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Using line intensity mapping (LIM) of the redshifted [CII] fine-structure line, the design covers 210–420 GHz with a scanning Fabry-Perot interferometer and KID detector subarrays. The optical system uses four silicon lenses with anti-reflection metamaterial layers and targets angular resolution around 30–50 arcseconds.",{"@graph":69,"@context":123},[70,84,106],{"@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/ccat-prime-the-epoch-of-reionization-spectrometer-for-prime-cam-on-fyst/501646/",{"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/ccat-prime-the-epoch-of-reionization-spectrometer-for-prime-cam-on-fyst/501646.png","ImageObject",300,407,{"name":92,"@type":93},"Đào","Person",{"url":74,"name":95,"@type":96},"DocShare","Organization","application/pdf","2026-10-20","2026-10-03",true,{"@type":102,"interactionType":103,"userInteractionCount":105},"InteractionCounter",{"@type":104},"ViewAction",12,{"@type":107,"mainEntity":108},"FAQPage",[109,115,119],{"name":110,"@type":111,"acceptedAnswer":112},"What instrument and science goal does EoR-Spec pursue on FYST?","Question",{"text":113,"@type":114},"EoR-Spec is a spectrometer module hosted by Prime-Cam on FYST, targeting the Epoch of Reionization through line intensity mapping of the redshifted [CII] line.","Answer",{"name":116,"@type":111,"acceptedAnswer":117},"How does the EoR-Spec design provide spectral coverage and resolution?",{"text":118,"@type":114},"It uses a scanning Fabry-Perot interferometer positioned at the pupil, covering 210–420 GHz in two orders to achieve spectral resolution around R ~ 100.",{"name":120,"@type":111,"acceptedAnswer":121},"How is the detector array organized and tuned for frequency ranges?",{"text":122,"@type":114},"The KID detector array comprises three subarrays: two tuned for 210–315 GHz and one tuned for 315–420 GHz.","https://schema.org",{"og:url":83,"og:type":125,"og:title":65,"og:site_name":95,"og:description":67},"article",{"robots":127,"canonical":83},"index,follow",{"doc_id":129,"site_id":62},501646,1791029235,{"code":4,"msg":5,"data":132},{"doc_id":129,"user_id":133,"nickname":92,"user_avatar":134,"doc_module":4,"category_id":39,"category_name":40,"doc_title":65,"doc_description":67,"doc_content":135,"file_id":136,"file_url":137,"file_type":138,"file_size":139,"view_count":105,"is_deleted":4,"is_public":8,"is_downloadable":8,"audit_status":8,"page_count":140,"language":141,"language_code":63,"site_id":62,"html_lang":63,"table_of_contents":142,"faqs":143,"seo_title":144,"seo_description":67,"update_tm":145,"read_time":36},1374402968488,"https://ap-avatar.wpscdn.com/davatar_29158cc5080c5b710cf443261637dec0","CCAT-prime: The Epoch of Reionization Spectrometer for  \nPrime-Cam on FYST  \nThomas Nikolaa , Steve K. Choia , Cody J. Duella , Rodrigo G. Freundta , Zachary B. Hubera , Yaqiong Lia , Kshama Malavallia , Mike Niemacka , Kayla M. Rossia , Gordon J. Staceya , Eve M. Vavagiakisa , Bugao Zoua , Nick F. Cothardb , Jason Austermannc , Jordan D. Wheelerc , Jiansong Gaoc , Michael R. Vissersc , Johannes Hubmayrc , James Beallc , Joel Ullomc , and  \nPrime-Cam Team  \na Cornell University, Ithaca, NY, 14853, USA b Goddard Space Flight Center, Greenbelt, MD, 20771, USAcNIST, Boulder, CO, 80305, USA  \nABSTRACT  \nThe Fred Young Submillimeter Telescope (FYST), which is the telescope of the CCAT-prime project, will be located at 5600 m near the summit of Cerro Chajnantor in northern Chile, and will host the modular instrument called Prime-Cam. Two of the instrument modules in Prime-Cam will be a spectrometer with a resolving power of R ∼ 100 and populated with a detector array of several thousand KIDs (Kinetic Inductance Detectors) . The main science goal of this spectrometer module, called EoR-Spec, is to probe the Epoch of Reionization (EoR) in the early universe using the Line Intensity Mapping (LIM) technique with the redshifted [CII] fine-structure line. This presentation provides an overview of the optical, mechanical, and spectral design of EoR-Spec, as well as of the detector array that will be used. The optical design consists of four silicon lenses that have anti-reflection metamaterial layers. A scanning Fabry-Perot Interferometer (FPI) will be located at the pupil and provides the spectral resolution over the full spectral coverage of 210 GHz to 420 GHz in two orders, resulting in a redshift coverage of the [CII] line from z = 3 .5 to z = 8 . The detector array consists of three subarrays of KIDs, two of which are tuned for the frequency range between 210 GHz and 315 GHz, and one that is tuned for the 315 GHz to 420 GHz range. The angular resolution will be between about 30′′ to 50′′. This presentation also addresses the spectral and spatial scanning strategy of EoR-Spec on FYST. EoR-Spec is expected to be installed into Prime-Cam about 1 year after first light of FYST.  \nKeywords: Spectroscopy, Fabry-Perot Interferometer, Kinetic Inductance Detector, Submillimeter, Cosmology, Line Intensity Mapping, CCAT, Silicon  \n1. INTRODUCTION  \nThe general, accepted picture about the early evolution of the universe is that after recombination at about 370,000 years after the Big Bang, when the Cosmic Microwave Background (CMB) was released, the gas content of the universe was neutral. Then, in the epoch between the first few 100 million years (z > 10) and about 1 billion years (z ∼ 6), as the matter of the universe contracted and cooled sufficiently, the first star and galaxies formed and started to re-ionize the universe. This is the epoch of re-ionization (EoR) . Today most of the gas in the universe outside of galaxies is ionized. The details of the re-ionization process of the universe, however, are not well understood. For example, the re-ionization could be dominated by high-energetic radiation from powerful Active Galactic Nuclei (AGN), or from ionization radiation of Milky-Way-type galaxies, or other sources. Powerful AGNs are expected to be much less distributed than Milky-Way-type galaxies. Hence, if AGNs would be the dominant source of the re-ionization, ionization “bubbles” would emerge in more isolated regions and expand, while if Milky-Way-type galaxies would be dominating the process, the re-ionization would be expected to begin more uniformly distributed.  \nFurther author information: (Send correspondence to T.N.)  \nT.N.: E-mail: [tn46@cornell.edu](tn46@cornell.edu)  \nMillimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy XI, edited by Jonas Zmuidzinas, Jian-Rong Gao, Proc. of SPIE Vol. 12190, 121900G · © 2022 SPIE · 0277-786X · doi: 10. 1117/12 .2629338  \nProc. of SPIE Vol. 12190 121900G-1  \n","cbCainPvH4Dz3iyl","https://ap.wps.com/l/cbCainPvH4Dz3iyl","pdf",1145165,16,"English","# Abstract\n# Introduction\n## Early universe and re-ionization context\n## Observational challenges and LIM approach\n## EoR-Spec on FYST and Prime-Cam overview","[{\"question\":\"What instrument and science goal does EoR-Spec pursue on FYST?\",\"answer\":\"EoR-Spec is a spectrometer module hosted by Prime-Cam on FYST, targeting the Epoch of Reionization through line intensity mapping of the redshifted [CII] line.\"},{\"question\":\"How does the EoR-Spec design provide spectral coverage and resolution?\",\"answer\":\"It uses a scanning Fabry-Perot interferometer positioned at the pupil, covering 210–420 GHz in two orders to achieve spectral resolution around R ~ 100.\"},{\"question\":\"How is the detector array organized and tuned for frequency ranges?\",\"answer\":\"The KID detector array comprises three subarrays: two tuned for 210–315 GHz and one tuned for 315–420 GHz.\"}]","CCAT-prime - The Epoch of Reionization Spectrometer for Prime-Cam on FYST | PDF",1791021937]