Visible and Near-infrared Colors of TNOs from the Second ESO Large Program

Details Visible and Near-infrared Colors of TNOs from the Second ESO Large Program Visible and Near-infrared Colors of TNOs from the Second ESO Large Program

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.4705d&link_type=abstract

American Astronomical Society, DPS meeting #40, #47.05; Bulletin of the American Astronomical Society, Vol. 40, p.482

Astronomy and Astrophysics

Astrophysics

2

Scientific paper

We report the visible and near-infrared photometric results from October 2006 through September 2007 for 23 objects, 9 of which have never been previously observed, obtained in the framework of a second ESO Large Program (PI=M.A. Barucci) devoted to observe TNOs with different techniques. All observations were performed at the European Southern Observatory 8m Very Large Telescope, UT1 and UT2 at the Paranal Observatory in Chile; visible and near-infrared observations were carried out simultaneously when possible. We report colors and show a plot of reflectivities. We determine taxonomic types when sufficient data is available and verify the types for previously observed objects. Classification was performed with G-mode analysis expanded by Fulchignoni et al. (2000; Icarus 146, 204) using the Barucci classification system (Barucci 2005; Astron J. 130, 1291) using two to five color data per object. We classify 18 of the 23 objects in our sample: six BB, four BR, two RR and six falling in two or more categories due to insufficient data. Three objects (83982, 119951, 2003 UZ117) had only one color and were therefore unclassifiable. Two objects (26375, 145452) did not fall within the range of the 4 taxonomic groups. Three objects that had been previously observed and classified, changed classes: 26375 (1999 DE9), 28978 (Ixion), and 32532 (Thereus). Two objects, 47932 (2000 GN171) and 54598 (Bienor), had absolute magntitude values Hv(1,1,0) that were significantly different from previously published results. For 47932 and Bienor, large lightcurve amplitudes (Sheppard and Jewitt 2002; Astron J. 124, 1757; Ortiz et al. 2002; Astron Astrophys; 388, 661) can explain the variable Hv(1,1,0) magnitude.

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