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Spectroscopic Survey of M--Type Asteroids

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Spectroscopic Survey of M--Type Asteroids Spectroscopic survey of M–type asteroids1 S. Fornasier1,2, B. E. Clark3,1, E. Dotto4, A. Migliorini5, M. Ockert-Bell3, M.A. Barucci1 1 LESIA, Observatoire de Paris, 5 Place Jules Janssen, F-92195 Meudon Principal Cedex, France 2 Universit´ede Paris 7 Denis Diderot, France 3 Department of Physics, Ithaca College, Ithaca, NY 14850, USA 4 INAF, Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monteporzio Catone (Roma), Italy 5 IASF-INAF, via del Fosso del Cavaliere 100, 00133 Roma, Italy Submitted to Icarus: September 2009 e-mail: [email protected]; fax: +33145077144; phone: +33145077746 Manuscript pages: 60; Figures: 10; Tables: 6 1Based on observations carried out at the European Southern Observatory (ESO), La Silla, arXiv:1007.2582v1 [astro-ph.EP] 15 Jul 2010 Chile, ESO proposals 073.C-0622, 074.C-0049 and 078.C-0115 and at the Telescopio Nazionale Galileo, Canary Islands, Spain. Preprint submitted to Icarus September 28, 2018 Running head: Investigation of M–type asteroids Send correspondence to: Sonia Fornasier LESIA-Observatoire de Paris Batiment 17 5, Place Jules Janssen 92195 Meudon Cedex France e-mail: [email protected] fax: +33145077144 phone: +33145077746 2 Spectroscopic survey of M–type asteroids1 S. Fornasier1,2, B. E. Clark3,1, E. Dotto4, A. Migliorini5, M. Ockert-Bell3, M.A. Barucci1 Abstract M-type asteroids, as defined in the Tholen taxonomy (Tholen, 1984), are medium albedo bodies supposed to have a metallic composition and to be the progenitors both of differentiated iron-nickel meteorites and enstatite chondrites. We carried out a spec- troscopic survey in the visible and near infrared wavelength range (0.4-2.5 µm) of 30 asteroids chosen from the population of asteroids initially classified as Tholen M-types, aiming to investigate their surface composition. The data were obtained during several observing runs during the years 2004-2007 at the TNG, NTT, and IRTF telescopes. We computed the spectral slopes in several wavelength ranges for each observed asteroid, and we searched for diagnostic spectral features. We confirm a large variety of spectral be- haviors for these objects as their spectra are extended into the near-infrared, including the identification of weak absorption bands, mainly of the 0.9 µm band tentatively attributed to orthopyroxene, and of the 0.43 µm band that may be associated to chlorites and Mg- rich serpentines or pyroxene minerals such us pigeonite or augite. A comparison with previously published data indicates that the surfaces of several asteroids belonging to the M-class may vary significantly. We attempt to constrain the asteroid surface compositions of our sample by looking for 1Based on observations carried out at the European Southern Observatory (ESO), La Silla, Chile, ESO proposals 073.C-0622, 074.C-0049 and 078.C-0115 and at the Telescopio Nazionale Galileo, Canary Islands, Spain. Preprint submitted to Icarus September 28, 2018 meteorite spectral analogues in the RELAB database and by modelling with geographi- cal mixtures of selected meteorites/minerals. We confirm that iron meteorites, pallasites, and enstatite chondrites are the best matches to most objects in our sample, as suggested for M-type asteroids. For 22 Kalliope, we demonstrate that a syntetic mixture obtained enriching a pallasite meteorite with small amounts (1-2%) of silicates well reproduce the spectral behaviour including the observed 0.9 µm feature. The presence of subtle absorption features on several asteroids confirms that not all objects defined by the Tholen M-class have a pure metallic composition. A statistical analysis of spectral slope distribution versus orbital parameters shows that our sample originally defined as Tholen M-types tend to be dark in albedo and red in slope for increasing value of the semi-major axis. However, we note that our sam- ple is statistically limited by our number of objects (30) and slightly varying results are found for different subsets. If confirmed, the albedo and slope trends could be due to a difference in composition of objects belonging to the outer main belt, or alternatively to a combination of surface composition, grain size and space weathering effects. Keywords: Asteroids, Spectroscopy, Meteorites 4 1. Introduction Within the taxonomic system of Tholen (1984), M asteroids have featureless spectra and red spectral slope over the visible wavelength range (0.34 – 1.04 µm) and medium visual albedos (0.1 – 0.3). Tholen and Barucci (1989) identify ap- proximately 40 M-type asteroids using the Tholen (1984) class definition. The M-types are presumed to be the progenitors both of differentiated iron-nickel me- teorites and enstatite chondrites (Gaffey 1976; Cloutis et al. 1990; Gaffey et al. 1993). Some authors have proposed alternative meteorite linkages, such as CH, CB (Bencubbinite) (Hardersen et al. 2005), or other carbonaceous chondrites (Vilas 1994). M-class albedos generally match those of nickel-iron meteorites, leading some to propose that these asteroids are the collisionally-produced frag- ments of differentiated metal cores (Bell et al. 1989). This interpretation requires parent bodies heated to at least 2000 ◦C to produce iron meteorites (Taylor, 1992). However, based on recent findings, these interpretations are being challenged. Polarimetric measurements (Lupisko & Belskaya 1989) and radar observations (Ostro et al. 1991; 2000; Magri et al. 2007; Shepard et al. 2008) of selected M- type asteroids have revealed a large variety of surface properties that are in some cases inconsistent with only a metallic composition. Shepard et al. (2008), in a radar survey of 14 M-type asteroids, find that only four objects (16 Psyche, 216 Kleopatra, 758 Mancunia, and 785 Zwetana) have radar albedos high enough to be dominantly metallic. The first estimations of the bulk density of M-asteroids 16 Psyche (1.4–1.8 g/cm3) and 22 Kalliope (2.4 g/cm3) gave values surprisingly lower than expected (Viateau 2000; Kocheva 2003; Britt et al. 2002; Margot & Brown 2003). These low den- sities are not consistent with predominantly metal composition, and require very high values for the bulk porosity. However, these values have been disputed and recently Shepard et al. (2008) estimates a very high bulk density for 16 Psy- che (7.6±3.0 g/cm3), more consistent with a metal composition. Descamps et al. (2008) find a bulk density of 3.35±0.33 g/cm3 for 22 Kalliope, higher than the first estimation but still implying a high bulk porosity. Of note is the evidence for hydrated minerals on the surfaces of some M- type asteroids (Jones et al. 1990; Rivkin et al. 1995; 2000; 2002), inferred from the identification of an absorption feature around 3 µm typically due to the first overtone of H2O and to OH vibrational fundamentals in hydrated silicates. Rivkin et al. (1995; 2000) proposed splitting the M-types into wet W-class asteroids (those which show the 3 µm band), and dry M-class asteroids (those which do not show the 3 µm band). If the 3 µm band on M-type asteroids is due to hydrated 5 minerals, then these objects might not be anhydrous and igneous as previously believed and the thermal scenarios for the inner main belt may need a revision (e.g. Bell et al. 1989). Gaffey et al. (2002) propose alternative explanations for the 3 µm band: materials normally considered to be anhydrous containing structural OH; troilite, an anhydrous mineral that shows a feature at 3 µm, or xenolithic hydrous meteorite components on asteroid surfaces from impacts and solar wind implanted H. Recent spectroscopic observations in the visible and near infrared region show that the spectra of M asteroids are not uniformly featureless as previously be- lieved. In addition to the 3 µm band, faint absorption bands in the 0.9 µm re- gion have been identified on the surfaces of some M-type asteroids (Chapman & Gaffey, 1979; Hardersen et al. 2005; Clark et al. 2004a; Ockert-Bell et al. 2008), and attributed to orthopyroxene. Busarev (1998) detected weak features tenta- tively attributed to pyroxenes (0.51 µm) and oxidized or aqueously altered mafic silicates (0.62 and 0.7 µm) in the spectra of the M-type asteroids 75 Eurydike and 201 Penelope (Busarev 1998). In this paper we present new spectroscopic data obtained in the visible and near infrared wavelength range (0.4-2.5 µm) of 30 asteroids sampled from the population of objects whose visible wavelength and albedo properties satisfy the definition of the Tholen M-class. In this work, we (1) identify faint absorption bands which may help reconstruct surface composition, (2) search for meteorite spectral analogues, and (3) model surface composition with geographical mixtures of selected minerals when a meteorite match is not found. 2. Data Acquisition [HERE TABLE 1] The data presented in this work were obtained during 2 runs (February and November 2004) at the italian Telescopio Nazionale Galileo (TNG) of the Eu- ropean Northern Observatory (ENO) in la Palma, Spain, and 3 runs (May 2004, August 2005, and January 2007) at the New Technology Telescope (NTT) of the European Southern Observatory (ESO), in Chile. Six asteroids, investigated in the visible range at the NTT and TNG telescopes, were separately observed in the near infrared at the Mauna Kea Observatory 3.0 m NASA Infrared Telescope Facility (IRTF) in Hawaii during several runs in 2004-2008 (Table 1). Our survey was devoted to the investigation of asteroids belonging to the E, M and X classes, following the Tholen (1984) taxonomy. Here we present the results of our ob- servations sampling within the Tholen M-class. The results from Tholen E-type 6 asteroids were published in Fornasier et al. (2008) and the results from Tholen X-type observations will be presented in a separate paper.
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