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Spectral Properties of Nine M-Type Asteroids

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Spectral Properties of Nine M-Type Asteroids A&A 475, 747–754 (2007) Astronomy DOI: 10.1051/0004-6361:20077914 & c ESO 2007 Astrophysics Spectral properties of nine M-type asteroids M. Birlan1, P. Vernazza2, and D. A. Nedelcu1,3 1 Institut de Mécanique Céleste et de Calcul des Éphémérides (IMCCE), Observatoire de Paris, 77 avenue Denfert-Rochereau, 75014 Paris Cedex, France e-mail: [email protected] 2 LESIA, Observatoire de Paris-Meudon, 5 place Jules Janssen, 92195 Meudon Cedex, France e-mail: [email protected] 3 Astronomical Institute of the Romanian Academy, 5 Cu titul de Argint, 75212 Bucharest, Romania e-mail: [email protected] Received 19 May 2007 / Accepted 27 August 2007 ABSTRACT Aims. We present spectroscopic results for nine M-type asteroids (325 Heidelberga, 497 Iva, 558 Carmen, 687 Tinette, 766 Moguntia, 860 Ursina, 909 Ulla, 1280 Baillauda, and 1564 Srbija) in the 0.8−2.5 µm spectral region. One visible spectrum is also presented for the asteroid 497 Iva. These asteroids were observed during several runs between 2003 and 2007, and the main goal was to investigate the NIR spectral region of M-type asteroids. Methods. The data was obtained with SpeX/IRTF in Prism mode and Dolores/TNG in LR-B mode. Spectral analysis was performed by comparing the M-type spectra and the meteorite ones (χ2 approach) and the Modified Gaussian Model. Results. With one exception, the asteroids present positive slopes of the spectra, with no absorption features, in good agreement with the spectra of metallic meteorites. The analysis of the asteroid 766 Moguntia was done by means of χ2, MGM techniques, and the Shkuratov scattering law. We conclude that the mineralogy is dominated by olivine. Its NIR spectrum is similar to those of CO/CV meteorites. Key words. minor planets, asteroids 1. Introduction parameter, and radiometry. They proposed a classification for these objects (the last column in their Table 1). The M-type asteroid class was initially defined by seven param- Lightcurve investigations of M-type asteroids (Lagerkvist eters directly measurable from four observational techniques, et al. 1998) revealed an excess of fast rotators among them com- namely photometry, polarimetry, radiometry and spectropho- pared to other taxonomic types. According to Harris (1979), a tometry (Bowell et al. 1978). Historically, this taxonomic class tendency towards more rapid rotation among asteroids must be brought an end to previous ideas concerning bimodality in the interpreted as indicating high material strength. asteroid population, largely dominated by the C-type asteroids Various approaches of mass determination (bulk density re- (associated with carbonaceous materials) and the S-type ones spectively) of M-asteroids gave contradictory results. The bulk (associated with silicate minerals). density estimation a few of them revealed very low values (Ostro Several articles confirmed this taxonomic class. et al. 2002; Margot & Brown 2003; Birlan 2000). These re- Between 1984 and 1994 several articles reinforced the sults imply very high values for the bulk porosity (Britt & definition of the M taxonomic class (Tholen 1984; Barucci Consolmagno 2000), that is difficult to reconcile with high et al. 1987; Tholen & Barucci 1989; Tholen 1989; Fulchignoni strength materials. et al. 1995), with various statistical tests combined with cluster All these references brings forth the conclusion that M-type analysis techniques. The analyzed colors revealed a taxonomic objects are still important in deciphering the history of formation class with a slightly positive spectral slope, and a moderate and evolution of the main belt. thermal albedo (0.151 ± 0.063 in Birlan et al. 1996). This It is important to mention the limitations of taxonomical M class has been degenerated into the so-called X-complex classes designation, as long as the classification could not reveal when the thermal albedo is not taken into account. the real geologic diversity that occurs among the main-belt as- Several results of polarimetric surveys have been pub- teroids. It is now accepted that spectroscopy provides data which lished (Belskaya et al. 1985, 1987; Lupishko & Belskaya 1989; are relevant for obtaining results concerning the mineralogy and Belskaya et al. 1991; Gil-Hutton 2007). Lupishko & Belskaya chemical interpretation of atmosphereless bodies. (1989) give a wide range of polarimetric measurements for Spectra of M-type asteroids are consistent with the presence M-type asteroids, inconsistent with only a metallic composition of Fe-bearing minerals (or metallic surfaces) and usually they are of their surface. Magri et al. (2007) also found a wide inter- interpreted as parent bodies of metallic meteorites (Dollfus et al. val of radar albedos among M-asteroids, again in disagreement 1979; Cloutis et al. 1990a,b). This interpretation is also sup- with metal-rich surfaces for some M-type objects. Belskaya & ported by radar observations, where the strength of the reflected Lagerkvist (1996) synthesized the knowledge for all M or M-like radar echoes is consistent with a high concentration of metals asteroids, based on colors, spectrophotometry, polarization on their surfaces (e.g. Ostro et al. 2000; Magri et al. 2007). Article published by EDP Sciences and available at http://www.aanda.org or http://dx.doi.org/10.1051/0004-6361:20077914 748 M. Birlan et al.: Spectral properties of nine M-type asteroids Table 1. Date of observations with the fraction of the day for the beginning of the observation, number and name of the asteroid, semimajor axis, eccentricity, inclination, the apparent magnitude, phase angle, as well as heliocentric and geocentric distance. Date (UT) Asteroid aeiVΦ (◦) r (UA) ∆ (UA) 2003/10/29.911 497 Iva 2.85918514 0.296270 4.811626 12.05 4.2 2.03 1.04 2003/11/04.482 497 Iva 2.85918514 0.296270 4.811626 12.26 6.4 2.06 1.08 2003/11/05.612 766 Moguntia 3.02032355 0.092544 10.078727 14.78 17.6 2.74 2.07 2003/11/05.630 558 Carmen 2.90676856 0.043101 8.365791 14.29 20.8 2.78 2.54 2006/04/18.226 860 Ursina 2.79537340 0.109044 13.314103 15.81 18.6 3.10 2.75 2006/04/18.321 325 Heidelberga 3.20389760 0.167631 8.540609 14.22 19.4 2.83 2.32 2006/04/18.408 1564 Srbija 3.17462507 0.199762 11.018214 16.27 4.3 3.70 2.72 2006/04/19.353 1280 Baillauda 3.41409115 0.060099 6.457478 16.10 12.9 3.56 2.86 2006/04/19.406 687 Tinette 2.72578375 0.271155 14.853600 16.90 7.4 3.43 2.50 2007/03/13.552 909 Ulla 3.54127850 0.099305 18.747663 15.03 10.6 3.89 3.14 Meanwhile Hardersen et al. (2005) claimed weak absorption fea- with an airmass of less then 1.25. No other correction for the dif- tures around 0.9 µm for six M-types asteroids. They associate the ferential refraction was performed. Each observed asteroid was presence of this band with iron-poor orthopyroxenes and pro- preceded by observations of solar analogs in the vicinity (air- posed four possible interpretations for these asteroids. mass differences between the asteroid and the standard were less For some M-type asteroids, spectroscopic studies in the than 0.1). The seeing varied between 0.7−1.8 arcsec during the Near-InfraRed (NIR) region revealed the presence of hydrated observing runs, and the humidity was in the 25%−85% range. minerals, which is difficult to explain for an evolved (consti- In order to obtain a S/N in the 80−200 range, we needed 15 tuted by melted minerals) object. Thus, based on 3-µm obser- to 40 min of exposure time, depending on the asteroid magni- vations, Rivkin et al. (2000) and Rivkin et al. (1995) proposed tude, and counting both the effective exposure and CCD camera the split of this class into “M-class” asteroids (e.g. the absence readout time. Exposure times are presented in Table 2. of the 3-µm absorption band) and “W-class” asteroids (e.g. hy- For 497 Iva, one visible spectrum was obtained using the drated ones). However Gaffey et al. (2002) discussed the obser- Dolores/TNG facility. The Dolores spectrograph was used in vational difficulties associated with obtaining reliable spectra for the LR-B mode. MIDAS procedures for spectral reduction were the 3-µm spectral region, and proposed alternative explanations used for the final spectrum. to the aqueous alteration. For the asteroid spectra, the solar analogs SA 93-101, In this paper we present spectroscopic results for nine HD 76332, SA 98-1155, SA 93-1077, HD 103529, HD 95364, M-type targets in the 0.8−2.5 µm region. The asteroids were HD 103529, HD 257880 were observed. For the computation of observed during several runs between 2003 and 2007, to study the final reflectance (ratio between the asteroid spectrum and the M-type members in the NIR spectral region. star spectrum) we took into account the similar dynamic regimes of the detector (Vacca et al. 2004; Rayner et al. 2003). 2. The observing protocol The asteroids were observed in the 0.8−2.5 µm spectral region 3. Results / with SpeX IRTF instrument, located on Mauna Kea, Hawaii. The M-type asteroids observed are: 325 Heidelberga, 497 Iva, These observations were performed in remote mode from Centre 558 Carmen, 687 Tinette, 766 Moguntia, 860 Ursina, 909 Ulla, d’Observation à Distance en Astronomie à Meudon (CODAM) 1280 Baillauda, and 1564 Srbija. Their orbital elements the ob- (Birlan et al. 2004, 2006) using the low resolution Prism mode servations are presented in Table 1. = . × (R 100) of the spectrograph. We used a 0 8 15 arcsec slit The near-IR spectra are presented in Fig.
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