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The document then summarizes major CCAT science themes and supporting observational goals across cosmic FIR background radiation, star formation history, interstellar media, cluster formation via the SZE, and molecular cloud structure.",{"@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 & 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observe?","Question",{"text":63,"@type":64},"CCAT is a 25-meter FIR/submillimeter telescope designed to operate at wavelengths as short as about 200 μm.","Answer",{"name":66,"@type":61,"acceptedAnswer":67},"Why does CCAT use a 25 m aperture?",{"text":68,"@type":64},"The document lists key reasons: matching ALMA sensitivity in the submm regime, achieving strong integration times to confusion at 350 μm, improving source positioning to better than 0.5 arcseconds, and enabling detailed resolution of the FIR/submm cosmic background.",{"name":70,"@type":61,"acceptedAnswer":71},"What are CCAT’s main science themes?",{"text":72,"@type":64},"The themes include measuring galaxy star formation history, advancing resolution of the cosmic FIR background radiation field, characterizing atomic/molecular/solid-state interstellar media, probing galaxy cluster formation via the Sunyaev-Zel’dovich effect, and studying molecular cloud formation and the clump mass 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\n•A 25meter FIR/submillimeter telescope that will operate at wavelengths as short as 􀁏 = 200 􀁐m, an atmospheric limit  \n• To be located in a high (5617m) environment  \n• It will take advantage of one of the now fastest‐developing detector technologies of any spectral region, opening up for surveys one of the last, largely untapped frontiers of ground‐based astronomical research  \nBeam size􀀝 􀁏􀀾􀁐m]/100 arcsec  \ne.g. 2”@ 200 􀁐m FoV: 1 sq. deg.  \n@ 350 􀁐m  \nFirst‐light  \nshort 􀁏 camera: 50 kpix  \nSeveral instruments in Nasmith foci, some simultaneously accessible in very large FoV  \nWhy 25m?  \n‐ Match ALMA sensitivity in submm regime  \n‐ Integration time to confusion(?) at 350 um ~ 1 hr or to fully resolve the FIR/submm CBR  \n‐ Better than 0.5” source positioning  \nWhat is CCAT?   \nCCAT is not intended to be a “national” observatory: a consortium of mostly academic partners, it is intended to be run – inasmuch as possible – as an academic facility, training ground for the instrumentalists, observers, telescope makers of tomorrow; nimble in rapidly responding to new discoveries as in testing new technologies; with “lean & mean” bureaucracy and eager to release its data with short “proprietary periods”, in order to maximize science fall‐out.  \nWhat’s CCAT for?. . .  \n5  \nMain CCAT Science Themes  \n• Measuring the History of Star Formation in Galaxies from the Epoch of Reionization, Through the Peak of Activity, to today  \n• Advancing the Resolution of the Cosmic FIR Background Radiation Field  \n• Characterizing the Atomic, Molecular, and Solid‐State Interstellar Media of Nearby Galaxies  \n• Probing the Formation of Galaxy Clusters with the Sunyaev‐Zel’dovich Effect (SZE )  \n• Characterizing the Formation of Molecular Clouds and the Clump Mass Function  \nThe Cosmic FIR Background Radiation Field  \nCCAT  \n• Dust reprocesses starlight into FIR  \n• Cosmic expansion shifts light of early galaxies further into submm and mm bands  \nLagache, Puget, & Dole 2005  \nDUST STARLIGHT  \nCOBE (1996)  \nGalaxy Counts and the Cosmic FIRB at Submm Wavelengths  \n• ~10% of CFIRB resolved directly with Herschel  \n• ~50% inferred statistically, yielding estimated number count models to a depth of 2 mJy/beam  \n• CCAT will resolve (directly) sources to 0.5‐1 mJy, likely resolving the totality of the CFIRB  \n• 􀃎 Large Scale surveys into the most active epoch of assembly of cosmic structures  \nHerMES Lockman Hole North Oliver et al. (2010, 2011)  \nModeling and Physical Characterization of Cluster Formation via the SZE  \nStructure of Molecular Clouds  \n2 degrees  \nMolinari et al. 2010  \nHerschel 70 μm, 160 μm, and 350 μm image at longitude = 59°  \nFilaments are pervasive ...  \nFiltered Herschel 250um image Molinari et al. 2010","cbCaiqRiLymBXeoc","https://ap.wps.com/l/cbCaiqRiLymBXeoc","pdf",2836327,25,"English","# What is CCAT?\n## CCAT concept and operating context\n## Why 25m?\n# What’s CCAT for?\n## Main CCAT Science Themes\n## The Cosmic FIR Background Radiation Field\n## Modeling and Physical Characterization of Cluster Formation via the SZE\n## Structure of Molecular Clouds","[{\"question\":\"What is CCAT and what wavelengths will it observe?\",\"answer\":\"CCAT is a 25-meter FIR/submillimeter telescope designed to operate at wavelengths as short as about 200 μm.\"},{\"question\":\"Why does CCAT use a 25 m aperture?\",\"answer\":\"The document lists key reasons: matching ALMA sensitivity in the submm regime, achieving strong integration times to confusion at 350 μm, improving source positioning to better than 0.5 arcseconds, and enabling detailed resolution of the FIR/submm cosmic background.\"},{\"question\":\"What are CCAT’s main science themes?\",\"answer\":\"The themes include measuring galaxy star formation history, advancing resolution of the cosmic FIR background radiation field, characterizing atomic/molecular/solid-state interstellar media, probing galaxy cluster formation via the Sunyaev-Zel’dovich effect, and studying molecular cloud formation and the clump mass function.\"}]","CCAT - Project Overview, Science & Instrumentation Plans | PDF",1791030104,63]