[{"data":1,"prerenderedAt":-1},["ShallowReactive",2],{"detail-sidebar-cat-0-en-105":3,"doc-seo-149054-105":59,"doc-detail-149054-en":130},{"code":4,"msg":5,"data":6},0,"success",[7,13,18,23,28,33,38,43,48,51,55],{"id":8,"doc_module":4,"doc_module_name":9,"category_name":10,"show_sort_weight":11,"slug":12},1,"Document","Story & Novel",90,"story-novel",{"id":14,"doc_module":4,"doc_module_name":9,"category_name":15,"show_sort_weight":16,"slug":17},2,"Literature",80,"literature",{"id":19,"doc_module":4,"doc_module_name":9,"category_name":20,"show_sort_weight":21,"slug":22},4,"Exam",70,"exam",{"id":24,"doc_module":4,"doc_module_name":9,"category_name":25,"show_sort_weight":26,"slug":27},5,"Comic",60,"comic",{"id":29,"doc_module":4,"doc_module_name":9,"category_name":30,"show_sort_weight":31,"slug":32},6,"Technology",50,"technology",{"id":34,"doc_module":4,"doc_module_name":9,"category_name":35,"show_sort_weight":36,"slug":37},7,"Healthcare",40,"healthcare",{"id":39,"doc_module":4,"doc_module_name":9,"category_name":40,"show_sort_weight":41,"slug":42},8,"Research & Report",30,"research-report",{"id":44,"doc_module":4,"doc_module_name":9,"category_name":45,"show_sort_weight":46,"slug":47},9,"Religion & Spirituality",20,"religion-spirituality",{"id":46,"doc_module":4,"doc_module_name":9,"category_name":49,"show_sort_weight":46,"slug":50},"World Cup","world-cup",{"id":52,"doc_module":4,"doc_module_name":9,"category_name":53,"show_sort_weight":52,"slug":54},10,"Lifestyle","lifestyle",{"id":56,"doc_module":4,"doc_module_name":9,"category_name":57,"show_sort_weight":24,"slug":58},19,"General","general",{"code":4,"msg":60,"data":61},"ok",{"site_id":62,"language":63,"slug":64,"title":65,"keywords":66,"description":67,"schema_data":68,"social_meta":123,"head_meta":125,"extra_data":127,"updated_unix":129},105,"en","cosmic-quenching-and-scaling-laws-for-evolution-of-galaxies-and-smbhs-read-online-free","Cosmic Quenching and Scaling Laws for Evolution of Galaxies and SMBHs - read online free","","Observations indicate a strong coupling between supermassive black hole growth and star formation in host galaxies. Using Illustris simulations together with astronomical observations, the study proposes cosmic quenching as a regulating process over cosmic time to synchronize the evolution of both SMBHs and their hosts. A key quantity, the parameter α, governs gas mass/energy inflow along the bulge radial direction, controlling cooling efficiency and cold-gas supply. Its decline with cosmic time yields faster early co-evolution and progressively quenched growth at later epochs.",{"@graph":69,"@context":122},[70,84,105],{"@type":71,"itemListElement":72},"BreadcrumbList",[73,77,79,82],{"item":74,"name":75,"@type":76,"position":8},"https://docshare.wps.com","Home","ListItem",{"item":78,"name":9,"@type":76,"position":14},"https://docshare.wps.com/document/",{"item":80,"name":40,"@type":76,"position":81},"https://docshare.wps.com/document/research-report/",3,{"item":83,"name":65,"@type":76,"position":19},"https://docshare.wps.com/document/cosmic-quenching-and-scaling-laws-for-evolution-of-galaxies-and-smbhs-read-online-free/149054/",{"url":83,"name":65,"@type":85,"image":86,"author":91,"headline":65,"publisher":94,"fileFormat":97,"inLanguage":63,"description":67,"dateModified":98,"datePublished":99,"encodingFormat":97,"isAccessibleForFree":100,"interactionStatistic":101},"DigitalDocument",{"url":87,"@type":88,"width":89,"height":90},"https://docshare.wps.com/thumbnails/cosmic-quenching-and-scaling-laws-for-evolution-of-galaxies-and-smbhs-read-online-free/149054.png","ImageObject",300,407,{"name":92,"@type":93},"Felix Montgomery","Person",{"url":74,"name":95,"@type":96},"DocShare","Organization","application/pdf","2026-10-17","2026-08-27",true,{"@type":102,"interactionType":103,"userInteractionCount":44},"InteractionCounter",{"@type":104},"ViewAction",{"@type":106,"mainEntity":107},"FAQPage",[108,114,118],{"name":109,"@type":110,"acceptedAnswer":111},"What relationship does the paper propose between SMBH growth and star formation?","Question",{"text":112,"@type":113},"The paper proposes a tight coupling regulated by a cosmic quenching process, synchronizing the evolution of SMBHs and their host galaxies over cosmic time.","Answer",{"name":115,"@type":110,"acceptedAnswer":116},"What is the role of the cosmic quenching parameter α?",{"text":117,"@type":113},"α characterizes the rate of mass and energy flow of gas along the bulge radial direction and determines gas cooling efficiency and cold-gas supply.",{"name":119,"@type":110,"acceptedAnswer":120},"How does cosmic time evolution of α affect galaxy and SMBH growth?",{"text":121,"@type":113},"A larger α at early times enables more efficient gas cooling and faster initial co-evolution, while a smaller α at lower redshifts reduces cold-gas supply, slowing star formation and black hole growth (quenching).","https://schema.org",{"og:url":83,"og:type":124,"og:title":65,"og:site_name":95,"og:description":67},"article",{"robots":126,"canonical":83},"index,follow",{"doc_id":128,"site_id":62},149054,1787790831,{"code":4,"msg":5,"data":131},{"doc_id":128,"user_id":132,"nickname":92,"user_avatar":133,"doc_module":4,"category_id":39,"category_name":40,"doc_title":65,"doc_description":67,"doc_content":134,"file_id":135,"file_url":136,"file_type":137,"file_size":138,"view_count":44,"is_deleted":4,"is_public":8,"is_downloadable":8,"audit_status":8,"page_count":41,"language":139,"language_code":63,"site_id":62,"html_lang":63,"table_of_contents":140,"faqs":141,"seo_title":142,"seo_description":67,"update_tm":129,"read_time":143,"preview_page_count":4},549768064778,"https://ap-avatar.wpscdn.com/davatar_6f874abed73319feea01a86fa6f0fab8","Paci¦c Northwest National Laboratory  \nEvolution, Galaxy, Quenching  March 11th, 2024  \n [https://doi.org/10.21203/rs.3.rs-4039565/v1](https://doi.org/10.21203/rs.3.rs-4039565/v1)  \n 􀁱 􀅏 This work is licensed under a Creative Commons Attribution 4.0 International License.  \nRead Full License  \n No competing interests reported.  \nCosmic quenching and scaling laws for evolution of galaxies and SMBHs  \nZhijie (Jay) Xu, 1 ★  \n1 Physical and Computational Sciences Directorate, Paci􀀜c Northwest National Laboratory; Richland, WA 99354, USA  \nAccepted XXX. Received YYY; in original form ZZZ  \nABSTRACT  \nObservations suggest a tight coupling between spuermassive black hole (SMBH) growth and star formation in the host galaxy. Based on Illustris simulations and astronomical observations, a cosmic quenching over the cosmic time scale is proposed to regulate the synchronized evolution of both SMBH and host. A central quantity of cosmic quenching is the parameter 􀁙 􀀱 (unit:􀀼 2/􀁂3 ) that describes the rate of mass and energy ŕow of gases along the bulge radial direction. The parameter 􀁙 􀀱 also controls the efficiency of gas cooling and the supply of cold gas. The value 􀁙 􀀱 ≈ 10−4(1 + 􀁉)5/2􀀼 2 /􀁂3 can be determined which decreases with time. For a larger 􀁙 􀀱 in the early universe, gas cooling is more efficient in providing a richer supply of cold gas for a rapid initial evolution of both SMBH and host. At lower redshifts, a smaller 􀁙 􀀱 means less efficient gas cooling, less cold gas supply, and slower star formation and black hole growth (quenched) . The rate of mass accretion naturally exhibits a peak at 􀁉 ≈ 2 due to the decrease in 􀁙 􀀱 . Scaling laws involving 􀁙 􀀱 are identiőed that govern the evolution of both SMBHs and their hosts. For host galaxies, we identify the mass-size relation 􀀢􀀱 ∝ 􀁙2􀀱/3􀁁5􀀱/3􀀜 −1 and the dispersion-size relation 􀁦2􀀱 ∝ (􀁙 􀀱􀁁 􀀱)2/3 ∝ (1 + 􀁉) , where 􀁁 􀀱 ∝ (1 + 􀁉)−1 is the bulge size. For SMBH, an initial rapid growth is identiőed with a sharp increase in luminosity 􀀡 􀀗 ∝ (􀁙 􀀱􀀢􀀗􀀝)4/5􀀜 −1/5􀀲, followed by a transition stage with a decreasing luminosity 􀀡 􀀗 ∝ 􀁙2􀀱􀀢􀀗􀀝 ∝ (1 + 􀁉)5 , and a dormant stage with 􀀡 􀀗 ∝ (􀁙 􀀱􀀢􀀗􀀝)4/3􀀜 1/3􀀲 −5/3 . Here 􀀜 is the gravitational constant, 􀀲 is the speed of light, 􀀢􀀗􀀝 is the mass of BH. For SMBH-galaxy co-evolution, the observed M-σ correlation can be analytically derived as 􀀢􀀗􀀝 ∝ 􀁦5􀀱/(􀁙 􀀱􀀜). Using these scaling laws, analytical solutions are formulated for the evolution of the SMBH mass function Φ 􀀗􀀝(􀀢, 􀁉), the AGN mass function Φ 􀀖􀀜 􀀣 (􀀢, 􀁉), duty cycle 􀀪(􀀢, 􀁉), and the Eddington ratio distribution. The model predicts Φ 􀀡 ∝ 􀀡 −1/5 for the faint-end quasar luminosity function, Φ 􀀖􀀜 􀀣 ∝ 􀀢 −1/5 for a small-mass-end AGN mass function, and 􀀪 ∝ 􀀢 −1/5 for the duty cycle at high redshift. Finally, the complete redshift evolution of some observed high-redshift SMBHs can be modeled. The results suggest an initial super-Eddington growth in a short period when the SMBHs are still small, followed by a slow growth due to cosmic quenching when the SMBHs become large.  \nKey words: Evolution; Galaxy; Quenching;  \n1 INTRODUCTION  \nSupermassive black holes (SMBHs) are ubiquitously associated with the center of massive galaxies that contain bulges [1] . Numerous observations suggest that SMBHs and their host galaxies are \"coevolving\". The őrst evidence can be the strong and tight correlations between SMBHs and host galaxies. Early black hole demography reveals the correlation between the BH mass 􀀢􀀗􀀝 and the bulge luminosity 􀀡 􀀱 [2, 3, 4, 5] . Since bulge luminosity 􀀡 􀀱 is related to bulge mass 􀀢􀀱 and velocity dispersion 􀁦􀀱 [6, 7], the 􀀢􀀗􀀝-􀀡 􀀱 correlation strongly hints direct correlation between 􀀢􀀗􀀝 and 􀀢􀀱 or 􀁦􀀱. The mass of the bulge 􀀢􀀱 can be directly related to the velocity dispersion 􀁦􀀱 of the bulge by the virial theorem (that is, 􀀢􀀱 ∝ 􀁁 􀀱􀁦2􀀱 , where 􀁁 􀀱 is the size of the bulge) or by dynamical modeling. The correlation between SMBH and bulge mass is generally consistent with a linear relation 􀀢􀀗􀀝 ∝ 􀀢","cbCaibsfx7eUXc94","https://ap.wps.com/l/cbCaibsfx7eUXc94","pdf",7360064,"English","# Abstract\n# Introduction\n## SMBH–galaxy co-evolution observations\n## Proposed mechanisms for tight correlations","[{\"question\":\"What relationship does the paper propose between SMBH growth and star formation?\",\"answer\":\"The paper proposes a tight coupling regulated by a cosmic quenching process, synchronizing the evolution of SMBHs and their host galaxies over cosmic time.\"},{\"question\":\"What is the role of the cosmic quenching parameter α?\",\"answer\":\"α characterizes the rate of mass and energy flow of gas along the bulge radial direction and determines gas cooling efficiency and cold-gas supply.\"},{\"question\":\"How does cosmic time evolution of α affect galaxy and SMBH growth?\",\"answer\":\"A larger α at early times enables more efficient gas cooling and faster initial co-evolution, while a smaller α at lower redshifts reduces cold-gas supply, slowing star formation and black hole growth (quenching).\"}]","Cosmic Quenching and Scaling Laws for Evolution of Galaxies and SMBHs - read online free | PDF",76]