[{"data":1,"prerenderedAt":-1},["ShallowReactive",2],{"detail-sidebar-cat-0-en-105":3,"doc-seo-142806-105":59,"doc-detail-142806-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","exploring-the-star-formation-histories-of-galaxies-in-different-environments-from-manga-spectra-proceedings","Exploring the Star Formation Histories of Galaxies in Different Environments from MaNGA Spectra - Proceedings","","The star formation history (SFH) of galaxies reveals when they formed their stars and assembled their mass. Using resolved stellar populations, SFH can be constrained with high precision because spectra distinguish stars of different ages. MaNGA will deliver resolved spectroscopy for nearly 10,000 nearby galaxies and aims to trace the lifecycle from birth and assembly through growth, merging, and late-time quenching. This collaboration program examines SFH across environments, including isolated systems and a galaxy merger.",{"@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/exploring-the-star-formation-histories-of-galaxies-in-different-environments-from-manga-spectra-proceedings/142806/",{"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/exploring-the-star-formation-histories-of-galaxies-in-different-environments-from-manga-spectra-proceedings/142806.png","ImageObject",300,407,{"name":92,"@type":93},"\tJames","Person",{"url":74,"name":95,"@type":96},"DocShare","Organization","application/pdf","2026-10-06","2026-08-25",true,{"@type":102,"interactionType":103,"userInteractionCount":34},"InteractionCounter",{"@type":104},"ViewAction",{"@type":106,"mainEntity":107},"FAQPage",[108,114,118],{"name":109,"@type":110,"acceptedAnswer":111},"Why are star formation histories (SFH) important for understanding galaxies?","Question",{"text":112,"@type":113},"SFH indicates when galaxies formed their stars and accumulated their mass, encoding past and current physical processes that drive evolution across cosmic time.","Answer",{"name":115,"@type":110,"acceptedAnswer":116},"What enables high-precision constraints on SFH in resolved stellar populations?",{"text":117,"@type":113},"Resolved spectroscopy allows discrimination of stellar ages from the spectrum each age produces, enabling precise reconstruction of SFH.",{"name":119,"@type":110,"acceptedAnswer":120},"How do the collaboration results apply to different environments?",{"text":121,"@type":113},"The program uses MaNGA data to constrain SFH in nearby galaxies across environments, demonstrating the methodology for isolated galaxies and for a galaxy merger.","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},142806,1787688484,{"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":34,"is_deleted":4,"is_public":8,"is_downloadable":8,"audit_status":8,"page_count":81,"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":39},2336474466412,"https://ap-avatar.wpscdn.com/davatar_155a257f0dc6eb9ab79c44ca47cae57d","M.Argudo-Fernández¹,2,M.Boquien²,F.Yuan³,S.Shen³,J.Yin³&R.Chang³  \n1 Centro de Astrononia,Universidad de Antofagasta,Chile  \n²Chinese Academy of Sciences,South America Center for Astronomy,China-Chile Joint Center for Astronomy,Santiago,Chile3 Shanghai Astronomical Observatory,Chinese Acadeny of Scierces,Shanghai,Chira  \nContact /maria.argudo@uantof.cl  \nAbstract/The star formation history(SFH)of galaxies allow us to investigate when galaxies formed their starsand assembled their mass.We can constrain the SFH with high level of precision from galaxies with resolvedstellar populations,since we are able to discriminate between stars of different ages from the spectrum they emit.MaNGA(Mapping Nearby Galaxies at APO)willprovide resolved spectroscopy for nearly 10000 galaxies in thelocal Universe.MaNGA's key goals are to understand the “life cycle”of present day galaxies from imprinted cluesof their birth and assembly through their ongoing growth via star formation and merging,to their death fromquenching at late times.However,the relative importance of secular evolution(nature)over nurture is not yetclear,and separating the effects of interaction-driven evolution in the observed galaxy properties is not trivial.Wepresent here the current state of a China-Chile collaboration program where we use MaNGA data to constrainthe SFH of nearby galaxies in different environments to investigate how they form and evolve.In particular,weshow the results of our methodology applied to a sample of isolated galaxies and a galaxy merger.  \nKeywords/galaxies:general—galaxies:formation—galaxies:evolution  \n# 1.Introduction\n\nThe electromagnetic emission of galaxies is our mainwindow into their formation and their evolution.Youngstellar populations dominate the UV-optical energybudget of galaxies.As they evolve and die they pro-duce dust and inject vast amounts of metals in the in-terstellar medium,which have a direct impact on theformation of new stars,shielding and cooling molecu-lar clouds,but also reddening and dimming the UV-to-near-infrared spectrum.In case of intense feedbackfrom young,massive stars,star formation can even bequenched altogether,affecting the shape and appear-ance of galaxies.At the same time,galaxy can be redand dim simply because they are not forming stars any-  \nExploring the star formation histories of galaxies in differentenvironments from MaNGA spectra  \nResumen/La historia de formación estelar(SFH)de las galaxias nos permite investigar cuándo las galaxiasformaron sus estrellas y ensamblaron su masa.Podemos restringir la SFH con un alto nivel de precisión de lasgalaxias con poblaciones estelares resueltas,ya que somos capaces de discriminar entre las estrellas de diferen-tes edades del espectro que emiten.MaNGA(Mapping Nearby Galaries at APO)proporcionará espectroscopíaresuelta para casi 10000 galaxias en el universo local.Los principales objetivos de MaNGA son comprender el\"ciclo de vida\"de las galaxias actuales a partir de pistas impresas de su nacimiento y ensamblaje a través de sucrecimiento continuo y de la formación y fusión de galaxias,hasta su muerte por extinción en los últimos tiempos.En este programa de investigación pretendemos utilizar datos MaNGA para restringir el SFH de las galaxiascercanas e investigar cómo se formaron y evolucionaron.Sin embargo,aún no está clara la importancia relativade la evolución secular(naturaleza)sobre la crianza,y la separación de los efectos de la evolución impulsadapor la interacción en las propiedades de galaxias observadas no es trivial.Nuestro equipo cuenta con expertosen el campo de la formación y evolución de galaxias,el entorno de galaxias,el modelado espectral de galaxiasy los modelos de evolución química de galaxias,con experiencia en el trabajo conjunto.En esta contribuciónpresentamos un programa de investigación entre China y Chile en el que usamos datos de MaNGA para restringiria SFH en galaxias cercanas que se encuentran en diferentes entornos para investigar cómo se ","cbCaitBLtWl7TRw5","https://ap.wps.com/l/cbCaitBLtWl7TRw5","pdf",1781678,"English","# 1. Introduction\n## Observational window into galaxy evolution\n## Modeling tools: spectral and photometric constraints\n## MaNGA and collaboration scope","[{\"question\":\"Why are star formation histories (SFH) important for understanding galaxies?\",\"answer\":\"SFH indicates when galaxies formed their stars and accumulated their mass, encoding past and current physical processes that drive evolution across cosmic time.\"},{\"question\":\"What enables high-precision constraints on SFH in resolved stellar populations?\",\"answer\":\"Resolved spectroscopy allows discrimination of stellar ages from the spectrum each age produces, enabling precise reconstruction of SFH.\"},{\"question\":\"How do the collaboration results apply to different environments?\",\"answer\":\"The program uses MaNGA data to constrain SFH in nearby galaxies across environments, demonstrating the methodology for isolated galaxies and for a galaxy merger.\"}]","Exploring the Star Formation Histories of Galaxies in Different Environments from MaNGA Spectra - Proceedings | PDF"]