Minor planets and related objects. XVIII - UBV photometry and surface composition

Zellner, B.; Wisniewski, W. Z.; Andersson, L.; Bowell, E.

doi:10.1086/111831

Cited by 33 publications

(11 citation statements)

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“…To assess the completeness of optical asteroid surveys, we assume that they are complete to a V = 21.5 mag, commensurate with the 95% completeness limit from the SDSS (Juric et al 2002) and other surveys such as the Sub-Kilometer Asteroid Diameter Survey (Gladman et al 2009) and Spacewatch (Larsen et al 2007). Assuming that an asteroid will be detected at opposition by one of a number of surveys, we utilize the relation m V = H + 5 log[r h (r h − 1)], and calculate the completeness limits in terms of H in each of the four Main Belt asteroids zones as defined in Zellner et al (1975), adopting opposition and a heliocentric distance which corresponds to the outer semimajor axis range of each respective zone. These values range from absolute magnitudes of 18.6 in the inner Main Belt to 16.57 in the outer Main Belt.…”

Section: Completenessmentioning

confidence: 99%

“…Assuming a 5σ limiting flux of 10 mJy at 22 μm, a beaming parameter, η = 1.07, geometric albedo p V = 0.14, and an asteroid observed at opposition (phase angle α = 0) at a heliocentric distance of 2.5 AU and a geocentric distance (Δ) of 1.5 AU, WISE can only detect asteroids with diameters > ∼ 1.65 km, whereas under these same orbital assumptions and a flux completeness limit of 2 mJy, our Spitzer data is sensitive to asteroids with diameters D > ∼ 0.79 km. Zellner et al (1975) Main Belt Asteroid (MBA) I region (2.06 < a ≤ 2.5), the dotted line corresponds to MBAII (2.5 < a ≤ 2.82), the dashed line corresponds to MBAIII (2.82 < a ≤ 3.27). Bottom: diameter distributions of the Spitzer detected asteroids in the same regions.…”

Section: Completenessmentioning

confidence: 99%

“…Carvano et al (2010) find that the distribution of small C-and X-type asteroids observed by the SDSS are fairly evenly distributed as a function of semimajor axis; however, we leave the detailed statistical interpretation of the C-type inner belt population to a later paper. To determine if C-and S-types asteroids in our sample (Zellner et al 1975) Main Belt regions, and values on the right of each plot give the number of asteroids of specified taxonomic type in each Main Belt region. The distribution of the low albedo small and large asteroids is interesting; only 9% of all large (D > 10 km) asteroids with C-type albedos are found in the inner Main Belt, but 24% of all small (D < 10 km) asteroids with C-type albedos are found in the inner Main Belt.…”

Section: Albedo Gradient Across Main Beltmentioning

confidence: 99%

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The kilometer-sized Main Belt asteroid population revealed bySpitzer

Ryan

Mizuno

Shenoy

et al. 2015

A&A

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Aims. Multi-epoch Spitzer Space Telescope 24 μm data is utilized from the MIPSGAL and Taurus Legacy surveys to detect asteroids based on their relative motion. Methods. Infrared detections are matched to known asteroids and average diameters and albedos are derived using the near Earth asteroid thermal model (NEATM) for 1865 asteroids ranging in size from 0.2 to 169 km. A small subsample of these objects was also detected by IRAS or MSX and the single wavelength albedo and diameter fits derived from these data are within the uncertainties of the IRAS and/or MSX derived albedos and diameters and available occultation diameters, which demonstrates the robustness of our technique. Results. The mean geometric albedo of the small Main Belt asteroids in this sample is p V = 0.134 with a sample standard deviation of 0.106. The albedo distribution of this sample is far more diverse than the IRAS or MSX samples. The cumulative size-frequency distribution of asteroids in the Main Belt at small diameters is directly derived and a 3σ deviation from the fitted size-frequency distribution slope is found near 8 km. Completeness limits of the optical and infrared surveys are discussed.

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Section: Completenessmentioning

confidence: 99%

Section: Completenessmentioning

confidence: 99%

Section: Albedo Gradient Across Main Beltmentioning

confidence: 99%

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The kilometer-sized Main Belt asteroid population revealed bySpitzer

Ryan

Mizuno

Shenoy

et al. 2015

A&A

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“…Hapke (1971) noted the large variation of UBV colors of a material with particle size. Zellner et al (1975) shows that the scatter of UBV colors for specimens of a variety of diverse meteorite types (e.g. Eucrites, Howardites, H, L, LL and C3 chondrites) is larger than the difference in mean colors between types.…”

Section: Introductionmentioning

confidence: 97%

Asteroid surface materials: Mineralogical characterizations from reflectance spectra

1978

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“…We finally averaged the corresponding determinations and obtained (U − B) = 0.22 ± 0.01, (B − V) = 0.68 ± 0.01, (V − R) = 0.39 ± 0.01, and (R − I) = 0.32 ± 0.01. It is interesting to recall the implications of these color indices, in particular those involving the UBV bands, for classifying Lutetia (e.g., Zellner et al 1975). In the color-color diagram (U − V) versus (B − V), Lutetia strikingly lies well inside the taxonomy group M and completely outside the C group.…”

Section: The Color Of Asteroid 21 Lutetiamentioning

confidence: 99%

Multi-color, rotationally resolved photometry of asteroid 21 Lutetia from OSIRIS/Rosetta observations

Lamy¹,

Faury²,

Jordá³

et al. 2010

A&A

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Context. Asteroid 21 Lutetia is the second target of the Rosetta space mission. Extensive pre-encounter, space-, and ground-based observations are being performed to prepare for the flyby in July 2010. Aims. The aim of this article is to accurately characterize the photometric properties of this asteroid over a broad spectral range from the ultraviolet to the near-infrared and to search for evidence of surface inhomogeneities. Methods. The asteroid was imaged on 2 and 3 January 2007 with the Narrow Angle Camera (NAC) of the Optical, Spectroscopic, and Infrared Remote Imaging System (OSIRIS) during the cruise phase of the Rosetta spacecraft. The geometric conditions were such that the aspect angle was 44 • (i.e., mid-northern latitudes) and the phase angle 22.4 • . Lutetia was continuously monitored over 14.3 h, thus exceeding one rotational period and a half, with twelve filters whose spectral coverage extended from 271 to 986 nm. An accurate photometric calibration was obtained from the observations of a solar analog star, 16 Cyg B. Results. High-quality light curves in the U, B, V, R and I photometric bands were obtained. Once they were merged with previous light curves from over some 45 years, the sidereal period is accurately determined: P rot = 8.168271 ± 0.000002 h. Color variations with rotational phase are marginally detected with the ultraviolet filter centered at 368 nm but are absent in the other visible and near-infrared filters. The albedo is directly determined from the observed maximum cross-section obtained from an elaborated shape model that results from a combination of adaptive-optics imaging and light curve inversion. Using current solutions for the phase function, we find geometric albedos p V = 0.130 ± 0.014 when using the linear phase function and p V (H − G) = 0.180 ± 0.018 when using the (H − G) phase function, which incorporates the opposition effect. The spectral variation of the reflectance indicates a steady decrease with decreasing wavelength rather than a sharp fall-off.

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Minor planets and related objects. XVIII - UBV photometry and surface composition

Cited by 33 publications

References 0 publications

The kilometer-sized Main Belt asteroid population revealed bySpitzer

The kilometer-sized Main Belt asteroid population revealed bySpitzer

Asteroid surface materials: Mineralogical characterizations from reflectance spectra

Multi-color, rotationally resolved photometry of asteroid 21 Lutetia from OSIRIS/Rosetta observations

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