{"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/redshift-evolution-of-galaxy-group-x-ray","title":"Redshift Evolution of Galaxy Group X-ray Properties in Simba","arxiv_id":"2107.01206","date":"2021-07-02","proceeding":null,"authors":["Dylan Robson","Romeel Davé"],"abstract":"We examine the evolution of intragroup gas X-ray scaling relations for group-sized halos ($M_{500}=10^{12.3-15}M_{\\odot}$) in the Simba galaxy formation simulation. X-ray luminosity $L_X$ vs $M_{500}$ shows increasing deviation from self-similarity from $z=3\\to 0$, with $M_{500}<10^{13.5} M_{\\odot}$ halos exhibiting a large reduction in $L_X$ and slight increase in X-ray luminosity-weighted temperature $T_X$. These shifts are driven by a strong drop in $f_{\\rm gas}$ with time for these halos, and coincides with the onset of black hole jet feedback in these systems at $z\\sim 1.5$ in Simba. The connection with black hole feedback is corroborated by $f_{BH}\\equiv M_{BH}/M_{500}$ in $M_{500}<10^{13.5} M_{\\odot}$ halos being strongly anti-correlated with $L_X$ and $f_{\\rm gas}$ at $z\\la 1.5$. This is further reflected in the scatter of $L_X-T_X$: halos with small $f_{BH}$ lie near self-similarity, while those with the highest $f_{BH}$ lie furthest below. Turning off jet feedback results in mostly self-similar behaviour down to $z=0$. For the X-ray weighted metallicity $Z_X$, stellar feedback impacts the enrichment of halo gas. Finally, halo profiles show that jet feedback flattens the electron density and entropy profiles, and introduces a core in X-ray surface brightness particularly at $M_{500}<10^{13.5} M_{\\odot}$. This argues that intragroup X-ray evolution is largely driven by jet feedback removing hot gas from the cores of massive groups, and expelling gas altogether in less massive groups.","url_abs":"https://arxiv.org/abs/2107.01206v1","url_pdf":"https://arxiv.org/pdf/2107.01206v1.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":"redshift-evolution-of-galaxy-group-x-ray","repo_url":"https://bitbucket.org/broett/pygad","is_official":1,"mentioned_in_paper":1,"mentioned_in_github":0,"framework":"none","reach":null}],"tasks":[],"methods":[],"datasets_introduced":[],"methods_introduced":[],"results":[],"syntology":{"syntology_url":null,"atlas_url":null,"mcp":null,"developers":"https://syntology.ai/developers"},"arxiv_metadata":null,"syntology_extracted_results":null}