Observation of the asteroid light curve indicates it is rotating with a period of 9.93 ± 0.01 hours. During this interval, the magnitude varies by an amplitude of 0.12 ± 0.02. By combining the results of multiple light curves, the approximate ellipsoidal shape of the object can be estimated. It appears to be slightly elongated, being about 28.2% longer along one axis compared to the other two. Atalante was observed by Areciboradar in October 2010.
^Brinsfield, James W. (September 2007), "The Rotation Periods of 36 Atalante and 416 Vaticana", The Minor Planet Bulletin (Minor Planets Section of the Association of Lunar and Planetary Observers) 34 (3): 58–59, Bibcode:2007MPBu...34...58B
^Šidlichovský, M. (1999), "Resonances and chaos in the asteroid belt", in Svoren, J.; Pittich, E. M.; Rickman, H., Evolution and source regions of asteroids and comets : proceedings of the 173rd colloquium of the International Astronomical Union, held in Tatranska Lomnica, Slovak Republic, August 24–28, 1998: 297–308, Bibcode:1999esra.conf..297S.