outer belt: (7472) Kumakiri, (10537) 1991 RY16, (44496) 1998 XM5,
(55613) 2002 TY49, and (105041) 2000 KO41. However, these �ndings need to be con�rmed
by accurate spectroscopic observations.
The aim of this work is to describe the visible spectroscopic observations of two of these
candidates: (7472) Kumakiri and (10537) 1991 RY16. Our goal is to provide a more reliable
taxonomic classi�cation of these asteroids indicating that they would the second and third
basaltic asteroids discovered up to now in the outer belt. Our observations also reveal certain
peculiarities of their spectra that deserve special attention in future studies. Last but not
least, our results help to validate the approach of Roig & Gil-Hutton (2006) to predict V-type
asteroids. It is worth recalling that a similar study has been performed by Roig et al. (2007),
who used visible spectroscopic observations taken at the Gemini Observatory to con�rm the
classi�cation of two candidate V-type asteroids in the middle belt: (21238) 1995 WV7 and
(40521) 1999 RL95.
In Sect. 2, we describe the observations and the reduction procedures. In Sect. 3, we
present and discuss the results obtained. Finally, Sect. 4 is devoted to conclusions.
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2. Observations
Low resolution spectroscopy of (7472) Kumakiri and (10537) 1991 RY16 were obtained
on November 14, 2006, as part of a 4 nights observational run, using the Calar Alto Faint
Object Spectrograph (CAFOS) at the 2.2m telescope in Calar Alto Observatory, Spain. The
prime aim of the run was to characterize V-type asteroids inside and outside the Vesta
family. Asteroid (7472) Kumakiri was observed again on December 29, 2006, using the same
instrument and telescope, under Director's Discretionary Time (DDT). Table 1 summarizes
the observational circumstances.
CAFOS1 is equipped with a 2048×2048 CCD detector SITe-1d (pixel size 24 µm/pixel,
plate scale 0.53"/pixel). We used the R400 grism allowing to obtain an observable spectral
range between 0.50 and 0.92 µm. To remove the solar component of the spectra and obtain
the re�ectance spectra, the solar analog stars HD 191854, HD 20630 and HD 28099 (Hardorp,
1978) were also observed at similar airmasses as the asteroids. In order to estimate the
quality of each night, at least two solar analogs were observed per night and we veri�ed that
the ratios between the corresponding spectra show no signi�cant variations. Bias frames,
spectral dome �at �elds and calibration lamps spectra were also taken in each night to allow
reduction of the science images. Spectrum exposures for each asteroid were splitted in two
exposures at two di�erent slit positions, A and B, separated by 20" (the width of the slit was
2.0"). The observations were performed with the telescope tracking at the proper motion
of the asteroid. Hence by subtracting A from B and B from A, a very accurate background
removal is achieved. Finally, standard methods for spectra extraction were applied.
3. Results and discussion
The re�ectance spectra of (7472) Kumakiri and (10537) 1991 RY16 are shown in Figs.
1 and 2. Both spectra show a steep slope shortwards of 0.70 µm and a deep absorption
band longwards of 0.75 µm. Using the algorithm of Bus (1999), we determine that the
spectra can be classi�ed as V-type. Figure 1 show that our observations are compatible
with the spectra of previously known V-type asteroids (gray lines) taken from the SMASS
survey (Bus & Binzel, 2002) and the S3OS2 survey (Lazzaro et al., 2004). Figure 2 show the
good agreement between the �ve band photometry of the SDSS-MOC (black lines) and the
observed spectra. It is worth noting that the values of maximum and minimum re�ectance
prevents to attribute to these spectra other taxonomic classi�cation, like R-, O- or Q-type.
1See http://www.caha.es/alises/cafos/cafos22.pdf for more details.
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In view of this, (7472) Kumakiri and (10537) 1991 RY16 may be considered, together with
(1459) Magnya, the only V-type asteroids discovered up to now in the outer belt.
Notwithstanding, the spectra of (7472) Kumakiri and (10537) 1991 RY16 show a shal-
low absorption feature around 0.60-0.70 µm that has never been reported before in V-type
asteroids. This feature is more evident in the spectrum of (10537) 1991 RY16. After the its
identi�cation in the November 14 observations, and excluding possible reduction artifacts or
solar analogs problems, we requested Director Discretionary Time (DDT) for another obser-
vational run on December 29. Only the spectra of (7472) Kumakiri was able to be observed
during this run, con�rming the presence of the absorption band. Nevertheless, the band in
the spectrum of (10537) 1991 RY16 has also been observed independently by Moskovitz et
al. (2007).
To analyze this band, we recti�ed the spectra by subtracting a linear continuum in the
interval 0.55 and 0.75 µm and then �tted several polynomials of di�erent degrees. This
allowed to determine the center of the band at 0.63± 0.01 µm and the FWHM of ∼ 0.1 µm
(e.g. Fig. 3).
The origin of this absorption band is unclear. Such kind of bands are usually believed to
arise from the Fe2+ → Fe3+ charge transfer absorptions in phyllosilicate (hydrated) minerals
(Vilas & Ga�ey, 1989; Vilas et al., 1993). However, it is di�cult to explain the presence of
a hydrated mineral in the surface of a basaltic object, because the heating and melting that
produce the basalt also eliminate any traces of water.
It is known that pyroxene crystals Fe2+ cations do not show any absorption bands in the
spectral region from 0.56 to 0.72 µm. Therefore, the origin of the observed band might be
related to other impurity cations like Mn2+, Cr3+, and Fe3+, usually located in the M1 site
of terrestrial and meteorite orthopyroxenes (Shestopalov et al., 2007). In particular, broad
spin-allowed bands of trivalent chromium around 0.430-0.455 µm and 0.620-0.650 µm have
been observed in both re�ectance and transmitted spectra of Cr-containing terrestrial ortho
and clinopyroxenes (see Cloutis, 2002), as well as in diogenite re�ectance spectra (McFadden
et al., 1982). Cr3+ cations also give spin-forbidden bands near 0.480, 0.635, 0.655, and 0.670
µm but they do not give absorptions near 0.57 µm.
Cloutis (2002) speci�cally found that Cr3+ gives rise to an absorption band near 0.455
µm and a more complex absorption feature in the 0.65 µm region. However, changes in
the grain size of the pyroxenes may have an e�ect on the depth of these absorption bands
(Cloutis and Ga�ey 1991; Sunshine and Pieters 1993). Therefore, the presence of speci�c
absorption bands can be taken as an evidence for the presence of a particular cation, but the
characteristics of these bands (depth and width) are probably not reliable enough to constrain
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the cation abundance (Cloutis 2002). For example, the grain size may be responsible of the
di�erent band depth observed between the spectra of (7472) Kumakiri and (10537) 1991
RY16. The slight di�erences in the band pro�le between the November and December
spectra of (7472) Kumakiri might be attributed to di�erent rotational phases2.
Another interesting feature observed in our spectra is that the band center of the major
absorption feature at 0.90 µm is displaced to larger wavelenghts. In our spectra, this region
is the noisiest but using di�erent polynomial �ts it was possible to estimate the center of
the band nearer to 0.92-0.93 µm. This behavior may also be attributed to the presence of
chromium on the surface. Actually, Cloutis and Ga�ey (1991) suggested that the Cr-rich
pyroxene samples in their study have the two major absorption features (i.e. the one centered
at 0.9 and the one centered at 1.9 µm, respectively) displaced to larger wavelengths than
expected, relative to their Fe contents. These authors also presented the predicted versus
actual wavelength position of the major Fe2+ absorption band center in the 1 µm region,
and this center is closer to 0.92 µm than to 0.90 µm. Therefore, the observational evidence
points to a possible Cr-rich basaltic composition on the surfaces of (7472) Kumakiri and
(10537) 1991 RY16.
Concerning the dynamical behavior of these two asteroids, Table 2 lists their proper
elements and diameters, as well as those of (1459) Magnya. The three asteroids are too small
to be di�erentiated bodies by themselves, they are quite spread in proper elements space and
do not belong to any of the asteroid dynamical families identi�ed in the outer belt. Therefore,
they are likely to be fragments from more than one di�erentiated parent bodies. Nevertheless,
at variance with (1459) Magnya, (7472) Kumakiri and (10537) 1991 RY16 evolve very close to
the non linear secular resonance de�ned by the combination g0+s0−g5−s7 ' 0, where gi and
si represent the frequencies of the perihelion $ and node Ω, respectively (i = 0 for asteroid,
i = 5 for Jupiter, i = 7 for Uranus; see Milani & Kneºevi¢, 1992). A 50 My simulation of
the orbits of these two asteroids, including gravitational perturbations from the four major
planets, indicate that they have quite stable orbits showing a slow circulation of the angle
$0+Ω0−$5−Ω7. Although this may be just a coincidence, a dynamical connection between
(7472) Kumakiri and (10537) 1991 RY16 cannot be ruled out and should be addressed by
more detailed studies.
2We have veri�ed that these di�erences cannot be related to observation/reduction problems, since we
do not �nd any di�erences between the spectra of the solar analog stars used in the di�erent nights.
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4. Conclusions
We presented visible spectroscopic observations of two asteroids, (7472) Kumakiri and
(10537) 1991 RY16, located in the outer belt. The main goal of our work was to show that
these observations are compatible with the V-type taxonomic class. Therefore, these bodies
would constitute the second and third basaltic asteroids discovered up to now in that part
of the Main Belt.
However, the presence of a shallow absorption band in the spectra around 0.65 µm opens
some questions about the actual mineralogy of these two asteroids. This band is likely to
be related to the presence of Cr3+ cations, and provides evidence for a possible a Cr-rich
basaltic surface.
The spectroscopic similarities among the two asteroids, together with some shared dy-
namical properties, point to the idea of a common origin from the breakup of a di�erentiated
parent body in the outer belt. Further studies, including near infrared (NIR) spectroscopic
observations, are mandatory to better address these issues.
We thank Calar Alto Observatory for allocation of Director's Discretionary Time to this
programme. Fruitful discussions with D. Nesvroný are also highly appreciated. Based on
observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto,
operated jointly by the Max- Planck Institut für Astronomie and the Instituto de Astrofísica
de Andalucía (CSIC). RD acknowledges �nancial support from the MEC (contract Juan de
la Cierva).
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This preprint was prepared with the AAS LATEX macros v5.2.
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Table 1: Observational circumstances for the targets: Universal Time (UT), heliocentric
distance (r), geocentric distance (∆), phase angle (φ), visual magnitude (V ), airmass and
total exposure time (Texp).
Asteroid UT r [AU] ∆ [AU] φ [deg] V [mag] airmass Texp
November 14
(7472) Kumakiri 03:25:00 2.920 2.123 13.5 16.6 1.037 3400 sec
(10537) 1991 RY16 00:05:08 3.040 2.053 1.8 17.1 1.091 4000 sec
December 29
(7472) Kumakiri 21:48:52 2.873 1.901 3.8 15.9 1.094 3600 sec
Table 2: Proper elements and sizes of V-type asteroids in the outer belt. For (1459) Magnya,
the last column gives the diameter from Delbo et al. (2006). For (7472) Kumakiri and
(10537) 1991 RY16, the diameter was computed assuming an albedo of 0.40.
Asteroid ap [AU] ep sin Ip D [km]
(1459) Magnya 3.14986 0.2183 0.2651 17.0± 1.0
(7472) Kumakiri 3.01033 0.1372 0.1562 8.5
(10537) 1991 RY16 2.84958 0.1023 0.1101 7.3
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Fig. 1.� Re�ectance spectra of (7472) Kumakiri and (10537) 1991 RY16 (black lines)
compared to the spectra of several known V-type asteroids taken from the SMASS and
S3OS2 surveys (gray lines). The spectra are normalized to 1 at 0.55 µm and shifted by 0.5
units in re�ectance for clarity. To remove the solar contribution, we have used the solar
analog HD 191854 in the November 14 observations and the solar analog HD 28099 in the
December 29 observation.
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Fig. 2.� Re�ectance spectra of (7472) Kumakiri and (10537) 1991 RY16 (gray lines) com-
pared to the photometric observations of the SDSS-MOC (black lines). The spectra are
normalized to 1 at 0.477 µm (i.e. the center of the g band in the SDSS photometric system),
and shifted by 0.5 units in re�ectance for clarity. The errors in the SDSS-MOC �uxes are
less than 3%.
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(10537) 1991 RY16
-0.15
-0.05
0.54 0.59 0.64 0.69 0.74
Fig. 3.� Re�ectance spectrum of (10537) 1991 RY16 in the 0.55-0.75 µm interval. The
spectrum has been recti�ed by subtracting a linear continuum in this interval. From a
polynomial �t (thick line), the center of the absorption band is detected at 0.63 µm with a
FWHM of 0.1 µm.
	Introduction
	Observations
	Results and discussion
	Conclusions
