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Lightcurves for 5 asteroids were obtained from the Center for Solar System Studies from 2015 October to December.

CCD photometric observations of seven asteroids were obtained from the Center for Solar System Studies from 2016 April to June.

CCD photometry observations made in 2015 October and November of the Vestoid asteroid 5425 Vojtech showed it to be binary. The primary lightcurve has a period of 2.64759 ± 0.000004 h and an amplitude 0.27 ± 0.02 mag. The orbital period of the satellite is 25.43 ± 0.02 h. Based on mutual events ranging from 0.05 to 0.09 mag, the estimated effective diameter ratio of the two bodies is Ds/Dp ≥ 0.22 ± 0.02.

CCD photometric observations of two Hungaria asteroids were obtained from the Center for Solar System Studies from 2017 January to March.

Lightcurves for 18 Jovian Trojan asteroids were obtained at the Center for Solar System Studies (CS3) from 2017 January to March.

Lightcurves for six Jovian Trojan asteroids were obtained at the Center for Solar System Studies (CS3) from 2016 October to December.

CCD photometric observations of 9 asteroids were obtained from the Center for Solar System Studies from 2016 January to March.

CCD photometric observations of 10 main-belt asteroids were obtained from the Center for Solar System Studies from 2018 July to September.

Lightcurves for 45 Near-Earth asteroids (NEAs) obtained at the Center for Solar System Studies (CS3) from 2018 July-September were analyzed for rotation period and signs of satellites or tumbling. NEA 13553 Massakikoyama appears to be in non-principal axis rotation, i.e., tumbling. 2011 UA (D = 0.6 km) is a super-fast rotator with a period of 0.316391 ± 0.000007 h. The period and size place it well above the spin barrier. The period for 2018 RQ2 is multiply ambiguous, with possible solutions of 4.28 h or 5.17 h (monomdal lightcurve) and 8.58 h or 10.60 h (bimodal lightcurve). 2018 KE3 may be a binary asteroid.

Lightcurves for 32 near-Earth asteroids (NEAs) obtained at the Center for Solar System Studies (CS3) from 2018 September-December were analyzed for rotation period and signs of satellites or tumbling.

Lightcurves for four L(5) Jovian Trojan asteroids were obtained at the Center for Solar System Studies (CS3) from 2019 January to March. The suspected binary Trojan, 2207 Antenor was observed again and a single attenuation event was detected.

CCD photometry observations made in 2016 October and November of the Hungaria asteroid (24465) 2000 SX155 showed it to be binary. The primary lightcurve has a period of 2.66087 ± 0.00005 h and an amplitude 0.08 ± 0.02 mag. The orbital period of the satellite is 9.252 ± 0.001 h, the shortest detected so far.

Lightcurves for 19 Hilda asteroids were obtained at the Center for Solar System Studies (CS3) from 2016 August through December.

Lightcurves for 16 Hilda asteroids were obtained at the Center for Solar System Studies (CS3) from 2016 June to September.

CCD photometric observations of twelve asteroids were obtained at the Center for Solar System Studies from 2016 July to September.

Lightcurves for four Hilda asteroids were obtained at the Center for Solar System Studies (CS3) from 2018 September-November: 3514 Hooke, 3557 Sokolsky, 4495 Dassanowksy, and 10331 Peterbluhm. 4495 Dassanowksy appears to be a binary asteroid with a primary period of either 2.6314 hr or 5.263 hr and an orbital period of 18.516 hr. The secondary-to-primary ratio of the effective diameters is 0.26 ± 0.02.

CCD photometric observations of 10 main-belt asteroids were obtained from the Center for Solar System Studies from 2019 January to March. In light of recent period analysis, images of 2120 Tyumenia obtained in 2004 were re-examined. The resulting analysis found a period of 17.515 h, which is consistent with the recent results.

CCD photometric observations of three Hilda asteroids were made at the Center for Solar System Studies (CS3) from 2019 January-March. For 1038 Tuckia, the period solution was ambiguous at either P = 18.020 h, amplitude 0.22 mag or P = 14.401 h, amplitude 0.20 mag. For 2246 Bowell, the analysis found P = 4.997 and amplitude 0.46 mag. For 4317 Garibaldi, we found a dual-period solution with P(1) = 17.843 or 8.92 h and P(2) = 11.426 h. The shorter value for P(1) is similar to previously reported results but this is the first time a true dual-period solution, i.e., not an ambiguous single period solution, has been reported.

CCD photometric observations of 25 main-belt asteroids were obtained at the Center for Solar System Studies (CS3) from 2019 July to September.

CCD photometric observations of 18 main-belt asteroids were obtained from the Center for Solar System Studies from 2018 October to December. A pole solution was found for 4910 Kawasato of (λ, β, P(SID)) = (355°, 35°, 4.66271 h). (31320) 1998 HX2 is a binary asteroid with a P(1) of 2.8149 ± 0.0001 h and P(2) of 47.06 ± 0.05 h.

Lightcurves for 11 L(4) Jovian Trojan asteroids were obtained at the Center for Solar System Studies (CS3) from 2019 July to September.

Lightcurves for five Jovian Trojan asteroids were obtained at the Center for Solar System Studies (CS3) from 2018 July to September.

Lightcurves for 38 near-Earth asteroids (NEAs) obtained at the Center for Solar System Studies (CS3) from 2019 March-July were analyzed for rotation period, peak-to-peak amplitude, and signs of satellites or tumbling.

Lightcurves for 28 near-Earth asteroids (NEAs) obtained at the Center for Solar System Studies (CS3) from 2019 July to September were analyzed for rotation period, peak-to-peak amplitude, and signs of satellites or tumbling. 2059 Baboquivari, (90403) 2003 YE45, and 2016 AU130 are candidates for membership within the very wide binary asteroids class. The 2019 data led to a seemingly unambiguous period of 4.7906 h for (441987) 2010 NY65, which overturned previous results that have now been updated.