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

We extend the local stellar galaxy-(sub)halo connection to the atomichydrogen (HI) component by seeding semi-empirically galaxies into a largeN-body dark matter (DM) simulation. The main input to construct the mock galaxycatalogue are: our constrained stellar mass-to-(sub)halo circular velocity($M_{\ast}$-$V_{\rm DM}$) relation, assuming a scatter independent of anygalaxy property, and the empirical $M_{\rm HI}$ conditional probabilitydistributions given $M_{\ast}$ for central and satellite galaxies. We find thatthe $\langle\log M_{\rm HI}\rangle-\log M_{\rm DM}$ relation is not a monotonicincreasing function. It increases with mass up to $M_{\rm DM}\sim 10^{12}$$M_{\odot}$, attaining a maximum of $\langle\log(M_{\rm HI}/M_{\odot})\rangle\sim 9.2$, and at higher (sub)halo masses, $\langle\log(M_{\rm HI})\rangle$decreases slightly with $M_{\rm DM}$. The scatter around it is also large andmass dependent. The bivariate $M_{\rm HI}$ and $M_{\rm DM}$ distribution isbroad and bimodal, specially at $M_{\rm DM}\gtrsim 10^{12}$ $M_\odot$, which isinherited from the input $M_{\rm HI}$ conditional distributions. We also reportthe total (central+satellites) HI gas mass within halos, $\langle M^{\rmtot}_{\rm HI}(M_{\rm DM})\rangle$, as a function of $M_{\rm DM}$. The mean$M^{\rm tot}_{\rm HI}-M_{\rm DM}$ relation is an increasing monotonic function.The galaxy spatial clustering increases weakly as the $M_{\rm HI}$ thresholdincreases. Our HI mock galaxies cluster more in comparison to the blind HIALFALFA (Arecibo Fast Legacy ALFA) survey but we show that it is mainly due tothe selection effects. We discuss the implications of our results in the lightof predictions from semi-analytical models and hydrodynamics simulations ofgalaxy evolution.

The galaxy HI-(sub)halo connection and the HI spatial clustering of local galaxies