Estimating infall times of galaxies around clusters: how accurately can it be done with observational data?

TL;DR

This study assesses the accuracy of current observational methods for estimating galaxy infall times into clusters, finding fundamental limitations due to orbital overlap and suggesting potential improvements with relaxed cluster samples and dual estimates.

Contribution

The paper systematically compares four infall time estimation methods using simulations and identifies the intrinsic dispersion caused by orbital overlap as a fundamental limit.

Findings

All methods have limited accuracy (~2.6 Gyr) due to intrinsic dispersion.

Relaxed clusters show smaller infall time dispersion.

Using two estimates can reduce dispersion to below 1.5 Gyr.

Abstract

Context. The environment plays a crucial role in galaxy evolution, particularly for galaxies infalling into clusters. Accurately estimating the infall times of galaxies from observations can significantly enhance our understanding of the environmental effects on galaxy evolution. Aims. This paper aims to evaluate existing methods for estimating infall times via the $R-V$ diagram, explore possible strategies to improve accuracy in estimating infall times, and discuss fundamental limitations. Methods. We utilize a TNG300-1 simulation and construct the $R-V$ diagram that is directly comparable to the observations. Using the same dataset, we systematically compare four commonly used methods, including the projected radii, caustic profiles, and two discrete methods. A simple linear partition is also considered as a reference. Results. Each method exhibits distinct characteristics. While the linear partition slightly outperforms other methods, all methods suffer from limited accuracy ($\gtrsim 2.6$ Gyr), constrained by the intrinsic dispersion ($2.53$ Gyr) of infall times in the $R-V$ diagram. Given this limit, we explore two potential approaches that can improve accuracy: (1) the infall time dispersion is smaller in more dynamically relaxed clusters, and (2) employing two estimates of infall times instead of one reduces the dispersion to $\lesssim1.5$ Gyr. We further demonstrate that the intrinsic dispersion primarily arises from orbital overlap: galaxies in different orbital phases overlap with each other in the $R-V$ diagram and thus appear indistinguishable. Conclusions. Orbital overlap fundamentally limits the accuracy of infall time estimation. The linear partition approach could be a simple and robust estimation.