  Hydrogen atmosphere pulsating white dwarfs, also known as DAV stars, are the
most abundant type of pulsating white dwarfs. High-temperature DAV stars
exhibit in general a small number of pulsation modes and stable frequencies.
G132-12 is one of the pulsating hydrogen atmosphere white dwarf stars which
lies close to the blue edge of the instability strip. Previous researches
reported that G132-12 might have only one pulsation mode with the period of
212.69 s. To study the pulsation properties of G132-12 in detail, we carried
out a bi-site observation campaign in October 2019. Time series photometric
data were collected during around 154 hours in total. A Fourier Analysis
reveals 3 frequencies which are identified as the triplet of a $l = 1$ g-mode
pulsation with the period of 212.499 s. The rotational period is derived as
$P_{rot} = 35.0\pm6.7$ hours and the inclination of the rotational axis to the
line of sight is $70^{\circ}$. G132-12 could be an ideal target for measuring
the cooling scale of this white dwarf star with only one excited pulsation mode
detected.
