Columba: isolated dwarf galaxy populations in diverse cosmological environments simulated with a cold interstellar medium

Briggs, JM ORCID: 0009-0003-9791-1782, Fattahi, A ORCID: 0000-0002-6831-5215, Crain, RA ORCID: 0000-0001-6258-0344, Bahe, YM ORCID: 0000-0002-3196-5126, Ploeckinger, S ORCID: 0000-0002-1965-1650, Schaller, M ORCID: 0000-0002-2395-4902, Benítez-Llambay, A ORCID: 0000-0001-8261-2796, Chaikin, E ORCID: 0000-0003-2047-3684, Richings, AJ ORCID: 0000-0003-0502-9235 and Schaye, J ORCID: 0000-0002-0668-5560 (2026) Columba: isolated dwarf galaxy populations in diverse cosmological environments simulated with a cold interstellar medium. Monthly Notices of the Royal Astronomical Society, 550 (2). ISSN 0035-8711

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Abstract

We introduce a suite of Lambda cold dark matter ((Formula presented) CDM) cosmological, hydrodynamical simulations that track the evolution of a large population of dwarf galaxies. The suite comprises zoom-in simulations of 25 spherical, underdense regions of (Formula presented), selected to span (Formula presented) dex in mean enclosed density, covering voids to filamentary structures, whilst excluding haloes of Milky Way-mass or larger. The simulations achieve a mass resolution of (Formula presented) with a galaxy formation model including cold, dense interstellar gas and whose subgrid stellar feedback efficiency reproduces the (Formula presented) galaxy stellar mass function. We investigate the impact of the cosmic environment on dwarf galaxy formation and evolution. We find that the (Formula presented) environment influences the normalization of the halo and galaxy mass functions, but does not significantly affect the stellar mass–halo mass (SMHM) relation and halo occupation fraction for galaxies with (Formula presented). Instead, host halo concentration, estimated from DM-only counterparts, is more important: both the fraction of haloes hosting a resolved galaxy and the scatter about the SMHM relation correlate positively with concentration. Owing to halo assembly bias, concentration also influences galaxy formation times, such that at fixed halo mass more concentrated haloes host galaxies that are both older and more massive. The offset from the mean SMHM relation also anticorrelates with (Formula presented), the time at which 90 per cent of a galaxy’s stellar mass has assembled. These correlations between halo properties and galaxy star formation histories present testable predictions for forthcoming observational surveys.

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:	Oxford University Press
Date of acceptance:	18 June 2026
Date of first compliant Open Access:	22 July 2026
Date Deposited:	22 Jul 2026 13:17
Last Modified:	22 Jul 2026 13:17
DOI or ID number:	10.1093/mnras/stag1228
URI:	https://researchonline.ljmu.ac.uk/id/eprint/29041

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