{"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/mass-assembly-and-morphological","title":"Mass assembly and morphological transformations since $z\\sim3$ from CANDELS","arxiv_id":"1606.04952","date":"2016-06-15","proceeding":null,"authors":["M. Huertas-Company","M. Bernardi","P. G. Pérez-González","M. L. N. Ashby","G. Barro","C. Conselice","E. Daddi","A. Dekel","P. Dimauro","S. M. Faber","N. A. Grogin","J. S. Kartaltepe","D. D. Kocevski","A. M. Koekemoer","D. C. Koo","S. Mei","F. Shankar"],"abstract":"[abridged] We quantify the evolution of the stellar mass functions of star-forming and quiescent galaxies as a function of morphology from $z\\sim 3$ to the present. Our sample consists of ~50,000 galaxies in the CANDELS fields ($\\sim880$ $arcmin^2$), which we divide into four main morphological types, i.e. pure bulge dominated systems, pure spiral disk dominated, intermediate 2-component bulge+disk systems and irregular disturbed galaxies. Our main results are: Star-formation: At $z\\sim 2$, 80\\% of the stellar mass density of star-forming galaxies is in irregular systems. However, by $z\\sim 0.5$, irregular objects only dominate at stellar masses below $10^9M\\odot$. A majority of the star-forming irregulars present at $z\\sim 2$ undergo a gradual transformation from disturbed to normal spiral disk morphologies by $z\\sim 1$ without significant interruption to their star-formation. Rejuvenation after a quenching event does not seem to be common except perhaps for the most massive objects. Quenching: We confirm that galaxies reaching a stellar mass of $M_*\\sim10^{10.8}M_\\odot$ ($M^*$) tend to quench. Also, quenching implies the presence of a bulge: the abundance of massive red disks is negligible at all redshifts over 2~dex in stellar mass. However the dominant quenching mechanism evolves. At $z>2$, the SMF of quiescent galaxies above $M^*$ is dominated by compact spheroids. Quenching at this early epoch destroys the disk and produces a compact remnant unless the star-forming progenitors at even higher redshifts are significantly more dense. At $1<z<2$, the majority of newly quenched galaxies are disks with a significant central bulge. This suggests that mass-quenching at this epoch starts from the inner parts and preserves the disk. At $z<1$, the high mass end of the passive SMF is globally in place and the evolution mostly happens at stellar masses below $10^{10}M_\\odot$.","url_abs":"http://arxiv.org/abs/1606.04952v1","url_pdf":"http://arxiv.org/pdf/1606.04952v1.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":"mass-assembly-and-morphological","repo_url":"https://github.com/MegaMorph/galapagos","is_official":0,"mentioned_in_paper":0,"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}