{"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-magpi-survey-the-kinematic-morphology","title":"The MAGPI Survey: the kinematic morphology-density relation (or lack thereof) and the Hubble sequence at $z\\sim0.3$","arxiv_id":"2502.16751","date":"2025-02-23","proceeding":null,"authors":["Caroline Foster","Mark W. Donoghoe","Andrew Battisti","Francesco D'Eugenio","Katherine Harborne","Thomas Venville","Claudia Del P. Lagos","J. Trevor Mendel","Ryan Bagge","Stefania Barsanti","Sabine Bellstedt","Alina Boecker","Qianhui Chen","Caro Derkenne","Anna Ferre-Matteu","Eda Gjergo","Anshu Gupta","Eric G. M. Muller","Giulia Santucci","Hye-Jin Park","Rhea-Silvia Remus","Sabine Thater","Jesse van de Sande","Sam Vaughan","Sarah Brough","Scott M. Croom","Lucas M. Valenzuela","Emily Wisnioski","the MAGPI Team"],"abstract":"This work presents visual morphological and dynamical classifications for 637 spatially resolved galaxies, most of which are at intermediate redshift ($z\\sim0.3$), in the Middle-Ages Galaxy Properties with Integral field spectroscopy (MAGPI) Survey. For each galaxy, we obtain a minimum of 11 independent visual classifications by knowledgeable classifiers. We use an extension of the standard Dawid-Skene bayesian model introducing classifier-specific confidence parameters and galaxy-specific difficulty parameters to quantify classifier confidence and infer reliable statistical confidence estimates. Selecting sub-samples of 86 bright ($r<20$ mag) high-confidence ($>0.98$) morphological classifications at redshifts ($0.2 \\le z \\le0.4$), we confirm the full range of morphological types is represented in MAGPI as intended in the survey design. Similarly, with a sub-sample of 82 bright high-confidence stellar kinematic classifications, we find that the rotating and non-rotating galaxies seen at low redshift are already in place at intermediate redshifts. We \\textit{do not} find evidence that the kinematic morphology-density relation seen at $z\\sim0$ is established at $z\\sim0.3$. We suggest that galaxies without obvious stellar rotation are dynamically pre-processed sometime before $z\\sim0.3$ within lower mass groups before joining denser environments.","url_abs":"https://arxiv.org/abs/2502.16751v1","url_pdf":"https://arxiv.org/pdf/2502.16751v1.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-magpi-survey-the-kinematic-morphology","repo_url":"https://github.com/MagpiSurvey/MAGPIClassApp_public","is_official":1,"mentioned_in_paper":0,"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}