Introduction

Lyman-$\alpha$ spectra can provide insights into the small-scale structure and kinematics of neutral hydrogen (HI) within galaxies as well as the ionization state of the intergalactic medium (IGM). The former defines the intrinsic spectrum of a galaxy, which is modified by the latter. These two effects are degenerate: While at low redshifts, double peaked Lyman-$\alpha$ spectra are the norm, we find more and more spectra only showing a red peak at high redshifts. Does this reflect imprints of larger outflow velocities on the galaxy scale or is this rather just an attenuation effect of increasing neutral hydrogen density of the IGM voiding flux bluewards of the Lyman-$\alpha$ line-center? Are there certain spectral features imprinted by the IGM break this degeneracy?

Approach

We investigate the IGM impact on Ly$\alpha$ spectral shapes using the IllustrisTNG100 simulations between redshifts $0$ to $5$, where we integrate the Ly$\alpha$ optical depth

$\tau(\lambda_{\mathrm{i}}) = \int_{s_0}^\infty \mathrm{d}s \, n_\mathrm{HI}(s) \, \sigma\left(\lambda(\lambda_{\mathrm{i}},v,s),T_{\mathrm{HI}} \right)$

for a range of input wavelengths $\lambda_i$ starting at some $s_0$ outside of the galaxy, typically $1.5$ times the virial radius of the host halo.

Calculating the optical depth this way for a large set of lines of sight, and halos as potential sites of Lyman-$\alpha$ emitting galaxies, gives us a catalogue of transmission curves for our further analysis.

Public Data Release

We make a reasonably sized subset of our transmission curves available here. See below for a simple example how to load and use this data set in python.