  Graham et al. (2015a) reported a periodically varying quasar and supermassive
black hole binary candidate, PG1302-102 (hereafter PG1302), which was
discovered in the Catalina Real-Time Transient Survey (CRTS). Its combined
Lincoln Near-Earth Asteroid Research (LINEAR) and CRTS optical light curve is
well fitted to a sinusoid of an observed period of $\approx 1,884$ days and
well modeled by the relativistic Doppler boosting of the secondary mini-disk
(D'Orazio et al. 2015). However, the LINEAR+CRTS light curve from MJD $\approx
52700$ to MJD $\approx 56400$ covers only $\sim 2$ cycles of periodic
variation, which is a short baseline that can be highly susceptible to normal,
stochastic quasar variability (Vaughan et al. 2016). In this Letter, we present
a re-analysis of PG1302, using the latest light curve from the All-Sky
Automated Survey for Supernovae (ASAS-SN), which extends the observational
baseline to the present day (MJD $\approx 58200$), and adopting a maximum
likelihood method which searches for a periodic component in addition to
stochastic quasar variability. When the ASAS-SN data are combined with the
previous LINEAR+CRTS data, the evidence for periodicity decreases. For genuine
periodicity one would expect that additional data would strengthen the
evidence, so the decrease in significance may be an indication that the binary
model is disfavored.
