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 Plus annual

Presents the access of premium content as premium feature

Premium Content

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 annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Systematic uncertainties in the mass measurement of galaxy clusters limit thecosmological constraining power of future surveys that will detect more than$10^5$ clusters. Previously, we argued that aperture masses can be inferredmore accurately and precisely than 3D masses without loss of cosmologicalconstraining power. Here, we use the Baryons and Haloes of Massive Systems(BAHAMAS) cosmological, hydrodynamical simulations to show that aperture massesare also less sensitive to changes in mass caused by galaxy formationprocesses. For haloes with $m_\mathrm{200m,dmo} > 10^{14} \, h^{-1} \,\mathrm{M}_\odot$, binned by their 3D halo mass, baryonic physics affectsaperture masses and 3D halo masses similarly when measured within aperturessimilar to the halo virial radius, reaching a maximum reduction of $\approx 3\, \%$. For lower-mass haloes, $10^{13.5} < m_\mathrm{200m,dmo} / (h^{-1} \,\mathrm{M}_\odot) < 10^{14}$, and aperture sizes $\sim 1 \, h^{-1} \,\mathrm{cMpc}$, representative of weak lensing observations, the aperture massis consistently reduced less ($\lesssim 5 \, \%$) than the 3D halo mass($\lesssim 10 \, \%$ for $m_\mathrm{200m}$). The halo mass reduction evolvesonly slightly, by up to $2$ percentage points, between redshift 0.25 and 1 forboth the aperture mass and $m_\mathrm{200m}$. Varying the strength of thesimulated feedback so the mean simulated hot gas fraction covers the observedscatter inferred from X-ray observations, we find that the aperture mass isconsistently less biased than the 3D halo mass, by up to $2 \, $ percentagepoints at $m_\mathrm{200m,dmo} = 10^{14} \, h^{-1} \, \mathrm{M}_\odot$.Therefore, cluster aperture mass calibrations provide a fruitful path forwardfor future cluster surveys to reduce their sensitivity to systematicuncertainties.

Galaxy cluster aperture masses are more robust to baryonic effects than 3D halo masses