The kinematic Sunyaev-Zel'dovich effect of the large-scale structure
  (I): dependence on neutrino mass
  The study of neutrinos in astrophysics requires the combination of different
observational probes. The temperature anisotropies of the cosmic microwave
background induced via the kinematic Sunyaev-Zel'dovich (kSZ) effect may
provide interesting information since they are expected to receive significant
contribution from high-redshift plasma. We present a set of cosmological
hydrodynamical simulations that include a treatment of the neutrino component
considering four different sum of neutrino masses: $\Sigma
m_\nu=(0,0.15,0.3,0.6)$ eV. Using their outputs, we modelled the kSZ effect due
to the large-scale structure after the reionization by producing mock maps,
then computed the kSZ power spectrum and studied how it depends on $z_{\rm re}$
and $\Sigma m_\nu$. We also run a set of four simulations to study and correct
possible systematics due to resolution, finite box size and astrophysics. With
massless neutrinos we obtain $\mathcal{D}^{\rm kSZ}_{3000}=4.0$ $\mu {\rm K}^2$
($z_{\rm re}$=8.8), enough to account for all of the kSZ signal of
$\mathcal{D}^{\rm kSZ}_{3000}=(2.9\pm1.3)$ $\mu {\rm K}^2$ measured with the
South Pole Telescope. This translates into an upper limit on the kSZ effect due
to patchy reionization of $\mathcal{D}^{\rm kSZ,patchy}_{3000}<1.0$ $\mu {\rm
K}^2$ (95 per cent confidence level). Massive neutrinos induce a damping of kSZ
effect power of about 8, 12 and 40 per cent for $\Sigma m_\nu=(0.15,0.3,0.6)$
eV, respectively. We study the dependence of the kSZ signal with $z_{\rm re}$
and the neutrino mass fraction, $f_\nu$, and obtain $\mathcal{D}^{\rm
kSZ}_{3000}\propto z_{\rm re}^{0.26}(1-f_\nu)^{14.3}$. Interestingly, the
scaling with $f_\nu$ is significantly shallower with respect to the equivalent
thermal SZ effect, and may be used to break the degeneracy with other
cosmological parameters.
