English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Tools annual

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

Intensity mapping experiments are beginning to measure the spatialdistribution of neutral atomic hydrogen (HI) to constrain cosmologicalparameters and the large-scale distribution of matter. However, models of thebehaviour of HI as a tracer of matter is complicated by galaxy evolution. Inthis work, we examine the clustering of HI in relation to galaxy colour,stellar mass, and HI mass in IllustrisTNG at $z$ = 0, 0.5, and 1. We comparethe HI-red and HI-blue galaxy cross-power spectra, finding that HI-red has anamplitude 1.5 times higher than HI-blue at large scales. The cross-powerspectra intersect at $\approx 3$ Mpc in real space and $\approx 10$ Mpc inredshift space, consistent with $z \approx 0$ observations. We show that HIclustering increases with galaxy HI mass and depends weakly on detection limitsin the range $M_{\mathrm{HI}} \leq 10^8 M_\odot$. We also find that bluegalaxies in the greatest stellar mass bin cluster more than blue galaxies inother stellar mass bins. Red galaxies in the greatest stellar mass bin,however, cluster the weakest amongst red galaxies. These trends arise due tocentral-satellite compositions. Centrals correlate less with HI for increasingstellar mass, whereas satellites correlate more, irrespective of colour.Despite the clustering relationships with stellar mass, we find that thecross-power spectra are largely insensitive to detection limits in HI andgalaxy surveys. Counter-intuitively, all auto and cross-power spectra for redand blue galaxies and HI decrease with time at all scales in IllustrisTNG. Wedemonstrate that processes associated with quenching contribute to this trend.The complex interplay between HI and galaxies underscores the importance ofunderstanding baryonic effects when interpreting the large-scale clustering ofHI, blue, and red galaxies at $z \leq 1$.

Atomic Hydrogen Shows its True Colours: Correlations between HI and Galaxy Colour in Simulations