Eos, Koronis, and Maria Family Asteroids: Infrared (JHK) Photometry

Veeder, G. J.; Matson, D. L.; Owensby, P. D.; Gradie, J.; Bell, J. F.; Tedesco, E. F.

doi:10.1006/icar.1995.1053

Cited by 16 publications

(16 citation statements)

References 2 publications

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“…6. J −K comparisons of 50 objects commonly found in the DENIS catalog and previous JHK asteroid datasets (Hahn & Lagerkvist 1988;Veeder et al 1995).…”

Section: Resultsmentioning

confidence: 99%

“…Two other JHK datasets were used for comparison with DENIS: one sample of 151 objects (Hahn & Lagerkvist 1988) and an other of 56 objects (Veeder et al 1995). The comparison for the 50 objects in common are reported in Fig.…”

Section: Comparisons With Other Datasetsmentioning

confidence: 99%

“…These classes roughly correspond to certain kinds of mineralogies. Previous near-infrared studies (Veeder et al 1982(Veeder et al , 1983a(Veeder et al , 1983b(Veeder et al , 1995 have indicated that some of these distinctions carry from visual wavelengths into the nearinfrared, so some of these classes might be distinguishable on the basis of their near-infrared colors alone. Presently, the 2MASS Asteroid and Comet Survey (Sykes et al 2000), has made available a large and uniform body of asteroid JHK-photometry.…”

Section: Introductionmentioning

confidence: 99%

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Asteroidal I, J, K magnitudes recovered in the DENIS Survey: First release

Baudrand

Bec-Borsenberger

Borsenberger

et al. 2001

A&A

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Abstract. The DENIS programme (Deep European Near-Infrared southern sky Survey) is carrying out a groundbased survey of the southern sky with the aim of providing an extensive I, J, K photometric catalog of point and extended sources. The limiting magnitudes of the three bands I, J, K centered at 0.8, 1.25 and 2.15 µm are respectively 18.5, 16.5 and 13.5. With respect to the exposure time of the observations, asteroids are included in the point source catalog as any other regular point-like object. Up to now, we have identified 1233 asteroids, numbered between 1 and 8000, on the basis of their predicted positions following a recognition procedure described here. Their I, J, K magnitudes are being compiled in electronic tables available at the CDS via anonymous ftp 130.79.128.5.

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“…6. J −K comparisons of 50 objects commonly found in the DENIS catalog and previous JHK asteroid datasets (Hahn & Lagerkvist 1988;Veeder et al 1995).…”

Section: Resultsmentioning

confidence: 99%

Section: Comparisons With Other Datasetsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Asteroidal I, J, K magnitudes recovered in the DENIS Survey: First release

Baudrand

Bec-Borsenberger

Borsenberger

et al. 2001

A&A

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“…They also found that NEAs occupy a very large region in (J − H) vs. (H − K) plot, corresponding to all taxonomic types. Veeder et al (1995) observed 56 asteroids members of Eos, Koronis, and Maria families using J, H, and K filters. They found that the objects belonging to a specific family have a similar surface composition.…”

Section: General Overviewmentioning

confidence: 99%

“…These results are discussed in (J − H) vs. (H − Ks) space and are compared with the regions mapped by S, C, D, and A taxonomic classes. These regions were defined using data from Hahn & Lagerkvist (1988), Smith et al (1992) and Veeder et al (1995). They found that even there are significant regions in which the colors of different taxonomic types overlap, there are some areas in which a specific one dominates.…”

Section: General Overviewmentioning

confidence: 99%

Near-infrared colors of minor planets recovered from VISTA-VHS survey (MOVIS)

Popescu

Licandro

Morate

et al. 2016

A&A

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Context. The Sloan Digital Sky Survey (SDSS) and Wide-field Infrared Survey Explorer (WISE) provide information about the surface composition of about 100 000 minor planets. The resulting visible colors and albedos enabled us to group them in several major classes, which are a simplified view of the diversity shown by the few existing spectra. A large set of data in the 0.8−2.5 µm, where wide spectral features are expected, is required to refine and complement the global picture of these small bodies of the solar system. Aims. We aim to obtain the near-infrared colors for a large sample of solar system objects using the observations made during the VISTA-VHS survey. Methods. We performed a serendipitous search in VISTA-VHS observations using a pipeline developed to retrieve and process the data that corresponds to solar system objects (SSo). The resulting photometric data is analyzed using color−color plots and by comparison with the known spectral properties of asteroids. Results. The colors and the magnitudes of the minor planets observed by the VISTA survey are compiled into three catalogs that are available online: the detections catalog (MOVIS-D), the magnitudes catalog (MOVIS-M), and the colors catalog (MOVIS-C). They were built using the third data release of the survey (VISTA VHS-DR3). A total of 39 947 objects were detected, including 52 NEAs, 325 Mars Crossers, 515 Hungaria asteroids, 38 428 main-belt asteroids, 146 Cybele asteroids, 147 Hilda asteroids, 270 Trojans, 13 comets, 12 Kuiper Belt objects and Neptune with its four satellites. The colors found for asteroids with known spectral properties reveal well-defined patterns corresponding to different mineralogies. The distributions of MOVIS-C data in color−color plots shows clusters identified with different taxonomic types. All the diagrams that use (Y − J) color separate the spectral classes more effectively than the (J − H) and (H − Ks) plots used until now: even for large color errors (<0.1), the plots (Y − J) vs. (Y − Ks) and (Y − J) vs. (J − Ks) provide the separation between S-complex and C-complex. The end members A, D, R, and V-types occupy well-defined regions.

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