[{"data":1,"prerenderedAt":-1},["ShallowReactive",2],{"doc-seo-135659-105":3,"detail-sidebar-cat-0-en-105":81,"doc-detail-135659-en":131},{"code":4,"msg":5,"data":6},0,"ok",{"site_id":7,"language":8,"slug":9,"title":10,"keywords":11,"description":12,"schema_data":13,"social_meta":74,"head_meta":76,"extra_data":78,"updated_unix":80},105,"en","modeling-the-panchromatic-spectral-energy-distributions-of-galaxies-review-focus","Modeling the Panchromatic Spectral Energy Distributions of Galaxies - Review Focus","","Galaxy spectral energy distributions (SEDs) encode a wide range of physical properties, spanning the star-formation history, metal content and abundance patterns, dust mass and grain-size distribution, dust–starlight geometry, and the interstellar radiation field. Stellar population synthesis (SPS) uses these observed SEDs to infer such underlying variables and to test which quantities can be measured reliably. This review surveys the SPS methodology and summarizes what it enables for stellar masses, star-formation rates and histories, metallicities, dust properties, and the stellar initial mass function.",{"@graph":14,"@context":73},[15,34,56],{"@type":16,"itemListElement":17},"BreadcrumbList",[18,23,27,31],{"item":19,"name":20,"@type":21,"position":22},"https://docshare.wps.com","Home","ListItem",1,{"item":24,"name":25,"@type":21,"position":26},"https://docshare.wps.com/document/","Document",2,{"item":28,"name":29,"@type":21,"position":30},"https://docshare.wps.com/document/research-report/","Research & Report",3,{"item":32,"name":10,"@type":21,"position":33},"https://docshare.wps.com/document/modeling-the-panchromatic-spectral-energy-distributions-of-galaxies-review-focus/135659/",4,{"url":32,"name":10,"@type":35,"image":36,"author":41,"headline":10,"publisher":44,"fileFormat":47,"inLanguage":8,"description":12,"dateModified":48,"datePublished":49,"encodingFormat":47,"isAccessibleForFree":50,"interactionStatistic":51},"DigitalDocument",{"url":37,"@type":38,"width":39,"height":40},"https://docshare.wps.com/thumbnails/modeling-the-panchromatic-spectral-energy-distributions-of-galaxies-review-focus/135659.png","ImageObject",300,407,{"name":42,"@type":43},"Jacob","Person",{"url":19,"name":45,"@type":46},"DocShare","Organization","application/pdf","2026-10-17","2026-08-21",true,{"@type":52,"interactionType":53,"userInteractionCount":55},"InteractionCounter",{"@type":54},"ViewAction",11,{"@type":57,"mainEntity":58},"FAQPage",[59,65,69],{"name":60,"@type":61,"acceptedAnswer":62},"What physical properties of galaxies are encoded in their spectral energy distributions (SEDs)?","Question",{"text":63,"@type":64},"Galaxy SEDs reflect the star-formation history, stellar metallicity and abundance patterns, the stellar initial mass function, and the physical state and quantity of dust and gas.","Answer",{"name":66,"@type":61,"acceptedAnswer":67},"What is stellar population synthesis (SPS) used for in the context of galaxy SEDs?",{"text":68,"@type":64},"SPS aims to extract intrinsic variables—such as masses, star-formation histories, metallicities, dust properties, and the IMF—from observed galaxy SEDs, highlighting which quantities can be measured reliably.",{"name":70,"@type":61,"acceptedAnswer":71},"Why are UV and IR SED regions more challenging to study, and what role does dust play?",{"text":72,"@type":64},"UV and IR observations are hindered by atmospheric obscuration. Dust strongly affects these regions by absorbing and scattering UV light and reradiating the absorbed energy in the infrared.","https://schema.org",{"og:url":32,"og:type":75,"og:title":10,"og:site_name":45,"og:description":12},"article",{"robots":77,"canonical":32},"index,follow",{"doc_id":79,"site_id":7},135659,1787316820,{"code":4,"msg":82,"data":83},"success",[84,88,92,96,101,106,111,115,120,123,127],{"id":22,"doc_module":4,"doc_module_name":25,"category_name":85,"show_sort_weight":86,"slug":87},"Story & Novel",90,"story-novel",{"id":26,"doc_module":4,"doc_module_name":25,"category_name":89,"show_sort_weight":90,"slug":91},"Literature",80,"literature",{"id":33,"doc_module":4,"doc_module_name":25,"category_name":93,"show_sort_weight":94,"slug":95},"Exam",70,"exam",{"id":97,"doc_module":4,"doc_module_name":25,"category_name":98,"show_sort_weight":99,"slug":100},5,"Comic",60,"comic",{"id":102,"doc_module":4,"doc_module_name":25,"category_name":103,"show_sort_weight":104,"slug":105},6,"Technology",50,"technology",{"id":107,"doc_module":4,"doc_module_name":25,"category_name":108,"show_sort_weight":109,"slug":110},7,"Healthcare",40,"healthcare",{"id":112,"doc_module":4,"doc_module_name":25,"category_name":29,"show_sort_weight":113,"slug":114},8,30,"research-report",{"id":116,"doc_module":4,"doc_module_name":25,"category_name":117,"show_sort_weight":118,"slug":119},9,"Religion & Spirituality",20,"religion-spirituality",{"id":118,"doc_module":4,"doc_module_name":25,"category_name":121,"show_sort_weight":118,"slug":122},"World Cup","world-cup",{"id":124,"doc_module":4,"doc_module_name":25,"category_name":125,"show_sort_weight":124,"slug":126},10,"Lifestyle","lifestyle",{"id":128,"doc_module":4,"doc_module_name":25,"category_name":129,"show_sort_weight":97,"slug":130},19,"General","general",{"code":4,"msg":82,"data":132},{"doc_id":79,"user_id":133,"nickname":42,"user_avatar":134,"doc_module":4,"category_id":112,"category_name":29,"doc_title":10,"doc_description":12,"doc_content":135,"file_id":136,"file_url":137,"file_type":138,"file_size":139,"view_count":55,"is_deleted":4,"is_public":22,"is_downloadable":22,"audit_status":22,"page_count":140,"language":141,"language_code":8,"site_id":7,"html_lang":8,"table_of_contents":142,"faqs":143,"seo_title":144,"seo_description":12,"update_tm":80,"read_time":145},962084931830,"https://ap-avatar.wpscdn.com/davatar_a8503ba1806abce46bf441b54a3ca4cd","[Astrophys. 2013.51:393-455. Downloaded from www.annualreviews.org](Astrophys. 2013.51:393-455. Downloaded from www.annualreviews.org)[ ](Astrophys. 2013.51:393-455. Downloaded from www.annualreviews.org)[University of Maryland-College Park on 06/11/15. For personal use only.](University of Maryland-College Park on 06/11/15. For personal use only.)  \nModeling the Panchromatic Spectral Energy Distributions of Galaxies  \nCharlie Conroy  \nDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, California 95064; email: [conroy@ucsc.edu](conroy@ucsc.edu)  \nAnnu . Rev . Astro . Access provided by  \nAnnu. Rev. Astron. Astrophys. 2013. 51:393–455 The Annual Review of Astronomy and Astrophysics is online at [astro.annualreviews.org](astro.annualreviews.org)  \nThis article’s doi:  \n10.1146/annurev-astro-082812-141017 Copyright 􀀂c 2013 by Annual Reviews.  \nAll rights reserved  \nKeywords  \nstars, abundances, dust, stellar populations, galaxies: stellar content, galaxy evolution  \nAbstract  \nThe spectral energy distributions (SEDs) of galaxies are shaped by nearly every physical property of the system, including the star-formation history, metal content, abundance pattern, dust mass, grain size distribution, stardust geometry, and interstellar radiation field. The principal goal of stellar population synthesis (SPS) is to extract these variables from observed SEDs. In this review I provide an overview of the SPS technique and discuss what can be reliably measured from galaxy SEDs. Topics include stellar masses, star-formation rates and histories, metallicities and abundance patterns, dust properties, and the stellar initial mass function.  \n[Annu. Rev. Astro. Astrophys. 2013.51:393-455. Downloaded from www.annualreviews.org](Annu. Rev. Astro. Astrophys. 2013.51:393-455. Downloaded from www.annualreviews.org)[ ](Annu. Rev. Astro. Astrophys. 2013.51:393-455. Downloaded from www.annualreviews.org)[Access provided by University of Maryland-College Park on 06/11/15. For personal use only.](Access provided by University of Maryland-College Park on 06/11/15. For personal use only.)  \nSpectral energy distribution (SED):  \nlight emitted over all or a portion of the FUV-FIR spectral domain, including broadband data and/or moderate-resolution spectra  \nSFH: star-formation history  \nIMF: initial mass function  \nFUV: far-ultraviolet  \nFIR: far-infrared  \nNIR: near-infrared  \nSPS: stellar population synthesis AGB: asymptotic giant branch  \nHB: horizontal branch  \n394  \n1. INTRODUCTION  \nMany of the fundamental properties of unresolved stellar populations are encoded in their spectral energy distributions (SEDs) . These properties include the star-formation history (SFH), stellar metallicity and abundance pattern, stellar initial mass function (IMF), total mass in stars, and the physical state and quantity of dust and gas. Some of these properties are easier to measure than others, and each provides important clues regarding the formation and evolution of galaxies. It is precisely these quantities, measured from the SEDs of galaxies, that have provided the foundation for our modern understanding of galaxy formation and evolution.  \nOver the past several decades considerable effort has been devoted to extracting information from the SEDs of galaxies, exploiting information from the far-ultraviolet (FUV) to the far-infrared (FIR) . Early attempts at understanding the visible and near-infrared (NIR) spectral windows approached the problem by combining mixtures ofstars in ad hoc ways until a match was achieved with observations (e.g., Spinrad & Taylor 1971) . More sophisticated versions of this technique were developed that incorporated physical constraints and automated fitting techniques (Faber 1972). At approximately the same time, synthesis models were being developed that relied on stellar evolution theory to constrain the range of possible stellar types at a given age and metallicity (e.g., Tinsley 1968; Searle, Sargent & Bagnuolo","cbCaibzar1dcGwev","https://ap.wps.com/l/cbCaibzar1dcGwev","pdf",2154449,64,"English","# Introduction\n## Spectral energy distributions and encoded galaxy properties\n## Historical development of SED modeling and SPS\n## UV, IR windows and the role of dust\n# Review focus and reliability of inferred physical parameters","[{\"question\":\"What physical properties of galaxies are encoded in their spectral energy distributions (SEDs)?\",\"answer\":\"Galaxy SEDs reflect the star-formation history, stellar metallicity and abundance patterns, the stellar initial mass function, and the physical state and quantity of dust and gas.\"},{\"question\":\"What is stellar population synthesis (SPS) used for in the context of galaxy SEDs?\",\"answer\":\"SPS aims to extract intrinsic variables—such as masses, star-formation histories, metallicities, dust properties, and the IMF—from observed galaxy SEDs, highlighting which quantities can be measured reliably.\"},{\"question\":\"Why are UV and IR SED regions more challenging to study, and what role does dust play?\",\"answer\":\"UV and IR observations are hindered by atmospheric obscuration. Dust strongly affects these regions by absorbing and scattering UV light and reradiating the absorbed energy in the infrared.\"}]","Modeling the Panchromatic Spectral Energy Distributions of Galaxies - Review Focus | PDF",161]