H i discs of L[ast] galaxies as probes of the baryonic physics of galaxy evolution

• Verfasst von: Gensior, Jindra [VerfasserIn]
• Verfasst von: Feldmann, Robert [VerfasserIn]
• Verfasst von: Reina-Campos, Marta [VerfasserIn]
• Verfasst von: Trujillo-Gomez, Sebastian [VerfasserIn]
• Verfasst von: Mayer, Lucio [VerfasserIn]
• Verfasst von: Keller, Benjamin W [VerfasserIn]
• Verfasst von: Wetzel, Andrew [VerfasserIn]
• Verfasst von: Kruijssen, J M Diederik [VerfasserIn]
• Verfasst von: Hopkins, Philip F [VerfasserIn]
• Verfasst von: Moreno, Jorge [VerfasserIn]
• Titel: H i discs of L[ast] galaxies as probes of the baryonic physics of galaxy evolution
• Verf.angabe: Jindra Gensior, Robert Feldmann, Marta Reina-Campos, Sebastian Trujillo-Gomez, Lucio Mayer, Benjamin W. Keller, Andrew Wetzel, J.M. Diederik Kruijssen, Philip F. Hopkins and Jorge Moreno
• E-Jahr: 2024
• Jahr: June 2024
• Umfang: 21 S.
• Illustrationen: Illustrationen
• Fussnoten: Im Titel ist [ast] als Tropfensternchen dargestellt ; Veröffentlicht: 11. Mai 2024 ; Gesehen am 29.11.2024
• Titel Quelle: Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
• Ort Quelle: Oxford : Oxford Univ. Press, 1827
• Jahr Quelle: 2024
• Band/Heft Quelle: 531(2024), 1 vom: Juni, Seite 1158-1178
• ISSN Quelle: 1365-2966
• DOI: doi:10.1093/mnras/stae1217
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1909916196

Abstract

Understanding what shapes the cold gas component of galaxies, which both provides the fuel for star formation and is strongly affected by the subsequent stellar feedback, is a crucial step towards a better understanding of galaxy evolution. Here, we analyse the H i properties of a sample of 46 Milky Way halo-mass galaxies, drawn from cosmological simulations (EMP-Pathfinder and Firebox). This set of simulations comprises galaxies evolved self-consistently across cosmic time with different baryonic sub-grid physics: three different star formation models [constant star formation efficiency (SFE) with different star formation eligibility criteria, and an environmentally dependent, turbulence-based SFE] and two different feedback prescriptions, where only one sub-sample includes early stellar feedback. We use these simulations to assess the impact of different baryonic physics on the H i content of galaxies. We find that the galaxy-wide H i properties agree with each other and with observations. However, differences appear for small-scale properties. The thin H i discs observed in the local universe are only reproduced with a turbulence-dependent SFE and/or early stellar feedback. Furthermore, we find that the morphology of H i discs is particularly sensitive to the different physics models: galaxies simulated with a turbulence-based SFE have discs that are smoother and more rotationally symmetric, compared to those simulated with a constant SFE; galaxies simulated with early stellar feedback have more regular discs than supernova-feedback-only galaxies. We find that the rotational asymmetry of the H i discs depends most strongly on the underlying physics model, making this a promising observable for understanding the physics responsible for shaping the interstellar medium of galaxies.