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Mineralogical Analysis of the Eos Family from Near-Infrared Spectra

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Mineralogical Analysis of the Eos Family from Near-Infrared Spectra Icarus 195 (2008) 277–294 www.elsevier.com/locate/icarus Mineralogical analysis of the Eos family from near-infrared spectra T. Mothé-Diniz a,b,∗,J.M.Carvanoa,b,S.J.Busc,R.Duffardd, T.H. Burbine e a LESIA, Observatoire de Paris, 92195 Meudon, France b COAA, Observatório Nacional, Rua Gal. José Cristino, 77, São Cristóvão, 20921-400 Rio de Janeiro, Brazil c Institute for Astronomy, University of Hawaii at Hilo, Hilo, HI 96720-2700, USA d Max Planck Institute for Solar System Research, 37191 Katlenburg-Lindau, Germany e Astronomy Department, Mount Holyoke College, South Hadley, MA 01075, USA Received 2 January 2007; revised 19 November 2007 Available online 31 December 2007 Abstract The aim of this work is to analyze the mineralogy of the Eos family, which exhibits considerable taxonomic diversity. Its biggest fragment, (221) Eos has previously been associated, through direct spectral comparisons, with such diverse mineralogies as CV/CO and achondrite mete- orites [Burbine, T.H., Binzel, R.P., Bus, S.J., Clark, B.E., 2001. Meteorit. Planet. Sci. 36, 245–253; Mothé-Diniz, T., Carvano, J.M., 2005. Astron. Astrophys. 174, 54–80]. In order to perform such analysis we obtained spectra of 30 family members in the 0.8–2.5 µm range, and used three different methods of mineralogical inference: direct spectral comparison with meteorites, intimate mixing using Hapke’s theory, and fitting ab- sorption features with the MGM. Although the direct comparison failed to yield good matches—the best candidates being R-chondrites—both mixing model and MGM analysis suggest that the bulk of the family is dominated by forsteritic (Fa∼20) olivine, with a minor component of or- thopyroxene. This composition can be compatible with what would be expected from the partial differentiation of a parent-body with an original composition similar to ordinary chondrites, which probably formed and differentiated closer to the Sun than the present location of the family. A CK-like composition is also possible, from the inferred mineralogy, as well as from the similarities of the spectra in the NIR. © 2008 Elsevier Inc. All rights reserved. Keywords: Asteroids, composition; Spectroscopy 1. Introduction authors compared the spectra of the family members with the meteorites measured by Gaffey (1976). Recently, Burbine et al. The first attempts of deciphering the mineralogy of minor (2001) compared the NIR (0.44–1.65 µm) spectrum of (221) planets date back to the 1980s. In particular, the Eos family, Eos with a number of CO3/CV3 meteorites and the meteorite located in the outer part of the main belt, was first associated CO3 Warrenton was found to be the best analog to Eos among with CO/CV anhydrous meteorites (Bell, 1988). In that work, the carbonaceous chondrites. However, they did not use the en- Bell compared the spectrum of Eos in the near-infrared (NIR) tire meteorite database available in their comparison. By using the entire RELAB database (Pieters and Hiroi, 2004), Mothé- (0.33–2.5 µm) with the available meteorite spectral data, and Diniz and Carvano (2005) found that, in the same range spec- noticed that the spectra and albedo of some Eos family objects tral used by Burbine et al. (2001), the spectrum of (221) Eos were best matched by CV and CO chondrites. Ten years lat- and (653) Berenike (also a member of the Eos dynamical fam- ter, Doressoundiram et al. (1998) reinforced the association of ily) were more similar to the anomalous achondrite Divnoe, an the Eos family with CO/CV chondrites by showing similari- olivine-rich meteorite whose parent-body suffered partial melt- ties between the spectra of 45 Eos family members and these ing. This association suggested a completely different thermal types of meteorites in the visible range (0.48–0.92 µm). These history for the parent-body of the Eos family than if a CO/CV composition was assumed. * Corresponding author at: COAA, Observatório Nacional, Rua Gal. José From the dynamical point of view, the Eos family has re- Cristino, 77, São Cristóvão, 20921-400 Rio de Janeiro, Brazil. cently been analyzed by Vokrouhlický et al. (2006) in an at- E-mail address: [email protected] (T. Mothé-Diniz). tempt to understand the structure and history of the family 0019-1035/$ – see front matter © 2008 Elsevier Inc. All rights reserved. doi:10.1016/j.icarus.2007.12.005 278 T. Mothé-Diniz et al. / Icarus 195 (2008) 277–294 through modern dynamical tools. Their work suggests that NASA Infrared Telescope Facility (IRTF) equipped with a drifting produced by the Yarkovsky effect could inject frag- 1024 × 1024 InSb array spectrograph (SpeX), and located at ments of the Eos family in the 9/4 and 7/3 resonances. They the Mauna Kea Observatory in Hawaii during three nights, from were also able to constrain the age of the family to 1.3 Gyr, February 7 to 9, 2005. The other 10 spectra (two of which were and to determine a number of suspected interlopers in the fam- also observed in the run of February 2005) were observed in the ily, based on their orbital position which was inconsistent with IRTF with the same configuration in previous years, as shown in Yarkovsky evolution. Table 1. We have used a 0.8 arcsec slit oriented in the east–west The purpose of this work is to perform a detailed mineralog- direction. In the low resolution prism-mode, this slit provides a ical analysis of high signal-to-noise visible and near-infrared resolution R ∼ 100, with a spectrum covering the entire inter- (VNIR) spectra of members of the Eos dynamical family. To val from 0.8 to 2.5 µm in a single exposure. For the reduction of accomplish this goal we analyzed the spectra of 30 Eos fam- the data, we followed the standard procedures of flat field cor- ily members obtained in the Infrared Telescope Facility (IRTF). rection and sky subtraction. The spectra were then extracted, A brief description of the physical and orbital characteristics calibrated in wavelength, and finally each of them was fit with of the Eos family is presented in the next section. In Section 3 the ATRAN model for telluric absorption features (Lord, 1992). we detail the observation reduction procedures, as well as the This process is described in detail by Clark et al. (2004a) and observational circumstances of each object. In Section 4.1 we Sunshine et al. (2004). Several spectra of solar analog stars were search for meteorites spectroscopically similar to our objects. taken during each night. These stars were used to produce nor- Section 4.2 contains a detailed mineralogical analysis of all malized reflectance spectra of the asteroids. The final spectra objects through the absorption band modified Gaussian model presented in this paper are the averages of all ratios obtained (MGM) (Sunshine and Pieters, 1993). The radiative transfer for each object. The error bars are not plotted, but the errors model of Hapke (1993) was also used to infer the surface min- eralogy of some of the objects. The results of this analysis is propagated through the reduction are usually less than the scat- presented in Section 4.3. In Section 5, we compare the results ter in the data. So, we assume that the scatter in the data is the from the different methods and discuss their significance. best estimate of the uncertainties of each measurement. Table 1 lists the asteroids, some observational circumstances and phys- 2. Physical and dynamical characteristics of the family ical characteristics for the objects observed, and in Fig. 1 shows the calibrated spectra of all objects. Located at 2.95 ap 3.13, 0.03 ep 0.11 and 0.155 sin(ip) 0.2, the Eos family accounts for about 4400 mem- 3.1. Spectral features bers if a cutoff1 of 55 m s−1 is considered (Vokrouhlický et al., 2006), where ap, ep and ip denote respectively the proper orbital elements: semi-major axis, eccentricity and inclination. As a general characteristic of the observed objects, we can The biggest fragment of the family, (221) Eos, is ∼104 km in say that all the spectra obtained present a clear absorption band diameter and belongs to the K taxonomic class. The diameter around 1 µm, with a minimum between 1.0 and 1.1 µm. Most of distribution has a median of ∼31 km, and the median albedo is the objects have a negative continuum slope in the wavelength ∼0.15. The size of the parent-body that originated the family is range 1.5–2.5 µm. A weak 2-µm absorption due to pyroxenes estimated to be 218 km (Tanga et al., 1999). can also be seen in the spectrum of a few objects: 633, 669, Ninety-two of the family members have taxonomic classi- 1413, 1416, 1903, 2957 and 3469. A more subtle absorption in fication (Mothé-Diniz et al., 2005), and the family is the only the same position seems to be present in other spectra also, sug- 2 known to present a high “taxonomic inhomogeneity,” with rep- gesting a mixture of olivine and pyroxene as a main component resentatives among a wide range of the Bus’ classes (Bus and in the surface of the Eos family members. Binzel, 2002):T,D,Ld,Xk,Xc,X,L,S,CandB(Mothé-Diniz Whenever a visible (VIS) spectrum was available from et al., 2005). Nevertheless it is quite well distinguished from the SMASSII (Bus and Binzel, 2002) or S3OS2 (Lazzaro et al., background asteroids, which is mostly composed by C-type ob- 2004) for a given object in the family (Table 1), it was joined jects.
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