# White dwarfs in the building blocks of the Galactic spheroid

## TL;DR

This study explores how the properties of galactic building blocks influence the halo white dwarf population and luminosity functions, revealing subtle differences linked to age and metallicity, but also highlighting observational challenges.

## Contribution

It introduces a detailed modeling approach combining binary population synthesis with galaxy formation simulations to analyze halo white dwarf populations from different building blocks.

## Key findings

- WDs from younger and/or metal-rich building blocks can be distinguished from others.
- Halo WD luminosity functions are very similar across different building blocks.
- IMF choice affects the fit to observed luminosity functions, with Kroupa or Salpeter performing slightly better.

## Abstract

The galactic halo likely grew over time in part by assembling smaller galaxies, the so-called building blocks. We investigate if the properties of these building blocks are reflected in the halo white dwarf (WD) population in the Solar neighborhood. Furthermore, we compute the halo WD luminosity functions (WDLFs) for four major building blocks of five cosmologically motivated stellar haloes. We couple the SeBa binary population synthesis model to the Munich-Groningen semi-analytic galaxy formation model, applied to the high-resolution Aquarius dark matter simulations. Although the semi-analytic model assumes an instantaneous recycling approximation, we model the evolution of zero-age main sequence stars to WDs, taking age and metallicity variations of the population into account. Although the majority of halo stars is old and metal-poor and therefore the WDs in the different building blocks have similar properties (including present-day luminosity), we find in our models that the WDs originating from building blocks that have young and/or metal-rich stars can be distinguished from WDs that were born in other building blocks. In practice however, it will be hard to prove that these WDs really originate from different building blocks, as the variations in the halo WD population due to binary WD mergers result in similar effects. The five joined stellar halo WD populations that we modelled result in WDLFs that are very similar to each other. We find that simple models with a Kroupa or Salpeter initial mass function (IMF) fit the observed luminosity function slightly better, since the Chabrier IMF is more top-heavy, although this result is dependent on our choice of the stellar halo mass density in the Solar neighborhood.