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The hierarchical model of galaxy evolution suggests that the impact of mergers is substantial on the intricate processes that drive stellar assembly within a galaxy. Here, we present theory-motivated predictions for the fraction of stellar mass originating from mergers in a statistically significant sample of nearby galaxies, using data from MaNGA. Notably, the ex-situ stellar mass in the nearby universe exhibits significant dependence on galaxy characteristics, with higher accreted fractions favored by elliptical, quenched galaxies and slow rotators, as well as galaxies at the center of more massive dark matter halos.
This hierarchical process of evolution not only orchestrates the creation of larger structures but also carries crucial consequences in shaping the physical characteristics of galaxies. Mergers are known to trigger structural transformations [ 2 ] , rejuvenate star formation [ 3 ] , and fuel the activity of Active Galactic Nuclei AGN [ 4 ] , as well as contribute to the buildup of massive early-type galaxies ETGs [ 5 ]. A primary challenge lies in detecting merging events in observational data.
Traditionally, this has been accomplished through the identification of pairs of galaxies, sufficiently close both spatially and dynamically, under the assumption that they will merge over a relatively short timescale [ 7 , 8 ]. Alternatively, direct evidence of galaxy interactions, such as tidal tails and structural asymmetries, has been utilized to develop non-parametric methods for the calculation of merger rates across various redshifts [ 9 , 10 ]. However, both approaches require high quality observational data and carry distinct biases, such as resolution-sensitive thresholds or misidentification of galaxy flybys as merging systems, which may not capture the entire spectrum of merger appearances.
An alternative to direct merger detection is to quantify the integrated effect of mergers in a galaxy, following a more challenging archaeological approach. Focusing on our cosmic neighborhood, there exist a number of works on deriving the ex-situ stellar mass for a small sample of nearby galaxies through N-body simulations that account for stellar halo buildup only through accretion of dwarf satellite galaxies [ 11 , 12 ]. Moving further away is an observational challenge, as sufficiently high-quality data is required for unveiling distinctions between the in-situ and the ex-situ stellar populations.