Kavli Affiliate: Debora Sijacki
| First 5 Authors: Yuxuan Yuan, Sergio Martin-Alvarez, Martin G. Haehnelt, Thibault Garel, Debora Sijacki
| Summary:
Ly$alpha$ emission is an exceptionally informative tracer of the life cycle
of evolving galaxies and the escape of ionising photons. However, theoretical
studies of Ly$alpha$ emission are often limited by insufficient numerical
resolution, incomplete sets of physical models, and poor line-of-sight (LOS)
statistics. To overcome such limitations, we utilize here the novel PANDORA
suite of high-resolution dwarf galaxy simulations that include a comprehensive
set of state-of-the-art physical models for ionizing radiation, magnetic
fields, supernova feedback and cosmic rays. We post-process the simulations
with the radiative transfer code textsc{RASCAS} to generate synthetic
observations and compare to observed properties of Ly$alpha$ emitters. Our
simulated Ly$alpha$ haloes are more extended than the spatial region from
which the intrinsic emission emanates and our spatially resolved maps of
spectral parameters of the Ly$alpha$ emission are very sensitive to the
underlying spatial distribution and kinematics of neutral hydrogen. Ly$alpha$
and LyC emission display strongly varying signatures along different LOS
depending on how each LOS intersects low-density channels generated by stellar
feedback. Comparing galaxies simulated with different physics, we find the
Ly$alpha$ signatures to exhibit systematic offsets determined by the different
levels of feedback strength and the clumpiness of the neutral gas. Despite this
variance, and regardless of the different physics included in each model, we
find universal correlations between Ly$alpha$ observables and LyC escape
fraction, demonstrating a robust connection between Ly$alpha$ and LyC
emission. Ly$alpha$ observations from a large sample of dwarf galaxies should
thus give strong constraints on their stellar feedback-regulated LyC escape and
confirm their important role for the reionization of the Universe.
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