Photometric observations of the minor planet in 2010 gave a rotation periodof7.2798±0.0001 h with an amplitudeof0.19±0.02 in magnitude. This result is consistent with previous determinations.[13]Anoccultation by Athor was observed, on October 15, 2002, showing an estimated diameter of 47.0 kilometres (29.2 mi).[7] The spectra is similar to that of carbonaceous chondrites, with characteristics of ferric oxides and little or no hydrated minerals.[14]
^Pilcher & Higgins (2008). "Period Determination for 161 Athor". The Minor Planet Bulletin. 35 (4): 147. Bibcode:2008MPBu...35..147P.
^Debehogne & Zappala (1980). "Photoelectric lightcurves of the asteroids 139 Juewa and 161 Athor, obtained with the 50 CM photometric telescope at ESO, La Silla". Astronomy and Astrophysics Supplement Series. 42: 85–89. Bibcode:1980A&AS...42...85D.
^Pilcher, Frederick (July 2011), "Rotation Period Determinations for 28 Bellona, 81 Terpsichore, 126 Velleda 150 Nuwa, 161 Athor, 419 Aurelia, and 632 Pyrrha", The Minor Planet Bulletin, 38 (3): 156−158, Bibcode:2011MPBu...38..156P.
^Busarev, V. V.; Taran, M. N. (November 2002), "On the spectral similarity of carbonaceous chondrites and some hydrated and oxidized asteroids", Proceedings of Asteroids, Comets, Meteors - ACM 2002. International Conference, 29 July - 2 August 2002, Berlin, Germany. Ed. Barbara Warmbein. ESA SP-500., Noordwijk, Netherlands: ESA Publications Division, pp. 933−936, Bibcode:2002ESASP.500..933B, ISBN92-9092-810-7.
