Measuring Mass of Gas in Central Galaxies using weak lensing and satellite kinematics in MOND

TL;DR

This study uses weak lensing and satellite kinematics in MOND to measure hot gas halos around central galaxies, confirming the distribution of baryonic matter and the reliability of these methods in galaxy mass estimation.

Contribution

It demonstrates the consistency of weak lensing and satellite kinematics in MOND for measuring baryonic mass and gas distribution in central galaxies, including hot gas halos.

Findings

Hot gas halos follow Plummer's profile across mass bins.

Good agreement between weak lensing and satellite kinematics methods.

Simple models suffice to match observations without complex anisotropy profiles.

Abstract

In Milgrom's modified Newtonian dynamics (MOND) framework, the dynamical mass of a galaxy is fully determined by its baryonic matter distribution. We fit the distribution of cold and hot gas halos, focusing on hot gas, around SDSS central galaxies using weak lensing signals from the DECaLS survey in MOND. The central galaxies are classified into two samples, the total galaxies and star-forming galaxies. We find that hot gas halo densities nearly follow Plummer's profile for both samples across all mass bins. The rotation curves of the galaxy samples are also demonstrated. The efficiency of converting gas into stars, $M_*/(M_* + M_{\rm g})$, is between 0.3 and 0.8 in all mass bins of the star-forming sample, which is higher than in the total sample. We also calculate gas mass using the satellite kinematics method in MOND. A constant, mildly radial anisotropy or isotropy in satellite motion leads to good agreement between the satellite kinematics and weak lensing methods. Combining both methods, we observe a baryonic mass to line-of-sight velocity dispersion of satellites ($M_{\rm b}$-$\sigma_{\rm s}$) relation. In addition, we examine more sophisticated models in MOND, including external field effects and Osipkov-Merritt anisotropy profiles, and find them unnecessary. A simple, mildly radial constant anisotropic model or an isotropic model, even when isolated, already aligns with observations. The strong concordance between the two methods suggests that weak lensing signals reliably measure the dynamical mass of central galaxies and can constrain the distribution of missing baryons in galaxy clusters.