A measurement of the secondary-CMB and millimeter-wave-foreground
  bispectrum using 800 square degrees of South Pole Telescope data
  We present a measurement of the angular bispectrum of the millimeter-wave sky
in observing bands centered at roughly 95, 150, and 220 GHz, on angular scales
of $1^\prime \lesssim \theta \lesssim 10^\prime$ (multipole number $1000
\lesssim l \lesssim 10000$). At these frequencies and angular scales, the main
contributions to the bispectrum are expected to be the thermal
Sunyaev-Zel'dovich (tSZ) effect and emission from extragalactic sources,
predominantly dusty, star-forming galaxies (DSFGs) and active galactic nuclei.
We measure the bispectrum in 800 $\mathrm{deg}^2$ of three-band South Pole
Telescope data, and we use a multi-frequency fitting procedure to separate the
bispectrum of the tSZ effect from the extragalactic source contribution. We
simultaneously detect the bispectrum of the tSZ effect at $>$10$\sigma$, the
unclustered component of the extragalactic source bispectrum at $>$5$\sigma$ in
each frequency band, and the bispectrum due to the clustering of DSFGs---i.e.,
the clustered cosmic infrared background (CIB) bispectrum---at $>$5$\sigma$.
This is the first reported detection of the clustered CIB bispectrum. We use
the measured tSZ bispectrum amplitude, compared to model predictions, to
constrain the normalization of the matter power spectrum to be $\sigma_8 =
0.787 \pm 0.031$ and to predict the amplitude of the tSZ power spectrum at $l =
3000$. This prediction improves our ability to separate the thermal and
kinematic contributions to the total SZ power spectrum. The addition of
bispectrum data improves our constraint on the tSZ power spectrum amplitude by
a factor of two compared to power spectrum measurements alone and demonstrates
a preference for a nonzero kinematic SZ (kSZ) power spectrum, with a derived
constraint on the kSZ amplitude at $l=3000$ of A_kSZ $ = 2.9 \pm 1.6 \
\mu$K$^2$, or A_kSZ $ = 2.6 \pm 1.8 \ \mu$K$^2$ if the default A_kSZ > 0 prior
is removed.
