Applying a star formation model calibrated on high-resolution interstellar medium simulations to cosmological simulations of galaxy formation
Fuente:
arXiv
Salvato in:
| Autori principali: | , , , , , , , , , , , , , |
|---|---|
| Natura: | Preprint |
| Pubblicazione: |
2025
|
| Soggetti: | |
| Accesso online: | |
| Tags: |
Aggiungi Tag
Nessun Tag, puoi essere il primo ad aggiungerne!!
|
| _version_ | 1866915611265728512 |
|---|---|
| author | Burger, Jan D. Springel, Volker Ostriker, Eve C. Kim, Chang-Goo Jeffreson, Sarah M. R. Smith, Matthew C. Pakmor, Rüdiger Hassan, Sultan Fielding, Drummond Hernquist, Lars Bryan, Greg L. Somerville, Rachel S. Bennett, Jake S. Weinberger, Rainer |
| author_facet | Burger, Jan D. Springel, Volker Ostriker, Eve C. Kim, Chang-Goo Jeffreson, Sarah M. R. Smith, Matthew C. Pakmor, Rüdiger Hassan, Sultan Fielding, Drummond Hernquist, Lars Bryan, Greg L. Somerville, Rachel S. Bennett, Jake S. Weinberger, Rainer |
| contents | Modern high-resolution simulations of the interstellar medium (ISM) have shown that key factors in governing star formation are the competing influences of radiative dissipation, pressure support driven by stellar feedback, and the relentless pull of gravity. Cosmological simulations of galaxy formation, such as IllustrisTNG or ASTRID, are however not able to resolve this physics in detail and therefore need to rely on approximate treatments. These have often taken the form of empirical subgrid models of the ISM expressed in terms of an effective equation of state (EOS) that relates the mean ISM pressure to the mean gas density. Here we seek to improve these heuristic models by directly fitting their key ingredients to results of the high-resolution TIGRESS simulations, which have shown that the dynamical equilibrium of the ISM can be understood in terms of a pressure-regulated, feedback modulated (PRFM) model for star formation. Here we explore a simple subgrid model that draws on the PRFM concept but uses only local quantities. It accurately reproduces PRFM for pure gas disks, while it predicts slightly less star formation than PRFM in the presence of an additional thin stellar disk. We compare the properties of this model with the older Springel and Hernquist and TNG prescriptions, and apply all three to isolated simulations of disk galaxies as well as to a set of high-resolution zoom-in simulations carried out with a novel 'multi-zoom' technique that we introduce in this study. The softer EOS implied by TIGRESS produces substantially thinner disk galaxies, which has important ramifications for disk stability and galaxy morphology. The total stellar mass of galaxies is however hardly modified at low redshift, reflecting the dominating influence of large-scale gaseous inflows and outflows to galaxies, which are not sensitive to the EOS itself |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2502_13244 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Applying a star formation model calibrated on high-resolution interstellar medium simulations to cosmological simulations of galaxy formation Burger, Jan D. Springel, Volker Ostriker, Eve C. Kim, Chang-Goo Jeffreson, Sarah M. R. Smith, Matthew C. Pakmor, Rüdiger Hassan, Sultan Fielding, Drummond Hernquist, Lars Bryan, Greg L. Somerville, Rachel S. Bennett, Jake S. Weinberger, Rainer Astrophysics of Galaxies Modern high-resolution simulations of the interstellar medium (ISM) have shown that key factors in governing star formation are the competing influences of radiative dissipation, pressure support driven by stellar feedback, and the relentless pull of gravity. Cosmological simulations of galaxy formation, such as IllustrisTNG or ASTRID, are however not able to resolve this physics in detail and therefore need to rely on approximate treatments. These have often taken the form of empirical subgrid models of the ISM expressed in terms of an effective equation of state (EOS) that relates the mean ISM pressure to the mean gas density. Here we seek to improve these heuristic models by directly fitting their key ingredients to results of the high-resolution TIGRESS simulations, which have shown that the dynamical equilibrium of the ISM can be understood in terms of a pressure-regulated, feedback modulated (PRFM) model for star formation. Here we explore a simple subgrid model that draws on the PRFM concept but uses only local quantities. It accurately reproduces PRFM for pure gas disks, while it predicts slightly less star formation than PRFM in the presence of an additional thin stellar disk. We compare the properties of this model with the older Springel and Hernquist and TNG prescriptions, and apply all three to isolated simulations of disk galaxies as well as to a set of high-resolution zoom-in simulations carried out with a novel 'multi-zoom' technique that we introduce in this study. The softer EOS implied by TIGRESS produces substantially thinner disk galaxies, which has important ramifications for disk stability and galaxy morphology. The total stellar mass of galaxies is however hardly modified at low redshift, reflecting the dominating influence of large-scale gaseous inflows and outflows to galaxies, which are not sensitive to the EOS itself |
| title | Applying a star formation model calibrated on high-resolution interstellar medium simulations to cosmological simulations of galaxy formation |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2502.13244 |