  In our Ultra-Fast Astronomy (UFA) program, we aim to improve measurements of
variability of astronomical targets on millisecond and shorter time scales. In
this work, we present initial on-sky measurements of the performance of silicon
photomultiplier detectors (SiPMs) for UFA. We mounted two different SiPMs at
the focal plane of the 0.7-meter aperture Nazarbayev University Transient
Telescope at the Assy-Turgen Astrophysical Observatory (NUTTelA-TAO), with no
filter in front of the detector. The $3mm\times3mm$ SiPM single-channel
detectors have a field of view of $2.2716'\times2.2716'$. During the nights of
2019 October 28-29, we measured sky background, bright stars, and an artificial
source with a 100Hz flashing frequency. We compared detected SiPM counts with
Gaia satellite G-band flux values to show that our SiPMs have a linear
response. With our two SiPMs (models S14520-3050VS and S14160-3050HS), we
measured a dark current of $\sim$130 and $\sim$85 kilo counts per second
(kcps), and a sky background of $\sim$201 and $\sim$203 kcps, respectively. We
measured an intrinsic crosstalk of 10.34$\%$ and 10.52$\%$ and derived a
5$\sigma$ sensitivity of 13.9 and 14.0 Gaia G-band magnitude for 200ms
exposures, for the two detectors respectively. For a 10 $\mu$s window, and
allowing a false alarm rate of once per 100 nights, we derived a sensitivity of
22 detected photons, or 6 Gaia G-band magnitudes. For nanosecond timescales,
our detection is limited by crosstalk to 12 detected photons, which corresponds
to a fluence of $\sim$155 photons per square meter.
