Multi-Messenger Astrophysics with the Cosmic Neutrino Background. (arXiv:2103.01274v2 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Tully_C/0/1/0/all/0/1">Christopher G. Tully</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_G/0/1/0/all/0/1">Gemma Zhang</a>
The massive neutrinos of the Cosmic Neutrino Background (C$nu$B) are
fundamental ingredients of the radiation-dominated early universe and are
important non-relativistic probes of the large-scale structure formation in the
late universe. The dominant source of anisotropies in the neutrino flux
distribution on the sky are highly amplified integrals of metric perturbations
encountered during the non-relativistic phase of the C$nu$B. This paper
numerically compares the line-of-sight methods for computing C$nu$B
anisotropies with the Einstein-Boltzmann hierarchy solutions in linear theory
for a range of neutrino masses. Angular power spectra are computed that are
relevant to a future polarized tritium target run of the PTOLEMY experiment.
Correlations between the C$nu$B sky maps and galactic survey data are derived
using line-of-sight techniques and discussed in the context of multi-messenger
astrophysics.
The massive neutrinos of the Cosmic Neutrino Background (C$nu$B) are
fundamental ingredients of the radiation-dominated early universe and are
important non-relativistic probes of the large-scale structure formation in the
late universe. The dominant source of anisotropies in the neutrino flux
distribution on the sky are highly amplified integrals of metric perturbations
encountered during the non-relativistic phase of the C$nu$B. This paper
numerically compares the line-of-sight methods for computing C$nu$B
anisotropies with the Einstein-Boltzmann hierarchy solutions in linear theory
for a range of neutrino masses. Angular power spectra are computed that are
relevant to a future polarized tritium target run of the PTOLEMY experiment.
Correlations between the C$nu$B sky maps and galactic survey data are derived
using line-of-sight techniques and discussed in the context of multi-messenger
astrophysics.
http://arxiv.org/icons/sfx.gif
