Mineralogical Variations within the S-Type Asteroid Class

Gaffey, M. J.; Bell, J. F.; Brown, R. H.; Burbine, T. H.; Piatek, J. L.; Reed, K. L.; Chaky, D. A.

doi:10.1006/icar.1993.1194

Cited by 456 publications

(697 citation statements)

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“…Based on the asteroid colour recompilation by McCheyne et al (1985) we derived a mean colour of (R − Ks) = 1.49 ± 0.28 and (J − Ks) = 0.45 ± 0.11 based on a sample of seven asteroids. An independent sample of albedos of nine asteroids reported by Gaffey et al (1993) gives (R − Ks) = 1.27 ± 0.23 (J − Ks) = 0.57 ± 0.27, consistent with the first sample. Thus, the location of asteroids in the (J − Ks) vs. (R − Ks) colour-colour diagram is far from the region where we find GRB afterglows, ensuring that the colour-colour technique is effectively screening out asteroids.…”

Section: Location Of Other Astrophysical Objects In the Diagramsupporting

confidence: 73%

“…Lower left panel: the figure displays synthetic colour-colour traces for stars (filled circles), galaxies (dashed curves) and quasars (dotted curves). The shaded polygonal background region represents the loci occupied by the asteroid samples of McCheyne et al (1985) and Gaffey et al (1993). As can be seen, the bunch of objects in the left upper panel (located outside the shaded area) can be reproduced by asteroid, stellar, galaxy and quasar synthetic colours.…”

Section: Candidate Selection Using Colour-colour Diagramsmentioning

confidence: 96%

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Strategies for prompt searches for GRB afterglows: The discovery of the GRB 001011 optical/near-infrared counterpart using colour-colour selection

Gorosabel¹,

Fynbo²,

Hjorth

et al. 2002

A&A

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Abstract.We report the discovery of the optical and near-infrared counterparts to GRB 001011. The GRB 001011 error box determined by Beppo-SAX was simultaneously imaged in the near-infrared by the 3.58-m New Technology Telescope and in the optical by the 1.54-m Danish Telescope ∼8 hr after the gamma-ray event. Here we implement the colour-colour discrimination technique proposed by Rhoads (2001) and extend it using near-IR data as well. We present the results provided by an automatic colour-colour discrimination pipe-line developed to discern the different populations of objects present in the GRB 001011 error box. Our software revealed three candidates based on single-epoch images. Second-epoch observations carried out ∼3.2 days after the burst revealed that the most likely candidate had faded, thus identifying it with the counterpart to the GRB. In deep R-band images obtained 7 months after the burst a faint (R = 25.38 ± 0.25) elongated object, presumably the host galaxy of GRB 001011, was detected at the position of the afterglow. The GRB 001011 afterglow is the first discovered with the assistance of colour-colour diagram techniques. We discuss the advantages of using this method and its application to error boxes determined by future missions.

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Section: Location Of Other Astrophysical Objects In the Diagramsupporting

confidence: 73%

Section: Candidate Selection Using Colour-colour Diagramsmentioning

confidence: 96%

Strategies for prompt searches for GRB afterglows: The discovery of the GRB 001011 optical/near-infrared counterpart using colour-colour selection

Gorosabel¹,

Fynbo²,

Hjorth

et al. 2002

A&A

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“…The spectrum was then continuum subtracted and the result was fitted with three-degree polynomial function. We find the center of the feature localized at 1.01 ± 0.06 micron, which is a slightly shorter wavelength than the one found by Gaffey et al (1993). Two series of near-infrared spectra were obtained in March 30, 2003, with the ratio S/N of 50 and 70 (obtained in both A and B beams) for the spectrum obtained at airmass 1.001 and 1.018 respectively ( Figure 5).…”

Section: Juliamentioning

confidence: 63%

“…Multivariate statistics classified the asteroid as part of the S cluster (Barucci et al (1987), Tholen, (1989)). The mineralogical classification of the S-type asteroids (Gaffey et al (1993)) based on the ECAS data and 52-Color spectrophotometric Survey (Bell et al (1988)) data assigns 89 Julia (together with the asteroid 9 Metis) as 'ungrouped' S-asteroids. The main reason of this 'unclassification' is the long wavelength position of the 1-micron feature, which could be the presence of the abundant calcic clinopyroxene component (Gaffey et al (1993)).…”

Section: Juliamentioning

confidence: 99%

Near-IR spectroscopy of asteroids , , , and , potential targets for the Rosetta mission; remote observations campaign on IRTF

et al. 2004

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In the frame of the international campaign to observe potential target asteroids for the Rosetta mission, remote observations have been carried out between Observatoire de Paris, in Meudon-France, and the NASA Infrared Telescope Facility on Mauna Kea. The SpeX instrument was used in the 0.8-2.5 microns spectral region, for two observing runs in March and June 2003. This paper presents near-IR spectra of the asteroids 21 Lutetia, 89 Julia, 140 Siwa, 2181 Fogelin, and 5480 (1989YK8).Near-IR spectra of the asteroids 21 Lutetia and 140 Siwa are flat and featureless. The spectrum of 89 Julia reveals absorption bands around 1 and 2 microns, which may indicate the presence of olivine and olivine-pyroxene mixtures and confirm the S-type designation.The small main-belt asteroids 2181 Fogelin and 5480 (1989YK8) are investigated spectroscopically for the first time. Near-IR spectra of these asteroids also Preprint submitted to New Astronomy 1 May 2018show an absorption feature around 1 micron, which could be and indicator of igneous/metamorphic surface of the objects; new observations in visible as well as thermal albedo data are necessary to draw a reliable conclusion on the surface mineralogy of both asteroids.

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“…Other classification systems created using near-IR data include Howell et al (1994) who created a neural network taxonomy. Gaffey et al (1993) created an S-complex taxonomy of olivine-and pyroxine-rich asteroids based on near-infrared data. Our goal was to create a taxonomy extending from 4…”

Section: Introductionmentioning

confidence: 99%

An extension of the Bus asteroid taxonomy into the near-infrared

DeMeo

Binzel

Slivan

et al. 2009

Icarus

774

978

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The availability of asteroid spectral measurements extending to the near-infrared, resulting from the development of new telescopic instruments (such as SpeX; Rayner 2003), provides a new basis for classifying asteroid reflectance spectra. We present an asteroid taxonomy classification system based on reflectance spectrum characteristics for 371 asteroids measured over the wavelength range 0.45 to 2.45 microns.This system of 24 classes is constructed using principal component analysis, following most closely the visible wavelength taxonomy of Bus (1999), which itself builds upon the system of Tholen (1984)

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Mineralogical Variations within the S-Type Asteroid Class

Cited by 456 publications

References 0 publications

Strategies for prompt searches for GRB afterglows: The discovery of the GRB 001011 optical/near-infrared counterpart using colour-colour selection

Strategies for prompt searches for GRB afterglows: The discovery of the GRB 001011 optical/near-infrared counterpart using colour-colour selection

Near-IR spectroscopy of asteroids , , , and , potential targets for the Rosetta mission; remote observations campaign on IRTF

An extension of the Bus asteroid taxonomy into the near-infrared

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