The role of accreted and in situ populations in shaping the stellar halos of low-mass galaxies

Tau, EA, Monachesi, A, Gomez, FA, Grand, RJJ ORCID: 0000-0001-9667-1340, Pakmor, R, van de Voort, F, Gonzalez-Jara, J, Tissera, PB, Marinacci, F and Bieri, R (2025) The role of accreted and in situ populations in shaping the stellar halos of low-mass galaxies. Astronomy & Astrophysics, 699. ISSN 0004-6361

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Abstract

The stellar halos of low-mass galaxies (M_* ≤ 10^ M_⊙) are becoming objects of interest among the extragalactic community due to a recent set of observations with the capacity to detect such structures. Additionally, new and very-high-resolution cosmological simulations have been performed, enabling the study of this faint component in low-mass galaxies. The presence of stellar halos in low-mass systems could help shed light on our understanding of the assembly of low-mass observed galaxies and their evolution. It could also allow us to test whether the hierarchical model for the formation of structures is applicable at small scales. In this work, we aim to characterise the stellar halos of simulated low-mass galaxies and analyse their evolution and accretion history. We used a sample of $17$ simulated low-mass galaxies from the Auriga Project with a stellar mass range from $3.28 10^8 , M_⊙$ to $2.08 M_⊙$. These are cosmological magneto-hydrodynamical zoom-in simulations that have a very high resolution $5 10^4 , M_⊙$ in dark matter (DM) mass and ∼ 6 10^3 , M_⊙ in baryonic mass. We defined the stellar halo as the stellar material located outside of an ellipsoid with semi-major axes equal to four times the half-light radius of each galaxy. We analysed the stellar halos of these galaxies and studied their formation channels. We find that the inner regions of the stellar halo (between four and six times the half-light radius) are dominated by in situ material. For the less massive simulated dwarfs (M_* ≤ 4.54 10^8 , M_⊙), this dominance extends to all radii. We find that this in situ stellar halo is mostly formed in the inner regions of the galaxies and was subsequently ejected into the outskirts during interactions and merger events with satellite galaxies. In ∼ 50% of the galaxies, the stripped gas from satellite galaxies (likely mixed with the gas from the host dwarf) contributed to the formation of this in situ halo. The stellar halos of the galaxies more massive than M_* ≥ 1 10^9 , M_⊙ are dominated by the accreted component beyond six half-light radii. We find that the more massive dwarf galaxies (M_* ≥ 6.30 10^9 , M_⊙) accrete stellar material until later times ≈ 4.44 Gyr ago, with τ_90 as the formation time) than the less massive ones (τ_ ≈ 8.17 Gyr ago). This has an impact on the formation time of the accreted stellar halos. These galaxies have between one and seven significant progenitors that contribute to the accreted component of these galaxies; however, there is no clear correlation between the amount of accreted mass of the galaxies and their number of significant progenitors.

Item Type:	Article
Uncontrolled Keywords:	5101 Astronomical Sciences; 51 Physical Sciences; 0201 Astronomical and Space Sciences; Astronomy & Astrophysics; 5101 Astronomical sciences; 5107 Particle and high energy physics; 5109 Space sciences
Subjects:	Q Science > QB Astronomy Q Science > QC Physics
Divisions:	Astrophysics Research Institute
Publisher:	EDP Sciences
Date of acceptance:	20 May 2025
Date of first compliant Open Access:	3 July 2025
Date Deposited:	03 Jul 2025 11:37
Last Modified:	03 Jul 2025 11:45
DOI or ID number:	10.1051/0004-6361/202453488
URI:	https://researchonline.ljmu.ac.uk/id/eprint/26702

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