{"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/measuring-the-x-ray-luminosities-of-desi","title":"Measuring the X-ray luminosities of DESI groups from eROSITA Final Equatorial-Depth Survey: I. X-ray luminosity -- halo mass scaling relation","arxiv_id":"2306.02594","date":"2023-06-05","proceeding":null,"authors":["Yunliang Zheng","Xiaohu Yang","Min He","Shi-Yin Shen","Qingyang Li","Xuejie Li"],"abstract":"We use the eROSITA Final Equatorial-Depth Survey (eFEDS) to measure the rest-frame 0.1-2.4 keV band X-ray luminosities of $\\sim$ 600,000 DESI groups using two different algorithms in the overlap region of the two observations. These groups span a large redshift range of $0.0 \\le z_g \\le 1.0$ and group mass range of $10^{10.76}h^{-1}M_{\\odot} \\le M_h \\le 10^{15.0}h^{-1}M_{\\odot}$. (1) Using the blind detection pipeline of eFEDS, we find that 10932 X-ray emission peaks can be cross matched with our groups, $\\sim 38 \\%$ of which have signal-to-noise ratio $\\rm{S}/\\rm{N} \\geq 3$ in X-ray detection. Comparing to the numbers reported in previous studies, this matched sample size is a factor of $\\sim 6$ larger. (2) By stacking X-ray maps around groups with similar masses and redshifts, we measure the average X-ray luminosity of groups as a function of halo mass in five redshift bins. We find, in a wide halo mass range, the X-ray luminosity, $L_{\\rm X}$, is roughly linearly proportional to $M_{h}$, and is quite independent to the redshift of the groups. (3) We use a Poisson distribution to model the X-ray luminosities obtained using two different algorithms and obtain best-fit $L_{\\rm X}=10^{28.46\\pm0.03}M_{h}^{1.024\\pm0.002}$ and $L_{\\rm X}=10^{26.73 \\pm 0.04}M_{h}^{1.140 \\pm 0.003}$ scaling relations, respectively. The best-fit slopes are flatter than the results previously obtained, but closer to a self-similar prediction.","url_abs":"https://arxiv.org/abs/2306.02594v2","url_pdf":"https://arxiv.org/pdf/2306.02594v2.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":"measuring-the-x-ray-luminosities-of-desi","repo_url":"https://github.com/al-yl/xlumsfordesigroups","is_official":1,"mentioned_in_paper":1,"mentioned_in_github":1,"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}