Trading kinetic energy: How late kinetic decoupling of dark matter changes $N_{textrm{eff}}$. (arXiv:1811.05601v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Diacoumis_J/0/1/0/all/0/1">James A. D. Diacoumis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wong_Y/0/1/0/all/0/1">Yvonne Y. Y. Wong</a>
Elastic scattering between dark matter particles and a relativistic species
such as photons or neutrinos leads to a transfer of energy from the latter due
to their intrinsically different temperature scaling relations. In this work,
we point out that this siphoning of energy from the radiation bath manifests as
a change in the effective number of neutrinos $N_{rm eff}$, and compute the
expected shift $Delta N_{rm eff}$ for dark matter-photon and dark
matter-neutrino elastic scattering as a function of the dark matter mass
$m_psi$ and scattering cross section $sigma_{psi-X}$. For
$(m_psi,sigma_{psi-X})$-parameter regions already explored by nonlinear
probes such as the Lyman-$alpha$ forest through collisional and/or
free-streaming damping, we find shifts of $|Delta N_{rm eff}| simeq
O(10^{-2})$, which may be within the reach of the proposed CMB-S4 experiment.
For most of the as-yet-unexplored parameter space, however, we expect $|Delta
N_{rm eff}| lesssim O(10^{-3})$. An ideal 21 cm tomography survey of the dark
ages limited only by cosmic variance is potentially sensitive to $|Delta
N_{rm eff}| simeq O(10^{-6})$, in which case dark matter masses up to
$m_{psi} sim 10 , textrm{MeV}$ may be probed via their effect on $N_{rm
eff}$.
Elastic scattering between dark matter particles and a relativistic species
such as photons or neutrinos leads to a transfer of energy from the latter due
to their intrinsically different temperature scaling relations. In this work,
we point out that this siphoning of energy from the radiation bath manifests as
a change in the effective number of neutrinos $N_{rm eff}$, and compute the
expected shift $Delta N_{rm eff}$ for dark matter-photon and dark
matter-neutrino elastic scattering as a function of the dark matter mass
$m_psi$ and scattering cross section $sigma_{psi-X}$. For
$(m_psi,sigma_{psi-X})$-parameter regions already explored by nonlinear
probes such as the Lyman-$alpha$ forest through collisional and/or
free-streaming damping, we find shifts of $|Delta N_{rm eff}| simeq
O(10^{-2})$, which may be within the reach of the proposed CMB-S4 experiment.
For most of the as-yet-unexplored parameter space, however, we expect $|Delta
N_{rm eff}| lesssim O(10^{-3})$. An ideal 21 cm tomography survey of the dark
ages limited only by cosmic variance is potentially sensitive to $|Delta
N_{rm eff}| simeq O(10^{-6})$, in which case dark matter masses up to
$m_{psi} sim 10 , textrm{MeV}$ may be probed via their effect on $N_{rm
eff}$.
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