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Title: Why are we still using 3D masses for cluster cosmology?

Abstract

The abundance of clusters of galaxies is highly sensitive to the late-time evolution of the matter distribution, since clusters form at the highest density peaks. However, the 3D cluster mass cannot be inferred without deprojecting the observations, introducing model-dependent biases and uncertainties due to the mismatch between the assumed and the true cluster density profile and the neglected matter along the sightline. Since projected aperture masses can be measured directly in simulations and observationally through weak lensing, we argue that they are better suited for cluster cosmology. Using the Mira–Titan suite of gravity-only simulations, we show that aperture masses correlate strongly with 3D halo masses, albeit with large intrinsic scatter due to the varying matter distribution along the sightline. Nonetheless, aperture masses can be measured ≈2–3 times more precisely from observations, since they do not require assumptions about the density profile and are only affected by the shape noise in the weak lensing measurements. We emulate the cosmology dependence of the aperture mass function directly with a Gaussian process. Comparing the cosmology sensitivity of the aperture mass function and the 3D halo mass function for a fixed survey solid angle and redshift interval, we find the aperture mass sensitivity is higher for $$Ω_{\text{m}}$$ and $$w_a$$, similar for $$σ_8$$, $$n_{\text{s}}$$, and $$w_0$$, and slightly lower for $$\textit{h}$$. With a carefully calibrated aperture mass function emulator, cluster cosmology analyses can use cluster aperture masses directly, reducing the sensitivity to model-dependent mass calibration biases and uncertainties.

Authors:
ORCiD logo; ORCiD logo; ORCiD logo; ;
Publication Date:
Research Org.:
Argonne National Laboratory (ANL), Argonne, IL (United States). Argonne Leadership Computing Facility (ALCF); Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States). Oak Ridge Leadership Computing Facility (OLCF)
Sponsoring Org.:
Dutch Research Council (NWO); USDOE Office of Science (SC), High Energy Physics (HEP); USDOE Office of Science (SC), Basic Energy Sciences (BES). Scientific User Facilities Division
OSTI Identifier:
1880138
Alternate Identifier(s):
OSTI ID: 1967902
Grant/Contract Number:  
AC02-06CH11357; AC05-00OR22725; 639.043.409; 639.043.512
Resource Type:
Published Article
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Name: Monthly Notices of the Royal Astronomical Society Journal Volume: 515 Journal Issue: 3; Journal ID: ISSN 0035-8711
Publisher:
Oxford University Press
Country of Publication:
United Kingdom
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; clusters: general; cosmological parameters; cosmology; gravitational lensing; large-scale structure of Universe; observations; theory; weak, galaxies

Citation Formats

Debackere, Stijn N. B., Hoekstra, Henk, Schaye, Joop, Heitmann, Katrin, and Habib, Salman. Why are we still using 3D masses for cluster cosmology?. United Kingdom: N. p., 2022. Web. doi:10.1093/mnras/stac1687.
Debackere, Stijn N. B., Hoekstra, Henk, Schaye, Joop, Heitmann, Katrin, & Habib, Salman. Why are we still using 3D masses for cluster cosmology?. United Kingdom. https://doi.org/10.1093/mnras/stac1687
Debackere, Stijn N. B., Hoekstra, Henk, Schaye, Joop, Heitmann, Katrin, and Habib, Salman. Fri . "Why are we still using 3D masses for cluster cosmology?". United Kingdom. https://doi.org/10.1093/mnras/stac1687.
@article{osti_1880138,
title = {Why are we still using 3D masses for cluster cosmology?},
author = {Debackere, Stijn N. B. and Hoekstra, Henk and Schaye, Joop and Heitmann, Katrin and Habib, Salman},
abstractNote = {The abundance of clusters of galaxies is highly sensitive to the late-time evolution of the matter distribution, since clusters form at the highest density peaks. However, the 3D cluster mass cannot be inferred without deprojecting the observations, introducing model-dependent biases and uncertainties due to the mismatch between the assumed and the true cluster density profile and the neglected matter along the sightline. Since projected aperture masses can be measured directly in simulations and observationally through weak lensing, we argue that they are better suited for cluster cosmology. Using the Mira–Titan suite of gravity-only simulations, we show that aperture masses correlate strongly with 3D halo masses, albeit with large intrinsic scatter due to the varying matter distribution along the sightline. Nonetheless, aperture masses can be measured ≈2–3 times more precisely from observations, since they do not require assumptions about the density profile and are only affected by the shape noise in the weak lensing measurements. We emulate the cosmology dependence of the aperture mass function directly with a Gaussian process. Comparing the cosmology sensitivity of the aperture mass function and the 3D halo mass function for a fixed survey solid angle and redshift interval, we find the aperture mass sensitivity is higher for $Ω_{\text{m}}$ and $w_a$, similar for $σ_8$, $n_{\text{s}}$, and $w_0$, and slightly lower for $\textit{h}$. With a carefully calibrated aperture mass function emulator, cluster cosmology analyses can use cluster aperture masses directly, reducing the sensitivity to model-dependent mass calibration biases and uncertainties.},
doi = {10.1093/mnras/stac1687},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 3,
volume = 515,
place = {United Kingdom},
year = {Fri Jun 17 00:00:00 EDT 2022},
month = {Fri Jun 17 00:00:00 EDT 2022}
}

Journal Article:
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https://doi.org/10.1093/mnras/stac1687

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