Phase II of the Small Main-Belt Asteroid Spectroscopic Survey: A Feature-Based Taxonomy

By S. Bus, R. Binzel. 2002

919 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Ecology, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/7332ce5163551b5ad96203e710f02ede89a832d9

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Citations in the corpus

Bias-corrected population, size distribution, and impact hazard for the near-Earth objects (2004, neutral): “Bus and Binzel (2002b)present in their Fig.”
SPACE WEATHERING OF ASTEROID SURFACES (2004, background): “Thus began the C-S-M. . . asteroid taxonomy that has now been expanded to include most letters of the alphabet and has been further refined by many researchers (the latest taxonomy is due to Bus & Binzel 2002).”
Keck observations of near-Earth asteroids in the thermal infrared (2003, methodology): “…of the three objects with the highest η-values, namely (3671) Dionysus and 2002 BM26, are fast rotators with periods of around 2.7 h (however, the FRM solution for (3671) from Harris and Davies, 1999, requires pv > 0.3, which is inconsistent with the taxonomic class Cb from Bus and Binzel 2002).”
The Compositional Structure of the Asteroid Belt (2015, methodology): “At the time of Asteroids III, the majority of reflectance spectra were taken at visible wavelengths to one micron, and were classified according to the Bus or Tholen taxonomies (Bus & Binzel 2002b, Tholen & Barucci, 1989).”
Absolute magnitudes of asteroids and a revision of asteroid albedo estimates from WISE thermal observations (2012, neutral): “The taxonomy data were taken from Tholen (1989), Bus and Binzel (2002), DeMeo et al. (2009), Xu et al. (1995), and Lazzaro et al. (2004), as compiled in Neese (2010); they are given in columns Taxon.”
Phase reddening on near-Earth asteroids: Implications for mineralogical analysis, space weathering and taxonomic classification (2012, methodology): “, Tholen, 1984; Bus and Binzel, 2002b,a), in part because only during the last decade sufficient high-quality NIR spectral data became available to extend the classification to the near-infrared wavelengths. Two of the most common systems used to classify asteroids using VIS–NIR data are those intro”
MAIN BELT ASTEROIDS WITH WISE/NEOWISE. I. PRELIMINARY ALBEDOS AND DIAMETERS (2011, background): “Compositional gradients for the Main Belt have been shown in the past from both infrared and spectral surveys (e.g. Zellner 1979; Gradie & Tedesco 1982; Tedesco et al. 2002; Bus & Binzel 2002), but only for a limited number of objects.”
Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion (2005, neutral): “More examples could be the 22 A-type asteroids identified by the SMASS and SMASSII surveys (out of a total sample of 950), with the largest body having D ∼ 60 km (Xu et al., 1995; Bus and Binzel, 2002a, 2002b).”
Ion irradiation of carbonaceous chondrites: A new view of space weathering on primitive asteroids (2017, background): “Primitive asteroids (C-complex; [Bus & Binzel, 2002; DeMeo et al., 2009]) are especially studied because they are thought to contain organic compounds and some water, key elements for life on Earth.”
Phase II of the Small Main-Belt Asteroid Spectroscopic Survey: The Observations (2002, methodology): “The application of asteroid taxonomy to the SMASSII data set is discussed at length in a companion paper (Bus and Binzel 2002).”
An extension of the Bus asteroid taxonomy into the near-infrared (2009, methodology): “As discussed below, the over-riding criterion of similarity of spectral properties in a class, as examined over the full 0.45 - 2.45 μm range, led to some objects in the Bus (Bus, 1999; Bus and Binzel, 2002b) classification receiving new class designations here.”
Evidence for asteroid space weathering from the Sloan Digital Sky Survey (2005, methodology): “5 The SMASS spectra were obtained fromhttp://smass.mit.edu/. ed itude 15.0, ASS e- d no loba ati- the viduch by .”
The Size Distributions of Asteroid Families in the SDSS Moving Object Catalog 4 (2008, result): “For example, a comparison of SDSS sample with the Small Main-Belt Asteroid Spectroscopic Survey (Xu et al. 1995; Bus & Binzel 2002ab) is discussed in detail by N05.”
SDSS-based taxonomic classification and orbital distribution of main belt asteroids (2010, methodology): “We use here the objects observed by the SMASSII (Bus & Binzel 2002b) and S3OS2 surveys (Lazzaro et al. 2004).”
Mineralogies and source regions of near-Earth asteroids (2013, methodology): “Therefore, it is necessary to combine SpeX data with visible spectra (0.4–1.1 lm) from SMASS (small-main-belt asteroid survey) (Xu et al., 1995; Bus and Binzel, 2002a, 2002b) or Palomar (Binzel et al., 2001) to achieve full wavelength coverage between 0.4 and 2.5 lm. Visible wavelength coverage was…”
NEAR-INFRARED SPECTROSCOPY OF TROJAN ASTEROIDS: EVIDENCE FOR TWO COMPOSITIONAL GROUPS (2008, methodology): “The redder group lies at the red end of the traditional D-type classification, whereas the less red group straddles the boundary between C-type and P-type (subset of the X-type in the Bus & Binzel (2002b) taxonomy).”