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It then extends to long-term goals: imaging spectroscopy with high detector multiplexing and spectral resolution, a weather-wavelength allocation framework, and a strategy for imager channel splitting by wavelength to avoid survey-mode weather splits while preserving overlap considerations.",{"@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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capabilities are targeted for CCAT at first light?","Question",{"text":63,"@type":64},"The notes call for multicolor broadband wide-field imaging with large detector counts, plus multi-object moderate-resolution spectrometers to obtain CO and [CII] sensitivity over broad redshift ranges for follow-up target selection.","Answer",{"name":66,"@type":61,"acceptedAnswer":67},"How does the long-term plan expand on the first-light goals?",{"text":68,"@type":64},"It emphasizes large-area visible-sky imaging, discovery of rare objects, serious submm/mm transient studies, and high spectral resolution heterodyne imaging spectroscopy with wide-field line mapping and high detector multiplexing.",{"name":70,"@type":61,"acceptedAnswer":71},"How is the weather and wavelength allocation intended to work?",{"text":72,"@type":64},"A wavelength-band allocation is proposed using a reference PWV threshold for each band, with time availability at or better than the reference PWV and accounting for confusion-limited field counts per year.","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},501470,1791419371,{"code":4,"msg":82,"data":83},"success",[84,88,92,96,101,105,110,114,119,122,126],{"id":22,"doc_module":4,"doc_module_name":25,"category_name":85,"show_sort_weight":86,"slug":87},"Story & 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behalf of the CCAT Consortium and with many thanks to  \nthe CCAT science and instrument working groups  \nTools for CCAT Science: First Light  \n• There is general consensus on what is needed for CCAT to do the most exciting science quickly:  \n• Multicolor, broadband wide-field imaging with N ~ 10,000-50,000 and R ~ 3-10  \n• Enough colors to measure SEDs of galaxies and doT/(1+z) selection of high-z sources  \n• FoV large enough (= enough detectors) to yield high-statistics studies in multiple z bins  \n• FoV wide enough to study clustering of ~confusion-limit sources on interesting scales  \n‣ Criterion relaxes if one only wants to study clustering of high-S/N sources  \n• Not the ultimate photometric survey at first light  \n‣ Except perhaps at long λ where filling FoV is not challenging  \n• Multi-object (N ~ 10) moderate resolution (R~1000) spectrometers  \n• Focus is on sensitivity to CO and [CII] in very broad redshift ranges at R appropriate to velocity dispersions in high-z galaxies  \n• Use SED andT/(1+z) selection to define target list for such followup  \nCCAT Instrumentation 2 Sunil Golwala  \nTools for CCAT Science: Long-Term  \n• One person’s view of what is needed for CCAT to do definitive science (given D = 25 m) during its lifetime:  \n• Imaging large fractions of visible sky with FoV-filling cameras  \n• Finding unique and rare objects  \n• First serious study of transients in submm/mm  \n• Not discussed here except to note that focal planes with 5x106 detectors are expected during CCAT lifetime  \n• High spectral resolution heterodyne imaging spectroscopy in the galaxy and nearby galaxies  \n• Wide-field mapping in many lines, with spectral resolution sufficient to separate dominant species, obtain infall information.  \n• Imaging spectroscopy with N = 1000-10000, R ~ 100-1000, NxR ~ 5x106  \n• N = 50,000 @ R = 100 for finer spectral bins for continuum SED studies in wide fields  \n• N = 10,000 @ R = 1000 for definitive extragalactic imaging spectroscopy in smaller but cosmologically representative fields  \nCCAT Instrumentation 3 Sunil Golwala  \nPardo et a l 2002 ATM mode l, p lot courtesy S. Radford  \nCCAT Instrumentation  \n4 Sunil Golwala  \nWeather-Wavelength Allocation, Mappable Area  \n\n| • best 30-50% devoted to “short submm”(λ ≤ 620 µm)\u003Cbr>• substantial fraction for “trans-mm”(λ ≥ 740 µm)\u003Cbr>• focal plane technologies can obviate choosing between“long submm” and mm |  |  |  |  |  |  | first-light access to cosmological volumes:\u003Cbr>access to largest structures, beat down cosmic variance |  |\n| --- | --- | --- | --- | --- | --- | --- | --- | --- |\n| Band Time Ref. CCAT (5612 m)\u003Cbr>λ ν to CLa PWV b Time Availablec CL fields d\u003Cbr>(µm) (GHz) (hr) (mm) (hr yr −1) (%) (yr −1) |  |  |  |  |  |  | 1st light\u003Cbr>∅FoV\u003Cbr>(’) | area to CL (deg2 yr-1) |\n| 200\u003Cbr>350\u003Cbr>620\u003Cbr>740\u003Cbr>865\u003Cbr>1400 | 1500\u003Cbr>857\u003Cbr>484\u003Cbr>405\u003Cbr>347\u003Cbr>214 | 1248\u003Cbr>0.86\u003Cbr>1.14\u003Cbr>0.43\u003Cbr>0.28\u003Cbr>0.30 | 0.26\u003Cbr>0.47\u003Cbr>0.64\u003Cbr>0.75\u003Cbr>0.86\u003Cbr>1.00 | 281\u003Cbr>1936\u003Cbr>716\u003Cbr>639\u003Cbr>1223\u003Cbr>1517 | 3\u003Cbr>22\u003Cbr>8 7\u003Cbr>14\u003Cbr>17 | 2244\u003Cbr>629\u003Cbr>1488\u003Cbr>4413\u003Cbr>5093 | 7 26 13 23\u003Cbr>20 319 20 436 |  |\n| Total time for PWV \u003C 1.1 mm: 6312 72 |  |  |  |  |  |  | (assumes~50 kpix/band) |  |\n| a Time to reach the confusion limit (CL)– see Table 2. |  |  |  |  |  |  |  |  |\n\nCCAT facility submission to Astro2010  \nb The reference precipitable water vapor (PWV) is the adopted maximum value for observations in a given wavelength band. Several bands have equivalent thresholds (e.g. 350/450 µm) and for simplicity only one band is listed.  \nc Time available at Ref. PWV or better, not already used at lower λ . c.f.: CSO typically does 350 µm observations  \nd Number of confusion-limited fields per [year.](year. in)[ in](year. in) 20-25%Cof tCATi me witmuchhbPWetteVr! ≲ 1 mm;  \nCCAT Instrumentation 5 Sunil Golwala  \n!\"\\#$%&$'(  \n))*+ -./0  \n!\"'$;  \n&$&&  \n'$7 8 9\\#$ µ:!\"'$\\#  \nWhat  \nCan We Imagine?  \nZmuidzinas  \nCCAT Instrumentatio","cbCaiflmvN07XhR9","https://ap.wps.com/l/cbCaiflmvN07XhR9","pdf",3737749,22,"English","# Tools for CCAT Science: First Light\n## Tools for CCAT Science: Long-Term\n# Weather-Wavelength Allocation, Mappable Area\n## Band time and confusion-limit allocation\n# Why to Focus on Multi-Object Spectroscopy\n# Imager Strategy","[{\"question\":\"What capabilities are targeted for CCAT at first light?\",\"answer\":\"The notes call for multicolor broadband wide-field imaging with large detector counts, plus multi-object moderate-resolution spectrometers to obtain CO and [CII] sensitivity over broad redshift ranges for follow-up target selection.\"},{\"question\":\"How does the long-term plan expand on the first-light goals?\",\"answer\":\"It emphasizes large-area visible-sky imaging, discovery of rare objects, serious submm/mm transient studies, and high spectral resolution heterodyne imaging spectroscopy with wide-field line mapping and high detector multiplexing.\"},{\"question\":\"How is the weather and wavelength allocation intended to work?\",\"answer\":\"A wavelength-band allocation is proposed using a reference PWV threshold for each band, with time availability at or better than the reference PWV and accounting for confusion-limited field counts per year.\"}]","Instrumentation for CCAT - Tools for CCAT Science: First Light - Long-Term and Imager Strategy | PDF",1791019716,55]