Cosmological baryon spread and impact on matter clustering in CAMELS. Gebhardt, M., Anglés-Alcázar, D., Borrow, J., Genel, S., Villaescusa-Navarro, F., Ni, Y., Lovell, C. C., Nagai, D., Davé, R., Marinacci, F., Vogelsberger, M., & Hernquist, L. Monthly Notices of the Royal Astronomical Society, 529:4896–4913, April, 2024. Publisher: OUP ADS Bibcode: 2024MNRAS.529.4896G![Cosmological baryon spread and impact on matter clustering in CAMELS [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper doi abstract bibtex We quantify the cosmological spread of baryons relative to their initial neighbouring dark matter distribution using thousands of state-of-the-art simulations from the Cosmology and Astrophysics with MachinE Learning Simulations (CAMELS) project. We show that dark matter particles spread relative to their initial neighbouring distribution owing to chaotic gravitational dynamics on spatial scales comparable to their host dark matter halo. In contrast, gas in hydrodynamic simulations spreads much further from the initial neighbouring dark matter owing to feedback from supernovae (SNe) and active galactic nuclei (AGN). We show that large-scale baryon spread is very sensitive to model implementation details, with the fiducial SIMBA model spreading ~40 per cent of baryons \textgreater1 Mpc away compared to ~10 per cent for the IllustrisTNG and ASTRID models. Increasing the efficiency of AGN-driven outflows greatly increases baryon spread while increasing the strength of SNe-driven winds can decrease spreading due to non-linear coupling of stellar and AGN feedback. We compare total matter power spectra between hydrodynamic and paired N-body simulations and demonstrate that the baryonic spread metric broadly captures the global impact of feedback on matter clustering over variations of cosmological and astrophysical parameters, initial conditions, and (to a lesser extent) galaxy formation models. Using symbolic regression, we find a function that reproduces the suppression of power by feedback as a function of wave number (k) and baryonic spread up to $k {\}sim 10{\}, h$ Mpc-1 in SIMBA while highlighting the challenge of developing models robust to variations in galaxy formation physics implementation.
@article{gebhardt_cosmological_2024,
title = {Cosmological baryon spread and impact on matter clustering in {CAMELS}},
volume = {529},
issn = {0035-8711},
url = {https://ui.adsabs.harvard.edu/abs/2024MNRAS.529.4896G},
doi = {10.1093/mnras/stae817},
abstract = {We quantify the cosmological spread of baryons relative to their initial neighbouring dark matter distribution using thousands of state-of-the-art simulations from the Cosmology and Astrophysics with MachinE Learning Simulations (CAMELS) project. We show that dark matter particles spread relative to their initial neighbouring distribution owing to chaotic gravitational dynamics on spatial scales comparable to their host dark matter halo. In contrast, gas in hydrodynamic simulations spreads much further from the initial neighbouring dark matter owing to feedback from supernovae (SNe) and active galactic nuclei (AGN). We show that large-scale baryon spread is very sensitive to model implementation details, with the fiducial SIMBA model spreading {\textasciitilde}40 per cent of baryons {\textgreater}1 Mpc away compared to {\textasciitilde}10 per cent for the IllustrisTNG and ASTRID models. Increasing the efficiency of AGN-driven outflows greatly increases baryon spread while increasing the strength of SNe-driven winds can decrease spreading due to non-linear coupling of stellar and AGN feedback. We compare total matter power spectra between hydrodynamic and paired N-body simulations and demonstrate that the baryonic spread metric broadly captures the global impact of feedback on matter clustering over variations of cosmological and astrophysical parameters, initial conditions, and (to a lesser extent) galaxy formation models. Using symbolic regression, we find a function that reproduces the suppression of power by feedback as a function of wave number (k) and baryonic spread up to \$k {\textbackslash}sim 10{\textbackslash}, h\$ Mpc-1 in SIMBA while highlighting the challenge of developing models robust to variations in galaxy formation physics implementation.},
urldate = {2024-08-21},
journal = {Monthly Notices of the Royal Astronomical Society},
author = {Gebhardt, Matthew and Anglés-Alcázar, Daniel and Borrow, Josh and Genel, Shy and Villaescusa-Navarro, Francisco and Ni, Yueying and Lovell, Christopher C. and Nagai, Daisuke and Davé, Romeel and Marinacci, Federico and Vogelsberger, Mark and Hernquist, Lars},
month = apr,
year = {2024},
note = {Publisher: OUP
ADS Bibcode: 2024MNRAS.529.4896G},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmology: large-scale structure of Universe, galaxies: evolution, galaxies: formation},
pages = {4896--4913},
}
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We show that dark matter particles spread relative to their initial neighbouring distribution owing to chaotic gravitational dynamics on spatial scales comparable to their host dark matter halo. In contrast, gas in hydrodynamic simulations spreads much further from the initial neighbouring dark matter owing to feedback from supernovae (SNe) and active galactic nuclei (AGN). We show that large-scale baryon spread is very sensitive to model implementation details, with the fiducial SIMBA model spreading ~40 per cent of baryons \\textgreater1 Mpc away compared to ~10 per cent for the IllustrisTNG and ASTRID models. Increasing the efficiency of AGN-driven outflows greatly increases baryon spread while increasing the strength of SNe-driven winds can decrease spreading due to non-linear coupling of stellar and AGN feedback. We compare total matter power spectra between hydrodynamic and paired N-body simulations and demonstrate that the baryonic spread metric broadly captures the global impact of feedback on matter clustering over variations of cosmological and astrophysical parameters, initial conditions, and (to a lesser extent) galaxy formation models. Using symbolic regression, we find a function that reproduces the suppression of power by feedback as a function of wave number (k) and baryonic spread up to $k {\\}sim 10{\\}, h$ Mpc-1 in SIMBA while highlighting the challenge of developing models robust to variations in galaxy formation physics implementation.","urldate":"2024-08-21","journal":"Monthly Notices of the Royal Astronomical Society","author":[{"propositions":[],"lastnames":["Gebhardt"],"firstnames":["Matthew"],"suffixes":[]},{"propositions":[],"lastnames":["Anglés-Alcázar"],"firstnames":["Daniel"],"suffixes":[]},{"propositions":[],"lastnames":["Borrow"],"firstnames":["Josh"],"suffixes":[]},{"propositions":[],"lastnames":["Genel"],"firstnames":["Shy"],"suffixes":[]},{"propositions":[],"lastnames":["Villaescusa-Navarro"],"firstnames":["Francisco"],"suffixes":[]},{"propositions":[],"lastnames":["Ni"],"firstnames":["Yueying"],"suffixes":[]},{"propositions":[],"lastnames":["Lovell"],"firstnames":["Christopher","C."],"suffixes":[]},{"propositions":[],"lastnames":["Nagai"],"firstnames":["Daisuke"],"suffixes":[]},{"propositions":[],"lastnames":["Davé"],"firstnames":["Romeel"],"suffixes":[]},{"propositions":[],"lastnames":["Marinacci"],"firstnames":["Federico"],"suffixes":[]},{"propositions":[],"lastnames":["Vogelsberger"],"firstnames":["Mark"],"suffixes":[]},{"propositions":[],"lastnames":["Hernquist"],"firstnames":["Lars"],"suffixes":[]}],"month":"April","year":"2024","note":"Publisher: OUP ADS Bibcode: 2024MNRAS.529.4896G","keywords":"Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmology: large-scale structure of Universe, galaxies: evolution, galaxies: formation","pages":"4896–4913","bibtex":"@article{gebhardt_cosmological_2024,\n\ttitle = {Cosmological baryon spread and impact on matter clustering in {CAMELS}},\n\tvolume = {529},\n\tissn = {0035-8711},\n\turl = {https://ui.adsabs.harvard.edu/abs/2024MNRAS.529.4896G},\n\tdoi = {10.1093/mnras/stae817},\n\tabstract = {We quantify the cosmological spread of baryons relative to their initial neighbouring dark matter distribution using thousands of state-of-the-art simulations from the Cosmology and Astrophysics with MachinE Learning Simulations (CAMELS) project. 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