Optical Photometry Of Jovian Trojan Asteroids: Are Color And Inclination Correlated?

Details Optical Photometry Of Jovian Trojan Asteroids: Are Color And Inclination Correlated? Optical Photometry Of Jovian Trojan Asteroids: Are Color And Inclination Correlated?

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21336305y&link_type=abstract

American Astronomical Society, AAS Meeting #213, #363.05; Bulletin of the American Astronomical Society, Vol. 41, p.514

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Were Jovian Trojans captured by Jupiter from the outer regions of the solar system or did they originate at their current location?The chemical and dynamical properties of these objects may help answer this question and shed light on the history of giant planet formation. Recently, Szabo et al. (2007) investigated the optical colors of 860 Trojans based on the Sloan Digital Sky Survey (SDSS). They found that the r' - z' color indices of Trojans are weakly correlated with their orbital inclinations over the range 0°< i < 30°. Fornasier et al (2007) also reported a similar weak correlation in the optical spectroscopy of 47 Trojans.
The significance of a color-inclination trend, if real, is not clear. One suggestion is that the trend could result from thermal processing of objects prior to capture, with those captured into higher inclination orbits being more (less?) thermally processed than others. Another possibility is that the color-inclination trend could result from the overlapping of Trojans captured from different sources, perhaps at different times.The statistical significance of the relation can be ascertained from observations of Trojans over a larger range of inclinations.To test the purported relation, we obtained broadband B, V, R photometry with the UH 2.2 meter telescope on Mauna Kea, for about 80 Trojan asteroids focussing specially on objects with high inclinations ( i > 30°). We will present our photometric results and address the implications of our findings for origins of Jovian Trojans.
This work was supported by grant NNG06GG08G to David Jewitt from the NASA Planetary Origins program

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