Near-infrared Reflectance Spectra Of 135 Hertha, 224 Oceana, 516 Amherstia, And 872 Holda

Near-infrared reflectance spectra of M-asteroids 135 Hertha, 224 Oceana, 516 Amherstia, and 872 Holda display spectral and mineralogical diversity that is becoming the norm for the M-asteroid taxonomic group. 224 Oceana exhibits a traditionally featureless M-asteroid spectrum, moderately reddish slope, and an IRAS albedo of 17%. Canonical interpretations include a NiFe metal-rich surface or a surface similar to that of the enstatite chondrites. 516 Amherstia, with an IRAS albedo of 16%, displays absorption features centered at 0.93- and 1.92-microns superimposed on an overall reddish slope. This suggests a surface with a single mafic silicate (i.e., pyroxene, Wo_10±4Fs_31±5) and NiFe metal. The Band I and II absorptions are 5% and 2% deep, respectively. Amherstia's features are similar to, but somewhat more intense and Fe-rich than, other M-asteroid spectra as discussed in Hardersen et al. (2005). 872 Holda displays a generally featureless NIR reflectance spectrum with the exception of a very broad and weak ( 2% depth) absorption that ranges from 0.5 to 1.2-microns. 872 Holda's overall spectrum is similar to that of synthetic troilite, but differs from spectra of meteoritic troilite as discussed in Cloutis and Burbine (1999). If troilite is present on Holda's surface, then a potential interpretation is a mixture of NiFe metal and troilite as seen in iron meteorites. The NIR reflectance spectrum for 135 Hertha will also be discussed and compared to this asteroid's 52-color survey spectrum, which indicates the presence of a weak 0.9-micron absorption feature. Of the 20 M-asteroid spectra that have been examined by this team thus far, 10 M-asteroids display the presence of low-Fe pyroxene absorption features at 0.9 microns, 3 suggest the presence of spinel, 2 indicate the presence of olivine, one suggests the possible presence of troilite, and 4 display featureless spectra that suggest a variety of potential interpretations.