{"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/the-galaxy-clustering-crisis-in-abundance","title":"The Galaxy Clustering Crisis in Abundance Matching","arxiv_id":"1705.06347","date":"2017-05-17","proceeding":null,"authors":["Duncan Campbell","Frank C. van den Bosch","Nikhil Padmanabhan","Yao-Yuan Mao","Andrew R. Zentner","Johannes U. Lange","Fangzhou Jiang","Antonia Villarreal"],"abstract":"Galaxy clustering on small scales is significantly under-predicted by sub-halo abundance matching (SHAM) models that populate (sub-)haloes with galaxies based on peak halo mass, $M_{\\rm peak}$. SHAM models based on the peak maximum circular velocity, $V_{\\rm peak}$, have had much better success. The primary reason $M_{\\rm peak}$ based models fail is the relatively low abundance of satellite galaxies produced in these models compared to those based on $V_{\\rm peak}$. Despite success in predicting clustering, a simple $V_{\\rm peak}$ based SHAM model results in predictions for galaxy growth that are at odds with observations. We evaluate three possible remedies that could \"save\" mass-based SHAM: (1) SHAM models require a significant population of \"orphan\" galaxies as a result of artificial disruption/merging of sub-haloes in modern high resolution dark matter simulations; (2) satellites must grow significantly after their accretion; and (3) stellar mass is significantly affected by halo assembly history. No solution is entirely satisfactory. However, regardless of the particulars, we show that popular SHAM models based on $M_{\\rm peak}$ cannot be complete physical models as presented. Either $V_{\\rm peak}$ truly is a better predictor of stellar mass at $z\\sim 0$ and it remains to be seen how the correlation between stellar mass and $V_{\\rm peak}$ comes about, or SHAM models are missing vital component(s) that significantly affect galaxy clustering.","url_abs":"http://arxiv.org/abs/1705.06347v1","url_pdf":"http://arxiv.org/pdf/1705.06347v1.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":"the-galaxy-clustering-crisis-in-abundance","repo_url":"https://github.com/duncandc/Clustering_Crisis","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}