Unveiling dark matter free streaming at the smallest scales with the high redshift Lyman-alpha forest

Abstract

This study introduces novel constraints on the free streaming of thermal relic warm dark matter (WDM) from Lyman-<a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:mi>α</a:mi></a:math> forest flux power spectra. Our analysis utilizes a high resolution, high redshift sample of quasar spectra observed using the HIRES and UVES spectrographs (<c:math xmlns:c="http://www.w3.org/1998/Math/MathML" display="inline"><c:mrow><c:mi>z</c:mi><c:mo>=</c:mo><c:mn>4.2</c:mn><c:mi>–</c:mi><c:mn>5.0</c:mn></c:mrow></c:math>). We employ a Bayesian inference framework and a simulation-based likelihood that encompasses various parameters including the free streaming of dark matter, cosmological parameters, the thermal history of the intergalactic medium, and inhomogeneous reionization to establish lower limits on the mass of a thermal relic WDM particle of 5.7 keV (at 95% CL). This result surpasses previous limits from the Lyman-<e:math xmlns:e="http://www.w3.org/1998/Math/MathML" display="inline"><e:mi>α</e:mi></e:math> forest through reduction of the measured uncertainties due to a larger statistical sample and by measuring clustering to smaller scales (<g:math xmlns:g="http://www.w3.org/1998/Math/MathML" display="inline"><g:mrow><g:msub><g:mrow><g:mi>k</g:mi></g:mrow><g:mrow><g:mi>max</g:mi></g:mrow></g:msub><g:mo>=</g:mo><g:mn>0.2</g:mn><g:mtext> </g:mtext><g:mtext> </g:mtext><g:mrow><g:msup><g:mrow><g:mi>km</g:mi></g:mrow><g:mrow><g:mo>−</g:mo><g:mn>1</g:mn></g:mrow></g:msup><g:mtext> </g:mtext><g:mi mathvariant="normal">s</g:mi></g:mrow></g:mrow></g:math>). The approximately two-fold improvement due to the expanded statistical sample suggests that the effectiveness of Lyman-<j:math xmlns:j="http://www.w3.org/1998/Math/MathML" display="inline"><j:mi>α</j:mi></j:math> forest constraints on WDM models at high redshifts are limited by the availability of high quality quasar spectra. Restricting the analysis to comparable scales and thermal history priors as in prior studies (<l:math xmlns:l="http://www.w3.org/1998/Math/MathML" display="inline"><l:mrow><l:msub><l:mrow><l:mi>k</l:mi></l:mrow><l:mrow><l:mi>max</l:mi></l:mrow></l:msub><l:mo>&lt;</l:mo><l:mn>0.1</l:mn><l:mtext> </l:mtext><l:mtext> </l:mtext><l:mrow><l:msup><l:mrow><l:mi>km</l:mi></l:mrow><l:mrow><l:mo>−</l:mo><l:mn>1</l:mn></l:mrow></l:msup><l:mtext> </l:mtext><l:mi mathvariant="normal">s</l:mi></l:mrow></l:mrow></l:math>) lowers the bound on the WDM mass to 4.1 keV. As the precision of the measurements increases, it becomes crucial to examine the instrumental and modeling systematics. On the modeling front, we argue that the impact of the thermal history uncertainty on the WDM particle mass constraint has diminished due to improved independent observations. At the smallest scales, the primary source of modeling systematic arises from the structure in the peculiar velocity of the intergalactic medium and inhomogeneous reionization. Published by the American Physical Society 2024

Topics & Concepts