Albedos and diameters of three Mars Trojan asteroids

We observed the Mars Trojan Asteroids (5261) Eureka and (101429) 1998 VF 31 and the candidate Mars Trojan 2001 FR 127 at 11.2 and 18.1 microns using Michelle on the Gemini North telescope. We derive diameters of 1.28, 0.78, and <0.52 km, respectively, with corresponding geometric visible albedos...

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Published inIcarus (New York, N.Y. 1962) Vol. 192; no. 2; pp. 442 - 447
Main Authors Trilling, David E., Rivkin, Andrew S., Stansberry, John A., Spahr, Timothy B., Crudo, Richard A., Davies, John K.
Format Journal Article
LanguageEnglish
Published San Diego, CA Elsevier Inc 15.12.2007
Elsevier
Subjects
Astronomy
Earth, ocean, space
Exact sciences and technology
Infrared observations
Regoliths
Solar system
Trojan asteroids
USA, California, Eureka
Trojan asteroids
Regoliths
Infrared observations
Albedo
Asteroids
Infrared observation
Regolith
Solar system
Diameter
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ISSN0019-1035
1090-2643
DOI10.1016/j.icarus.2007.08.002

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Summary:We observed the Mars Trojan Asteroids (5261) Eureka and (101429) 1998 VF 31 and the candidate Mars Trojan 2001 FR 127 at 11.2 and 18.1 microns using Michelle on the Gemini North telescope. We derive diameters of 1.28, 0.78, and <0.52 km, respectively, with corresponding geometric visible albedos of 0.39, 0.32, and >0.14. The albedos for Eureka and 1998 VF 31 are consistent with the taxonomic classes and compositions (S(I)/angritic and S(VII)/achondritic, respectively) and implied histories presented in a companion paper by Rivkin et al. Eureka's surface likely has a relatively high thermal inertia, implying a thin regolith that is consistent with predictions and the small size that we derive.
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ISSN:0019-1035
1090-2643
DOI:10.1016/j.icarus.2007.08.002