Electronic Telegram No. 5738 Central Bureau for Astronomical Telegrams Mailing address: Hoffman Lab 209; Harvard University; 20 Oxford St.; Cambridge, MA 02138; U.S.A. e-mail: cbatiau@eps.harvard.edu (alternate cbat@iau.org) URL http://www.cbat.eps.harvard.edu/index.html Prepared using the Tamkin Foundation Computer Network (4468) POGREBETSKIJ R. Brown, Trans-Tasman Occultation Alliance and Newcastle Astronomical Society reports the discovery of an apparent satellite of minor planet (4468) based on an occultation of the star UCAC4 330-155366 (which has catalogued Gaia magnitudes G = 14.5 and R = 13.8) on 2026 Aug. 24.452 UT. This main- belt asteroid had a magnitude of 18.9, which was 4.4 magnitudes fainter than the target star. Brown observed from Glen William, NSW, Australia, using a 36-cm telescope (+ Hyperstar lens + QHY 174M CMOS Camera with GPS timing). The recording showed two consecutive occultations of durations 0.61 and 2.60 s, separated by 11.80 s, corresponding to chord lengths of 0.97 and 4.13 km with a mid-chord separation of 18.73 km. The flux of the first drop fell to the level of the comparison star UCAC4 330-155331, which has catalogued Gaia magnitudes 15.5 (G) and 14.8 (R), and the flux for the second drop was to the limiting magnitude of the recording, which was approximately 16.0 (G). The depths of the two drops (1.0 and 1.5 in G, 1.0 and 2.2 in R) are sufficiently great to exclude a double star from being the explanation for the light curve. The NEOWISE-catalogue diameter of the asteroid is 4.2 +/- 0.4 km; the Gaia DR3 magnitude measurements suggest a rotational light variation on the order of 0.18 magnitude, and Carry et al. (2024, A.Ap. 687, A38) derive an oblateness of 0.95 +/- 0.51, both of which indicate that the main body is not significantly elongate. On this basis, the main body has been modeled as a circle having the NEOWISE-catalogued diameter. Fresnel modeling of the drop from the apparent satellite indicates that the chord was tangential to the limb. Modeling indicates that the minimum size of the apparent satellite is 1.3 km, with a maximum diameter of about 2.0 km for a circular body. The separation of the satellite was 0".0145 in p.a. 274 +/- 2 degrees, with a separation of 21.3 km. L. Liberato (GaiaMoons, Observatoire de la Cote d'Azur) advises that a binary-search analysis of this minor planet in the Gaia FPR astrometry (cf. website URL https://doi.org/10.1051/0004-6361/202659515; Liberato et al. 2026, A.Ap. 711, A299) detected two different periods (13.5 and 8.7 hours) in three different observation epochs. These periods have very low statistical confidence and, while they are much shorter than the expected orbital period of this apparent satellite, they are not contradictory to the satellite evidence from this occultation. The sky-plane configuration showing the observed occultation chords is posted at the following website URL: http://www.cbat.eps.harvard.edu/iau/cbet/005700/CBET5738_Fig1.png. Representative models of the system, and the observed light curves with superimposed Fresnel modeled light curves, are posted at website URL http://www.cbat.eps.harvard.edu/iau/cbet/005700/CBET5738_Fig2.png D. Herald and D. Gault, Trans-Tasman Occultation Alliance; and C. Weber, European Section of the IOTA, aided in the analysis; the reader is also referred to the end notes on CBET 5679. NOTE: These 'Central Bureau Electronic Telegrams' are sometimes superseded by text appearing later in the printed IAU Circulars. (C) Copyright 2026 CBAT 2026 September 14 (CBET 5738) Daniel W. E. Green