{"about":{"site":"https://codewithpapers.app","non_affiliation":"Code with Papers and Syntology are not affiliated with, endorsed by, or sponsored by Papers with Code, Meta, or the pwc-archive mirror.","licence":"CC BY-SA 4.0","licence_url":"https://creativecommons.org/licenses/by-sa/4.0/legalcode","attribution":"https://codewithpapers.app/attribution","modified":"archive material modified by Syntology; see the attribution page"},"url":"/paper/cozmic-i-cosmological-zoom-in-simulations","title":"COZMIC. I. Cosmological Zoom-in Simulations with Initial Conditions Beyond Cold Dark Matter","arxiv_id":"2410.03635","date":"2024-10-04","proceeding":null,"authors":["Ethan O. Nadler","Rui An","Vera Gluscevic","Andrew Benson","Xiaolong Du"],"abstract":"We present 72 cosmological dark matter-only $N$-body zoom-in simulations with initial conditions beyond cold, collisionless dark matter (CDM), as the first installment of the COZMIC suite. We simulate Milky Way (MW) analogs with linear matter power spectra $P(k)$ for i) thermal-relic warm dark matter (WDM) with masses $m_{\\mathrm{WDM}}\\in [3,4,5,6,6.5,10]~\\mathrm{keV}$, ii) fuzzy dark matter (FDM) with masses $m_{\\mathrm{FDM}}\\in [25.9,69.4,113,151,185,490]\\times 10^{-22}~\\mathrm{eV}$, and iii) interacting dark matter (IDM) with a velocity-dependent elastic proton scattering cross section $\\sigma=\\sigma_0 v^n$ relative particle velocity scaling $n\\in [2,4]$, and dark matter mass $m_{\\mathrm{IDM}}\\in[10^{-4},~ 10^{-2},~ 1]$ GeV. Subhalo mass function (SHMF) suppression is significantly steeper in FDM versus WDM, while dark acoustic oscillations in $P(k)$ can reduce SHMF suppression for IDM. We fit SHMF models to our simulation results and derive new bounds on WDM and FDM from the MW satellite population, obtaining $m_{\\mathrm{WDM}}>5.9~\\mathrm{keV}$ and $m_{\\mathrm{FDM}}>1.4\\times 10^{-20}~\\mathrm{eV}$ at $95\\%$ confidence; these limits are $\\approx 10\\%$ weaker and $5\\times$ stronger than previous constraints owing to the updated transfer functions and SHMF models, respectively. We estimate IDM bounds for $n=2$ ($n=4$) and obtain $\\sigma_0 < 1.0\\times 10^{-27}$, $1.3\\times 10^{-24}$, and $3.1\\times 10^{-23}~\\mathrm{cm}^2$ ($\\sigma_0 < 9.9\\times 10^{-27}$, $9.8\\times 10^{-21}$, and $2.1\\times 10^{-17}~\\mathrm{cm}^2$) for $m_{\\mathrm{IDM}}=10^{-4}$, $10^{-2}$, and $1$ GeV, respectively. Thus, future development of IDM SHMF models can improve IDM cross section bounds by up to a factor of $\\sim 20$ with current data. COZMIC presents an important step toward accurate small-scale structure modeling in beyond-CDM cosmologies, critical to upcoming observational searches for dark matter physics.","url_abs":"https://arxiv.org/abs/2410.03635v3","url_pdf":"https://arxiv.org/pdf/2410.03635v3.pdf","source":{"archive":"pwc-archive (Hugging Face), CC BY-SA 4.0","snapshot":"2025-07-28","licence_url":"https://creativecommons.org/licenses/by-sa/4.0/legalcode","row_kind":"links_only","authors_date_abstract":"arXiv metadata, CC0 1.0 (https://info.arxiv.org/help/license), from the Kaggle arXiv metadata snapshot of 2026-09-12"},"code_links":[{"paper_slug":"cozmic-i-cosmological-zoom-in-simulations","repo_url":"https://github.com/Xiaolong-Du/axionCAMB_patch","is_official":1,"mentioned_in_paper":1,"mentioned_in_github":1,"framework":"none","reach":null}],"tasks":[],"methods":[],"datasets_introduced":[],"methods_introduced":[],"results":[],"syntology":{"atlas_url":null,"mcp":null,"developers":"https://syntology.ai/developers"},"arxiv_metadata":null,"syntology_extracted_results":null}