Phase II of the Small Main-Belt Asteroid Spectroscopic Survey: The Observations

By S. Bus, R. Binzel. 2002

388 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Ecology, Geophysics

View Paper: https://www.semanticscholar.org/paper/6b075c177e75cc383865fb045f27a2f9833d8964

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Citations in the corpus

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).”
Phase II of the Small Main-Belt Asteroid Spectroscopic Survey: A Feature-Based Taxonomy (2002, methodology): “In developing this taxonomy, we use the slope values and principal component scores that were computed for the SMASSII data by Bus and Binzel (2002).”
Bias-corrected population, size distribution, and impact hazard for the near-Earth objects (2004, neutral): “Bus and Binzel (2002b)present in their Fig.”
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).”
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).”
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.”
Compositional distributions and evolutionary processes for the near-Earth object population: Results from the MIT-Hawaii Near-Earth Object Spectroscopic Survey (MITHNEOS) (2019, methodology): “If more extensive data are available, we move down the progression applying the Bus taxonomy (Bus 1999; Bus and Binzel 2002b) when visible spectra are available or the near-infrared only taxonomy of DeMeo et al. (2009).”
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…”
Phase reddening on near-Earth asteroids: Implications for mineralogical analysis, space weathering and taxonomic classification (2012, methodology): “Most of the current classification systems are based on visible data (e.g., Tholen, 1984; Bus and Binzel, 2002a,b), 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.”
Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion (2005, methodology): “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).”
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.”