The body's observation arc begins with its first observation as 1951 XE1 at McDonald Observatory in December 1951, nearly 34 years prior to its official discovery observation at Nauchnij.[1]
In November 2008, photometric follow-up observations by Robert Stephens at his Goat Mountain Astronomical Research Station (G79) gave a divergent period of 14.51 hours and a low amplitude of 0.08 (U=2),[12] while in March 2013, Mottola's original result was confirmed by astronomers at the Palomar Transient Factory, California, measuring a period 10.436 hours and a brightness variation of 0.16 magnitude in the R-band (U=2).[4][11]
Diameter and albedo
According to the surveys carried out by the Japanese Akari satellite, the Infrared Astronomical Satellite IRAS, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Podalirius measures between 85.49 and 86.89 kilometers in diameter and its surface has an albedo between 0.050 and 0.056.[7][8][9] The Collaborative Asteroid Lightcurve Link adopts the results obtained by IRAS, that is, an albedo of 0.0536 and a diameter of 86.89 kilometers based on an absolute magnitude of 9.1.[4]
100+ largest Jupiter trojans
Largest Jupiter Trojans by survey(A) (mean-diameter in kilometers; YoD: Year of Discovery)
Note: missing data was completed with figures from the JPL SBDB (query) and from the LCDB (query form) for the WISE/NEOWISE and SIMPS catalogs, respectively. These figures are given in italics. Also, listing is incomplete above #100.
^ abcdUsui, Fumihiko; Kuroda, Daisuke; Müller, Thomas G.; Hasegawa, Sunao; Ishiguro, Masateru; Ootsubo, Takafumi; et al. (October 2011). "Asteroid Catalog Using Akari: AKARI/IRC Mid-Infrared Asteroid Survey". Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi:10.1093/pasj/63.5.1117. (online, AcuA catalog p. 153)
^ abcdTedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System – IRAS-A-FPA-3-RDR-IMPS-V6.0. 12: IRAS–A–FPA–3–RDR–IMPS–V6.0. Bibcode:2004PDSS...12.....T. Retrieved 15 June 2018.
^ abcWaszczak, Adam; Chang, Chan-Kao; Ofek, Eran O.; Laher, Russ; Masci, Frank; Levitan, David; et al. (September 2015). "Asteroid Light Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry". The Astronomical Journal. 150 (3): 35. arXiv:1504.04041. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75. S2CID8342929.
^ abStephens, Robert D. (April 2009). "Asteroids Observed from GMARS and Santana Observatories". The Minor Planet Bulletin. 36 (2): 59–62. Bibcode:2009MPBu...36...59S. ISSN1052-8091.
^Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. S2CID53493339.