ࡱ> $   ` b o ftta  jbjbA]A] ם+?+?Of:(>  j  D+B+`j"'L>>$HAp$sRuRuRuRuRuRuR,\eRg*RA "pe*&@f"eeR}llZ_}}}eDlRZ(sR} %^RllpesR}}r "G  zG,wz`x`h}hG}l 6+$,W$+W Keck Adaptive Optics Note 456 Next Generation Adaptive Optics: System Requirements Document Version 1.1016543 June August 12922DecMarchOct. 1393Sept 7, 20087 Summary  TOC \o "1-5" \h \z HYPERLINK \l "_Toc168464453"1 Introduction  PAGEREF _Toc168464453 \h 1 HYPERLINK \l "_Toc168464454"2 Scope and Applicability  PAGEREF _Toc168464454 \h 1 HYPERLINK \l "_Toc168464455"3 References  PAGEREF _Toc168464455 \h 2 HYPERLINK \l "_Toc168464456"3.1 Related Documents  PAGEREF _Toc168464456 \h 2 HYPERLINK \l "_Toc168464457"3.2 Referenced Drawings  PAGEREF _Toc168464457 \h 2 HYPERLINK \l "_Toc168464458"4 Revision History  PAGEREF _Toc168464458 \h 2 HYPERLINK \l "_Toc168464459"5 Background  PAGEREF _Toc168464459 \h 4 HYPERLINK \l "_Toc168464460"5.1 Purpose  PAGEREF _Toc168464460 \h 4 HYPERLINK \l "_Toc168464461"5.2 Motivation for the Development of NGAO  PAGEREF _Toc168464461 \h 4 HYPERLINK \l "_Toc168464462"5.3 Overview  PAGEREF _Toc168464462 \h 5 HYPERLINK \l "_Toc168464464"6 Overall Requirements  PAGEREF _Toc168464464 \h 7 HYPERLINK \l "_Toc168464465"6.1 Science Requirements  PAGEREF _Toc168464465 \h 7 HYPERLINK \l "_Toc168464466"6.1.1 Purpose and Objectives  PAGEREF _Toc168464466 \h 7 HYPERLINK \l "_Toc168464467"6.1.2 Science Performance Requirements  PAGEREF _Toc168464467 \h 7 HYPERLINK \l "_Toc168464468"6.1.3 Science Instrument Requirements  PAGEREF _Toc168464468 \h 26 HYPERLINK \l "_Toc168464469"6.1.4 Science Operations Requirements  PAGEREF _Toc168464469 \h 27 HYPERLINK \l "_Toc168464470"6.2 Observatory Overall Requirements  PAGEREF _Toc168464470 \h 30 HYPERLINK \l "_Toc168464471"6.2.1 Purpose and Objectives  PAGEREF _Toc168464471 \h 30 HYPERLINK \l "_Toc168464472"6.2.2 Facility Requirements  PAGEREF _Toc168464472 \h 30 HYPERLINK \l "_Toc168464473"6.2.3 Observatory Science Instrument Requirements  PAGEREF _Toc168464473 \h 32 HYPERLINK \l "_Toc168464474"6.2.4 Observatory Operational Requirements  PAGEREF _Toc168464474 \h 33 HYPERLINK \l "_Toc168464475"6.2.5 Observatory Implementation Requirements  PAGEREF _Toc168464475 \h 36 HYPERLINK \l "_Toc168464476"7 Optical Requirements  PAGEREF _Toc168464476 \h 37 HYPERLINK \l "_Toc168464477"7.1 Purpose and Objectives  PAGEREF _Toc168464477 \h 37 HYPERLINK \l "_Toc168464478"7.2 Performance Requirements  PAGEREF _Toc168464478 \h 37 HYPERLINK \l "_Toc168464479"7.3 Implementation Requirements  PAGEREF _Toc168464479 \h 40 HYPERLINK \l "_Toc168464480"7.4 Design Requirements  PAGEREF _Toc168464480 \h 40 HYPERLINK \l "_Toc168464481"8 Mechanical Requirements  PAGEREF _Toc168464481 \h 47 HYPERLINK \l "_Toc168464482"8.1 Purpose and Objectives  PAGEREF _Toc168464482 \h 47 HYPERLINK \l "_Toc168464483"8.2 Performance Requirements  PAGEREF _Toc168464483 \h 47 HYPERLINK \l "_Toc168464484"8.3 Implementation Requirements  PAGEREF _Toc168464484 \h 47 HYPERLINK \l "_Toc168464485"8.4 Design Requirements  PAGEREF _Toc168464485 \h 48 HYPERLINK \l "_Toc168464486"9 Electronic/Electrical Requirements  PAGEREF _Toc168464486 \h 50 HYPERLINK \l "_Toc168464487"9.1 Purpose and Objectives  PAGEREF _Toc168464487 \h 50 HYPERLINK \l "_Toc168464488"9.2 Performance Requirements  PAGEREF _Toc168464488 \h 50 HYPERLINK \l "_Toc168464489"9.3 Implementation Requirements  PAGEREF _Toc168464489 \h 50 HYPERLINK \l "_Toc168464490"9.4 Design Requirements  PAGEREF _Toc168464490 \h 50 HYPERLINK \l "_Toc168464491"10 Safety Requirements  PAGEREF _Toc168464491 \h 51 HYPERLINK \l "_Toc168464492"10.1 Purpose and Objectives  PAGEREF _Toc168464492 \h 51 HYPERLINK \l "_Toc168464493"10.2 Scope  PAGEREF _Toc168464493 \h 51 HYPERLINK \l "_Toc168464494"10.3 Laser Safety Requirements  PAGEREF _Toc168464494 \h 51 HYPERLINK \l "_Toc168464495"10.4 Laser Projection Safety Requirements  PAGEREF _Toc168464495 \h 51 HYPERLINK \l "_Toc168464496"10.4.1 Aircraft Safety  PAGEREF _Toc168464496 \h 51 HYPERLINK \l "_Toc168464497"10.4.2 Space Command  PAGEREF _Toc168464497 \h 51 HYPERLINK \l "_Toc168464498"11 Software Requirements  PAGEREF _Toc168464498 \h 52 HYPERLINK \l "_Toc168464499"11.1 Purpose and Objectives  PAGEREF _Toc168464499 \h 52 HYPERLINK \l "_Toc168464500"11.2 Scope  PAGEREF _Toc168464500 \h 52 HYPERLINK \l "_Toc168464501"11.3 Performance Requirements  PAGEREF _Toc168464501 \h 52 HYPERLINK \l "_Toc168464502"11.4 Implementation Requirements  PAGEREF _Toc168464502 \h 52 HYPERLINK \l "_Toc168464503"11.5 Design Requirements  PAGEREF _Toc168464503 \h 52 HYPERLINK \l "_Toc168464504"12 Interface Requirements  PAGEREF _Toc168464504 \h 53 HYPERLINK \l "_Toc168464505"12.1 Purpose and Objectives  PAGEREF _Toc168464505 \h 53 HYPERLINK \l "_Toc168464506"12.2 Performance Requirements  PAGEREF _Toc168464506 \h 53 HYPERLINK \l "_Toc168464507"12.3 Implementation Requirements  PAGEREF _Toc168464507 \h 53 HYPERLINK \l "_Toc168464508"12.4 Design Requirements  PAGEREF _Toc168464508 \h 53 HYPERLINK \l "_Toc168464509"12.4.1 Optical Interface  PAGEREF _Toc168464509 \h 53 HYPERLINK \l "_Toc168464510"12.4.2 Mechanical Interface  PAGEREF _Toc168464510 \h 53 HYPERLINK \l "_Toc168464511"12.4.3 Electrical/Electronic Interface  PAGEREF _Toc168464511 \h 54 HYPERLINK \l "_Toc168464512"12.4.4 Software Interface  PAGEREF _Toc168464512 \h 54 HYPERLINK \l "_Toc168464513"13 Reliability Requirements  PAGEREF _Toc168464513 \h 56 HYPERLINK \l "_Toc168464514"13.1 Purpose  PAGEREF _Toc168464514 \h 56 HYPERLINK \l "_Toc168464515"13.2 Scope  PAGEREF _Toc168464515 \h 56 HYPERLINK \l "_Toc168464516"13.3 Performance  PAGEREF _Toc168464516 \h 56 HYPERLINK \l "_Toc168464517"14 Spares Requirements  PAGEREF _Toc168464517 \h 56 HYPERLINK \l "_Toc168464518"15 Service and Maintenance Requirements  PAGEREF _Toc168464518 \h 56 HYPERLINK \l "_Toc168464519"16 Documentation Requirements  PAGEREF _Toc168464519 \h 57 HYPERLINK \l "_Toc168464520"16.1 Documentation Package  PAGEREF _Toc168464520 \h 57 HYPERLINK \l "_Toc168464521"16.2 Drawings  PAGEREF _Toc168464521 \h 57 HYPERLINK \l "_Toc168464522"16.3 Electrical/Electronic Documentation  PAGEREF _Toc168464522 \h 57 HYPERLINK \l "_Toc168464523"16.4 Software  PAGEREF _Toc168464523 \h 57 HYPERLINK \l "_Toc168464524"17 Glossary  PAGEREF _Toc168464524 \h 58  Table of Contents  TOC \o "1-1" \h \z \u  HYPERLINK \l "_Toc193192156" 1 Introduction  PAGEREF _Toc193192156 \h 1  HYPERLINK \l "_Toc193192157" 2 Scope and Applicability  PAGEREF _Toc193192157 \h 1  HYPERLINK \l "_Toc193192158" 3 References  PAGEREF _Toc193192158 \h 2  HYPERLINK \l "_Toc193192159" 4 Revision History  PAGEREF _Toc193192159 \h 2  HYPERLINK \l "_Toc193192160" 5 Background  PAGEREF _Toc193192160 \h 4  HYPERLINK \l "_Toc193192161" 6 Overall Requirements  PAGEREF _Toc193192161 \h 7  HYPERLINK \l "_Toc193192162" 7 Optical Requirements  PAGEREF _Toc193192162 \h 54  HYPERLINK \l "_Toc193192164" 8 Mechanical Requirements  PAGEREF _Toc193192164 \h 61  HYPERLINK \l "_Toc193192165" 9 Electronic/Electrical Requirements  PAGEREF _Toc193192165 \h 65  HYPERLINK \l "_Toc193192166" 10 Safety Requirements  PAGEREF _Toc193192166 \h 66  HYPERLINK \l "_Toc193192167" 11 Software Requirements  PAGEREF _Toc193192167 \h 67  HYPERLINK \l "_Toc193192169" 12 Interface Requirements  PAGEREF _Toc193192169 \h 68  HYPERLINK \l "_Toc193192170" 13 Reliability Requirements  PAGEREF _Toc193192170 \h 71  HYPERLINK \l "_Toc193192171" 14 Spares Requirements  PAGEREF _Toc193192171 \h 71  HYPERLINK \l "_Toc193192172" 15 Service and Maintenance Requirements  PAGEREF _Toc193192172 \h 71  HYPERLINK \l "_Toc193192173" 16 Documentation Requirements  PAGEREF _Toc193192173 \h 72  HYPERLINK \l "_Toc193192174" 17 Glossary  PAGEREF _Toc193192174 \h 73  Table of Contents  TOC \o "1-4" \h \z \u  HYPERLINK \l "_Toc193192270" 1 Introduction  PAGEREF _Toc193192270 \h 1  HYPERLINK \l "_Toc193192271" 2 Scope and Applicability  PAGEREF _Toc193192271 \h 1  HYPERLINK \l "_Toc193192272" 3 References  PAGEREF _Toc193192272 \h 2  HYPERLINK \l "_Toc193192273" 3.1 Related Documents  PAGEREF _Toc193192273 \h 2  HYPERLINK \l "_Toc193192274" 3.2 Referenced Drawings  PAGEREF _Toc193192274 \h 2  HYPERLINK \l "_Toc193192275" 4 Revision History  PAGEREF _Toc193192275 \h 2  HYPERLINK \l "_Toc193192276" 5 Background  PAGEREF _Toc193192276 \h 4  HYPERLINK \l "_Toc193192277" 5.1 Purpose  PAGEREF _Toc193192277 \h 4  HYPERLINK \l "_Toc193192278" 5.2 Motivation for the Development of NGAO  PAGEREF _Toc193192278 \h 4  HYPERLINK \l "_Toc193192279" 5.3 Overview  PAGEREF _Toc193192279 \h 5  HYPERLINK \l "_Toc193192280" 6 Overall Requirements  PAGEREF _Toc193192280 \h 7  HYPERLINK \l "_Toc193192281" 6.1 Science Requirements  PAGEREF _Toc193192281 \h 7  HYPERLINK \l "_Toc193192282" 6.1.1 Purpose and Objectives  PAGEREF _Toc193192282 \h 7  HYPERLINK \l "_Toc193192283" 6.1.2 Science Performance Requirements  PAGEREF _Toc193192283 \h 7  HYPERLINK \l "_Toc193192284" 6.1.2.1 High-Redshift Galaxies  PAGEREF _Toc193192284 \h 8  HYPERLINK \l "_Toc193192285" 6.1.2.2 Nearby AGNs: Black Hole Mass Measurements  PAGEREF _Toc193192285 \h 10  HYPERLINK \l "_Toc193192286" 6.1.2.3 General Relativity Effects in the Galactic Center  PAGEREF _Toc193192286 \h 12  HYPERLINK \l "_Toc193192287" 6.1.2.4 Planets Around Low-Mass Stars  PAGEREF _Toc193192287 \h 14  HYPERLINK \l "_Toc193192288" 6.1.2.5 Asteroid Companions Survey  PAGEREF _Toc193192288 \h 19  HYPERLINK \l "_Toc193192289" 6.1.2.6 Asteroid Companions Orbit Determination  PAGEREF _Toc193192289 \h 21  HYPERLINK \l "_Toc193192290" 6.1.2.7 QSO Host Galaxies  PAGEREF _Toc193192290 \h 23  HYPERLINK \l "_Toc193192291" 6.1.2.8 Gravitational Lensing  PAGEREF _Toc193192291 \h 24  HYPERLINK \l "_Toc193192292" 6.1.2.9 Astrometry Science in Sparse Fields  PAGEREF _Toc193192292 \h 28  HYPERLINK \l "_Toc193192293" 6.1.2.10 Resolved Stellar Populations in Crowded Fields  PAGEREF _Toc193192293 \h 29  HYPERLINK \l "_Toc193192294" 6.1.2.11 Debris Disks  PAGEREF _Toc193192294 \h 29  HYPERLINK \l "_Toc193192295" 6.1.2.12 Young Stellar Objects  PAGEREF _Toc193192295 \h 29  HYPERLINK \l "_Toc193192296" 6.1.2.13 Asteroid Size, Shape, and Composition  PAGEREF _Toc193192296 \h 29  HYPERLINK \l "_Toc193192297" 6.1.2.14 Gas Giant Planets  PAGEREF _Toc193192297 \h 30  HYPERLINK \l "_Toc193192298" 6.1.2.15 Ice Giants: Uranus and Neptune  PAGEREF _Toc193192298 \h 32  HYPERLINK \l "_Toc193192299" 6.1.2.16 Other: Backup Science  PAGEREF _Toc193192299 \h 34  HYPERLINK \l "_Toc193193915" 6.1.2.17 Atmospheric Seeing Assumptions  PAGEREF _Toc193193915 \h 37  HYPERLINK \l "_Toc193193932" 6.1.3 Science Instrument Requirements  PAGEREF _Toc193193932 \h 38  HYPERLINK \l "_Toc193193933" 6.1.4 Science Operations Requirements  PAGEREF _Toc193193933 \h 39  HYPERLINK \l "_Toc193193935"  Science-grade quality of the raw data  PAGEREF _Toc193193935 \h 40  HYPERLINK \l "_Toc193193936" 6.1.4.1  PAGEREF _Toc193193936 \h 40  HYPERLINK \l "_Toc193193937"  Science-grade quality of the data products  PAGEREF _Toc193193937 \h 42  HYPERLINK \l "_Toc193193940" 6.1.4.2  PAGEREF _Toc193193940 \h 42  HYPERLINK \l "_Toc193193941" 6.1.4.3 Science impact from a given data product  PAGEREF _Toc193193941 \h 42  HYPERLINK \l "_Toc193193942" 6.2 Observatory Overall Requirements  PAGEREF _Toc193193942 \h 43  HYPERLINK \l "_Toc193193943" 6.2.1 Purpose and Objectives  PAGEREF _Toc193193943 \h 43  HYPERLINK \l "_Toc193193944" 6.2.2 Facility Requirements  PAGEREF _Toc193193944 \h 43  HYPERLINK \l "_Toc193193945" 6.2.3 Telescope and Dome Environment Requirements:  PAGEREF _Toc193193945 \h 47  HYPERLINK \l "_Toc193193946" 6.2.4 Observatory Science Instrument Requirements  PAGEREF _Toc193193946 \h 48  HYPERLINK \l "_Toc193193947" 6.2.5 Observatory Operational Requirements  PAGEREF _Toc193193947 \h 49  HYPERLINK \l "_Toc193193948" 6.2.6 Observatory Implementation Requirements  PAGEREF _Toc193193948 \h 52  HYPERLINK \l "_Toc193193949" 7 Optical Requirements  PAGEREF _Toc193193949 \h 54  HYPERLINK \l "_Toc193193950" 7.1 Purpose and Objectives  PAGEREF _Toc193193950 \h 54  HYPERLINK \l "_Toc193193951" 7.2 Performance Requirements  PAGEREF _Toc193193951 \h 54  HYPERLINK \l "_Toc193193952" 7.3 Implementation Requirements  PAGEREF _Toc193193952 \h 54  HYPERLINK \l "_Toc193193953" 7.4 Design Requirements  PAGEREF _Toc193193953 \h 54  HYPERLINK \l "_Toc193193955" 8 Mechanical Requirements  PAGEREF _Toc193193955 \h 61  HYPERLINK \l "_Toc193193956" 8.1 Purpose and Objectives  PAGEREF _Toc193193956 \h 61  HYPERLINK \l "_Toc193193957" 8.2 Performance Requirements  PAGEREF _Toc193193957 \h 61  HYPERLINK \l "_Toc193193958" 8.3 Implementation Requirements  PAGEREF _Toc193193958 \h 62  HYPERLINK \l "_Toc193193960" 8.4 Design Requirements  PAGEREF _Toc193193960 \h 62  HYPERLINK \l "_Toc193193961" 9 Electronic/Electrical Requirements  PAGEREF _Toc193193961 \h 65  HYPERLINK \l "_Toc193193962" 9.1 Purpose and Objectives  PAGEREF _Toc193193962 \h 65  HYPERLINK \l "_Toc193193963" 9.2 Performance Requirements  PAGEREF _Toc193193963 \h 65  HYPERLINK \l "_Toc193193964" 9.3 Implementation Requirements  PAGEREF _Toc193193964 \h 65  HYPERLINK \l "_Toc193193965" 9.4 Design Requirements  PAGEREF _Toc193193965 \h 65  HYPERLINK \l "_Toc193193966" 10 Safety Requirements  PAGEREF _Toc193193966 \h 66  HYPERLINK \l "_Toc193193967" 10.1 Purpose and Objectives  PAGEREF _Toc193193967 \h 66  HYPERLINK \l "_Toc193193968" 10.2 Scope  PAGEREF _Toc193193968 \h 66  HYPERLINK \l "_Toc193193969" 10.3 Laser Safety Requirements  PAGEREF _Toc193193969 \h 66  HYPERLINK \l "_Toc193193970" 10.4 Laser Projection Safety Requirements  PAGEREF _Toc193193970 \h 66  HYPERLINK \l "_Toc193193971" 10.4.1 Aircraft Safety  PAGEREF _Toc193193971 \h 66  HYPERLINK \l "_Toc193193972" 10.4.2 Space Command  PAGEREF _Toc193193972 \h 66  HYPERLINK \l "_Toc193193973" 11 Software Requirements  PAGEREF _Toc193193973 \h 67  HYPERLINK \l "_Toc193193974" 11.1 Purpose and Objectives  PAGEREF _Toc193193974 \h 67  HYPERLINK \l "_Toc193193975" 11.2 Scope  PAGEREF _Toc193193975 \h 67  HYPERLINK \l "_Toc193193976" 11.3 Performance Requirements  PAGEREF _Toc193193976 \h 67  HYPERLINK \l "_Toc193193977" 11.4 Implementation Requirements  PAGEREF _Toc193193977 \h 67  HYPERLINK \l "_Toc193193978" 11.5 Design Requirements  PAGEREF _Toc193193978 \h 67  HYPERLINK \l "_Toc193193980" 12 Interface Requirements  PAGEREF _Toc193193980 \h 68  HYPERLINK \l "_Toc193193981" 12.1 Purpose and Objectives  PAGEREF _Toc193193981 \h 68  HYPERLINK \l "_Toc193193982" 12.2 Performance Requirements  PAGEREF _Toc193193982 \h 68  HYPERLINK \l "_Toc193193983" 12.3 Implementation Requirements  PAGEREF _Toc193193983 \h 68  HYPERLINK \l "_Toc193193984" 12.4 Design Requirements  PAGEREF _Toc193193984 \h 68  HYPERLINK \l "_Toc193193985" 12.4.1 Optical Interface  PAGEREF _Toc193193985 \h 68  HYPERLINK \l "_Toc193193986" 12.4.2 Mechanical Interface  PAGEREF _Toc193193986 \h 68  HYPERLINK \l "_Toc193193987" 12.4.3 Electrical/Electronic Interface  PAGEREF _Toc193193987 \h 69  HYPERLINK \l "_Toc193193988" 12.4.4 Software Interface  PAGEREF _Toc193193988 \h 70  HYPERLINK \l "_Toc193193989" 13 Reliability Requirements  PAGEREF _Toc193193989 \h 71  HYPERLINK \l "_Toc193193990" 13.1 Purpose  PAGEREF _Toc193193990 \h 71  HYPERLINK \l "_Toc193193991" 13.2 Scope  PAGEREF _Toc193193991 \h 71  HYPERLINK \l "_Toc193193992" 13.3 Performance  PAGEREF _Toc193193992 \h 71  HYPERLINK \l "_Toc193193993" 14 Spares Requirements  PAGEREF _Toc193193993 \h 71  HYPERLINK \l "_Toc193193994" 15 Service and Maintenance Requirements  PAGEREF _Toc193193994 \h 71  HYPERLINK \l "_Toc193193995" 16 Documentation Requirements  PAGEREF _Toc193193995 \h 72  HYPERLINK \l "_Toc193193996" 16.1 Documentation Package  PAGEREF _Toc193193996 \h 72  HYPERLINK \l "_Toc193193997" 16.2 Drawings  PAGEREF _Toc193193997 \h 72  HYPERLINK \l "_Toc193193998" 16.3 Electrical/Electronic Documentation  PAGEREF _Toc193193998 \h 72  HYPERLINK \l "_Toc193193999" 16.4 Software  PAGEREF _Toc193193999 \h 72  HYPERLINK \l "_Toc193194000" 17 Glossary  PAGEREF _Toc193194000 \h 73   TOC \h \z \c "Figure" Figure 1 Keck telescope structure  PAGEREF _Toc50804675 \h 6 Figure 1 Keck telescope structure 5   TOC \h \z \c "Table"  HYPERLINK \l "_Toc193198241" Table 17. NGAO baseline Mauna Kea Cn2 Profile  PAGEREF _Toc193198241 \h 37  HYPERLINK \l "_Toc193198242" Table 2 Glossary of Terms  PAGEREF _Toc193198242 \h 73 Table 1 NGAO baseline Mauna Kea Cn2 Profile 36 Table 2 Glossary of Terms 69 Table 1 NGAO baseline Mauna Kea Cn2 Profile 10 Table 2 Glossary of Terms 40  Requirements Tables  TOC \h \z \t "RequirementsCaption,1"  HYPERLINK \l "_Toc193181756" Table 1. High-Redshift Galaxies derived requirements  PAGEREF _Toc193181756 \h 8  HYPERLINK \l "_Toc193181757" Table 2. Nearby AGNs derived requirements  PAGEREF _Toc193181757 \h 11  HYPERLINK \l "_Toc193181758" Table 3a. General relativity effects in the Galactic Center derived requirements  PAGEREF _Toc193181758 \h 12  HYPERLINK \l "_Toc193181759" Table 3b. Radial velocity measurements derived requirements  PAGEREF _Toc193181759 \h 14  HYPERLINK \l "_Toc193181760" Table 4. Planets Around Low Mass Stars derived requirements  PAGEREF _Toc193181760 \h 15  HYPERLINK \l "_Toc193181761" Table 5. Asteroid Companions Survey driven requirements  PAGEREF _Toc193181761 \h 20  HYPERLINK \l "_Toc193181762" Table 6. Asteroid Companions Orbit Determination driven requirements  PAGEREF _Toc193181762 \h 22  HYPERLINK \l "_Toc193181763" Table 7. QSO Host galaxies derived requirements  PAGEREF _Toc193181763 \h 23  HYPERLINK \l "_Toc193181764" Table 8a. Imaging studies of distant galaxies lensed by galaxies  PAGEREF _Toc193181764 \h 25  HYPERLINK \l "_Toc193181765" Table 8b. Spectroscopic studies of distant galaxies lensed by galaxies  PAGEREF _Toc193181765 \h 26  HYPERLINK \l "_Toc193181766" Table 9a. Imaging studies of distant galaxies lensed by clusters  PAGEREF _Toc193181766 \h 28  HYPERLINK \l "_Toc193181767" Table 9b. Spectroscopic studies of distant galaxies lensed by clusters  PAGEREF _Toc193181767 \h 28  HYPERLINK \l "_Toc193181768" Table 10. Astrometry Science in Sparse Fields derived requirements  PAGEREF _Toc193181768 \h 29  HYPERLINK \l "_Toc193181769" Table 11. Resolved Stellar Populations in Crowded Fields derived requirements  PAGEREF _Toc193181769 \h 29  HYPERLINK \l "_Toc193181770" Table 12. Debris Disks derived requirements  PAGEREF _Toc193181770 \h 29  HYPERLINK \l "_Toc193181771" Table 13. Young Stellar Objects derived requirements  PAGEREF _Toc193181771 \h 29  HYPERLINK \l "_Toc193181772" Table 14. Asteroid size, shape, and composition derived requirements  PAGEREF _Toc193181772 \h 29  HYPERLINK \l "_Toc193181773" Table 15. Moons of giant planets derived requirements  PAGEREF _Toc193181773 \h 31  HYPERLINK \l "_Toc193181774" Table 16. Ice Giants derived requirements  PAGEREF _Toc193181774 \h 33  HYPERLINK \l "_Toc193181775" Table 17. Alternate Science Observing Modes  PAGEREF _Toc193181775 \h 34  HYPERLINK \l "_Toc193181776" Table 18. Science Instrument Requirements  PAGEREF _Toc193181776 \h 38  HYPERLINK \l "_Toc193181777" Table 19. Science Operations Requirements, Raw Data Quality  PAGEREF _Toc193181777 \h 39  HYPERLINK \l "_Toc193181778" Table 20. Science Operations Requirements, Data Products Quality  PAGEREF _Toc193181778 \h 41  HYPERLINK \l "_Toc193181779" Table 21. Science Operations Requirements, Archiving and Retrieval  PAGEREF _Toc193181779 \h 42  HYPERLINK \l "_Toc193181780" Table 21. Facility Requirements  PAGEREF _Toc193181780 \h 43  HYPERLINK \l "_Toc193181781" Table 22. Telescope and Dome Environment Requirements  PAGEREF _Toc193181781 \h 47  HYPERLINK \l "_Toc193181782" Table 23. Observatory Science Instrument Requirements  PAGEREF _Toc193181782 \h 48  HYPERLINK \l "_Toc193181783" Table 24. Observatory Operational Requirements  PAGEREF _Toc193181783 \h 50  HYPERLINK \l "_Toc193181784" Table 25. Observatory Implementation Requirements  PAGEREF _Toc193181784 \h 52  HYPERLINK \l "_Toc193181785" Table 26. Implementation Requirements  PAGEREF _Toc193181785 \h 54  HYPERLINK \l "_Toc193181786" Table 27. Optical Design Requirements  PAGEREF _Toc193181786 \h 54  HYPERLINK \l "_Toc193181787" Table 28. Science Instrument Optical Design Requirements  PAGEREF _Toc193181787 \h 56  HYPERLINK \l "_Toc193181788" Table 29. Non-Interferometric Science Instrument Optical Design Requirements  PAGEREF _Toc193181788 \h 57  HYPERLINK \l "_Toc193181789" Table 30. Interferometry Science Instrument Optical Design Requirements  PAGEREF _Toc193181789 \h 58  HYPERLINK \l "_Toc193181790" Table 31. Mechanical Performance Requirements  PAGEREF _Toc193181790 \h 61  HYPERLINK \l "_Toc193181791" Table 32. Mechanical Implementation Requirements  PAGEREF _Toc193181791 \h 62  HYPERLINK \l "_Toc193181792" Table 33. Mechanical Design Requirements  PAGEREF _Toc193181792 \h 62  HYPERLINK \l "_Toc193181793" Table 34. Electrical Performance Requirements  PAGEREF _Toc193181793 \h 65  HYPERLINK \l "_Toc193181794" Table 35. Electrical Performance Requirements  PAGEREF _Toc193181794 \h 67  HYPERLINK \l "_Toc193181795" Table 36. Mechanical Interface Requirements  PAGEREF _Toc193181795 \h 68  HYPERLINK \l "_Toc193181796" Table 37. Electrical Interface Requirements  PAGEREF _Toc193181796 \h 69  HYPERLINK \l "_Toc193181797" Table 38. Software Interface Requirements  PAGEREF _Toc193181797 \h 70  HYPERLINK \l "_Toc193181798" Table 39. Reliability Performance Requirements  PAGEREF _Toc193181798 \h 71 Table 1. High-Redshift Galaxies derived requirements 8 Table 2. Nearby AGNs derived requirements 11 Table 3a. General relativity effects in the Galactic Center derived requirements 13 Table 3b. Radial velocity measurements derived requirements 14 Table 4. Planets Around Low Mass Stars derived requirements 15 Table 5. Asteroid Companions Survey driven requirements 20 Table 6. Asteroid Companions Orbit Determination driven requirements 22 Table 7. QSO Host galaxies derived requirements 23 Table 8a. Imaging studies of distant galaxies lensed by galaxies 25 Table 8b. Spectroscopic studies of distant galaxies lensed by galaxies 26 Table 9a. Imaging studies of distant galaxies lensed by clusters 28 Table 9b. Spectroscopic studies of distant galaxies lensed by clusters 28 Table 10. Astrometry Science in Sparse Fields derived requirements 29 Table 11. Resolved Stellar Populations in Crowded Fields derived requirements 29 Table 12. Debris Disks derived requirements 29 Table 13. Young Stellar Objects derived requirements 29 Table 14. Asteroid size, shape, and composition derived requirements 30 Table 15. Moons of giant planets derived requirements 31 Table 16. Ice Giants derived requirements 33 Table 17. Alternate Science Observing Modes 35 Table 18. Science Instrument Requirements 38 Table 19. Science Operations Requirements, Raw Data Quality 39 Table 20. Science Operations Requirements, Data Products Quality 41 Table 21. Science Operations Requirements, Archiving and Retrieval 42 Table 21. Facility Requirements 43 Table 22. Telescope and Done Environment Requirements 46 Table 23. Observatory Science Instrument Requirements 48 Table 24. Observatory Operational Requirements 49 Table 25. Observatory Implementation Requirements 51 Table 1. Asteroid Companions Survey driven requirements Table 2. Asteroid Companions Orbit Determination driven requirements Table 3. Asteroid size, shape, and composition derived requirements Table 4. Moons of giant planets derived requirements Table 5. Uranus and Neptune derived requirements Table 6. Planets Around Low Mass Stars derived requirements Table 7. Debris Disks derived requirements Table 8. Young Stellar Objects derived requirements Table 9. Astrometry Science in Sparse Fields derived requirements Table 10a. General relativity effects in the Galactic Center derived requirements Table 10b. Radial velocity measurements derived requirements Table 11. Resolved Stellar Populations in Crowded Fields derived requirements Table 12. Nearby AGNs derived requirements Table 13. QSO Host galaxies derived requirements Table 14. High-Redshift Galaxies derived requirements Table 15a. Spectroscopic studies of distant galaxies lensed by galaxies Table 15b. Imaging studies of distant galaxies lensed by galaxies. Table 16. Other: Backup Science derived requirements Table 18. Science Instrument Requirements Table 19. Science Operations Requirements, Raw Data Quality Table 20. Science Operations Requirements, Data Products Quality Table 21. Science Operations Requirements, Archiving and Retrieval Table 21. Facility Requirements Table 22. Telescope and Done Environment Requirements Table 23. Observatory Science Instrument Requirements Table 24. Observatory Operational Requirements Table 25. Observatory Implementation Requirements  Introduction This document describes the requirements for the Next Generation Adaptive Optics (NGAO) system to be built for the W.M. Keck Observatory (WMKO). The requirements in this document are intended to be at a level appropriate for the system design phase. Further development of the requirements will take place in the next phase of the project (preliminary design). In particular, parametric performance requirements given at this stage are intended to indicate the scope and format of the requirements, but do not in all cases establish final values for the specified parameters. In some cases values for these parameters have yet to be established and are given as TBD. A more generic set of requirements for new WMKO instrumentation is described in the Observatorys Instrumentation Baseline Requirements Document. These requirements are also applicable to NGAO. The NGAO System Requirements Document will take precedence over the Instrumentation Baseline Requirements Document in the event of a conflict. It is important to understand that at this stage of development the requirements provide a basis for identifying the parameters that will be part of the systems specifications, but the values given are subject to change as the development continues. During the next phases of the project work will be done to refine the requirements for review at the preliminary design review. The final requirements to be reviewed at the detailed design review will form the basis for the acceptance test criteria for the instrument. The purpose of this document is to define and communicate the requirements for the NGAO-specific design and implementation in terms of the needed scientific and technical performance. The document also expresses specific requirements for implementation or design where those requirements are essential to satisfactory integration and interoperation of NGAO with the observatory systems. The document avoids prescribing specific design or implementation solutions except for solutions that embody the Observatorys unique knowledge or experience. The document establishes requirements for the NGAO that will guide the design through the detailed design phase. Scope and Applicability This document establishes requirements for all aspects of NGAO beyond those already specified in the Instrumentation Baseline Requirements Document. This document also establishes requirements for changes to related Keck telescope subsystems and software where required. This document does not address the requirements for the science instruments that will work with NGAO, although it does cover the NGAO interfaces to these instruments. Separate system requirements documents will need to be prepared for each of these instruments as part of their design process. References Related Documents  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 572. Instrumentation Baseline Requirements Document. KAON 153. Coordination and Use of Laser Beacons for AO on Mauna Kea.  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/WebHome/NGAO_Proposal_Executive_Summary_Final.pdf" KAON 455. Science Case Requirements Document. KAON 399. NGAO Proposal Executive Summary.  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/WebHome/NGAO_Proposal_Final.pdf" KAON 400. NGAO Proposal.  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 428. Implications and requirements for Interferometry with NGAO.  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/NGAO_SCRD_Release2_v10a_sm.pdf" KAON 455. NGAO Science Case Requirements Document v1v2.0.  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/WorkProducts/KAON476.pdf" KAON 476. NGAO Science Operations Observing Model Trade Study ANSI Z136.1 Safe Use of Lasers Indoors (2000). ANSI Z136.6 Safe Use of Lasers Outdoors (2000). Architecture_reqments_summary_v7.xls This isTableS. Don.] [This table will be updated as part of the next official version of the SCRD. Claire Referenced Drawings Table X lists the drawing numbers, revisions and date, source and title for all drawings referenced in this documentNone at this time. Revision History VersionDateAuthorReason for revision / remarks0.1Jan. 16, 2007WizinowichInitial version0.3Feb. 1, 2007WizinowichMultiple edits0.4Feb. 6, 2007WizinowichMultiple edits. Included seeing & telescope environment in section 6.1.21.0Feb. 21, 2007WizinowichAdded Dekany performance requirements input1.1Apr. 17, 2007WizinowichEdited section 61.2May 15, 2007WizinowichIncorporated input from NGAO team meeting 61.3May 22, 2007WizinowichMiscellaneous1.4May 22, 2007WizinowichMods to the table in section 6.1.21.5May 25, 2007WizinowichAdditions to 6.1.4 based on KAON 4761.6May 30, 2007WizinowichScience requirement changes based on SRD telecom1.7May 31, 2007WizinowichSolar system science requirement input with Le Mignant & Marchis + minor mods to science operation requirements1.8June 1, 2007WizinowichGalactic Center & QSO host science cases. Mods to Observatory operational requirements1.9June 6, 2007WizinowichAGN science case from Adkins, Le Mignant, Max & McGrath1.10June 19, 2007WizinowichAdded planets around low mass stars & gravitational lensing requirement tables. First cut at asteroid shape & size table. Added H-band to GR Galactic Center case. Minor edits to asteroid companions table.1.11June 29, 2007WizinowichMinor edits to science performance requirements1.12August 15, 2007GavelReview and edits, highlighting gaps in the flow down from the ScRD. Added a requirements numbering system.1.13August 22, 2007GavelContinued edits, through all the science requirements tables and instrument requirements tables (to Table 13). Comments and questions are in red font.1.14Sept 4 thru 7, 2007Max, McGrath, Le MignantRevised science requirements tables. We have scrutinized Tables 1, 2, 3, 4, and 6 thoroughly. Things to follow up on are highlighted in yellow. 1.15Oct. 1 3rd, 2007D. Le MignantRevised observatory requirements (section 6). Things to follow up on are highlighted in yellow. Updated Table numbering and TOC. Removed the obsolete performance requirement tables from optical performance section 7. Consolidated Telescope and Dome Environment requirements in Table 22 and included in section 6.2.31.16Dec. 14 19, 2007E. McGrathRevised and re-ordered science requirements tables 1-17. Things to follow up on are highlighted in yellow.1.17March 13, 2008D. GavelFollow up on traceability of requirements. Revised Science Requirements section (E. McGrath, C. Max) Background Background Purpose The purpose of the background section of this document is to provide context and related information for the requirements defined in later sections of this document. Motivation for the Development of NGAO The Keck telescopes are the worlds largest optical and infrared telescopes. Because of their large apertures the Keck telescopes offer the highest potential sensitivity and angular resolution currently available. WMKO has already demonstrated scientific leadership in high angular resolution astronomy with the first NGS and LGS AO systems on 8-10 m telescopes. The importance of achieving the full potential of the Keck telescopes is recognized in the Observatorys strategic plan which identifies leadership in high angular resolution astronomy as a key long-term goal. In order to maintain our leadership in this field we must pursue new AO systems and the instrumentation to exploit them. We have examined, and are continuing to examine, a broad range of key science goals in order to identify the most compelling future science goals of our community and to determine what is needed to realize these goals. As a result we have identified that NGAO should provide the following suite of capabilities: Near diffraction-limited performance at near infrared wavelengths, producing a point spread function with unprecedented precision, stability and contrast; Increased sky coverage and a multiplexing capability, enabling a much broader range of science programs; and AO correction in the red portion of the visible spectrum (0.6-1.0 m), delivering the highest angular resolution images available for filled aperture telescopes. NGAO will be a broad and powerful facility with the potential to achieve major advances in astrophysics. It will provide dramatic gains in solar system and galactic science where AO has already demonstrated a strong scientific impact. NGAO will also allow for extraordinary advances in extragalactic astronomy, far beyond the initial gains being made with the Observatorys current AO systems. To be clear NGAO need not be a single facility. It may be that the requirements are best met with multiple AO systems. The NGAO proposal ( HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/WebHome/NGAO_Proposal_Final.pdf" KAON 400) and NGAO proposal executive summary ( HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/WebHome/NGAO_Proposal_Executive_Summary_Final.pdf" KAON 399) provide more background on the motivation for the development of NGAO. Further scientific motivation is provided in the NGAO science case requirements document ( HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/NGAO_SCRD_Release2_v10a_sm.pdf" KAON 455). Overview The scientific and technical requirements for NGAO result in the following basic systems: AO system. The AO system will likely consist of an AO enclosure, an opto-mechanical system, and software and electronics for both non real-time and real-time control. Laser facility. The laser facility will likely consist of a laser enclosure, the laser(s), the launch facility including a beam transport system and launch telescope, safety systems and laser system control electronics and software. Science operations facility. The science operations facility will primarily include the software and computers required to support operation of the AO system and science instruments. This includes operating the systems for nighttime observing as well as pre- and post-observing activities. Science instruments. The three highest priority instruments are currently a near-IR imager, a visible imager and a deployable near-IR integral field unit (IFU). Three lower priority instruments have also been identified including a near-IR IFU, a visible IFU and an L and M-band imager. There is also a requirement that the NGAO project be designed so as to allow the continued AO support of the Interferometer and the fiber injection module used for the OHANA (Optical Hawaiian Array for Nanoradian Astronomy) project. The AO and laser facilities and the science instruments will have to interface with the telescope structure.  REF _Ref158531988 \h Figure 1Figure 1 shows a schematic view of a Keck telescope. The most likely location for the NGAO system and science instruments is on one of the Nasmyth platforms of the telescope. Nominally we have chosen the left Nasmyth platform of the Keck II telescope as our starting point. The most likely location for the projection telescope is behind the f/15 secondary mirror in the top end of the telescope.  Figure  SEQ Figure \* ARABIC 1 Keck telescope structure Overall Requirements Overall Requirements Science Requirements Purpose and Objectives The purpose of the science overall requirements section is to summarize and convey requirements that apply generally to the overall NGAO system and its accessories. These are based on the NGAO Science Case Requirements Document (SCRD) ( HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/NGAO_SCRD_Release2_v10a_sm.pdf" KAON 455), various trade studies undertaken and error budgets developed to meet these science requirements, general and,observatory instrument and interface requirements ( HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 572) in this initial release, on the NGAO proposal () and on a summary architecture spreadsheet that was developed during NGAO team meetings in the spring and summer of 2007 (KAON 548), and general observatory obligations (KAONs  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" 428 and 153).. Science Performance Requirements Science Requirements Purpose and Objectives The purpose of the science overall requirements section is to summarize and convey requirements that apply generally to the overall NGAO system and its accessories. These are based on the Science Case Requirements Document (SCRD) (KAON 455) and, in this initial release, also on the NGAO proposal (KAON 399) and on a summary architecture spreadsheet that was developed during NGAO team meetings in the spring and summer of 2007 (Architecture_reqments_summary_v7.xls). The performance requirements developed in the SCRD are summarized in the following tables. These will be updated as the science case requirements and performance budgets become better defined. The relevant source of the requirement from the Science Requirements Document (SCRD), KAON 455, is referenced by section number. Some of the requirements have a source other than the SCRD. In these cases the additional source is listed. We have categorized the various science cases into two classes: those that push the limits of AO system, instrument, and telescope performance (designated Key Science Drivers), and those that are less technically demanding than the Key Science Drivers but still place important requirements on available observing modes, instruments, and PSF knowledge. We shall call the latter category Science Drivers. In the remainder of this section we present tables showing the requirements that flow down from both of these categories of science cases. The cases we shall discuss are listed below, together with their designation as Key Science Drivers (KSD) or Science Drivers (SD). Reference in Title and Number in This Report Summary Spreadsheet (KAON 548) High-redshift galaxies (KSD) X2 Nearby AGNs: black hole mass measurements (KSD) X3 General Relativity at Galactic Center (KSD) G2 a. Astrometric G2a b. Radial velocity G2b Planets around low-mass stars (KSD) G1 Asteroid companions survey (KSD) S1a Asteroid companions orbit determination (KSD) S1b QSO host galaxies (SD) X1 Gravitationally lensed galaxies by galaxies (SD) Imaging X4b Spectroscopy X4a Place holder for Gravitationally lensed galaxies by clusters (SD) Imaging X4b Spectroscopy X4a Place-holder for Astrometry in sparse fields (SD) GX1 Place-holder for Resolved stellar populations in crowded fields (SD) GX2 Place-holder for Debris disks (SD) G3 Place-holder for Young stellar objects (SD) G4 Asteroid size, shape, and composition (SD) S2 Moons of the Giant Planets (SD) S3 Uranus and Neptune (SD) S4 Backup science (SD) O High-Redshift Galaxies Science Performance Requirements The performance requirements developed in the SCRD are summarized in the following tables. These will be updated as the science case requirements and performance budgets become better defined. . In these cases the additional source is listed. reference [Don] We have categorized the various science cases into two classes: those that push the limits of AO system, instrument, and telescope performance (designated Key Science Drivers), and those that are less technically demanding than the Key Science Drivers but still place important requirements on available observing modes, instruments, and PSF knowledge. We shall call the latter category Science Drivers. In the remainder of this section we present tables showing the requirements that flow down from both of these categories of science cases. The cases we shall discuss are listed below, together with their designation as Key Science Drivers (KSD) or Science Drivers (SD). Reference in Title and Number in This Report Summary Spreadsheet Architecture_reqments_summary_v7.xls 1. High-redshift galaxies (KSD) X2 Nearby AGNs: black hole mass measurements (KSD) X3 General Relativity at Galactic Center (KSD) G2 a. Astrometric G2a b. Radial velocity G2b Planets around low-mass stars (KSD) G1 Asteroid companions survey (KSD) S1a Asteroid companions orbit determination (KSD) S1b QSO host galaxies (SD) X1 Gravitationally lensed galaxies by galaxies (SD) Imaging X4b Spectroscopy X4a Place holder for Gravitationally lensed galaxies by clusters (SD) Imaging X4b Spectroscopy X4a Place-holder for Astrometry in sparse fields (SD) GX1 Place-holder for Resolved stellar populations in crowded fields (SD) GX2 Place-holder for Debris disks (SD) G3 Place-holder for Young stellar objects (SD) G4 Asteroid size, shape, and composition (SD) S2 Moons of the Giant Planets (SD) S3 Uranus and Neptune (SD) S4 Other: Backup science (SD) O The requirements for the high-redshift galaxies science case are summarized in the following table (see the Galaxy Assembly and Star Formation History section of KAON 455 (Release 2.1)). Table 1. High-Redshift Galaxies derived requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements1.1Sensitivity. SNR e" 10 for a z = 2.6 galaxy in an integration time d" 3 hours for a spectral resolution R = 3500 with a spatial resolution of 50 mas [SCRD 2.1.4]Sufficiently high throughput and low emissivity of the AO system science path to achieve this sensitivity. Background due to emissivity less than 30% of unattenuated (sky + telescope). [SCRD 2.1.5.1 and SCRD Figure 1]1.2Target sample size of e" 200 galaxies in d" 3 years (assuming a target density of 4 galaxies per square arcmin) [SCRD 2.1.3]Multi-object AO system: one DM per arm, or an upstream MCAO system correcting the entire field of regard. 6-12 arms on 5 square arc minutes patrol field. Multiple (6-12) IFUs, deployable on the 5 square arc minute field of regard1.3Spectroscopic and imaging observing wavelengths = J, H and K (to 2.4 m) [SCRD 2.1.4, 2.1.5.3]AO system must transmit J, H, and K bands1Infrared imager and IFUs designed for J, H, and K.1 Each entire wavelength band should be observable in one exposure.1.4Spectral resolution = 3000 to 4000 [SCRD 2.1.5.1, 2.1.5.3]Spectral resolution of >3000 in IFUs1.5Narrow field imaging: diffraction limited at J, H, K [SCRD 2.1.5.3]Wavefront error 170 nm or betterNyquist sampled pixels at each wavelength1.6Encircled energy at least 50% in 70 mas for sky coverage of 30% (see 1.11) [SCRD 2.1.5.2] Wavefront error sufficiently low (~170 nm) to achieve the stated requirement in J, H, and K bands.IFU spaxel size: either 35 or 70 mas, to be determined during the design study for the multiplexed IFU spectrograph 1.7Velocity determined to d" 20 km/sec for spatial resolutions of 70 masPSF intensity distribution known to d" 10% per spectral channel. 1.8IFU field of view e" 1 x 3 in order to allow sky background measurement at same time as observing a ~1 galaxy [SCRD 2.1.5.1]Each MOAO IFU channel passes a 1x3 field. Each IFU units field of view is 1 x 31.9Simultaneous sky background measurements within a radius of 3 with the same field of view as the science field [SCRD 2.1.5.1]See #1.8 1.10Relative photometry to d" 5% for observations during a single night Knowledge of ensquared energy in IFU spaxel to 5%. Telemetry system that monitors tip/tilt star Strehl and other real-time data to estimate the EE vs. time, or other equivalent method to determine PSF to the required accuracy. 1.11Sky coverage e"30% at 170 nm wavefront error, to overlap with data sets from other instruments and telescopes [SCRD 2.1.5.2]Infrared tip/tilt sensors with AO correction of tip/tilt stars 1.12Should be able to center a galaxy to d" 10% of science field of view1.13Should know the relative position of the galaxy to d" 20% of spaxel size1.14Target drift should be d" 10% of spaxel size in 1 hr1.15The following observing preparation tools are required: PSF simulation and exposure time calculator1.16The following data products are required: calibrated spectral data cube [SCRD 2.1.5.3] High-Redshift Galaxies The requirements for the high-redshift galaxies science case are summarized in the following table (see the Galaxy Assembly and Star Formation History section of KAON 455 (V1)). Table 1. High-Redshift Galaxies derived requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements1.1Sensitivity. SNR e" 10 for a z = 2.6 galaxy in an integration time d" 3 hours for a spectral resolution R = 3500 with a spatial resolution of 50 mas [SCRD 2.1.1.4]Sufficiently high throughput and low emissivity of the AO system science path to achieve this sensitivity. Background due to emissivity less than 20% of sky + telescope. [SCRD 2.1.1.5.1 and SCRD Figure 1]1.2Target sample size of e" 200 galaxies in d" 3 years (assuming a target density of 4 galaxies per square arcmin) [SCRD 2.1.1.3]Multi-object AO system: one DM per arm, or an upstream MCAO system correcting the entire field of regard. 6-12 arms on 5 square arc minutes patrol field. Multiple (6-12) IFUs, deployable on the 5 square arc minute field of regard1.3Spectroscopic and imaging observing wavelengths = J, H and K (to 2.4 m) [SCRD 2.1.1.5.2, RollUp_v1 B13]AO system must transmit J, H, and K bands1Infrared imager and IFUs designed for J, H, and K.1 Each entire wavelength band should be observable in one exposure.1.4Spectral resolution = 3000 to 4000 [SCRD 2.1.1.5.2]Spectral resolution of >3000 in IFUs1.5Narrow field imaging: diffraction limited at J, H, K [SCRD 2.1.1.5.1]Wavefront error 170 nm or betterNyquist sampled pixels at each wavelength1.6Encircled energy at least 50% in 70 mas for sky coverage of 30% (see 1.12) [RollUp_v1 E13, N13] Wavefront error sufficiently low (~170 nm) to achieve the stated requirement in J, H, and K bands.IFU spaxel size: either 35 or 70 mas, to be determined during the design study for the multiplexed IFU spectrograph 1.7Velocity determined to d" 20 km/sec for spatial resolutions of 70 masPSF intensity distribution known to d" 10% per spectral channel. 1.8IFU field of view e" 1 x 3 in order to allow sky background measurement at same time as observing a ~1 galaxy [SCRD 2.1.1.5.1]Each MOAO IFU channel passes a 1x3 field. Each IFU units field of view is 1 x 31.9Simultaneous sky background measurements within a radius of 3 with the same field of view as the science fieldSee #1.8 1.10Relative photometry to d" 5% for observations during a single night [RollUp_v1 H13]Knowledge of ensquared energy in IFU spaxel to 5%. Telemetry system that monitors tip/tilt star Strehl and other real-time data to estimate the EE vs time, or other equivalent method to determine PSF to the required accuracy. 1.11Sky coverage e"30% at 170 nm wavefront error, to overlap with data sets from other instruments and telescopes [SCRD 2.1.1.5.2, RollUp_v1 N13]Infrared tip/tilt sensors with AO correction of tip/tilt stars 1.12Should be able to center a galaxy to d" 10% of science field of view1.13Should know the relative position of the galaxy to d" 20% of spaxel size1.14Target drift should be d" 10% of spaxel size in 1 hr1.15The following observing preparation tools are required: PSF simulation and exposure time calculator1.16The following data products are required: calibrated spectral data cube Nearby AGNs: Black Hole Mass Measurements The requirements for the Nearby AGN science case are summarized in the following table (see the Nearby AGN section of KAON 455 (Release 2.1)). Table 2. Nearby AGNs derived requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements2.1Number of targets required: to be specified in future versions of the SCRD [SCRD 2.2.3]2.2Required wavelength range 0.85 2.4 microns [SCRD 2.2.3]2.3Required spatial sampling at least two resolution elements across gravitational sphere of influence. [SCRD 2.2.2]50% enclosed energy radius < gravitational sphere of influence. Wavefront error requirement to be specified in future versions of this document.Spectral and imaging pixels/spaxels < gravitational sphere of influence (in the spatial dimension)2.4Required field of view for both spectroscopy and imaging > 10 radii of the gravitational sphere of influence. [e.g., SCRD 2.2.4 Figure 3]Will need to get sky background measurement as efficiently as possible. For IR, consider using a separate d-IFU on the sky.2.5Required SNR for spatially resolved spectroscopy of the central black hole region using stellar velocities > 30 per resolution element [SCRD 2.2.3]PSF stability and knowledge requirements will be discussed in future releases of the SCRDSpectral resolution R ~ 3000-4000 with at least two pixels per resolution element; detector limited SNR performance. Spatial sampling at least two resolution elements across the gravitational sphere of influence2.6Required observation planning tools: PSF simulation tools to plan for observations of Seyfert 1 galaxies which have strong central point sources2.7Required data reduction pipeline for IFU Nearby AGNs: Black Hole Mass Measurements The requirements for the Nearby AGN science case are summarized in the following table (see the Nearby AGN section of KAON 455 (V1)). The typical AGN that we are considering is at redshift <0.05, and if a Seyfert 1 galaxy has a magnitude yyy point source in the center, with a host galaxy of magnitude zzz per square arcsec. The region of interest for spatially resolved spectroscopy is within the gravitational sphere of influence of the central black hole: generally we will need at least two resolution elements across this distance. [convert to arcsecs as function of z] The scientific goals are the following: to measure the black hole mass using stellar kinematics in the cores of AGNs. In order to accomplish this, PSF subtraction will be crucial for Seyfert 1 galaxies. [This is a derived requirement.] Table 2. Nearby AGNs derived requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements2.1Number of targets required: sample size of TBD galaxies in TBD nights or years Requirement on sky coverage fraction may be implied here2.2Required wavelength range 0.85 2.4 microns2.3Required spatial sampling at least two resolution elements across gravitational sphere of influence80% enclosed energy radius < gravitational sphere of influence. This implies a total wavefront error of not more than TBD nm over a range from TBD to TBD microns.Spectral and imaging pixels/spaxels < gravitational sphere of influence (in the spatial dimension)2.4Required field of view for both spectroscopy and imaging > 10 radii of the gravitational sphere of influence [fill this in]Will need to get sky background measurement as efficiently as possible. For IR, consider using d-IFU on the sky; for visible, need solution2.5Required SNR for spatially resolved spectroscopy of the central black hole region using stellar velocities > 30 per resolution elementAO Strehl ratio > TBD at 0.85 microns (Ca infrared triplet). This implies a total wavefront error of TBD nm at 0.85 microns. PSF stability and knowledge, temporal and field of view [uniformity trade]; Spectral resolution R ~ 3000-4000 (TBD) with two pixels per resolution element; detector limited SNR performance; Spatial sampling at least two resolution elements across the gravitational sphere of influence2.6Required signal to noise ratio for imaging of the region around the central black hole [is this a contrast requirement?]AO Strehl ratio > TBD, this implies a total wavefront error of not more than TBD nm over a range from TBD to TBD microns. PSF stability and knowledge, temporal and field of view [uniformity trade]; Spatial sampling at least two resolution elements across the gravitational sphere of influence 2.7Photometric accuracy required for imaging the central point source and possible cusp: TBD at TBD wavelengths AO Strehl ratio > TBD, this implies a total wavefront error of not more than TBD nm over a range from TBD to TBD microns. AO background level < TBD; over TBD wavelength range; PSF stability and knowledge, temporal and field of view [uniformity trade];Calibration stability and accuracy, Zero-point stability and knowledge, Quality of flat-fielding; 2.8Velocity determined to d" TBD km/sec for spatial resolutions of TBD masPSF intensity distribution known to d" xxx% per spectral channel. Spatial and spectral model fitting valid to d" TBD2.9Required observation planning tools (e.g. guide stars); PSF simulation tools to plan for observations of Seyfert 1 galaxies which have strong central point sources2.10Required data reduction pipeline for IFU General Relativity Effects in the Galactic Center The requirements for the Measurement of General Relativity Effects in the Galactic Center science case on both precision astrometry and radial velocities are summarized in the following two tables, respectively (see the Precision Astrometry: Measurements of General Relativity Effects in the Galactic Center section of KAON 455 (Release 2.1)). Table 3a. General relativity effects in the Galactic Center derived requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements3a.1Astrometric accuracy d" 100 as for objects d" 5 from the Galactic Center [SCRD 2.3.8.1]High Strehl to reduce confusion limit: rms wavefront error d" 170 nm at G.C. IR tip/tilt sensors. Means of aligning and measuring position of tip-tilt sensors so that they permit astrometric accuracy of d" 100 as. Means of preventing WFS-blind field-distortion modes (if multi-DMs are in series). Will require ADC. Need astrometric error budget in order to determine ADC requirements.Nyquist sampling at H and K. Instrument distortion characterized and stable to d" 100 as.3a.2Observing wavelengths: H and K-band [SCRD 2.3.9]Transmit H and K band to science instrument3a.3Field of view e" 10 x 10 for imaging [SCRD 2.3.9]Science path shall allow an unvignetted 10 x 10 field.3a.4Ability to construct 40x40 mosaic to tie to radio astrometric reference frame [SCRD 2.3.5]3a.5The following observing preparation tools are required: PSF simulation as function of wavelength and seeing conditions, exposure time calculator.3a.6The following data products are required: Calibrated PSF, data reduction pipeline, accurate distortion map (see 3a.1) [SCRD 2.3.5] Table 3b. Radial velocity measurements derived requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements3b.1Radial velocity accuracy d" 10 km/sec for objects d" 5 from the Galactic Center [SCRD 2.3.8.2]170nm wavefront error at G.C. PSF estimation sufficient to measure a radial velocity to 10 km/sec. [suggestions from SCRD 2.3.8.2]Spectral resolution e" 4000 Calibration of one IFU relative to other ones sufficient to permit 10 km/sec radial velocity measurement 3b.2Observing wavelengths H, K-band [SCRD 2.3.6]Transmit H, K band to science instrument3b.3Spatial sampling d" 20 mas (H) or 35 mas (K) to control confusion within IFU field of view [SCRD 2.3.6]20 and 35 mas spaxel scales at H and K respectively3b.4Field of view e" 1 x 1 [SCRD 2.3.6]Field of view e" 1 x 1 3b.5The following observing preparation tools are required: PSF simulation as function of wavelength and seeing conditions, exposure time calculator.3b.6The following data products are required: IFU pipeline for wavelength/flux calibration [SCRD 2.3.6] General Relativity Effects in the Galactic Center The requirements for the Measurement of General Relativity Effects in the Galactic Center science case on both precision astrometry and radial velocities are summarized in the following two tables, respectively (see the Precision Astrometry: Measurements of General Relativity Effects in the Galactic Center section of KAON 455 (Release 2)). Table 3a. General relativity effects in the Galactic Center derived requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements3a.1Astrometric accuracy d" 100 as for objects d" 5 from the Galactic Center [SCRD 2.1.3.8, RollUp_v1 I6]High Strehl to reduce confusion limit: rms wavefront error d" 170 nm at G.C. IR tip/tilt sensors. Means of aligning and measuring position of tip-tilt sensors so that they permit astrometric accuracy of d" 100 as. Means of preventing WFS-blind field-distortion modes (if multi-DMs are in series). Will require ADC. Need astrometric error budget in order to determine ADC requirements.Nyquist sampling at H and K. Instrument distortion characterized and stable to d" 100 as.3a.2Observing wavelengths: H and K-band [SCRD 2.1.3.11, RollUp_v1 B6]Transmit H and K band to science instrument3a.3Field of view e" 10 x 10 for imaging [SCRD 2.1.3.11]Science path shall allow an unvignetted 10 x 10 field.3a.4Ability to construct 40 x40 mosaic to tie to radio astrometric reference frame [SCRD 2.1.3.5]3a.5The following observing preparation tools are required: PSF simulation as function of wavelength and seeing conditions, exposure time calculator.3a.6The following data products are required: Calibrated PSF, data reduction pipeline, accurate distortion map (see 3a.1) Table 3b. Radial velocity measurements derived requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements3b.1Radial velocity accuracy d" 10 km/sec for objects d" 5 from the Galactic Center [SCRD 2.1.3.10, RollUp_v1 J6]170nm wavefront error at G.C. PSF estimation sufficient to measure a radial velocity to 10 km/sec. [suggestions from SCRD 2.1.3.10]Spectral resolution e" 4000 Calibration of one IFU relative to other ones sufficient to permit 10 km/sec radial velocity measurement 3b.2Observing wavelengths H, K-band [SCRD 2.1.3.6]Transmit H, K band to science instrument3b.3Spatial resolution d" 20 mas or 35 mas to control confusion within IFU field of view [SCRD 2.1.3.6]20 and 30 mas plate scales3b.4Field of view e" 1 x 1 [SCRD 2.1.3.6]Field of view e" 1 x 1 3b.5The following observing preparation tools are required: PSF simulation as function of wavelength and seeing conditions, exposure time calculator.3b.6The following data products are required: IFU pipeline for wavelength/flux calibration [SCRD 2.1.3.6] Planets Around Low-Mass Stars The requirements for the planets around low-mass stars science case are summarized in the following table. The key area in which NGAO will excel is the detection of planets around low-mass stars and brown dwarfs because Keck, unlike GPI, will be able to use a laser guide star. NGAO will also be able to search for planets around young solar-type stars where dust extinction is significant. JWST will have coronagraphic capability in the 3 to 5 (m window, but will have significantly lower spatial resolution than Keck NGAO. In terms of the types of solar systems that can be studied, this means that JWST will focus on older, nearby main sequence stars (since older giant planets will remain visible in 3 to 5 (m for a longer time). JWST may be more limited than NGAO in doing large surveys, because of its longer slewing time and possibly a lifetime limit on the total number of slews. Note: this science will usually be in LGS mode. Depending on the target magnitude, may choose to use the parent star as one of the required tip-tilt stars. Table 4. Planets Around Low Mass Stars derived requirements Science Performance RequirementAO Derived RequirementsInstrument Requirements4.1Target sample 1: Old field brown dwarfs out to distance of 20 pc. Sample size several hundred, desired maximum survey duration 3 yrs (practical publication timescales). [SCRD 2.4.3]Observe 20 targets per night (each with e.g. 20 min integration time). Guide on a tip-tilt star with H=14. Talk to Mike Liu re guide star magnitude. Near infrared imager (possibly with coronagraph). Survey primary stars at J- and Hband. 4.2Target sample 2: Young (<100 Myr) field brown dwarfs and low-mass stars to distance of 80 pc. Sample size several hundred, desired maximum survey duration 3 yrs. [SCRD 2.4.3]Observe 20 targets per night (each with e.g. 20 min integration time). Near infrared imager (possibly with coronagraph). Survey primary at J- and Hband. Could benefit from dual- or multi-channel mode for rejecting speckle suppression, but not essential for this program.4.3Target sample 3: solar type stars in nearby star forming regions such as Taurus and Ophiuchus, and young clusters @ 100 to 150 pc distance. Bright targets (on-axis tip-tilt generally possible: V=14-15, J=10-12). Sample size several hundred, desired maximum survey duration 3 yrs.(May not require LGS if there is a good enough near-IR wavefront sensor available).Possible dual- or multi-channel mode for speckle suppression. Alternatively an IFU would help, provided it is Nyquist sampled at H and has FOV > 1 arc sec. Min. IFU spectral resolution is R~100. May need IR ADC for imaging or coronagraphic observations (J or H bands); typical airmass is 1.7 for Ophiuchus. 4.4Companion Sensitivity Sample 1: assume no companions beyond 15 AU. Targets at 20 to 30 pc; companion distribution peaks at 4 AU = 0.2"; this yields 2 MJupiter planets at a 0.2" separation with contrast H = 10. Planets have H=24, J=24.7. Parent stars are 2MASS Brown Dwarfs with H=14. [SCRD 2.4.2.1]Excellent (<10nm) calibration of both initial LGS spot size and quasi-static non-common path aberrations, especially at mid-spatial-frequencies. Needs algorithms such as phase retrieval or speckle nulling (on a fiber source + good stability). Small servo-lag error (<30nm) to avoid scattered light at 0.2 arc sec. Source: Error budget and simulations by Bruce Macintosh. Inner working angle of 6 /D general-purpose coronagraph with a contrast of 10-6. Detailed design of coronagraph will take place during PDR stage. Speckle suppression capability (multi-spectral imaging); dual-channel imager; stability of static errors ~5nm per sqrt(hr) for PSF subtraction or ADI. 4.5Companion Sensitivity Sample 2: Parent stars are T Tauri, J=11. A 1 MJupiter planet is at 300K, J=22, (2 MJupiter is J=19.5). This distribution could have a wider distribution of binaries a) 0.1" separation, J = 8.5 (2MJ) b) 0.2" separation, J = 11 (1MJ) c) Goal J = 11 at 0.1" separation (1MJ) based on properties of the planets you want to look for. [SCRD 2.4.2.2]Same as #4.4 a) 6 /D general-purpose coronagraph b) 6 /D general-purpose coronagraph c) (Goal) Not achievable with a general purpose coronagraph May need small Inner Working Distance (2 /D) coronagraph. Speckle suppression capability (multi-spectral imaging); dual-channel imager; stability of static errors ~5nm per  EMBED Equation.3  for PSF subtraction or ADI. 4.6Goal: Companion Sensitivity Case 3: at 5 Myr , 1 Msun primary; a) goal J = 13.5 to see 1 MJupiter or b) goal J = 9 for 5 MJupiter. 0.07" is needed. For apparent magnitudes of parent stars see 4.3 Excellent (10-20nm) calibration of both initial LGS spot size and quasi-static non-common path aberrations, at both low- and mid-spatial-frequencies. Needs algorithms such as phase retrieval or speckle nulling (on a fiber source + good stability). Small servo-lag error (<30nm) to avoid scattered light at 0.2 arc sec. Tomography errors 20-30nm. Source: error budget and simulations by Bruce Macintosh. Requires multi-  speckle suppression; very small inner working angle coronagraph (2 /D); static errors in 5-10nm range. 4.7Sensitivity of H=25 for 5-sigma detection in 20 minutes, at 1 arcsec separation from primary star. (Brown dwarf targets are limited by sky background at larger angles, of order ~1 arcsec). [SCRD 2.4.5.9]Sufficiently high throughput and low emissivity to permit detecting H=25 in 20 minutes at 5 sigma above background. 4.8H-band relative photometry (between primary and companion): accuracy d" 0.1 mag for recovered companions (to estimate mass of the companion); goal of measuring colors to 0.05 mags (0.03 mag per band) to measure temperatures and surface gravities sufficiently accurately (to ~10%). [SCRD 2.4.5.4]Diagnostics on AO data to measure Strehl fluctuations if it takes a while to move on and off the coronagraph (a possible more attractive solution is a specialized coronagraph that simultaneously images the primary)Induced ghost images of primary; or rapid interleaving of saturated and unsaturated images; or a partially transparent coronagraph4.9Requirement: Astrometric precision 2 mas (~1/10 PSF) relative between primary and planet, for initial rejection of background objects. [SCRD 2.4.5.5] Goal: For measuring orbits of nearby field objects, want 0.5 mas to measure masses to 10%. Note this gives you mass of primary star. Could be combined with Doppler measurements if thats practical for the brighter objects. Ways to do this: a) Position stability requirement for star behind coronagraph (e.g., stable to 0.5 or 2 mas over 10 min.). b) Induced ghost image method. Needs a wire grating ahead of the coronagraph, or use DM to induce ghost images. (papers by Marois et al. 2006, ApJ, 647, 612; Sivaramakrishnan & Oppenheimer 2006, ApJ, 647, 620).Stability of distortion as required for 0.5 or 2 mas. Also want ghost images of primary (as for photometry #4.8) in order to locate it accurately relative to planet.4.10Efficiency: 20 targets per night (30 goal) [SCRD 2.4.6.2]AO system must be able to absolutely steer objects so they land on the coronagraph. This implies 5 mas reproducibility of field steering or lock the tip/tilt to this accuracy relative to coronagraph field stop. Final requirement will depend on the details of the coronagraph (5 mas is consistent with GPI modeling).4.11Observing wavelengths JHK bands (strong goal: Y and z for companion temperature characterization) [SCRD 2.4.4, 2.4.7]Transmit JHK to science instrument. Goal: Y and z.JHK filters. Methane band filters for rapid discrimination, Y and z, and/or a custom filter for early characterization.4.12Able to register and subtract PSFs (with wavelength, time, etc.) for post-processing to get rid of residual speckles. Subtraction needs to be sufficient enough to meet req. #4.4. PSF knowledge and/ or stability to meet req. #4.4.At least 1.5 x better than Nyquist sampled at J (goal Y)4.13Field of view: must see companions at 100 AU scales at 30 pc (goal 20 pc) [SCRD 2.4.5.3]Field of view 3" radius (goal 5" radius)4.14Characterization of companion [SCRD 2.4.4]a) R ~150 IFU, sub-Nyquist sampling spectrograph, or if above not available, b) Nyquist spatial sampling IFU, R ~ 4,000, OH suppressing). c) or narrow-band filters. All must be sensitive to J = 22 or 23 in ~3 hrs. 4.15Sky Coverage >30%. (Survey several hundred Brown Dwarfs to H=15 of the ~1000 known targets.) [SCRD 2.4.7]Technical field for low-order wavefront guidestar pickoff large enough to achieve 30% sky coverage at high galactic latitude. Ability to acquire and track 3 tip/tilt stars. (More lenient if parent star can be used as one of the three TT stars.) Or ability to measure everything sufficiently with a single H=15 TT star (pyramid sensors).4.16The following observing preparation tools are required: guide star finder for high proper-motion stars The requirements for the planets around low-mass stars science case are summarized in the following table. The key area in which NGAO will excel is the detection of planets around low-mass stars and brown dwarfs because Keck, unlike GPI, will be able to use a laser guide star. NGAO will also be able to search for planets around young solar-type stars where dust extinction is significant. JWST will have coronagraphic capability in the 3 to 5 (m window, but will have significantly lower spatial resolution than Keck NGAO. In terms of the types of solar systems that can be studied, this means that JWST will focus on older, nearby main sequence stars (since older giant planets will remain visible in 3 to 5 (m for a longer time). JWST may be more limited than NGAO in doing large surveys, because of its longer slewing time and possibly a lifetime limit on the total number of slews. Note: this science will usually be in LGS mode. Depending on the target magnitude, may choose to use the parent star as one of the required tip-tilt stars. Table 4. Planets Around Low Mass Stars derived requirements Science Performance RequirementAO Derived RequirementsInstrument Requirements4.1Target sample 1: Old field brown dwarfs out to distance of 20 pc. Sample size several hundred, desired maximum survey duration 3 yrs (practical publication timescales).Observe 20 targets per night (each with e.g. 20 min integration time). Guide on a tip-tilt star with H=14 (talk to Mike Liu to see if this is OK) Near infrared imager (possibly with coronagraph). Survey primary stars at J- and Hband. 4.2Target sample 2: Young (<100 Myr) field brown dwarfs and low-mass stars to distance of 80 pc. Sample size several hundred, desired maximum survey duration 3 yrs. Observe 20 targets per night (each with e.g. 20 min integration time). Near infrared imager (possibly with coronagraph). Survey primary at J- and Hband. Could benefit from dual- or multi-channel mode for rejecting speckle suppression, but not essential for this program.4.3Target sample 3: solar type stars in nearby star forming regions such as Taurus and Ophiuchus, and young clusters @ 100 to 150 pc distance. Bright targets (on-axis tip-tilt generally possible: V=14-15, J=10-12). Sample size several hundred, desired maximum survey duration 3 yrs. (May not require LGS if there is a good enough near-IR wavefront sensor available).Possible dual- or multi-channel mode for speckle suppression. Alternatively an IFU would help, provided it is Nyquist sampled at H and has FOV > 1 arc sec. Min. IFU spectral resolution is R~100. May need IR ADC for imaging or coronagraphic observations (J or H bands); typical airmass is 1.7 for Ophiuchus. 4.4Companion Sensitivity Sample 1: assume no companions beyond 15 AU. Targets at 20 to 30 pc; companion distribution peaks at 4 AU = 0.2"; this yields 2 MJupiter planets at a 0.2" separation with contrast J = 10. Planets have H=24, J=24.7. Parent stars are 2MASS Brown Dwarves with H=14. Excellent (<10nm) calibration of both initial LGS spot size and quasi-static non-common path aberrations, especially at mid-spatial-frequencies. Needs algorithms such as phase retrieval or speckle nulling (on a fiber source + good stability). Small servo-lag error (<30nm) to avoid scattered light at 0.2 arc sec. Source: error budget and simulations by Bruce Macintosh. Inner working angle of 6 /D general-purpose coronagraph with a contrast of 10-6. Detailed design of coronagraph will take place during PDR stage. Speckle suppression capability (multi-spectral imaging); dual-channel imager; stability of static errors ~5nm per sqrt(hr) for PSF subtraction or ADI. 4.5Companion Sensitivity Sample 2: Parent stars are T Tauri, J=11. A 1 MJupiter planet is at 300K, J=22, (2 MJupiter is J=19.5). This distribution could have a wider distribution of binaries a) 0.1" separation, J = 8.5 (2MJ) b) 0.2" separation, J = 11 (1MJ) c) Goal J = 11 at 0.1" separation (1MJ) based on properties of the planets you want to look for. Same as #4.4 a) 6 /D general-purpose coronagraph b) 6 /D general-purpose coronagraph c) (Goal) Not achievable with a general purpose coronagraph May need small Inner Working Distance (2 /D) coronagraph. Speckle suppression capability (multi-spectral imaging); dual-channel imager; stability of static errors ~5nm per  EMBED Equation.3  for PSF subtraction or ADI. 4.6Goal: Companion Sensitivity Case 3: at 5 Myr , 1 Msun primary; a) goal J = 13.5 to see 1 MJupiter or b) goal J = 9 for 5 MJupiter. 0.07" is needed. For apparent magnitudes of parent stars see 4.3 Excellent (10-20nm) calibration of both initial LGS spot size and quasi-static non-common path aberrations, at both low- and mid-spatial-frequencies. Needs algorithms such as phase retrieval or speckle nulling (on a fiber source + good stability). Small servo-lag error (<30nm) to avoid scattered light at 0.2 arc sec. Tomography errors 20-30nm. Source: error budget and simulations by Bruce Macintosh. Requires multi-  speckle suppression; very small inner working angle coronagraph (2 /D); static errors in 5-10nm range. 4.7Sensitivity of H=25 for 5-sigma detection in 20 minutes, at 1 arcsec separation from primary star. (Brown dwarf targets are limited by sky background at larger angles, of order ~1 arcsec). Sufficiently high throughput and low emissivity to permit detecting H=25 in 20 minutes at 5 sigma above background. 4.8H-band relative photometry (between primary and companion): accuracy d" 0.1 mag for recovered companions (to estimate mass of the companion); goal of measuring colors to 0.05 mags (0.03 mag per band) to measure temperatures and surface gravities sufficiently accurately (to ~10%).Diagnostics on AO data to measure Strehl fluctuations if it takes a while to move on and off the coronagraph (a possible more attractive solution is a specialized coronagraph that simultaneously images the primary)Induced ghost images of primary; or rapid interleaving of saturated and unsaturated images; or a partially transparent coronagraph4.9Requirement: Astrometric precision 2 mas (~1/10 PSF) relative between primary and planet, for initial rejection of background objects. Goal: For measuring orbits of nearby field objects, want 0.5 mas to measure masses to 10%. Note this gives you mass of primary star. Could be combined with Doppler measurements if thats practical for the brighter objects. Ways to do this: a) Position stability requirement for star behind coronagraph (e.g., stable to 0.5 or 2 mas over 10 min.). b) Induced ghost image method. Needs a wire grating ahead of the coronagraph, or use DM to induce ghost images. (papers by Marois et al. 2006, ApJ, 647, 612; Sivaramakrishnan & Oppenheimer 2006, ApJ, 647, 620).Stability of distortion as required for 0.5 or 2 mas. Also want ghost images of primary (as for photometry #4.8) in order to locate it accurately relative to planet.4.10Efficiency: 20 targets per night (30 goal) [SCRD 2.1.4.6.2]AO system must be able to absolutely steer objects so they land on the coronagraph. This implies 5 mas reproducibility of field steering or lock the tip/tilt to this accuracy relative to coronagraph field stop. Final requirement will depend on the details of the coronagraph (5 mas is consistent with GPI modeling).4.11Observing wavelengths JHK bands (strong goal: Y and z for companion temperature characterization) [SCRD 2.1.4.4, 2.1.4.7.1, RollUp_v1 B5]Transmit JHK to science instrument. Goal: Y and z.JHK filters. Methane band filters for rapid discrimination, Y and z, and/or a custom filter for early characterization.4.12Able to register and subtract PSFs (with wavelength, time, etc.) for post-processing to get rid of residual speckles. Subtraction needs to be sufficient enough to meet req. #4.4. PSF knowledge and/ or stability to meet req. #4.4.At least 1.5 x better than Nyquist sampled at J (goal Y)4.13Field of view: must see companions at 100 AU scales at 30 pc (goal 20 pc) [SCRD 2.1.4.5.3]Field of view 3" radius (goal 5" radius)4.14Characterization of companion [SCRD 2.1.4.4, 2.3]a) R ~150 IFU, sub-Nyquist sampling spectrograph, or if above not available, b) Nyquist spatial sampling IFU, R ~ 4,000, OH suppressing). c) or narrow-band filters. All must be sensitive to J = 22 or 23 in ~3 hrs. 4.15Sky Coverage >30%. (Survey several hundred BDs to H=15 of the ~1000 known targets.) [SCRD 2.1.4.7.3, RollUp_v1 N5]Technical field for low-order wavefront guidestar pickoff large enough to achieve 30% sky coverage at high galactic latitude. Ability to acquire and track 3 tip/tilt stars. (More lenient if parent star can be used as one of the three TT stars.) Or ability to measure everything sufficiently with a single H=15 TT star (pyramid sensors).4.16The following observing preparation tools are required: guide star finder for high proper-motion stars Asteroid Companions Survey The requirements for the asteroid companions survey science case are summarized in the following table (see also the Multiplicity of Minor Planets section of KAON 455 (Release 2.1)). Table 5. Asteroid Companions Survey driven requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements5.1The companion sensitivity shall be J e" 5.5 mag at 0.5 separation for a V d" 17 asteroid (Jd" 15.9) (asteroid size < 0.2 ) with a proper motion of d" 50 arcsec/hour [ScRD 2.5.4.6]The asteroid can be used as tip/tilt guidestar (proper motion of d" 50 arcsec/hour). The AO system has sufficient field of view for objects and for their seeing disks (>3 arcsec, see # 5.6). The tip-tilt residual error will be less than 10 mas (limited by resolved primary) while guiding on one V=17 (J =15.9) object with relative motion of 50 arcsec/hr (14 mas/sec). The AO system has sufficient Strehl to achieve this contrast ratio and sensitivity in 15 min exposure time. KAON 529 suggests that 170nm wavefront error will suffice.Near-IR imager5.2J-band relative photometric accuracy (between primary and companion) of 5% at 0.6 for J = 3 for a V d" 17 (Jd" 15.9) asteroid (asteroid size < 0.2 ) with a proper motion of d" 50 arcsec/hour [ScRD 2.5.4.4]Near- IR imager (no coronagraph because many asteroids will be resolved)5.3Target sample e" 300 asteroids in d" 4 yr. [SCRD 2.5.3 4] Leads to requirement of e" 25 targets per 11 hour night. [SCRD 2.5.5.2]Assumes 3 good nights per year. Needs high observing efficiency: Able to slew to new target and complete the entire observation within 26 minutes on average.5.4Observing wavelengths I through H bands, for optimum companion sensitivity [Source: KAON 529]. J band is best when seeing is good. H band could be used when seeing is poor. [SCRD 2.5.6.6]Visible and IR imagers.5.5Spatial sampling d" Nyquist at each observing wavelength. [SCRD 2.5.6.4] Pixel sampling of l/3D optimal for photometry and astrometry [KAON 529].Spatial sampling d" Nyquist at the observing wavelength. Pixel sampling of l/3D is optimal at J through H-bands, and l/2D at I through z-band for both photometry and astrometry [see KAON 529]. 5.6Field of view e" 3 diameter [SCRD 2.5.6.2]AO system passes a >3 unvignetted field of viewImager fields of view e" 3 5.7The following observing preparation tools are required: guide star finder for asteroids too faint to use as the only TT star, PSF simulation as function of wavelength and seeing conditions. Guide star finder tool. PSF simulation tool (predict energy and width of central core to within 10%). 5.8The following data products are required: Access to archive with proper identification in World Coordinate System (to within 1 arc sec or better) and with associated calibrated PSF.Calibrated PSF capability. Accuracy requirement will be discussed in future releases of the SCRD document. Ability to collect AO telemetry data to support the required PSF calibration. FITS header system capable of handling non-sidereal offsets in reporting object coordinates in the World Coordinate System to within 1 arc sec or better.5.9Observing requirements: Observer present either in person or via remote observing rooms, because real-time observing sequence determination is needed.Classical observing mode or service mode with active observer participation. Remote observing capabilities must allow frequent real-time decisions by observer.  Asteroid Companions Orbit Determination The requirements for the asteroid companions orbit determination science case are summarized in the following table (see also the Multiplicity of Minor Planets section of KAON 455 (Release 2.1)). Table 6. Asteroid Companions Orbit Determination driven requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements6.1Companion sensitivity in the near-IR. Same as #5.1 Same as #5.1 Near-IR imager.6.2The companion sensitivity in the visible shall be I e" 7.5 mag at 0.75 separation for a V d" 17 (I d" 16.1) asteroid (asteroid size < 0.2 ) with a proper motion of d" 50 arcsec/hour [ScRD 2.5.4.6]Visible Imager. Optimum visible wavelength is I through z bands per KAON 529. Note that if the near-IR imager extends down to I band, a separate visible imager would not be needed for this science case.6.3Photometric accuracy: Same as #5.2Same as #5.26.4I-band relative astrometric accuracy of d" 1.5 mas for a V d" 17 (J d" 15.9) asteroid (asteroid size < 0.2 ) with a proper motion of d" 50 arcsec/hour [SCRD 2.5.4.5]Non-sidereal tracking accuracy sufficiently small to achieve I-band astrometric accuracy d" 1.5 mas for a V d" 17 (J d" 15.9) asteroid with a proper motion of d" 50 arcsec/hourUncalibrated detector distortion sufficiently small to achieve I-band astrometric accuracy d" 1.5 mas for a V d" 17 (J d" 15.9) asteroid6.5Target sample size of e" 100 asteroids in d" 3 years. [SCRD 2.5.3 4] Leads to requirement of e" 25 targets in an 11 hour night. [SCRD 2.5.5.2]Needs high observing efficiency: Able to slew to new target and complete the entire observation within 25 minutes on average. Will generally only observe at one wavelength (the one that gives the best astrometric information).6.6Observing wavelengths = I, z, J, H bands. (Note: R-band may become a future requirement if R-band Strehl > 15%) [SCRD 2.5.6.6]Imager(s) covering range I, z, J, H bands. Note that if the near-IR imager extends down to I band, a separate visible imager would not be needed for this science case.6.7Spatial sampling same as #5.5Same as #5.56.8Same as #5.6 Same as #5.6Same as #5.66.9Same as #5.7Same as #5.76.10Same as #5.8See #5.86.11Observing requirements: 7 epochs per target [SCRD 2.5.3 4]Observing model needs to accommodate split nights or some level of flexibility. QSO Host Galaxies The requirements for the QSO Host Galaxy science case are summarized in the following table (see also the QSO Host Galaxy section of KAON 455 (Release 2.1)). The typical QSO that we are considering is at redshift 2. Typical galaxy sizes are 0.5 to 2 arc sec. Contrast ratios between the central point source and a galaxy region arc sec away range from 50 to 200 or more. The scientific goals are the following: 1) measure colors and magnitudes for the point source; 2) measure morphology and surface brightness profile for the galaxy; 3) obtain spectrum of point source; 4) obtain spatially resolved spectrum of galaxy in order to study its kinematics and stellar populations. In order to accomplish these things, accurate PSF subtraction will be crucial. Table 7. QSO Host galaxies derived requirements Future releases of the SCRD will quantify the requirements for PSF subtraction and stability, required spatial resolution, and coronagraph design. The following table outlines the issues and should be viewed as a place-holder. #Science Performance RequirementAO Derived RequirementsInstrument Requirements7.1Number of targets required: to be specified in future versions of the SCRDSky coverage fraction >30% for 50% enclosed energy within 0.05 arc sec at J band7.2Required wavelength range: 0.85 2.4 micronsNear IR IFU spectrograph; near IR and visible imagers.7.3Required spatial resolution will be discussed in a future release of this document. Will be determined by considerations of PSF subtraction accuracy. Hence required resolution will be higher than in the high-z galaxy science case.Desirable to use central QSO point source as one of the tip-tilt reference stars, if possible.PSF must be oversampled in order to achieve required subtraction accuracy. Quantitative requirements will be discussed in future releases of the SCRD.7.4Photometric accuracy and PSF knowledge required for subtracting the central point source in order to characterize the host galaxy must be adequate to obtain host galaxy colors to 20% for a contrast ratio of up to 200 at a distance of arc sec from the point source.Requires excellent PSF stability and knowledge; future releases of the SCRD will discuss the quantitative requirements. Will have implications for required AO wavefront error, AO stability, and required signal to noise ratio.Required calibration stability and accuracy, zero-point stability and knowledge, quality of flat-fielding will be discussed quantitatively in future releases of the SCRD. PSF must be oversampled in order to achieve required subtraction accuracy. Quantitative requirements will be discussed in future releases of the SCRD.7.5SNR for spatially resolved spectroscopy of the host galaxy will be determined by accuracy of PSF subtraction and by minimization of scattered light from the central point source. May benefit from specialized coronagraph design to block light from central point source.7.6Required observation planning tools (e.g. guide stars); PSF simulation tools to plan for whether PSF subtraction will be good enough to see the host galaxy7.7Required data reduction pipeline for IFU Gravitational Lensing The requirements for the gravitational lensing science case are summarized in the following four tables (see the Gravitational Lensing section of KAON 455 (Release 2.1)). Table 8a. Imaging studies of distant galaxies lensed by galaxies Goal: screen potential lensed-galaxy targets for more detailed and lengthy spectroscopic study. #Science Performance RequirementAO Derived RequirementsInstrument Requirements8a.1Sensitivity: SNR e" 3 per pixel (100 per source) for a z = 1  2 galaxy in an integration time d" 1/2 hour. Background due to emissivity less than 30% of unattenuated (sky + tel). 8a.2Target sample size of e" 200 galaxies, with density on the sky of 10 per square degree. Survey time ~ 3 years.Overhead less than 10 min between targets.10 per square degree implies that you will only be able to observe one target at a time average of 1 in every ~19x19 patch.8a.3Observing wavelengths = I through K (to 2.4 m). Emphasis is on shorter wavelengths. Thermal part of K band less important. [SCRD 3.2.6.5]8a.4Spatial resolution better than 50 mas at J band, for 30% sky coverage.Need a good model of the PSF or a simultaneous image of a PSF star. Need a figure of merit for goodness of the PSF: how well the model fits the real PSF in two dimensions. Will quantify in future releases of the SCRD.Nyquist sampling of pixels at each wavelength.8a.5Field of view > 15 diameter for survey. Bigger is better. Some degradation between center and edge of field is tolerable. Will quantify in future releases of the SCRD. [SCRD 3.2.6.2]8a.6Relative photometry to d" 0.1 mag for observations during a single night [SCRD 3.2.4.4]8a.7Absolute photometry d" 0.3 mag [SCRD 3.2.4.4]8a.8Sky coverage at least 30% with enclosed energy radius within 0.07 arc sec at H or K. [SCRD 3.2.4.9]8a.9Dithering and offset considerations: 1) Initially should be able to center a galaxy to d" 10% of science field of view. 2) Should know the relative position of the galaxy after a dither to d" 20% of pixel size.8a.10The following observing preparation tools are required: PSF simulation and exposure time calculator8a.11The following data products are required: accurate distortion map (to 1% of the size of the galaxy, or 0.01 arc sec rms) Table 8b. Spectroscopic studies of distant galaxies lensed by galaxies #Science Performance RequirementAO Derived RequirementsInstrument Requirements8b.1SNR e" 10 for a z = 1  2 galaxy in an integration time d" 3 hours for a Gaussian width 20 km/sec Gaussian width (50 km/sec FWHM) with a spatial resolution of 50 masBackground due to emissivity less than 30% of unattenuated (sky + tel). R ~ 5000 (or whatever is needed to achieve 20 km/sec sigma on these targets)8b.2Target sample size of e" 50 galaxies, with density on the sky of 10 per square degree. Survey time ~ 3 years.Number of IFUs: at least one, plus preferably one to monitor the PSF and one to monitor the sky. The extra two IFUs could be dispensed with if there were other ways to monitor the PSF and the sky background.8b.3Observing wavelengths = J, H and K (to 2.4 m) required, with emphasis on J band. Goal: also use z and I bands. [SCRD 3.2.6.5]8b.4Spectral resolution: whatever is needed to get 20 km/sec radial velocity Gaussian sigma8b.5Spatial resolution 50 mas at J band8b.6Velocity determined to d" 20 km/sec Gaussian sigma for spatial resolutions of 50 masRequired level of PSF knowledge will be assessed in future releases of the SCRD. 8b.7Field of view: Typical lens is 2 to 6 arc sec diameter. For IFU fields of view smaller than the lens size, one would use mosaicing. Desirable to take in blank sky in addition to the lens (if possible). Requirement: FOV ( 3 diameter. Goal: ( 4 diameter. [SCRD 3.2.6.2]Requirement: IFU FOV ( 3 diameter. Goal: ( 4 diameter.8b.8Simultaneous sky background measurementsPreferably sky determination within the field of view of the IFU. Less preferably, through use of offsetting to sky or via a separate IFU looking at sky.8b.9Relative photometry to d" 0.1 mag for observations during a single night [SCRD 3.2.4.4]8b.10Absolute photometry d" 0.3 mag [SCRD 3.2.4.4]8b.11Sky coverage at least 30% with enclosed energy radius within 50 mas at J band. [SCRD 3.2.4.9]8b.12Dithering and offset considerations: 1) Initially should be able to center a galaxy to d" 10% of science field of view. 2) Should know the relative position of the galaxy after a dither to d" 20% of spaxel size.8b.13Target drift should be d" 10% of spaxel size in 1 hr8b.14The following observing preparation tools are required: PSF simulation and exposure time calculator8b.15The following data products are required: calibrated spectral data cube Table 9a. Imaging studies of distant galaxies lensed by clusters Table 9b. Spectroscopic studies of distant galaxies lensed by clusters Astrometry Science in Sparse Fields Text and tables will be included in a future release of the SRD. This science case will be a driver for low and/or very well calibrated instrument distortions, compensation for atmospheric differential refraction, and good temperature control of the AO system. Table 10. Astrometry Science in Sparse Fields derived requirements Resolved Stellar Populations in Crowded Fields Text and tables will be included in a future release of the SRD. Table 11. Resolved Stellar Populations in Crowded Fields derived requirements Debris Disks Text and tables will be included in a future release of the SRD. This science case will be a driver for coronagraph design. Table 12. Debris Disks derived requirements Young Stellar Objects Text and tables will be included in a future release of the SRD. This science case may be a driver towards having an infrared wavefront sensor. Table 13. Young Stellar Objects derived requirements Asteroid Size, Shape, and Composition The requirements for the asteroid size and shape (characterize surface and orbital parameters) science case are summarized in the following table. In addition to the requirement of a high resolution visible imager, the slope of the visible spectrum is needed to determine the asteroid age or surface type. This case requires a spectral resolution of R ~ 100 for 0.7 1.0 m wavelength with Nyquist sampling. If R ~ 100 is not available, some of this work can be achieved either with multiple narrow-band filters or with a higher-resolution spectrograph. Table 14. Asteroid size, shape, and composition derived requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements14.1Target sample size of e" 300 asteroids in d" 3yrs years. < 10 targets in an 11 hour night [SCRD 3.6.3]#6.5 is stricter requirement.14.2Observing wavelengths 0.7  1.0 m. Strong preference for R band because optimum to obtain shape of asteroid. [SCRD 3.6.6.6]AO system must pass 0.7 to 1.0 micron wavelengthsImagers (R through J band) with narrow-band filters or slit spectrograph (R~100), or possibly visible IFU (R~100).14.3Spatial sampling same as #5.5Same as #5.5Same as #5.514.4Field of view e" 3 diameter [SCRD 3.6.6.2]Same as #6.8Same as #6.814.5Ability to measure the spectral slope with R ~ 100 at 0.85-1.0 mm [SCRD 3.6.6.7]14.6Ability to measure the SO2 frost bands at R=1000 (R=5000 is acceptable) at 1.98 and 2.12 mm, crystalline ice band at 1.65 microns. [SCRD 3.6.6.7]Spectroscopic imaging at R~1000 to 5000 in the H and K bands. 14.7Same as #5.7Same as #5.714.8Same as #5.8Same as #5.8Gas Giant Planets The requirements for the Gas Giants science case (all three goals) are summarized in the following table (see the section on Characterization of Gas Giant Planets of KAON 455 (Release 2.1)). Table 15. Gas Giants derived requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements15.1Capability of tracking a moving target with rate up d" 50 arcseconds per hour (14 mas/second) [SCRD 3.7.5.1]15.2Capability of using at least one tip-tilt star that is moving with respect to the (moving) target planet. (For example, a moon of Jupiter or Saturn) [SCRD 3.7.5.1]Motion of low order wavefront sensor to track tip-tilt star.15.3Ability to acquire Io within 5 of Jupiter and to track it to within 2.5 of Jupiter. Note that this is a goal but perhaps not a rigid requirement: we know we can acquire within 10 today.May require either a diaphragm or a filter to attenuate the light from Jupiter.See AO derived requirement.15.4Sensitivity: comparable to the current Keck system15.5Absolute Photometric accuracy: comparable to the current Keck system (d" 0.05 mag) [SCRD 3.7.4.4]PSF knowledge Detector flat-fielding requirements, linearity, etc will flow down from required photometric accuracy. 15.6Targets: Jupiter and Saturn systems, with special focus on Io and TitanAO system capable of working in the presence of scattered light from nearby extended objects; NGS option for bright moonsJupiter & Saturn: near-IR imager from 0.8-2.4 m Io: IFU 0.8-2.4 Titan: IFU 0.8-2.4 m15.7Observing wavelengths I, z/Y, J, H, K [SCRD 3.7.6.5]AO system must pass these wavelengths to science instruments.Near- IR imager and IFU spectrometer, l= 0.8-2.4 m15.8Spatial sampling: for imager, d"Nyquist at the observing wavelengthFor imager, spatial sampling d" Nyquist at the observing wavelength. For IFU, spatial sampling ~l/D.15.9Imager field of view e" 30 diameter at K band, e" 20 diameter at J and H bands (goal 30 ) [SCRD 3.7.6.1]AO system passes a >30 unvignetted field of viewImager field of view e" 30 diameter at K band, e" 20 diameter at J and H bands (goal 30 )15.10IFU field of view as large as possible, up to 15 (Jupiter s diameter is 30, Great Red Spot is 13 diameter) [SCRD 3.7.6.1]If IFU FOV is only a few arc sec, desirable to be able to place different IFUs as close together as possible. No firm numerical requirement.15.11Moons are very bright: do not allow saturation. Typical brightness: 5 mag per square arc sec.Either need to use neutral density filters, or have a fast shutter, or have a detector with large wells or very short exposure times (and low read noise). Note: these observations will have high overhead.15.12The following observing preparation tools are required: PSF simulation, target ephemeris, exposure time calculator to enable choice of ND filter and exposure time.15.13The following data products are required: Calibrated PSF.15.14Observing requirements: Io and Titan are time domain targets; Io requires d" 1 hr notification of volcano activity. Typical timescales for clouds on Titan are of order days to weeks. Ice Giants: Uranus and Neptune The requirements for the Ice Giants science case (all four goals) are summarized in the following table (see the section on Characterization of Ice Giant Planets of KAON 455 (Release 2.1)). Table 16. Ice Giants derived requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements16.0Capability of tracking a moving target with rate up d" 5.0 arcseconds per hour (1.4 mas/sec) [SCRD 3.8.5.1]" The planet can be used as tip/tilt guidestar (proper motion of d" 5.0 arcsec/hour). " The AO system requires sufficient field of view for planets and for their seeing disks (>5 arcsec). The tip-tilt residual error will be less than 10 mas (limited by resolved primary) while guiding on one planet at 5.0 arcsec/hr (1.4 mas/sec). 16.1Sensitivity: comparable to the current Keck systemNear-IR imager, 0.8 - 2.4 m16.2Photometric accuracy: comparable to the current Keck system [SCRD 3.8.4.5]Near- IR imager16.3Targets: Uranus and Neptune systems. Observations of atmospheric vertical structure will require a near-IR IFU, to be described in more detail in a future release of the SCRD.AO system (both LGS and NGS) capable of correcting on extended objects. Uranus = 3.4 arcsec Neptune = 2.3 arcsecNear-IR imager, 0.8 2.4 m, Near-IR IFU 1.0 2.4 m16.4Observing wavelengths: J, H, K [SCRD 3.8.6.5]Near- IR imager, Near-IR IFU16.5Spatial sampling: d"Nyquist at the observing wavelengthsSpatial sampling d" Nyquist at the observing wavelength16.6Imager field of view: e" 15 diameter [SCRD 3.8.6.2]AO system passes a >15 unvignetted field of viewImager fields of view e" 15 16.7IFU field of view: as large as possible, up to e" 15 diameter [SCRD 3.8.6.2]If IFU FOV is only a few arc sec, desirable to be able to place different IFUs as close together as possible. No firm numerical requirement.16.8Spectral resolution: R e" 3000 to resolve methane absorption features. [SCRD 3.8.6.6]Near-IR IFU with R~300016.9Observing requirements: one run per semester with at least 4 contiguous (partial) nights; both targets can be studied during one run16.10The following observing preparation tools are required: PSF simulation, target ephemeris, exposure time calculator to enable choice of ND filter and exposure time.16.11The following data products are required: Calibrated PSF.16.12Observing requirements: some science goals would be well suited to queue or service observing modes  Other: Backup Science This will primarily be NGS science that can be done when the lasers cannot be propagated (e.g. due to cirrus), or less-demanding examples of LGS science that can be done when the laser power available is lower than nominal due to hardware problems. The derived requirements for Backup Science will largely involve science preparation and operations issues. Table 17. Backup Science Observing Modes: NGS #Science Performance RequirementAO Derived RequirementsInstrument Requirements17.1NGS mode. NGS as a backup observing mode for when conditions restrict propagation of the lasers.17.2Sky coverage e"5% to ensure at least one-sixth of the off-axis LGS targets will still be observable if it is necessary to go to an NGS backup mode. Assuming b=30, For 5% sky coverage: R=14 mag guide star with 60 diameter field of regard (FOR) R=15 mag guide star with 45 diameter FOR [Keck Observatory Report No. 208, p. 4-100]17.3Capability to switch between NGS and LGS modes in d" 15 minutes (not including target acquisition) to enable flexibility if conditions change.17.4Sensitivity. SNR e" 10 for a z = 2.6 galaxy in an integration time d" 3 hours for a spectral resolution R = 3500 with a spatial resolution of 50 mas Sufficiently high throughput and low emissivity of the AO system science path to achieve this sensitivity. Background due to emissivity less than 30% of unattenuated (sky + tel).17.5Observing wavelengths = J, H and K (to 2.4 m) AO system must transmit J, H, and K bandsInfrared single IFU and imager designed for J, H, and K.17.6Spectral resolution = 3000 to 4000Spectral resolution of >3000 in IFU17.7Imaging: Nyquist sampled at H-bandNyquist sampled IR imager (at H-band)17.8Encircled energy 50% in 70 mas for a bright NGS guide star within 10 arc sec Wavefront error sufficiently low (~170 nm) to achieve the stated requirement in J, H, and K bands.Optimum spaxel size will be determined during a detailed study of the IFU instrument.17.9If a new instrument: IFU field of view e" 1 x 3 to allow simultaneous background measurements while observing a 1 galaxy. OSIRIS FOV would be adequate.Narrow relay passes 1 x3 fieldIf a new instrument: IFU field of view e" 1 x 3 to allow simultaneous background measurements while observing a 1 galaxy. OSIRIS FOV would be adequate.17.10Imager FOV e" 10 x 10 for galactic center and gravitational lensing scienceImager FOV e" 10 x 10 17.11Relative photometry to d" 5% for observations during a single night, provided the night is photometric Knowledge of ensquared energy in IFU spaxel to 5%. 17.12Should be able to initially center a galaxy to d" 10% of science field of view17.13Should know the relative position of the galaxy to d" 20% of spaxel or pixel size17.14Target drift should be d" 10% of spaxel size in 1 hr17.15The following observing preparation tools are required: NGS guide star finding tool; PSF simulation and exposure time calculator17.16The following data products are required: calibrated spectral data cube Asteroid Companions Survey The requirements for the asteroid companions survey science case are summarized in the following table (see also the Multiple Asteroids 1: Survey mode to find new systems Observing Scenario). Table 5. Asteroid Companions Survey driven requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements5.1The companion sensitivity shall be J e" 5.5 mag at 0.5 separation for a V d" 17 asteroid (Jd" 15.9) (asteroid size < 0.2 ) with a proper motion of d" 50 arcsec/hour [ScRD 2.1.5.4.6, RollUp_v1 F3]The asteroid can be used as tip/tilt guidestar (proper motion of d" 50 arcsec/hour). The AO system has sufficient field of view for objects and for their seeing disks (>3 arcsec, see # 5.8). The tip-tilt residual error will be less than 10 mas (limited by resolved primary) while guiding on one V=17 (J =15.9) object at 50 arcsec/hr (14 mas/sec). The AO system has sufficient Strehl to achieve this contrast ratio and sensitivity in 15 min exposure time. (need further simulations to state wavefront error requirement. ~170nm?)Near-IR imager5.2J-band relative photometric accuracy (between primary and companion) of 5% at 0.6 for J = 3 for a V d" 17 (Jd" 15.9) asteroid (asteroid size < 0.2 ) with a proper motion of d" 50 arcsec/hour [ScRD 2.1.5.4.4, RollUp_v1 H3]System has facilities and tools for calibrating the PSF to within xxx percent during one observation. (This is likely the width of the peak for astrometry. For photometry?)Near- IR imager (no coronagraph because many asteroids will be resolved)5.3Target sample e" 300 asteroids in d" 4 yr [SCRD 2.1.5.3 4] Leads to requirement of e" 25 targets per 11 hour night [SCRD 2.1.5.5.2, RollUp_v1 M3] Assumes 3 good nights per year. Needs high observing efficiency: Able to slew to new target and complete the entire observation within 26 minutes on average.5.4Observing wavelengths = J and H-band (R-band pending simulations) [SCRD 2.1.5.6.6, RollUp_v1 B3]Transmit R through z to visible imager, z through H to IR imager. Visible and IR imagers.5.5Spatial sampling d" Nyquist at the observing wavelength. [SCRD 2.1.5.6.4] Spatial sampling d" Nyquist at the observing wavelength (l/3D is optimal for both photometry and astrometry). 5.6Field of view e" 3 diameter [SCRD 2.1.5.6.2]AO system passes a >3 unvignetted field of viewImager fields of view e" 3 5.7The following observing preparation tools are required: guide star finder for asteroids too faint to use as the only TT star, PSF simulation as function of wavelength and seeing conditions.Guide star finder tool. PSF simulation tool (predict energy and width of central core to within 10%). 5.8The following data products are required: Access to archive with proper identification in World Coordinate System (to within 1 arc sec or better) and with associated PSF calibrated to within xxx %.Calibrated PSF capability (to what accuracy? Why) Ability to collect AO telemetry data to support the required PSF calibration. FITS header system is capable of handling non-sidereal offsets in reporting object coordinates in the World Coordinate System to within 1 arc sec or better.5.9Observing requirements: Observer present either in person or via remote observing rooms, because real-time observing sequence determination is needed.Classical observing mode or service mode with active observer participation. Remote observing capabilities must allow frequent real-time decisions by observer. The requirements for the asteroid companions survey science case are summarized in the following table (see the Multiplicity, Size and Shape of Minor Planets section of KAON 455 (V1) and the Multiple Asteroids 1: Survey mode to find new systems Observing Scenario). #Science Performance RequirementAO Derived RequirementsInstrument Requirements1The companion sensitivity shall be H e" 5.5 mag at 0.5 separation for a V d" 17 asteroid (asteroid size < 0.2 ) with a proper motion of d" 50 arcsec/hourAssuming using just the asteroid for tip/tilt. Strehl ratio. PSF is calibrated. Ability to track on non-sidereal objects (assumes asteroid used for tip/tilt). AO requirements are modest compared to other companion sensitivity science cases. Near-IR imager2H-band relative photometric (between primary and companion accuracy) of d" 0.05 mag at 0.6 for H = 3 for a V d" 17 asteroid (asteroid size < 0.2 ) with a proper motion of d" 50 arcsec/hourPSF is calibrated.Near- IR imager (no coronagraph)3H-band relative astrometric accuracy of d" 10 mas for a V d" 17 asteroid (asteroid size < 0.2 ) with a proper motion of d" 50 arcsec/hourUncalibrated detector distortion < 1.5 mas SNR e" 100 on primary4Target sample size of e" 300 asteroids in d" 4 years5e" 25 targets in an 11 hour nightObserving efficiencyObserving efficiency6Observing wavelengths = J and H-bandTransmit J and H to science instrument.J and H-band filters and sensitivity.7Spatial sampling d" Nyquist at J-bandd" 12 mas pixels8Field of view e" 3 diametere" 300 x 300 pixels9The following observing preparation tools are required: guide star finder, field of view, PSF simulation.Guide star finder tool. PSF simulation tool.10The following data products are required: Calibrated PSF. Access to archive with proper identification in World Coordinate System.Calibrated PSF capabilityFITS header11Observing requirements: Observer present. Need to know when night will be.Classical observing mode or service mode with observer participation Asteroid Companions Orbit Determination The requirements for the asteroid companions orbit determination science case are summarized in the following table (see also the Multiple Asteroids 2: Orbits determination for the discovered system Observing Scenario). Table 6. Asteroid Companions Orbit Determination driven requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements6.1Companion sensitivity in the near-IR. Same as #5.1 Same as #5.1 Near-IR imager6.2The companion sensitivity in the visible shall be I e" 7.5 mag at 0.75 separation for a V d" 17 (I d" 16.1) asteroid (asteroid size < 0.2 ) with a proper motion of d" 50 arcsec/hour [ScRD 2.1.5.4.6, RollUp_v1 F3] Imager [need simulations for wavelength range]6.3Photometric accuracy: Same as #5.2Same as #5.26.4I-band relative astrometric accuracy of d" 1.5 mas for a V d" 17 (J d" 15.9) asteroid (asteroid size < 0.2 ) with a proper motion of d" 50 arcsec/hour [SCRD 2.1.5.4.5, RollUp_v1 I3]Non-sidereal tracking accuracy <10 mas. Thoughput, emissivity to the guider sufficient to achieve SNR e" 400 on the primary in <1 second. [Do we need this additional requirement on SNR if the non-sidereal tracking accuracy is < 10 mas? And where does the <1 sec requirement come from?]Uncalibrated detector distortion < 1.5 mas (Is this an edge to edge number? Over xxx pixels? Need to be more explicit.)6.5Target sample size of e" 100 asteroids in d" 4 years [SCRD 2.1.5.3 4]. Leads to requirement of e" 25 targets in an 11 hour night. [SCRD 2.1.5.5.2, RollUp_v1 M3]Needs high observing efficiency: Able to slew to new target and complete the entire observation within 25 minutes on average. Will generally only observe at one wavelength (the one that gives the best astrometric information).6.6Observing wavelengths = R, I, J or H-band (shorter wavelengths preferred, pending simulations) [SCRD 2.1.5.6.6, RollUp_v1 B3](Note: R-band may become a future requirement if R-band Strehl > 15%)Near-IR imager (R-band imager TBD)6.7Spatial sampling same as #5.5Same as #5.56.8Same as #5.6 Same as #5.6Same as #5.66.9Same as #5.7Same as #5.76.10Same as #5.8See #5.86.11Observing requirements: 7 epochs per target [SCRD 2.1.5.3 4]Observing model needs to accommodate split nights or some level of flexibility. QSO Host Galaxies The requirements for the QSO Host Galaxy science case are summarized in the following table (see the QSO Host Galaxy section of KAON 455 (V1)). The typical QSO that we are considering is at redshift xxx, had a magnitude yyy point source in the center, with a host galaxy of magnitude zzz per square arc sec. The galaxy is TBD arc sec across. [Say something about the profile of the galaxy] The scientific goals are the following: 1) measure colors and magnitudes for the point source; 2) measure morphology and surface brightness profile for the galaxy; 3) obtain spectrum of point source; 4) obtain spatially resolved spectrum of galaxy in order to study its kinematics and stellar populations. In order to accomplish these things, PSF subtraction will be crucial. [This is a derived requirement.] Table 7. QSO Host galaxies derived requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements7.1Number of targets required: sample size of TBD galaxies in TBD nights or yearsRequirement on sky coverage fraction may be implied here, particularly if data from space missions or radio surveys is required7.2Required signal to noise ratio for imaging of central point source: TBD at TBD wavelengthAO Strehl ratio > TBD AO background level < TBD; over TBD wavelength rangeInstrument background level; Need to be background limited (implications for detector)7.3Photometric accuracy required for imaging the central point source: TBD at TBD wavelengths. PSF stability and knowledge, temporal and field of view [uniformity trade]; Target drift should be d" TBD mas per hourCalibration stability and accuracy, Zero-point stability and knowledge, Quality of flat-fielding7.4Required SNR for spatially resolved spectroscopy of the point source > TBD at TBD wavelengthsAO Strehl ratio > TBD AO background level < TBD; over TBD wavelength range; PSF stability and knowledge, temporal and field of view [uniformity trade]; Target drift should be d" TBD mas per hour[What spatial sampling is optimum for good PSF subtraction?], spectral resolution R ~ TBD; detector limited SNR performance; FOV = TBD arc sec [e.g. larger for sky subtraction]7.5Required signal to noise ratio for imaging of host galaxy in presence of point source: TBD at TBD wavelength at TBD distance from the point sourceAO Strehl ratio > TBD AO background level < TBD; over TBD wavelength range; PSF stability and knowledge, temporal and field of view [uniformity trade]; Spatial sampling TBD 7.6Photometric accuracy required for imaging the host galaxy: TBD at TBD wavelengths at TBD distance from point source. AO Strehl ratio > TBD AO background level < TBD; over TBD wavelength range; PSF stability and knowledge, temporal and field of view [uniformity trade];Target drift should be d" TBD mas per hourCalibration stability and accuracy, Zero-point stability and knowledge, Quality of flat-fielding; FOV = TBD arc sec [e.g. larger for sky subtraction]7.7Required SNR for spatially resolved spectroscopy of the host galaxy > TBD; spatial resolution = TBD; velocity resolution and accuracy = TBD; wavelength range TBDAO Strehl ratio > TBD AO background level < TBD; over TBD wavelength range; PSF stability and knowledge, temporal and field of view [uniformity trade]; AO 80% enclosed energy radius = TBD; Target drift should be d" TBD mas per hourFOV = TBD; spectral resolution = TBD; spatial sampling (spaxel size); detector-limited performance; Calibration stability and accuracy, Zero-point stability and knowledge, Quality of flat-fielding; Requirement on persistence? Required minimum trade between single-shot spectral coverage and field of view7.8Required observation planning tools (e.g. guide stars); PSF simulation tools to plan for whether PSF subtraction will be good enough to see the host galaxy7.9Required data reduction pipeline for IFU Gravitational Lensing The requirements for the gravitational lensing science case are summarized in the following four tables (see the Gravitational Lensing section of KAON 455 (Release 2)). Tables for the galaxies lensed by galaxies will be included in a future release of the SCRD. Table 8a. Imaging studies of distant galaxies lensed by galaxies Goal: screen potential lensed-galaxy targets for more detailed and lengthy spectroscopic study. #Science Performance RequirementAO Derived RequirementsInstrument Requirements8a.1SNR e" 3 per pixel (100 per source) for a z = 1  2 galaxy in an integration time d" 1/2 hour. Strehl > 0.3 at J band. 8a.2Target sample size of e" 200 galaxies, with density on the sky of 10 per square degree. Survey time ~ 3 years.Overhead less than 10 min between targets.10 per square degree implies that you will only be able to observe one target at a time average of 1 in every ~19x19 patch.8a.3Observing wavelengths = J, H and K (to 2.4 m). Emphasis is on shorter wavelengths. Could use z if available. Thermal part of K band less important.8a.4Spatial resolution better than 50 masNeed a good model of the PSF or a simultaneous image of a PSF star. Need a figure of merit for goodness of the PSF: how well the model fits the real PSF in two dimensions. Need Nyquist sampling of pixels at each wavelength.8a.5Field of view > 15 diameter for survey. Bigger is better. Some degradation between center and edge of field is tolerable. (Need to quantify.)8a.6Relative photometry to d" 0.1 mag for observations during a single night8a.7Absolute photometry d" 0.3 mag8a.8Sky coverage at least 50% with enclosed energy radius within 0.1 arc sec at H or K. Sky coverage should be better than with current LGS.8a.9Should know the relative position of the galaxy to d" TBD of spaxel size. (Whatever works for high z galaxy case)8a.10The following observing preparation tools are required: 8a.11The following data products are required: accurate distortion map (to 1% of the size of the galaxy, or 0.01 arc sec rms) Table 8b. Spectroscopic studies of distant galaxies lensed by galaxies #Science Performance RequirementAO Derived RequirementsInstrument Requirements8b.1SNR e" 10 for a z = 1  2 galaxy in an integration time d" 3 hours for a Gaussian width 20 km/sec Gaussian width (50 km/sec FWHM) with a spatial resolution of 50 masR ~ 5000 (or whatever is needed to achieve 20 km/sec sigma on these targets)8b.2Target sample size of e" 50 galaxies, with density on the sky of 10 per square degree. Survey time ~ 3 years.Number of IFUs: at least one, plus preferably one to monitor the PSF and one to monitor the sky. The extra two IFUs could be dispensed with if there were other ways to monitor the PSF and the sky background.8b.3Observing wavelengths = J, H and K (to 2.4 m). Emphasis is on shorter wavelengths. Would use z and I bands if available. 8b.4Spectral resolution: whatever is needed to get 20 km/sec radial velocity Gaussian sigmaSpectral resolution8b.5Spatial resolution 50 mas[need to make the spatial resolution and the enclosed energy requirements consistent with each other]8b.6Velocity determined to d" 20 km/sec Gaussian sigma for spatial resolutions of 50 masPSF intensity distribution known to d" TBD% per spectral channel. 8b.7Field of view > 4 diameter (lenses are bigger than galaxies). Typical lens is 3 to 4 arc sec diameter.8b.8Simultaneous sky background measurements8b.9Relative photometry to d" 0.1 mag for observations during a single night8b.10Absolute photometry d" 0.3 mag8b.11Sky coverage at least 50% with enclosed energy radius within TBD mas. Sky coverage should be better than with current LGS.8b.12Should be able to center a galaxy to d" TBD of science field of view8b.13Should know the relative position of the galaxy to d" TBD of spaxel size. (Whatever works for high z galaxy case is OK here as well)8b.14Target drift should be d" TBD of spaxel size (Whatever works for high z galaxy case is OK here as well)8b.15The following observing preparation tools are required: 8b.16The following data products are required: calibrated spectral data cube Table 9a. Imaging studies of distant galaxies lensed by clusters Table 9b. Spectroscopic studies of distant galaxies lensed by clusters Notes: Wide field: Typical size of the highly magnified region of a cluster is 1 arc min. Need low background: lens arcs from z ~ 7 are at most Vega magnitude 23 or 24 in H (brightest arcs). Typical size small (half light radii 0.1 arc sec). Closer galaxies with giant arcs: deployable IFU application. Several arc sec long. Want field of regard of about an arc min. Usually 3 to 5 multiple arcs within a square arc min. (But each might be long, and require more than 1 IFU unit.) Less than 10 IFU units needed in a square arc min. Is a requirement needed on achieving a particular astrometric accuracy in a particular time needed for survey-type science (i.e., 1 mas in 10 min). Arent encircled energy requirements needed for the IFUs? Astrometry Science in Sparse Fields Text and tables will be included in a future release of the SCRD. This science case will be a driver for low and/or very well calibrated instrument distortions, compensation for atmospheric differential refraction, and good temperature control of the AO system. Table 10. Astrometry Science in Sparse Fields derived requirements Resolved Stellar Populations in Crowded Fields Text and tables will be included in a future release of the SCRD. Table 11. Resolved Stellar Populations in Crowded Fields derived requirements Debris Disks Text and tables will be included in a future release of the SCRD. This science case will be a driver for coronagraph design. Table 12. Debris Disks derived requirements Young Stellar Objects Text and tables will be included in a future release of the SCRD. This science case may be a driver towards having an infrared wavefront sensor. Table 13. Young Stellar Objects derived requirements The requirements for the asteroid companions orbit determination science case are summarized in the following table (see the Multiplicity, Size and Shape of Minor Planets section of KAON 455 (V1) and the Multiple Asteroids 2: Orbits determination for the discovered system Observing Scenario).. #Science Performance RequirementAO Derived RequirementsInstrument Requirements1The companion sensitivity shall be H e" 5.5 mag at 0.5 separation for a V d" 17 asteroid (asteroid size < 0.2 ) with a proper motion of d" 50 arcsec/hourAbility to track on non-sidereal objects (assumes asteroid used for tip/tilt). AO requirements are modest compared to other companion sensitivity science cases. Assuming using just the asteroid for tip/tilt. Strehl ratio. PSF is calibrated.Near-IR imager2The companion sensitivity shall be I e" 7.5 mag at 0.75 separation for a V d" 17 asteroid (asteroid size < 0.2 ) with a proper motion of d" 50 arcsec/hourI-band imager3H-band relative photometric (between primary and companion accuracy) of d" 0.05 mag at 0.6 for H = 3 for a V d" 17 asteroid (asteroid size < 0.2 ) with a proper motion of d" 50 arcsec/hourPSF is calibrated.4H-band relative astrometric accuracy of d" 1.5 mas for a V d" 17 asteroid (asteroid size < 0.2 ) with a proper motion of d" 50 arcsec/hourUncalibrated detector distortion < 1.5 mas SNR e" 400 on primary5Target sample size of e" 100 asteroids in d" 4 years6e" 10 targets in an 11 hour nightWill generally only observe at one wavelength (wavelength depends on Strehl)7Observing wavelengths = J and H-bandR-band may become a future requirement if Strehl > 15%Near-IR imager8Spatial sampling d" Nyquist at J-bandNyquist at J-band pixels (d" 13 mas pixels)9Field of view e" 3 diametere" 230 pixels at J-band Nyquist sampling10The following observing preparation tools are required: guide star finder, field of view, PSF simulation.11The following data products are required: Calibrated PSF. Access to archive with proper identification in World Coordinate System.12Observing requirements: 8 epochs per target per semester.  Asteroid Size, Shape, and Composition The requirements for the asteroid size and shape (characterize surface and orbital parameters) science case are summarized in the following table. In addition to the requirement of a high resolution visible imager, the slope of the visible spectrum is needed to determine the asteroid age or surface type. This case requires a spectral resolution of R ~ 100 for 0.7 1.0 m wavelength with Nyquist sampling. Since the slope of the spectra is of importance this could be accomplished with a visible IFU, a visible slit spectrograph, or narrow-band filters. Table 14. Asteroid size, shape, and composition derived requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements14.1Imaging capabilities with 2 elements of resolution in K band (90 mas) and 6 elements of resolution in I band. FWHM(I Band) ~ 16 -20 masI-band imager. 14.2Imaging capability with contrast 20-25% in I band.14.2Target sample size of e" 300 asteroids in d" 3yrs years. e" 10 targets in an 11 hour night [SCRD 2.2.6.5.2, RollUp_v1 M2]#6.5 is stricter requirement.14.3Observing wavelengths 0.7 1.0 m [SCRD 2.2.6.6.6, RollUp_v1 B2]AO system must pass 0.7 to 1.0 micron wavelengths with sufficient sensitivity to satisfy #14.1Visible imager (R through I band) with narrow-band filters or slit spectrograph (R~100), or possibly visible IFU (R~100).14.4Spatial sampling same as #5.5Same as #5.5Same as #5.514.5Field of view e" 1 diameter [SCRD 2.2.6.6.2]Same as #6.8Same as #6.814.6Ability to measure the spectral slope with R ~ 100 at 0.85-1.0 mm [SCRD 2.2.6.6.7, 2.3]Spectroscopic imaging at R ~ 100 across R and I-band, potentially with narrow-band filters (how many? at what spacing?)14.7Ability to measure the SO2 frost bands at R=1000 (R=4000 is acceptable) at 1.98 and 2.12 mm [SCRD 2.2.6.6.7, 2.3]Spectroscopic imaging at R ~ 1000 or 4000 in the K band. Are there other lines of interest possibly in H or J? yes cristalline ice at 1.6514.8Same as #5.7Same as #5.714.9Same as #5.8Same as #5.8 The requirements for the asteroid size and shape (characterize surface and orbital parameters) science case are summarized in the following table (see the Multiplicity, Size and Shape of Minor Planets section of KAON 455 (V1)). In addition to the requirement of a high resolution visible imager, the slope of the visible spectrum is needed to determine the asteroid age or surface type. This case requires a spectral resolution of R ~ 100 for 0.7 1.0 m wavelength with Nyquist sampling. Since the slope of the spectra is of importance this could be accomplished with a visible IFU, a visible slit spectrograph or narrow-band filters. #Science Performance RequirementAO Derived RequirementsInstrument Requirements1The companion sensitivity shall be I e" 7.5 mag at 0.75 separation for a V d" 17 asteroid (asteroid size < 0.2 ) with a proper motion of d" 50 arcsec/hourAbility to track on non-sidereal objects (assumes asteroid used for tip/tilt). AO requirements are modest compared to other companion sensitivity science cases. 2Target sample size of e" tbd asteroids in d" tbd years3e" 10 targets in an 11 hour night4Observing wavelengths = 0.7  1.0 mVisible imager5Spatial sampling d" Nyquist at R-bandd" 8 mas pixels6Field of view e" 3 diametere" 375 pixels along one-axis at R-band Nyquist sampling7Ability to measure the spectral slope with R ~ 100R ~ 100 across R and I-band8The following observing preparation tools are required: guide star finder, field of view, PSF simulation.9The following data products are required: Calibrated PSF. Access to archive with proper identification in World Coordinate System.10Observing requirements: Moons of the Giant Planets The requirements for the moons of giant planets science case are summarized in the following table (see the TBD section of KAON 455 (V1) and the Io Observing Scenario).The requirements for the moons of giant planets science case are summarized in the following table (see the section on Characterization of Gas Giant Planets of KAON 455 (Release 2) and the Io Observing Scenario). Table 15. Moons of giant planets derived requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements15.1Able to map intensity distribution with a spatial resolution d" 20 mas at 0.7 m (are 0.8 or 0.9 microns OK? what science would be lost?) for a target with V = 5 to 8 with proper motion d" 30 per hour The moon will be used as the tip/tilt and NGS guidestar (at a non-sidereal rate of 30 arcsec/hr). Tracking (tip-tilt) accuracy must be better than 5 mas. Need to simulate and calculate what wavefront error would give the required spatial resolution at 0.7 or 0.8 or 0.9 microns. Visible imager.15.2Able to acquire Io within 5 of Jupiter and to track it to within 2.5 of Jupiter. Note that this is a goal but perhaps not a rigid requirement: we know we can acquire within 10 today.May require either a diaphragm or a filter to attenuate the light from Jupiter.See AO derived requirement at left.15.3Relative photometric accuracy of d" 0.05 mag on target. (What science is possible at a variety of levels of accuracy? Need to rephrase photometric requirement as a function of observing wavelength, and take into account possible cirrus)Puts a requirement on Strehl and PSF knowledge at each wavelength. What is this requirement?Detector flat-fielding requirements, linearity, etc will flow down from required photometric accuracy. Need to specify.15.4Absolute photometric accuracy d" 0.05 mag on target. (What science is possible at a variety of levels of accuracy? Need to rephrase photometric requirement as a function of observing wavelength, and take into account possible cirrus)Puts a requirement on Strehl and PSF knowledge at each wavelength. What is this requirement?Detector flat-fielding requirements, linearity, etc will flow down from required photometric accuracy. Need to specify.15.5Relative astrometric accuracy d" 2 mas on target to determine positions of features within disk of a moon (diameter d" 1.2 arc sec).Well-calibrated detector distortion (see # 2.4)15.6Observing wavelengths 0.7 to 2.4 m (how crucial is 0.7 microns to the science, compared with 0.8 or 0.9?)AO system must pass these wavelengths to science instruments.Visible imager. Near-IR imager. May require a number of (how many?) specific narrow-band filters; implies needed flexibility in filter wheels.15.7Spatial sampling d" Nyquist at all wavelengths 15.8Moons are very bright: do not allow saturation. Typical brightness: 5 mag per square arc sec. Check this.Either need to use neutral density filters, or have a fast shutter, or have a detector with large wells or very short exposure times (and low read noise). Note: these observations will have high overhead.15.9Field of view e" 2 diameter.Must pass e" 2 Minimum FOV 2 15.10The following observing preparation tools are required: PSF simulation, target ephemeris, exposure time calculator to enable choice of ND filter and exposure time.15.11The following data products are required: Calibrated PSF. (to what accuracy?)15.12Io and Titan are time domain targets; Io requires d" 1 hr notification of volcano activity. Typical timescales for clouds on Titan are of order days or weeks. #Science Performance RequirementAO Derived RequirementsInstrument Requirements1Able to map intensity distribution with a spatial resolution d" 20 mas at 0.7 m for a target with V = 5 to 8 with proper motion d" 30 per hour2Able to acquire Io within 5 of Jupiter and to track it to within 2.5 3Relative photometric accuracy of d" 0.01 mag on target4Absolute photometric accuracy of d" 0.05 mag on target5Relative astrometric accuracy of d" 2 mas on target6Target sample size of e" 127Observing wavelengths = 0.7 to 2.4 mVisible imager. Near-IR imager. May require a number of different filters8Spatial sampling d" Nyquist at all wavelengths d" 7 mas pixels at 0.7 m9Do not allow saturation10Field of view e" 2 diametere" 280 pixels at 0.7 m11The following observing preparation tools are required: guide star finder, field of view, PSF simulation, target ephemeris12The following data products are required: Calibrated PSF. 13Observing requirements: e" 4 epochs per target per semester. Time domain target; requires d"1 hour notification of activity. 14Time domain requirement: Requires d"1 hour notification of activity. Requires appropriate (TBD) responsiveness. Uranus and Neptune The requirements for the Ice Giants science case are summarized in the following table (see the section on Characterization of Ice Giant Planets of KAON 455 (Release 2)). Table 16. Ice Giants derived requirements #Science Performance RequirementAO Derived RequirementsInstrument Requirements16.0Capability of tracking a moving target with rate up d" 5.0 arcseconds per hour (1.4 mas/se)" The planet can be used as tip/tilt guidestar (proper motion of d" 5.0 arcsec/hour). " The AO system requires sufficient field of view for planets and for their seeing disks (>5 arcsec). " The tip-tilt residual error will be less than 10 mas (limited by resolved primary) while guiding on one planet at 5.0 arcsec/hr (1.4 mas/sec). 16.1Sensitivity: comparable to the current Keck systemNear-IR imager, 0.8 - 2.4 m16.2Photometric accuracy: comparable to the current Keck systemNear- IR imager16.3Targets: Uranus and Neptune systemsAO system (both LGS and NGS) capable of correcting on extended objects. Uranus = 3.4 arcsec Neptune = 2.3 arcsecNear-IR imager, 0.8 2.4 m16.4Observing wavelengths: J, H, KNear- IR imager16.5Spatial sampling: d"Nyquist at the observing wavelengthsSpatial sampling d" Nyquist at the observing wavelength16.6Field of view: e" 15 diameterAO system passes a >15 unvignetted field of viewImager fields of view e" 15 16.7Observing requirements: one run per semester with at least 4 contiguous (partial) nights; both targets can be studied during one run16.8Observing preparation tools: comparable to the current Keck system16.9Data products: comparable to the current Keck system16.10Observing requirements: comparable to the current Keck system; some science goals would be well suited to queue or service observing modes .The requirements for the planets around low mass stars science case are summarized in the following table (see the Imaging and Characterization of Extrasolar Planets around Nearby Stars section of KAON 455 (V1)). The key area in which NGAO will excel is the detection of planets around low-mass stars and brown dwarfs, because Keck, unlike GPI, will be able to use a laser guide star. NGAO will also be able to search for planets around young solar-type stars where dust extinction is significant. JWST will have coronagraphic capability in the 3 to 5 (m window, but will have significantly lower spatial resolution than Keck NGAO. In terms of the types of solar systems that can be studied, this means that JWST will focus on older, nearby main sequence stars (since older giant planets will remain visible in 3 to 5 (m for a longer time). JWST may be more limited than NGAO in doing large surveys, because of its longer slewing time and possibly a lifetime limit on the total number of slews. #Science Performance RequirementAO Derived RequirementsInstrument Requirements1 Target sample 1: Old field brown dwarfs out to 20 pc. Sample size several hundred with a desired maximum survey duration of 3 years.Typical integration times of ~20 min. with 10 min overheads, 10 hrs per night and 10 nights/yr gives a survey size of ~200 targets/ yr.Near infrared imager (possibly with coronagraph). Survey primary at J- and Hband. Possible dual- or multi-channel mode for rejecting background objects2Target sample 2: Young (<100 Myr) field brown dwarfs and low-mass stars out to 80 pc. Sample size several hundred with a desired maximum survey duration of 3 years.Typical integration times of ~20 min. with 10 min overheads, 10 hrs per night and 10 nights/yr gives a survey size of ~200 targets/ yr.Near infrared imager (possibly with coronagraph). Survey primary at J- and Hband. Possible dual- or multi-channel mode for rejecting background objects3Target sample 3: solar type stars in nearby star forming regions and young clusters @ 100 to 150 pc. Bright targets (on-axis self-guiding generally). Sample size several hundred with a desired maximum survey duration of 3 years.Possible dual- or multi-channel mode for speckle suppression. Need IR ADC. Companion Sensitivity Sample 1: 15 AU cutoff 20 to 30 pc; distribution peaks at 4 AU = 0.2"; this gets 2 MJupiter at a separation of 0.2" with a Jband delta magnitude of J = 10 Excellent calibration of nonstatic non-common path aberrations, especially at mid-frequencies. Small servo-lag error Speckle suppression techniques6 to 10 /D general-purpose coronagraph 4Companion SensitivityCompanion Sensitivity Sample 1: 15 AU cutoff  20 to 30 pc; distribution peaks at 4 AU = 0.2"; this gets us 2 MJupiter) at a separation of 0.2" with a Jband delta magnitude (J) = 10 Sample 2: 1 MJupiter is 300K, J=22, J = 11 (2 MJupiter is 2.5 mags brighter). This distribution could have a wider distribution of binaries a) 0.1" separation, J = 8.5, b) 0.2" separation, J = 11 c) , goal J = 11 at 0.1" separation Case 3 placeholder: at 5 Myr , 1 Msun primary; goal J = 13.5 to see 1 MJupiter or J = 9 for 5 MJupiter. 0.2" is uninteresting, 0.07" is needed. Should put in apparent magnitudes in a new table (probably J = 22 or 23)Excellent calibration of nonstatic non-common path aberrations, especially at mid-frequencies. Small servo-lag error Speckle suppression techniques Probably requires static errors (AO+tel+NCP+laser+etc.) to be less than 30 nm for the first requirement. Second sample requirement on static errors is TBD.a) 6 /D general-purpose coronagraph b) 6 or 10 /D general-purpose coronagraph c) Not achievable with a general purpose coronagraph (Sample 1: probably needs a general-purpose coronagraph Sample 2: mMay need small IWD coronagraph. Footnote for sample 2: nNon-redundant aperture masking is an interesting approach for this, limits currently unknown, probably requires low read noise in science detector.) Case 3 requires a very small IWA coronagraph, non-redundant masking maybe have conversation with one of the usual NRA suspects (Ireland, Lloyd, Tuthill). Companion Sensitivity Case 3 placeholder: at 5 Myr , 1 Msun primary; a) goal J = 13.5 to see 1 MJupiter or b) goal J = 9 for 5 MJupiter. 0.2" is uninteresting, 0.07" is needed. Should put in apparent magnitudes in a new table (probably J = 22 or 23)Excellent calibration of nonstatic non-common path aberrations, especially at mid-frequencies. Small servo-lag error Speckle suppression techniquesa) Not achievable with a general purpose coronagraph (requires a very small IWA coronagraph, non-redundant masking  maybe have a conversation with Ireland, Lloyd or Tuthill). b) 6 /D general-purpose coronagraph 5H-band relative photometry (between primary and companion) accuracy of d" 0.1 mag for recovered companions; goal of measuring colors to 0.05 mags (0.03 mag per band)Diagnostics on AO data to measure Strehl fluctuations if it takes a while to go on and off the coronagraph (but this is the least desirable option)Induced ghost images of primary; or rapid interleaving of saturated and unsaturated images; or a partially transparent coronagraph6For initial rejection of background objects: proper motion 0.1"/yr., so want 0.01" accuracy? For measuring orbits of nearby field objects, want 0.5 mas to measure masses to 10%. Note this gives you primary mass. To get secondary you need absolute astrometry at very low level (0.1 mas?). This is a goal. Its unclear if we can meet this goal. Could be combined with Doppler measurements if thats practical for the brighter objects.Position stability requirement TBD.Distortion requirement TBD (similar to asteroid science case). Also want ghost images etc. as per photometry710 minute acquisition (20 targets per night, 30 goal)AO system must be able to absolutely steer objects so they land on the coronagraph, implies 0.005" reproducibility of field steering?8Observing wavelengths = J- and H-band (also interested in Y and z for companion characterization)Methane band filters for rapid discrimination, Y or a custom filter for early characterization.9Able to register and subtract PSFs (with wavelength, time, etc.)1.5 x Nyquist sampled at J (goal Y)10Be able to see companions at 100 AU scales at 30 pc (goal 20 pc)Field of view 3" radius (goal 5" radius)11Characterization of companionR ~150 IFU, sub-Nyquist sampling spectrograph (or possibly Nyquist spatial sampling IFU, R ~ 4,000, OH suppressing). Sensitive to J = 22 or 23.12The following observing preparation tools are required: guide star finder, field of view, PSF simulation.13The following data products are required: Calibrated PSF. Access to archive with proper identification in World Coordinate System.14Observing requirements: Observer present. Need to know when night will be. The requirements for the Measurement of General Relativity Effects in the Galactic Center science case on both precision astrometry and radial velocities are summarized in the following two tables, respectively (see the Precision Astrometry: Measurements of General Relativity Effects in the Galactic Center section of KAON 455 (V1)). #Science Performance RequirementAO Derived RequirementsInstrument Requirements1Astrometric accuracy d" 100 as for objects d" 5 from the Galactic CenterHigh Strehl to reduce confusion limit: rms wavefront error d" 170 nm (this also implies the need for an IR tip/tilt sensor). Lower background than current AO system. 2Observing wavelengths = H and K-band 3Spatial resolution d" Nyquist at H and K4Spatial resolution consistent over field of view to TBD 5Field of view e" 10 diameter for imaging6Target drift should be d" TBD mas7Ability to construct 40x40 mosaic to tie to radio astrometric reference frame8The following observing preparation tools are required: 9The following data products are required:  #Science Performance RequirementAO Derived RequirementsInstrument Requirements1Radial velocity accuracy d" 10 km/sec for objects d" 5 from the Galactic CenterHigh Strehl, low background, differential atmospheric refraction correction, PSF estimationSpectral resolution e" 40002Observing wavelengths = H and K-band3Spatial resolution d" 20 or 35 mas4Field of view e" 1 x 1 for radial velocities5Target drift should be d" TBD mas6The following observing preparation tools are required: 7The following data products are required: IFU pipeline for wavelength/flux calibration. The requirements for the QSO Host Galaxy science case are summarized in the following table (see the QSO Host Galaxy section of KAON 455 (V1)). The typical QSO that we are considering is at redshift xxx, had a magnitude yyy point source in the center, with a host galaxy of magnitude zzz per square arc sec. The galaxy is TBD arc sec across. [Say something about the profile of the galaxy] The scientific goals are the following: 1) measure colors and magnitudes for the point source; 2) measure morphology and surface brightness profile for the galaxy; 3) obtain spectrum of point source; 4) obtain spatially resolved spectrum of galaxy in order to study its kinematics and stellar populations. In order to accomplish these things, PSF subtraction will be crucial. [This is a derived requirement.] . #Science Performance RequirementAO Derived RequirementsInstrument Requirements1Number of targets required: sample size of TBD galaxies in TBD nights or yearsRequirement on sky coverage fraction may be implied here, particularly if data from space missions or radio surveys is required2Required signal to noise ratio for imaging of central point source: TBD at TBD wavelengthAO Strehl ratio > TBD AO background level < TBD; over TBD wavelength rangeInstrument background level; Need to be background limited (implications for detector)3Photometric accuracy required for imaging the central point source: TBD at TBD wavelengths. PSF stability and knowledge, temporal and field of view [uniformity trade]; Target drift should be d" TBD mas per hourCalibration stability and accuracy, Zero-point stability and knowledge, Quality of flat-fielding4Required SNR for spatially resolved spectroscopy of the point source > TBD at TBD wavelengthsAO Strehl ratio > TBD AO background level < TBD; over TBD wavelength range; PSF stability and knowledge, temporal and field of view [uniformity trade]; Target drift should be d" TBD mas per hour[What spatial sampling is optimum for good PSF subtraction?], spectral resolution R ~ TBD; detector limited SNR performance; FOV = TBD arc sec [e.g. larger for sky subtraction]5Required signal to noise ratio for imaging of host galaxy in presence of point source: TBD at TBD wavelength at TBD distance from the point sourceAO Strehl ratio > TBD AO background level < TBD; over TBD wavelength range; PSF stability and knowledge, temporal and field of view [uniformity trade]; Spatial sampling TBD 6Photometric accuracy required for imaging the host galaxy: TBD at TBD wavelengths at TBD distance from point source. AO Strehl ratio > TBD AO background level < TBD; over TBD wavelength range; PSF stability and knowledge, temporal and field of view [uniformity trade];Target drift should be d" TBD mas per hourCalibration stability and accuracy, Zero-point stability and knowledge, Quality of flat-fielding; FOV = TBD arc sec [e.g. larger for sky subtraction]7Required SNR for spatially resolved spectroscopy of the host galaxy > TBD; spatial resolution = TBD; velocity resolution and accuracy = TBD; wavelength range TBDAO Strehl ratio > TBD AO background level < TBD; over TBD wavelength range; PSF stability and knowledge, temporal and field of view [uniformity trade]; AO 80% enclosed energy radius = TBD; Target drift should be d" TBD mas per hourFOV = TBD; spectral resolution = TBD; spatial sampling (spaxel size); detector-limited performance; Calibration stability and accuracy, Zero-point stability and knowledge, Quality of flat-fielding; Requirement on persistence? Required minimum trade between single-shot spectral coverage and field of view8Required observation planning tools (e.g. guide stars); PSF simulation tools to plan for whether PSF subtraction will be good enough to see the host galaxy9Required data reduction pipeline for IFU The requirements for the high-z galaxy science case are summarized in the following table (see the Galaxy Assembly and Star Formation History section of KAON 455 (V1)). #Science Performance RequirementAO Derived RequirementsInstrument Requirements1SNR e" 10 for a z = 2.6 galaxy in an integration time d" 3 hours for a spectral resolution R = 3500 with a spatial resolution of 50 mas2Target sample size of e" 200 galaxies in d" 3 years (assuming a target density of 4 galaxies per square arcmin)Minimum spacing of targets Field of regard Contiguous field Number of IFUs3Observing wavelengths = J, H and K (to 2.4 m)4Spectral resolution = 3500 to 4000Spectral resolution5Spatial resolution = 50 to 70 mas6Spatial resolution consistent over field of view to TBD7Velocity determined to d" TBD km/sec for spatial resolutions of 50 to 70 masPSF intensity distribution known to d" 10% per spectral channel. Spatial and spectral model fitting valid to d" TBD8Field of view e" 1.5 diameter9Simultaneous sky background measurements within a radius of 3 with the same field of view as the science field10Relative photometry to d" 0.1 mag for observations during a single night11Absolute photometry d" 0.3 mag12Overlap with TBD data setsSky coverage e" 20%13Should be able to center a galaxy to d" TBD of science field of view14Should know the relative position of the galaxy to d" TBD of spaxel size15Target drift should be d" TBD of spaxel size16The following observing preparation tools are required: 17The following data products are required: calibrated spectral data cube in World Coordinate System with absolute TBD accuracy The requirements for the Nearby AGN science case are summarized in the following table (see the Nearby AGN section of KAON 455 (V1)). The typical AGN that we are considering is at redshift <0.05, and if a Seyfert 1 galaxy has a magnitude yyy point source in the center, with a host galaxy of magnitude zzz per square arcsec. The region of interest for spatially resolved spectroscopy is within the gravitational sphere of influence of the central black hole: generally we will need at least two resolution elements across this distance. [convert to arcsecs as function of z] The scientific goals are the following: to measure the black hole mass using stellar kinematics in the cores of AGNs. In order to accomplish this, PSF subtraction will be crucial for Seyfert 1 galaxies. [This is a derived requirement.] #Science Performance RequirementAO Derived RequirementsInstrument Requirements Number of targets required: sample size of TBD galaxies in TBD nights or years Requirement on sky coverage fraction may be implied hereRequired wavelength range 0.85 2.4 micronsRequired spatial sampling at least two resolution elements across gravitational sphere of influence80% enclosed energy radius < gravitational sphere of influence. This implies a total wavefront error of not more than TBD nm over a range from TBD to TBD microns.Spectral and imaging pixels/spaxels < gravitational sphere of influence (in the spatial dimension)Required field of view for both spectroscopy and imaging > 10 radii of the gravitational sphere of influence [fill this in]Will need to get sky background measurement as efficiently as possible. For IR, consider using d-IFU on the sky; for visible, need solutionRequired SNR for spatially resolved spectroscopy of the central black hole region using stellar velocities > 30 per resolution elementAO Strehl ratio > TBD at 0.85 microns (Ca infrared triplet). This implies a total wavefront error of TBD nm at 0.85 microns. PSF stability and knowledge, temporal and field of view [uniformity trade]; Spectral resolution R ~ 3000-4000 (TBD) with two pixels per resolution element; detector limited SNR performance; Spatial sampling at least two resolution elements across the gravitational sphere of influenceRequired signal to noise ratio for imaging of the region around the central black hole [is this a contrast requirement?]AO Strehl ratio > TBD, this implies a total wavefront error of not more than TBD nm over a range from TBD to TBD microns. PSF stability and knowledge, temporal and field of view [uniformity trade]; Spatial sampling at least two resolution elements across the gravitational sphere of influence Photometric accuracy required for imaging the central point source and possible cusp: TBD at TBD wavelengths AO Strehl ratio > TBD, this implies a total wavefront error of not more than TBD nm over a range from TBD to TBD microns. AO background level < TBD; over TBD wavelength range; PSF stability and knowledge, temporal and field of view [uniformity trade];Calibration stability and accuracy, Zero-point stability and knowledge, Quality of flat-fielding; Velocity determined to d" TBD km/sec for spatial resolutions of TBD masPSF intensity distribution known to d" xxx% per spectral channel. Spatial and spectral model fitting valid to d" TBDRequired observation planning tools (e.g. guide stars); PSF simulation tools to plan for observations of Seyfert 1 galaxies which have strong central point sourcesRequired data reduction pipeline for IFU The requirements for the gravitational lensing science case are summarized in the following two tables. Spectroscopic studies of distant galaxies lensed by galaxies #Science Performance RequirementAO Derived RequirementsInstrument Requirements1SNR e" 10 for a z = 1  2 galaxy in an integration time d" 3 hours for a Gaussian width 20 km/sec Gaussian width (50 km/sec FWHM) with a spatial resolution of 50 masR ~ 5000 (or whatever is needed to achieve 20 km/sec sigma on these targets)2Target sample size of e" 50 galaxies, with density on the sky of 10 per square degree. Survey time ~ 3 years.Number of IFUs: at least one, plus preferably one to monitor the PSF and one to monitor the sky. The extra two IFUs could be dispensed with if there were other ways to monitor the PSF and the sky background.3Observing wavelengths = J, H and K (to 2.4 m). Emphasis is on shorter wavelengths. Would use z and I bands if available. 4Spectral resolution: whatever is needed to get 20 km/sec radial velocity Gaussian sigmaSpectral resolution5Spatial resolution 50 mas[need to make the spatial resolution and the enclosed energy requirements consistent with each other]7Velocity determined to d" 20 km/sec Gaussian sigma for spatial resolutions of 50 masPSF intensity distribution known to d" TBD% per spectral channel. 8Field of view > 4 diameter (lenses are bigger than galaxies). Typical lens is 3 to 4 arc sec diameter.9Simultaneous sky background measurements10Relative photometry to d" 0.1 mag for observations during a single night11Absolute photometry d" 0.3 mag12Sky coverage at least 50% with enclosed energy radius within TBD mas. Sky coverage should be better than with current LGS.13Should be able to center a galaxy to d" TBD of science field of view14Should know the relative position of the galaxy to d" TBD of spaxel size. (Whatever works for high z galaxy case is OK here as well)15Target drift should be d" TBD of spaxel size (Whatever works for high z galaxy case is OK here as well)16The following observing preparation tools are required: 17The following data products are required: calibrated spectral data cube .Imaging studies of distant galaxies lensed by galaxies. Goal: screen potential lensed-galaxy targets for more detailed and lengthy spectroscopic study. #Science Performance RequirementAO Derived RequirementsInstrument Requirements1SNR e" 3 per pixel (100 per source) for a z = 1  2 galaxy in an integration time d" 1/2 hour. Strehl > 0.3 at J band. 2Target sample size of e" 200 galaxies, with density on the sky of 10 per square degree. Survey time ~ 3 years.Overhead less than 10 min between targets.10 per square degree implies that you will only be able to observe one target at a time average of 1 in every ~19x19 patch.3Observing wavelengths = J, H and K (to 2.4 m). Emphasis is on shorter wavelengths. Could use z if available. Thermal part of K band less important.5Spatial resolution better than 50 masNeed a good model of the PSF or a simultaneous image of a PSF star. Need a figure of merit for goodness of the PSF: how well the model fits the real PSF in two dimensions. Need Nyquist sampling of pixels at each wavelength.8Field of view > 15 diameter for survey. Bigger is better. Some degradation between center and edge of field is tolerable. (Need to quantify.)10Relative photometry to d" 0.1 mag for observations during a single night11Absolute photometry d" 0.3 mag12Sky coverage at least 50% with enclosed energy radius within 0.1 arc sec at H or K. Sky coverage should be better than with current LGS.14Should know the relative position of the galaxy to d" TBD of spaxel size. (Whatever works for high z galaxy case)16The following observing preparation tools are required: 17The following data products are required: accurate distortion map (to 1% of the size of the galaxy, or 0.01 arc sec rms) Notes: Want to repeat this exercise with galaxies lensed by clusters. Wide field: Typical size of the highly magnified region of a cluster is 1 arc min. Need low background: lens arcs from z ~ 7 are at most Vega magnitude 23 or 24 in H (brightest arcs). Typical size small (half light radii 0.1 arc sec). Closer galaxies with giant arcs: deployable IFU application. Several arc sec long. Want field of regard of about an arc min. Usually 3 to 5 multiple arcs within a square arc min. (But each might be long, and require more than 1 IFU unit.) Less than 10 IFU units needed in a square arc min. Is a requirement needed on achieving a particular astrometric accuracy in a particular time needed for survey-type science (i.e., 1 mas in 10 min). Arent encircled energy requirements needed for the IFUs?Other: Backup Science This will primarily be NGS science that can be done when the lasers cannot be propagated (e.g. due to cirrus), or less-demanding examples of LGS science that can be done when the laser power available is lower than nominal due to hardware problems. The derived requirements for Backup Science will largely involve science preparation and operations issues. Table 17. Alternate Science Observing Modes #Science Performance RequirementAO Derived RequirementsInstrument Requirements17.1NGS mode. NGS as a backup observing mode for when conditions restrict propagation of the lasers.17.2Sky coverage e"5% to ensure at least one-sixth of the off-axis LGS targets will still be observable if it is necessary to go to an NGS backup mode. Assuming b=30, For 5% sky coverage: R=14 mag guide star with 60 diameter field of regard (FOR) R=15 mag guide star with 45 diameter FOR [Keck Observatory Report No. 208, p. 4-100]17.3Capability to switch between NGS and LGS modes in d" 15 minutes (not including target acquisition) to enable flexibility if conditions change.17.4Sensitivity. SNR e" 10 for a z = 2.6 galaxy in an integration time d" 3 hours for a spectral resolution R = 3500 with a spatial resolution of 50 mas [SCRD 2.1.1.4]Sufficiently high throughput and low emissivity of the AO system science path to achieve this sensitivity. Background due to emissivity less than 20% of sky + telescope. [SCRD 2.1.1.5.1 and SCRD Figure 1]17.5Observing wavelengths = J, H and K (to 2.4 m) [SCRD 2.1.1.5.2, RollUp_v1 B13]AO system must transmit J, H, and K bandsInfrared IFU and imager designed for J, H, and K.17.6Spectral resolution = 3000 to 4000 [SCRD 2.1.1.5.2]Spectral resolution of >3000 in IFU17.7Imaging: Nyquist sampled at H-band [SCRD 2.1.1.5.1]Nyquist sampled IR imager (at H-band)17.8Encircled energy 50% in 70 mas [RollUp_v1 E13, N13]Wavefront error sufficiently low (~170 nm) to achieve the stated requirement in J, H, and K bands.Spaxel size either 35 or 70 mas TBD during a detailed study of the IFU17.9Velocity determined to d" 20 km/secPSF intensity distribution known to d" 10% per spectral channel.17.10IFU field of view e" 1 x 3 to allow simultaneous background measurements while observing a 1 galaxy [SCRD 2.1.1.5.1]Narrow relay passes 1 x3 fieldIFU unit s field of view is 1 x 3 17.11Imager FOV e" 10 x 10 for galactic center and gravitational lensing scienceImager FOV e" 10 x 10 17.12Relative photometry to d" 5% for observations during a single night, provided the night is photometric [RollUp_v1 H13]Knowledge of ensquared energy in IFU spaxel to 5%. Telemetry system that monitors tip/tilt star Strehl and other real-time data to estimate the EE vs time.17.13Should be able to center a galaxy to d" 10% of science field of view17.14Should know the relative position of the galaxy to d" 20% of spaxel size17.15Target drift should be d" 10% of spaxel size in 1 hr17.16The following observing preparation tools are required: PSF simulation and exposure time calculator17.17The following data products are required: calibrated spectral data cube . The atmosphere and telescope parameters assumed for achieving these numbers are summarized below. Atmospheric Seeing Assumptions: The atmosphere and telescope parameters assumed for achieving these numbers are summarized below. The NGAO system shall provide its nominal performance when the atmospheric seeing is characterized by the following conditions. An evaluation of existing seeing data has been performed (KAON 303). The KAON 303 profile was modified to include a stronger ground layer and the standard r0 value was lowered from 20 to 18 cm. The resultant baseline median Cn2 profile is presented in Table 1. From this model we calculate the following turbulence parameters for 0.5 m wavelength (note that r0, 0 and 1/fG increase as 6/5): Fried s seeing parameter r0 = 18 cm Isoplanatic angle 0 = 2.5 arcsec Turbulence characteristic frequency fG = 39 Hz In addition, we have adopted a standard deviation for r0 of (r0 = 3 cm with a characteristic evolution time of t = 3 min. Table  SEQ Table \* ARABIC 17a. NGAO baseline Mauna Kea Cn2 Profile Altitude (km)Fractional CWind Speed (m/s)0.00.4716.72.10.18413.94.10.10720.86.50.08529.09.00.03829.012.00.09329.014.80.02329.0 Telescope and Dome Environment: (perhaps this should be in an appendix?) The NGAO system shall provide its nominal performance when the telescope and dome environment can be characterized by the following conditions. Dome & telescope seeing: The Keck dome and telescope environment degrades the intrinsic seeing by less than 0.1 arcsec, in quadrature, as measured from the effective increase in image FWHM (this change corresponds to decreasing the r0 parameter from 18 cm to 17.8 cm). Phasing: The phasing errors will be 10 nm rms wavefront or less before NGAO correction. Standard performance is 60 nm rms currently. Currently available algorithms have demonstrated 10 nm rms. This error interacts with the segment figure error discussed next. We may want to place an error on the overall telescope wavefront figure PSD instead. Segment figure: The wavefront error of the 36 segments will be less than 80 nm rms wavefront after warping, but before NGAO correction; this number is an average over all 36 segments segment. As a goal the wavefront error shall be 80 nm rms over each segment. Stacking: The segment stacking errors will contribute less than 20 nm rms wavefront to the overall wavefront error before NGAO correction. Line of sight jitter: The aggregate line of sight jitter (wavefront tip and tilt) resulting from motion of the primary, secondary and tertiary mirrors will be less than 0.020 arc seconds rms before correction by the NGAO. This vibration is known to currently be largely dominated by a narrow resonance at ~29 Hz. Segment motion: The motion of each segment as a solid body will be less than 0.015 arc seconds rms before correction by the NGAO. This vibration is known to currently be largely in a narrow resonance at ~29 Hz. Science Instrument Requirements The NGAO system must be capable of supporting the following science instruments (in rough order of priority), based on the NGAO proposal and SCRD: Visible imager. Wavelength range = 0.6 to 1.1 m. Field of view = 20x20. Image sampling = 6 mas pixels. Near-IR imager. Wavelength range = 1.0 to 2.45 m. Field of view = 20x20. Image sampling = 10 mas. Deployable near-IR Integral Field Unit (IFU). Wavelength range = 1.0 to 2.45 m. Field of Regard = 1.5x1.5 with 3x3.4 fields of view for each IFU. Image sampling = 100 mas. Near-IR IFU. Wavelength range = 1.0 to 2.45 m. Field of view from 2x1.25 to 16x5. Image sampling = 20 to 100 mas. Visible IFU. Wavelength range = 0.6 to 1.1 m. Field of view from 1.2x1.36 to 12x6.8. Image sampling = 20 to 100 mas. L and M-band imager. Wavelength range = 3.0 to 5.3 m. Field of view = 25x25. Image sampling = 25 mas. Future science instruments from the above list or completely new instruments. These future science instruments would need to be designed so as to fit at a movable port or to replace a fixed first generation instrument. Table 183. Science Instrument Requirements #Science Instrument RequirementDiscussionBased on 183.1Visible Imager: the field of view shall be e" few 2 arcsec (diameter?)diameterKAON 455 (v1)SCRD 2.1.6.2, Table 52.5: asteroid shapes and companions183.2NIR Imager: the field of view shall be e" few 2 arcsecKAON 455 (v1)SCRD 2.1.6.2, 2.5:Table 5: Io, Titan, debris disks and QSO host galaxies183.3NIR Imager: the field the field of view shall be e" 5 3 arcsecSCRD 2.2.5.3KAON 455 (v1) Table 5: planets around low mass stars183.4NIR Imager: the field the field of view shall be e" 10 x 10 arcsecSCRD 2.3.11KAON 455 (v1) Table 5: Galactic Center183.5NIR Imager: shall provide a coronagraphSCRD 2.2.4, RollUp_v1 G5 KAON 455 (v1) Table 5: planets around low mass stars, debris disks and QSO host galaxies183.6NIR Imager: wavelength coverage shall be at least 0.9 to 2.4 mSCRD 2.2.4, KAON 455 (v1) Table 5RollUp_v1 B5: planets around low mass stars183.7NIR IFU: field of view shall be e" few 2 arcsecOnly 1 is required for the Galactic CenterKAON 455 (v1)SCRD 2.1.6.2 Table 5: Asteroids, Titan 183.8Visible IFU: field of view shall be e" few2 arcsecKAON 455 (v1) Table 5SCRD 2.5: Nearby AGNs183.9Visible IFU: spectral resolution shall be R ~ 4000What range is acceptable? Note: Asteroid size and shape prefers R=1000 but tolerates 4000 [SCRD 2.1.6.6]KAON 455 (v1)SCRD Table 52.3.6: Galactic center radial velocity, Nearby AGNs183.10NIR ddeployable IFU: field of view shall be e" few 1 x3 arcsec1 x3 or larger required for high z galaxies. (see #9.8opt for an option to this) Galactic Center needs a dIFU.KAON 455 (v1) Table 5SCRD 2.4.5.1: High z galaxies, gravitational lensing183.11NIR deployable Imager: field of view shall be e" few 2 arcsecSCRD 2.4.5.1:KAON 455 (v1) Table 5: high z galaxies812NIR dImager: field of view shall be e" 10 arcsecKAON 455 (v1) Table 5: resolved stellar populations It is TBD whether the NGAO system will need be required to support any of the existing science instruments (NIRC2, NIRSPEC or OSIRIS), however we are baselining a requirement that OSIRIS be fed by the narrow field (high Strehl) NGAO optical feed. The Interferometer and OHANA requirements are discussed in section  REF _Ref158533116 \r \h 6.2.46.2.3. It is a goal for NGAO to support visitor science instruments. Science Operations Requirements The top-level science operations goals for the NGAO system including the science instruments are the following (see KAON 476): Science-grade quality of the raw data (i.e., image quality and completeness of observations). Science-grade quality of the data products (i.e., photometry, astrometry, etc.). Science impact from a given data product (i.e., number of publications and citations). The requirements that support these top-level goals are defined in the following tables. Science-grade quality of the raw data dataa (see KAON 476, section 6.2.1): Table 19.14 Science Operations Requirements, Raw Data Quality #Science Operations RequirementDiscussionBased on194.1Provide an extensive set of tools for instrument performance simulation and observing preparationsThe requirement is that an observer should be able to prepare the observing sequences and simulate the science performance in terms of SNR, EE, SR and total observing time given a set of observing parameters and observing conditions. The suite of functions from the planning tools includes: resolve target, check observability, find suitable NGS, select and simulate instrument setup, simulate AO and instrument performance for various parameters, simulate observing sequence and efficiency, exposure time calculator, save target information, save observing setup.ese The tools should be designed with the end user in mind: user friendly, configurable, stand-alone and available at the observing site. Required by most Science Cases. See e.g., #1.7, #6.16, #12.9. KAON 476 Observing Models Study, section 6.2.1. Discussions with science teams (see  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/ObservingEfficiency/ObsTimeline.xls" Observing Timeline document underand  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/ObservingEfficiency/sci_ops_rqts.doc" Science Operations Requirements (draft)194.2Document the instrument performance at an appropriate level to support observing preparationsThis is both a development and operations requirement, since a continued effort will be required to characterize, monitor and document the performance. This should be based on an extensive science verification phase. KAON 476, section 6.2.1 and 6.2.3194.3Provide a semi-real-time level 1 data reduction pipeline for each instrument to at minimum perform background subtraction, cosmetic correction and shift-and-add of images.This is an operation requirement to support # 14.2 and # 14.4 for any science instrument as well as a science requirements for IFU instruments. KAON 476, section 6.2.1194.45Provide semi-real-time tools to perform an assessment of the image quality on the level 1 data including SNR, Strehl and encircled energy.It is required that the observing support team as well as the observer have the tools to check the image performance at the focal plane of the science instrument. KAON 476, section 6.2.1194.56Provide a science operations paradigm that optimizes the completion rate for a significant fraction (TBD) of observing programs.It is ** not required ** to develop a plan for queue scheduling and service observing. Yet, it is required to provide the necessary tools to 1) simulate, prepare and run the observing sequences; 2) assess the science-grade quality of the data on-the-fly and subsequently 3) decide (or not) to switch to a different observing sequence, a different observing program either by the same observer or not. Particularly, a goal is to develop a science operations paradigm that allows for (and encourages?) flexible scheduling per TAC, to optimize the match between required observing conditions for a science program and real conditions.KAON 476, section 6.2.1 Science-grade quality of the data products Science-grade quality of the data products (see KAON 476, section 6.2.2): Table 20.15 Science Operations Requirements, Data Products Quality #Science Operations RequirementDiscussionBased on2015.1Provide the required calibration methods and tools to achieve the astrometry performance requirementsThis requires four important steps: 1) the tools and methods to calibrate for the astrometry are specified and designed, 2) the tools and methods are implemented, demonstrated, and optimized during the science engineering and verification phase, 3) the tools and methods are handed over to the observing support team, and 4) the performance is regularly documented and posted using the tools and methods. KAON 476, section 6.2.22015.2Provide the required calibration methods and tools to achieve the photometry performance requirementsSame as aboveKAON 476, section 6.2.22015.3Provide the required calibration methods and tools to achieve the PSF characterization requirementsThis is in support of # 15.1, 15.2. as well as 14.1 to 3; KAON 476, section 6.2.2 Science impact from a given data product (see KAON 476, section 6.2.2): Table 21.16 Science Operations Requirements, Archiving and Retrieval #Science Operations RequirementDiscussionBased on2016.1Develop a plan for data archivalData archival is critical for 1) science programs such as proper motion studies, transient phenomena (GRB, SN, Titan, etc), 2) the semi-automated monitoring of instrument performance and 3) the long-term visibility of Keck NGAO (either from direct science impact, or the use of the archive by the general public, e.g. CADC, google sky). Its very likely that the archive may not be supported at first, but its essential to develop a plan for it and understand the requirements for the FITS information, the data storage format, etcScience Case Requirement #1.8 KAON 476, section 6.2.32016.2Develop a plan for data retrieval from the data archiveSame as aboveKAON 476, section 6.2.32016.3Document the on-sky science performance of each science instrument with NGAOThis should be based on an extensive science verification phase.This is redundant with #14.2KAON 476, section 6.2.3 O Observatory Overall Requirements (this needs to be numbered) Purpose and Objectives The purpose of the overall requirements section is to convey requirements that apply generally to the overall instrument and its accessories based on the Observatorys requirements. Note that the Observatorys standard requirements for all new instrumentation are summarized in the Instrumentation Baseline Requirements Document. Additional Observatory requirements specific to NGAO are listed in the following sections. Facility Requirements The following are requirements imposed by the nature of the existing facility. Table 2117. Facility Requirements #Facility RequirementDiscussionBased on21.1The NGAO system must be facility-classFacility-class has many implications on safety, operability, reliability, maintainability, lifetime, documentation, configuration management, etc. KAON 572 (Baseline Instrument Requirements), KAON 463 and 476 (Observing model studies), and KAON XXX Operations Requirements (draft  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/ObservingEfficiency/sci_ops_rqts.doc" link)217.21The NGAO system & science instruments should be located on the Nasmyth platform of one of the Keck telescopesThe Keck telescope foci and Nasmyth deck storage locations are already heavily utilized. The current AO systems occupy the left Nasmyth platform locations of both telescopes. HIRES occupies the right Nasmyth on Keck I while DEIMOS and NIRSPEC share the right Nasmyth on Keck II. The Cassegrain foci are occupied by LRIS (and MOSFIRE in the future) on Keck I and by ESI on Keck II. The bent Cassegrain ports are believed to have inadequate space and weight capacities. The prime focus could potentially be available but there would be many constraints on an instrument at this location. The most viable option is in the location of an existing AO system. Alternatives would be to decommission HIRES or for the existing AO system and the NGAO system to be able to share the same platform.System architecture decision by NGAO engineering team (see  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON_499_v1.2.pdf" KAON 499)2117.32The NGAO system should accommodate the entire Keck pupilThe Keck primary has a maximum edge-to-edge diameter of 10.949 m. System architecture decision by NGAO engineering team (see KAON 499)2117.43If the existing f/15 or f/40 secondary mirrors are used then the NGAO system will be constrained by the resultant f/#, focal plane and pupil locationBoth telescopes have f/15 secondary mirrors, as well as chopping secondary units that can accommodate f/25 and f/40 secondary mirrors. The choice of f/15 secondary mirrors for the current AO systems was largely driven by the resultant reduced size of the AO systems and the availability of PCS (Phasing Camera System) via a rotation of the tertiary mirror. The inability of the current systems to chop at the telescope pupil has been a limitation for thermal IR observations. The focal length of the telescope with the f/15 secondary mirror is 150 m. The 10.949 m primary corresponds to an f/13.66 beam with an exit pupil diameter of 1.460 m located 19.948 m in front of the focal plane.Is this a facility requirement? Should it be an optical requirementEngineering decision to avoid the cost of constructing another secondary2117.54The NGAO facility must not compromise the performance of a non-NGAO instrument when that instrument is being used for science or engineering This requirement is intended to ensure that the NGAO facility, when not in use, does not introduce vibrations or stray light that might impact the performance of another science instrument or an engineering instrument such as PCS.KAON 572 Baseline Instrument Requirements, e.g. 8.2.2.2, 9.3.2.12117.65The NGAO facility must not compromise the performance of the telescope when the telescope is used for non-NGAO observations.The NGAO system should not impact the dynamic performance of the telescope through vibrations or different telescope dynamics. If NGAO hardware is to be mounted in the top-end then it must be designed/implemented not to compromise the secondary mirror performance.KAON 572 Baseline Instrument Requirements2117.76The NGAO facility / science instrument combination should provide compensation for science field rotationThe Alt-Az telescope design requires compensation for field rotation in order to keep the science field fixed on the science instrument.KAON 455 Science Case Requirements Document (various science case observing modes)2117.87The NGAO facility / science instrument combination should provide compensation for pupil rotationThe Alt-Az telescope design and the irregular shape of the Keck primary mirror require that NGAO system provide appropriate compensation for pupil rotation. Examples: The existing Keck AO system updates the reconstructor to compensate for pupil orientation. The NIRC2 coronagraph mask rotates to match the rotating pupil.KAON 455 Science Case Requirements Document, high contrast imaging mode 2.1.4.42117.98The NGAO facility should provide compensation for LGS projector rotationThe Alt-Az telescope design will cause the laser projector (and the resultant LGS asterism) to rotate with respect to the Nasmyth platform. Compensation will be required to maintain the off-axis LGS on the corresponding wavefront sensor.Practical requirement in order to accommodate LGS wavefront sensors Nasymth location (see requirement  REF reqmt21_2 \h 21.2)2117.109The NGAO facility should accommodate access for routine maintenance of the telescope For example, access to the elevation journal, elevation wrap, bent Cassegrain platform and stairwell to the mirror cellKAON 572 Baseline Instrument Requirements, section 1521.11The NGAO facility should not routinely require more than 30 minutes of daytime telescope restriction on an NGAO science night.KAON 463 and 476 (Observing model studies), and KAON XXX Operations Requirements (draft  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/ObservingEfficiency/sci_ops_rqts.doc" link)21.12The NGAO system must operate within specifications under the normal summit temperature and humidity conditions See the conditions specified in the Instrument Baseline Requirements Document.KAON 572 Baseline Instrument Requirements, 6.2.1.2.3 Telescope and Dome Environment Requirements: The NGAO system shall provide its nominal performance when the telescope and dome environment can be characterized by the following conditions. Table 22. Telescope and Domne Environment Requirements #Observatory Instrument RequirementDiscussionBased on22.1Dome & telescope seeing less than 0.1The Keck dome and telescope environment degrades the intrinsic seeing by less than 0.1 arcsec, in quadrature, as measured from the effective increase in image FWHM (this change corresponds to decreasing the r0 parameter from 18 cm to 17.8 cm). HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/WorkProducts/KAON482_TelescopeErr.pdf" KAON482, Keck Telescope Wavefront Error trade study, and references therin22.2The phasing errors will be 10 nm rms wavefront or less before NGAO correction.Standard performance is 60 nm rms currently. Currently available algorithms have demonstrated 10 nm rms. This error interacts with the segment figure error discussed next. We may want to place an error on the overall telescope wavefront figure PSD instead. KAON482, Keck Telescope Wavefront Error trade study, and references therin22.3Segment figure : The wavefront error of the 36 segments will be less than 80 nm rms wavefront after warping, but before NGAO correction.This number is an average over all 36 segments segment. As a goal the wavefront error shall be 80 nm rms over each segment. KAON482, Keck Telescope Wavefront Error trade study, and references therin22.4Stacking: The segment stacking errors will contribute less than 20 nm rms wavefront to the overall wavefront error before NGAO correction. KAON482, Keck Telescope Wavefront Error trade study, and references therin22.5Line of sight jitter: The aggregate line of sight jitter (wavefront tip and tilt) resulting from motion of the primary, secondary and tertiary mirrors will be less than 0.020 arc seconds rms before correction by the NGAO.This vibration is known to currently be largely dominated by a narrow resonance at ~29 Hz. KAON482, Keck Telescope Wavefront Error trade study, and references therin22.6Segment motion: The motion of each segment as a solid body will be less than 0.015 arc seconds rms before correction by the NGAO.This vibration is known to currently be largely in a narrow resonance at ~29 Hz. KAON482, Keck Telescope Wavefront Error trade study, and references therin Observatory Science Instrument Requirements In addition to the science instrument requirements specified in section  REF _Ref158533406 \r \h 6.1.3 the NGAO facility must allow the Observatory to continue supporting Interferometer science with the two Keck telescopes. Should we move this paragraph to section 6.1..3 then? The requirements for these instruments are developed in  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 428 and are further specified in later sections. Table 23 18. Observatory Science Instrument Requirements #Observatory Instrument RequirementDiscussionBased on2318.1The NGAO facility should support the Keck Interferometer (KI) with performance as good or better than provided by the pre-NGAO Keck AO systemsThe KI dual star modules (DSM) currently move into both AO enclosures on rails to feed the KI. The requirement to feed the KI requires that collimated and f/15 light can be fed to the DSM and that the field rotation, pupil rotation, longitudinal dispersion and polarization from the NGAO system and the AO system on the other telescope be identical. See  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 428 Implications and Requirements for Interferometry with NGAO.Same idea: should these requirements be part of the Science Instrument Requirements (6.1.3)?Existing Keck Observatory commitments to NASA and NSF2318.2The NGAO system should support the OHANA interferometer with performance as good or better than provided by the pre-NGAO Keck AO systems Injection modules are currently placed on each AO bench to feed an optical fiber that goes to the KI. In future the output from these fibers will be interfered with those from multiple telescopes. Same as aboveExisting Keck Observatory commitments to NASA and NSF Observatory Operational Requirements The purpose of this section is to document the Observatorys overall requirements for the support of science operations. These requirements can be divided into the following categories: Percent of time collecting science quality data. Capability to support a certain number of nights per year of science operations. Operational costs. Impact on daytime and nighttime operations. Compliance with regulations, including safety, Mauna Kea policies, FAA and U.S. Space Command. Each of these categories is represented in one of the following tables. In addition, all of the above categories require a facility-class NGAO system and science instruments, and this requirement is reflected in the final table. Table 24. Observatory Operational Requirements #Observatory Operational RequirementAO Derived RequirementsInstrument Derived RequirementsBased on24.1Assuming a classical observing model* and adequate observing conditions for the science program, mMore than 880% of thee allocated observing time is spent on collecting science-quality data for the deployable science instruments.a *See KAON 476 for definitions of observing modelsObserving model should allow flexible scheduling and quick-and-easy switching of observing modes and instrument. Observing overhead and efficiencyareis minimized, particularly by being able to center multiple targets and reference guide stars with a < 0.3 accuracy. Observing reliability is critical to avoid canceling long integration:. t here should be less than 2 faults per night (one system fault is equivalent ~ 20-30 min lost time on faint targets for the worst cases). Observing tools should allow for automated observing sequences. The deployable instrument are used for faint object spectroscopy with much longer time on target, hence less observing setup overhead. One should be able to stop, abort and restart an integration on command. HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/NGAO_SCRD_Release2_v10a_sm.pdf" KAON 455 (ScRD) science target samples and survey durations, combined with efficiency analyses given in  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/WorkProducts/KAON476.pdf" KAON 47624.2Assuming a classical observing model and adequate observing conditions for the science program, more than 70% of the observing time is spent on collecting science-quality data for the narrow-field science instruments.Same as above. In addition, observing efficiency is critical for survey mode (see Science Case 1) Acquisition sequences must be fully automated. Overhead must be reduced by allowing parallel sequences between telescope, AO, laser and science instrument. The narrow field science instruments are used on brighter targets in imaging, coronagraphy and spectroscopy modes. The science instrument interface command must allow for parallel sequences, e.g, start a nod/dither sequence immediately after the pixel readout. KAON 455 (ScRD) science target samples and survey durations, combined with efficiency analyses given in KAON 47624.3The NGAO system must be capable of supporting 200 nights/year of science operations and keep the total annual operational personnel within the 5-year plan Observatory operation budget, including non-personnel costs. Observatory currently willing to support 140 nights/year.KAON 455 (ScRD) science target samples and survey durations, combined with efficiency analyses given in KAON 47624.4 The NGAO facility should not require more than TBD engineering nights per year for system maintenance.KAON 572 Baseline Instrument Requirements, section 1324.5The Mauna Kea laser projection requirements must be satisfied This includes requirements on laser power, wavelength, laser traffic control participation, aircraft safety and space command. See KAON 153. The current policy only accepts sodium wavelength lasers, and requires that a single laser beacon not exceed 50W and that a maximum of 200 W be projected from a single facility, and that laser beacons not be projected below 70 zenith angle.Mauna Kea laser projection requirementKAON 153 Requirements on laser traffic control participation, aircraft safety, and space command compliance for satellite safety. Discussion: Should this efficiency number include any of the weather statistic? The Keck Strategic Planning document calls for a 90% efficiency goals in 2020. #Observatory Operational RequirementAO Derived RequirementsInstrument Derived Requirements1The NGAO system must be capable of supporting 240 nights/year of science operationObservatory currently willing to support 140 nights/year. #Observatory Operational RequirementAO Derived RequirementsInstrument Derived Requirements1The NGAO facility should be designed to keep the total annual operational personnel and non-personnel costs below the following budgets: Four FTEs and $200k (FY07 dollars) in non-personnel costs for the first 100 nights/year of science operations An additional cost of 0.5 FTEs and $25k (FY07 dollars) in non-personnel costs for each additional 50 nights of science operations. #Observatory Operational RequirementAO Derived RequirementsInstrument Derived Requirements1The NGAO facility should not require more than two engineering nights per year for system maintenance2The NGAO facility should not routinely require more than 30 minutes of daytime telescope restriction on an NGAO science night #Observatory Operational RequirementAO Derived RequirementsInstrument Derived Requirements1The Mauna Kea laser projection requirements must be satisfied This includes requirements on laser power, wavelength, laser traffic control participation, aircraft safety and space command. See KAON 153. The current policy only accepts sodium wavelength lasers, and requires that a single laser beacon not exceed 50W and that a maximum of 200 W be projected from a single facility, and that laser beacons not be projected below 70 zenith angle.Mauna Kea laser projection requirement #Observatory Operational RequirementAO Derived RequirementsInstrument Derived Requirements1The NGAO system must be facility-classFacility-class has many implications on safety, operability, reliability, maintainability, lifetime, documentation, configuration management, etc. 2The NGAO system must operate within specifications under the normal summit temperature and humidity conditions See the conditions specified in the Instrument Baseline Requirements Document. Observatory Implementation Requirements Table 25. Observatory Implementation Requirements #Observatory Implementation RequirementDiscussionBased on25.1The NGAO system and instruments must complete the Observatory standard design review process.Sean Adkins, An Overview of the WMKO Development Phases, WM Keck Observatory Instrument Program Management Memo, December 8, 2005  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NGAOProcessGuidelines/Overview_of_the_WMKO_Development_Phases.pdf" link25.21The time between decommissioning an AO capability on the telescope where the NGAO system is to be installed and making NGAO available for limited shared-risk science must be agreed upon with the SSCObservatory Director. (it used to be(suggested: must not be longer than 6 months) Down Minimize down time impact on Interferometer and AO science at the Observatory.Directors discretion25.3The telescope downtime required to implement NGAO must not be longer than 5 daysan amount agreed upon with the Observatory Director (5 days was suggested)Minimize down time impact on Interferometer and AO science at the Observatory.This should be agreed on and should be retrofitted in the Instrument Baseline RequirementsDirectors discretion25.4The NGAO system must complete an operations transition review where operational responsibility is transferred from development to operations This has implications on defining transition requirements and on training.Sean Adkins, An Overview of the WMKO Development Phases, WM Keck Observatory Instrument Program Management Memo, December 8, 2005  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NGAOProcessGuidelines/Overview_of_the_WMKO_Development_Phases.pdf" link Optical Requirements Optical Requirements Purpose and Objectives The purpose of this section is to describe optical requirements for the performance, implementation and design of the NGAO optical system. Performance Requirements The following performance requirements are duplicated from the Science Performance Requirements in section 6.1.2 since these are direct optical performance requirements. THIS TABLE SHOULD NOT BE HERE. IT IS BOTH REDUNDANT AND INCORRECT. CLAIRE #Performance RequirementDiscussionBased on1Telescope plus NGAO transmission to the input of the science instruments e" 70% at 0.7-2.4 m.The wavelength range is explicitly identified in the SCRD. The transmission is a placeholder. Need to determine if we should extend this down to H( (656.3 nm). May be better to write in terms of SNR.KAON 455 (v1) Table 42Goal: Telescope plus NGAO transmission to the input of the science instruments e" 70% at L-band.KAON 455 (v1) Table 4 low mass stars & Galactic Center science cases3NGAO background, including the science instrument shall be d" 100% of the sky plus telescope at K-band.The measured NIRC2 K-band background is 12.24 mag/arcsec2. The predicted sky background is 13.46.KAON 455 (v1) Table 4: for the asteroid science cases the background should be d" the current LGS background4Goal: NGAO background including the science instruments shall be d" 20% of the sky plus telescope at K-band.KAON 455 (v1) Table 4: High z galaxies.5Wavefront error d" 140 nm rms for V d" 17 on-axis guide starKAON 455 (v1) Table 4: asteroid shape & companions.6Wavefront error d" 140 nm rms for V d" 16 guide star d" 30 from science objectKAON 455 (v1) Table 4: planets around low mass stars.7Wavefront error d" 170 nm rms for objects d" 5 from the Galactic CenterKAON 455 (v1) Table 4: Galactic Center.8Encircled energy e" 50% within a 0.05 diameter circle at K-band for sky coverage e" 5% KAON 455 (v1) Table 4: High z galaxies.9Encircled energy e" 50% within a 0.075 diameter circle at K-band for sky coverage e" 30%KAON 455 (v1) Table 4: High z galaxies.10The companion sensitivity shall be H e" 5.5 mag at 0.5 separation for a V d" 17 on-axis guide starKAON 455 (v1) Table 4: asteroid companions.11The companion sensitivity shall be H e" 13 at 1 separation for a V d" 16 guide star d" 30 from science objectKAON 455 (v1) Table 4: planets around low mass stars.12Sensitivity? Does this just drive transmission?KAON 455 (v1) Table 4: planets around low mass stars.13H-band photometric accuracy of d" 0.05 mag at 0.6 for H = 3 for a V d" 17 on-axis guide starKAON 455 (v1) Table 4: asteroid companions.14H-band photometric accuracy of d" 0.05 mag relative to the primary star at 1 separation for H = 13 for a V d" 16 guide star d" 30 from science objectKAON 455 (v1) Table 4: planets around low mass stars.15Uncalibrated detector distortion < 1.5 masIs this really the way we want to write this? Shouldnt we put the high level requirement here?KAON 455 (v1) Table 4: asteroid companions.161/10 of the PSF FWHMWouldnt be better off writing this as mas?KAON 455 (v1) Table 4: planets around low mass stars.17Astrometric accuracy d" 100 as at K-band for objects d" 5 from the Galactic CenterKAON 455 (v1) Table 4: Galactic Center.18Radial velocity accuracy d" 10 km/sec at K-band for objects d" 5 from the Galactic CenterKAON 455 (v1) Table 4: Galactic Center.19Overheads between targets d" 10 minKAON 455 (v1) Table 4: Asteroid size & companions, planets around low mass stars.20Strehl or PSF stability requirement?TBD The following performance requirements are derived from the Science Performance Requirements in Section 6.1.2 and the relevant performance budgets. OMIT THIS TABLE COMPLETELY. CLAIRE #Performance RequirementDiscussionBased on1The residual static wavefront errors from the NGAO system shall be d" 50 nm rms as delivered to the visible and NIR imagersCompanion sensitivity requirement & performance budget. 2The NGAO system shall introduce d" TBD % polarization in the path to the TBD science instruments3The stability of the focal ratio produced by the NGAO system shall be TBD as delivered to the TBD science instrumentsThe purpose of this requirement is to have a fixed plate scale.4Instability must not decrease the Strehl on the visible and NIR imagers by more than 5% during any 1-hour period or over a 3 C temperature change (Should look at changing the instability requirements to rms error.)The image improvement provided by the facility must be stable over periods of hours, under stable atmospheric conditions. The wavefront sensor calibrations must be stable with time, temperature and telescope position. This requirement does not include performance degradations due to changing atmospheric conditions, or different magnitude and location of NGS or LGS. This requirement could be tested using a point source (i.e., single mode fiber) at the NGAO system input.5Instability must not decrease the Strehl on the visible and NIR imagers by more than 10% during any 24-hour period or over a 5 C temperature change6The maximum intensity of any ghost images (of a science object) produced by the NGAO system shall be no more than TBD the maximum intensity of the source within the science field.Derived from the companion sensitivity requirement.7The maximum intensity of any ghost images (of a science object) produced by the imaging science instruments shall be no more than TBD the maximum intensity of the source within the science field.Derived from the companion sensitivity requirement. Implementation Requirements Table 26. Implementation Requirements #Optical Implementation RequirementDiscussionBased on26.1The NGAO optical axis shall be coincident to the telescope s elevation axis to d" TBD.This is intended to minimize pupil and image motionassures that the telescope achieves its nominal performance requirements delineated in  REF OLE_LINK2 \h Table 22.See  REF OLE_LINK2 \h  \* MERGEFORMAT Table 22Im not sure why this is a requirement. Perhaps it is a good suggestion. But there is no basis for it to be a requirement. Design Requirements NGAO is required to provide an AO corrected beam to each of the science instruments, including the Interferometer and OHANA fiber injection module. This may be accomplished with one or more AO systems. The following requirements are valid for all of these science instruments. Table 27. Optical Design Requirements #Optical Design RequirementDiscussionBased on27.1The focal ratio provided to the science instruments should be TBDThese requirements will be deferred pending an interface definition between KNGAO and new instruments, OSIRIS, and the interferometers, to be written during Preliminary Design Phase27.2The exit pupil location provided to the science instruments should be TBDThese requirements will be deferred pending an interface definition between KNGAO and new instruments, OSIRIS, and the interferometers, to be written during Preliminary Design Phase27.3The NGAO system and science instrument combination should be capable of keeping the field or pupil fixed on the science instrument. See requirements  REF reqmt21_7 \h 21.7 and  REF reqmt21_8 \h 21.827.4The NGAO system shall have d" TBD of non-common path aberration delivered to the science instruments.These requirements will be deferred pending an interface definition between KNGAO and new instruments, OSIRIS, and the interferometers, to be written during Preliminary Design Phase27.5The NGAO system should be capable of correcting e" TBD nm of low spatial frequency (Zernikes 4 to 15) non-common path aberration in the science instruments. Image sharpening can be used to correct for aberrations in the science instruments. New science instruments should be designed to have small optical aberrations. The interferometer and possible legacy instruments such as NIRC2 or OSIRIS may be allowed larger aberration budgets. Keck NGAO Error Budget requirements ( HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/SystemArchitecture/ngao_wfe_budget.pdf" KAON 471) in support of Science Case Requirements ( HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/NGAO_SCRD_Release2_v10a_sm.pdf" KAON 455)27.6The peak-to-peak range of tip/tilt correction provided by NGAO shall be e" 3 on sky.The existing Keck AO systems have a peak-to-peak range of 1.6 which has proven to be inadequate in windy conditions.See section 6.1.2.17  REF SeeingConditions \h Atmospheric Seeing Assumptions and  REF Table22 \h Table 22 Telescope and Dome Environment Assumptions REF SeeingConditions \h  REF SeeingConditions \h  REF SeeingConditions \h  REF SeeingConditions \h  REF SeeingConditions \h  The following design requirements are duplicated from the Science Performance Requirements in section 6.1.2 since these are direct optical performance requirements. Table 28. Science Instrument Optical Design Requirements #Science Instrument Optical Design RequirementDiscussionBased on28.1Unvignetted contiguous fields shall be provided to the NIR and visible science imagers and single field IFUs. These fields should be centered to within 1 of the telescopes optical axis. The maximum field size is 20x20.Driven by the science requirements on the contiguous field science instruments.Science requirements on the contiguous field science instruments. ( HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/NGAO_SCRD_Release2_v10a_sm.pdf" KAON 455, Tables 1-17)28.2Multiple unvignetted contiguous fields shall be provided to the NIR d-IFU. Each field should be e" 4 in diameter. Driven by science requirements on the NIR d-IFU.Science requirements on the NIR d-IFU. (KAON 455, Tables 1-17)28.3The unvignetted field of regard provided to the NIR d-IFU shall have a total area of e" 6 arcmin2 and shall have a maximum off-axis distance of d" 1.5 with respect to the telescope s optical axis. Driven by science requirements on the NIR d-IFU.Science requirements on the NIR d-IFU. (KAON 455, Tables 1-17)28.4NGAO shall provide appropriate outputs to e" TBD science instruments with a switching time of d" 5 min.KAON 463 and 476 (Observing model studies), and KAON XXX Operations Requirements (draft  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/ObservingEfficiency/sci_ops_rqts.doc" link) The following design requirements are imposed by the non-interferometric science instruments. Table 29. Non-Interferometric Science Instrument Optical Design Requirements #Science Instrument Optical Design RequirementDiscussionBased on29.1A wavelength range of 0.7 to 1.0 m must be provided to the visible science instruments (imager and IFU)Science Case Requirements Document (KAON 455), see Instrument Roll-up Chart, 2.329.2A wavelength range of 1.0 to 2.45 m must be provided to the NIR science instruments (imager, IFU and deployable IFU) Science Case Requirements Document (KAON 455), see Instrument Roll-up Chart, 2.329.3A wavelength range of 3.0 to 5.3 m must be provided to the thermal NIR imagerThis is currently low priority and should be discussed if this drives the design.Requirement deleted29.4An unvignetted field of view e" 20 x20 must be provided to the science imagers (visible and NIR)Should this only be 10x10 for the visible imager?Science Case Requirements Document (KAON 455), see Instrument Roll-up Chart, 2.329.5An unvignetted field of view e" 12 diameter must be provided to the visible IFUScience Case Requirements Document (KAON 455), see Instrument Roll-up Chart, 2.329.6An unvignetted field of view e" 16 diameter must be provided to the NIR IFUScience Case Requirements Document (KAON 455), see Instrument Roll-up Chart, 2.329.7A field of regard of e" 1.5 diameter must be provided to the NIR deployable IFU with vignetting by all sources d" TBD over TBD % of the field of regardScience Case Requirements Document (KAON 455), see Instrument Roll-up Chart, 2.329.8A field of view of 25 x25 must be provided to the L and M-band imagerLow priority.Requirement deleted29.9An unvignetted science target field e" 3 x 3.4 shall be provided to each channel of the NIR deployable IFUScience Case Requirements Document (KAON 455), see Instrument Roll-up Chart, 2.329.10The NGAO + deployable IFU system shall support simultaneous observations of at least two science targets separated by d" 5 There is no requirement for simultaneous nearest-neighbor target distances less than 5.Requirement deleted29.11The NGAO + deployable IFU system shall support simultaneous observations of at least six science target fields inscribed within a 30 diameter5 square arcminute fieldScience Case Requirements Document (KAON 455) requirement 1.2.29.12NGAO shall be capable of compensating for focus changes due to changing filters or modesWavefront error requirement (SCRD KAON 455) coupled to NGAO Error Budget The following design requirements are imposed by the Interferometer and/or OHANA support requirements. Table 30. Interferometry Science Instrument Optical Design Requirements #Interferometry Optical Design RequirementDiscussionBased on30.1A wavelength range of 1.1 to 14 m must be provided to the Interferometer HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 428 Requirements for Interferometry with NGAO30.2A wavelength range of 1.1 to 2.45 m must be provided to the OHANA injection module HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 42830.3A field of view of e" 1 diameter must be provided to the Interferometer HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 42830.4A field of view of 5 diameter must be provided to the OHANA injection module HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 42830.5NGAO must be able to support a chopping mode for the interferometer.The nuller requires small amplitude chopping with the AO loops closed at each end of the chop for alignment purposes.  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 42830.6The interferometer output of NGAO must be polarization matched to the interferometer output of the AO system on the other telescope in order to produce d" 3 of differential s-p phase shift The current KI achieves polarization matching by keeping the number, angle and coatings of all reflections the same in the beam trains from each telescope. The differential s-p phase shift in the current KI is measured at 6 resulting in a loss in V2 of 0.003. HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 42830.7The interferometer output of NGAO must have the same image rotation as the interferometer output of the AO system on the other telescope HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 42830.8The interferometer output of NGAO must have the same pupil rotation as the interferometer output of the AO system on the other telescope HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 42830.9The interferometer output of NGAO must have the same longitudinal chromatic dispersion as the interferometer output of the AO system on the other telescopeTransmissive optics fabricated from different materials can have different amounts of longitudinal chromatic dispersion resulting in the loss of fringe visibility HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 42830.10The ratio of the Strehls from the interferometer output of NGAO and the interferometer output of the AO system on the other telescope must be d" 1.2 and e" 0.9. A Strehl mismatch of 22% or an intensity ratio of 1.22 results in a V2 loss of 0.010. HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 42830.11NGAO must be able to accommodate the accelerometers needed to support the InterferometerOn the current AO bench one accelerometer is placed near the telescope focus and another near the output to the DSM. These are used to measure vibration along the optical path and are used in the fringe tracker control system. The accelerometer acquisition system is housed in an electronics rack in the AO electronics vault. HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 42830.12NGAO or NGAO in combination with a modified DSM must be capable of supporting the laser metrology beams from the interferometerThese metrology beams are a potential source of background light on the wavefront sensors  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 42830.13NGAO must incorporate the required tools and tolerances to support alignment to the interferometer For example, the current AO bench hosts a corner cube to aid in aligning the interferometer to the optical axis of the AO system and telescope HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 42830.14NGAO or NGAO in combination with a modified DSM must provide a collimated 100 mm diameter beam to the interferometerIn the current AO system a removable (on a translation stage) dichroic beamsplitter, located between the deformable mirror and second off-axis parabola, folds the collimated beam to the DSM HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 42830.15The rms residual tilt at the NGAO system output to the interferometer should be d" 0.007 for TBD guide star. HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 428 Mechanical Requirements Mechanical Requirements Purpose and Objectives The purpose of this section is to describe mechanical requirements for the performance, implementation and design of the NGAO mechanical systems. Performance Requirements Table 31. Mechanical Performance Requirements #Mechanical Performance RequirementDiscussionBased on31.1The NGAO AO system shall not exceed a thermal dissipation budget, into the dome environment, of 100 WInstrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 572, requirement 8.2.1.3These are based on Observatory standard heat load allocations. Note to myself (DG): find the relevant observatory requirements document.31.2The NGAO laser system shall not exceed a thermal dissipation budget, into the dome environment, of 100 WInstrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 572, requirement 8.2.1.331.3The NGAO AO system shall not exceed a thermal dissipation budget at the top-end of the telescope, into the dome environment, of 50 WInstrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 572, requirement 8.2.1.3 Implementation Requirements Table 32. Mechanical Implementation Requirements #Mechanical Implementation RequirementDiscussionBased on32.1The NGAO facility must allow a means to install the new science instruments delineated for NGAO optical feed, and to install the OSRIS instrument to the NGAO optical feed.Refer to KAON 531 for a discussion of instrument interface issues, and to KAON 493 for a discussion of OSIRIS instrument reuse.For example, if a new instrument can only be installed with the overhead crane then a means of removing the appropriate portion of the AO enclosure roof would be required.See  REF OLE_LINK1 \h Table 18, (which is derived from  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/NGAO_SCRD_Release2_v10a_sm.pdf" KAON 455, Science Case Requirements Document, Instrument Requirements sections for each science case.)See my comments below-DG***DG This one is vaguely worded. What does it mean must be able to install new instruments? We can always- install new instruments. Perhaps this is meant to limit the changes to infrastructure (such as the example given)? For example, does this mean the enclosure must be oversized to accommodate a new instrument? If so, the volume of the hypothetical new instrument must be given, as well as a heat load, electrical requirement, etc. I vote for dropping this requirement. Design Requirements Table 33. Mechanical Design Requirements #Mechanical Design RequirementDiscussionBased on33.1The maximum weight of the AO system on the Nasmyth platform shall not exceed 10,000 kg The weight requirements are imposed by limits on what the telescope can support at various locations without changing its performance.Instrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 57233.2The maximum weight of the laser facility on the azimuth rotating part of the telescope shall not exceed 10,000 kgInstrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 57233.3The maximum weight of the beam transport system on the elevation portion of the telescope shall not exceed 150 kgInstrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 57233.4The maximum weight of the laser launch facility in the top-end module shall not exceed 150 kgInstrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 57233.5If mounted behind the f/15 secondary mirror, the launch telescope facility must allow for the removal, storage and installation of the f/15 secondary moduleRequired to support regular observatory science operations with alternative secondary mirrors.33.6If mounted behind the f/15 secondary mirror, the launch telescope facility must 1) not extend beyond the module in the x,y-directions and 2) must not extend more than 1 m beyond the top of the telescope structure.1) Error and emissivity budgets  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON501_ngao_bkg_v1-1.pdf" KAON 501 do not allow for an increased secondary obscuration 2) The dimensions of the telescope structure, dome, and allowance for safety clearance refer to drawing or document number XXX33.7The NGAO facility must fit within the mechanical constraints of a Nasmyth platform (nominally the Keck II left Nasmyth platform)Observatory standards for safety clearance when moving the telescope. Instrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 572 33.8The NGAO facility must provide access and space for the installation of each science instrument and a mechanical interface on which to mount each instrumentInstrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 57233.9The NGAO facility must provide access for routine maintenance of the elevation bearing, elevation wrap, bent Cassegrain platform and mirror cell stairwellInstrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 572, Section 1533.10The required glycol flow rate and pressure for cooling the NGAO facility shall not exceed TBD and TBD, respectively Instrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 572 Electronic/Electrical Requirements Electronic/Electrical Requirments Purpose and Objectives The purpose of this section is to describe electronic and electrical requirements for the performance, implementation and design of the NGAO electronic and electrical systems. Performance Requirements Implementation Requirements Design Requirements Table 34. Electrical Performance Requirements #Electrical Performance RequirementDiscussionBased on34.1The entire NGAO facility must not exceed a total electrical power requirement of 30 kWInstrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 57234.2The NGAO facility cabling through the azimuth wrap must not require an area of more than TBDInstrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 57234.3The NGAO facility cabling through the left Nasmyth elevation wrap must not exceed an area of more than TBDInstrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 57234.4The NGAO facility cabling through the right Nasmyth elevation wrap must not exceed an area of more than TBDInstrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 572 Safety Requirements Safety Requirements Purpose and Objectives Safety is the paramount concern for all activities at the observatory. The purpose of this section is to provide requirements related to specific safety concerns during the operation and handling of NGAO. Scope The general Observatory safety requirements that are also applicable to NGAO are already contained in the Instrumentation Baseline Requirements Document. This section covers the additional laser safety and laser projection safety requirements. Adequate earthquake restraints are also required for all systems. Laser Safety Requirements A safety system will be implemented to ensure the safe use of the laser. This safety system will include both engineering and administrative/procedural controls to assure safe operations. The system will apply ANSI Z136.1 and Z136.6 standards for safe use of laser for indoor and outdoor. The NGAO system will conform to OSHA and local codes in addition to codes specified for each subsystem. Laser Projection Safety Requirements This section covers the additional requirements on safety for projecting the laser beams outside the dome. Aircraft Safety An aircraft safety system compliant with FAA requirements must be implemented and approved by the FAA. Space Command A system must be implemented to facilitate effective communication with U.S. Space Command of projection dates and targets, and to ensure that no projection occurs on a target without Space Command approval. This requirement may be deleted if it is determined that Space Command approval is no longer required. Software Requirements Purpose and Objectives The software requirements section describes requirements for performance, implementation and design. Scope Unless otherwise indicated all of the requirements of this section apply to all software components of NGAO. Performance Requirements Implementation Requirements Design Requirements Table 35. Electrical Performance Requirements #Software Design RequirementDiscussionBased on35.1The NGAO system must be able to support the external interfaces supported by the existing AO systemsThe external keywords and EPICS channels used by the existing AO systems are documented in KAON 315, Summary of External Interfaces in the Current WFC and Implications for the NGWFC DesignKAON 31535.2The NGAO system must be able to accept tip/tilt offloads from the science instrumentScience Case Requirments  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/NGAO_SCRD_Release2_v10a_sm.pdf" KAON 455 (wavefront error and tip/tilt error requirements) 35.3The NGAO system must be able to acquire and configure the AO system based on the star magnitude and spectral type provided in the target listScience Case Requirments  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/NGAO_SCRD_Release2_v10a_sm.pdf" KAON 455 (wavefront error and tip/tilt error requirements) and NGAO error budget assumptions35.4NGAO must be able to support a chopping mode for the Nuller mode of the interferometer HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 428 Requirements for Interferometry with NGAO Int Interface Requirements Purpose and Objectives This section is reserved for interface requirements that are not addressed by other portions of the document. Performance Requirements Implementation Requirements Design Requirements Optical Interface Mechanical Interface Table 36. Mechanical Interface Requirements #Mechanical Interface RequirementDiscussionBased on36.1An agreed upon kinematic interface between the NGAO opto-mechanical systems and the telescope structure must be providedKinematic interfaces are proposed so that thermal changes do not distort optical benches.Instrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 57236.2NGAO must be compatible with the interferometer dual star module (DSM) or replicate its functionalityThe current Keck AO systems interface to the interferometer via an opto-mechanical system known as the DSM.  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON428rev2.pdf" KAON 428 Requirements for Interferometry with NGAO36.3An agreed upon mechanical interface between the NGAO electronics and the telescope must be providedInstrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 57236.4An agreed upon mechanical interface between any NGAO enclosures and the telescope must be provided.Instrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 57236.5An agreed upon mechanical interface between any NGAO glycol cooled systems and the telescope instrument and/or facility glycol systems must be provided Instrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 57236.6An agreed upon mechanical interface between any NGAO CCR-cooled systems must be providedInstrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 572 Electrical/Electronic Interface Table 37. Electrical Interface Requirements #Electrical Interface RequirementDiscussionBased on37.1An agreed upon electrical interface for power between NGAO systems and the Observatory /telescope must be providedThe Observatory is responsible for providing power to the various NGAO system locations.Instrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 57237.2An agreed upon interface for communication between NGAO systems and the Observatory/telescope must be providedThe Observatory is responsible for the implementation of all cables between NGAO system locations. The Observatory must in particular approve all cabling required to go in the elevation or azimuth wraps.Instrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 572 Software Interface Table 38. Software Interface Requirements #Electrical Software Interface RequirementDiscussionBased on38.1An interface should be provided to offload tip/tilt errors to telescope pointing through the telescope drive and control system (DCS)Science Case Requirments  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/NGAO_SCRD_Release2_v10a_sm.pdf" KAON 455 (wavefront error and tip/tilt error requirements) and NGAO error budget assumptions38.2An interface should be provided to offload focus errors to the secondary mirror piston through DCSScience Case Requirments  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/NGAO_SCRD_Release2_v10a_sm.pdf" KAON 455 (wavefront error and tip/tilt error requirements) and NGAO error budget assumptions38.3An interface should be provided to offload coma errors to the secondary mirror tilt through DCSScience Case Requirments  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/NGAO_SCRD_Release2_v10a_sm.pdf" KAON 455 (wavefront error and tip/tilt error requirements) and NGAO error budget assumptions38.4An interface should be provided to offload segment stacking errors to the active control system (ACS)Science Case Requirments  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/NGAO_SCRD_Release2_v10a_sm.pdf" KAON 455 (wavefront error and tip/tilt error requirements) and NGAO error budget assumptions38.5An interface should be provided to write all appropriate NGAO keywords to the science instrument FITS headerInstrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 57238.6An interface should be provided to allow NGAO to read/write NGAO science instrument keywordsInstrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 572 Reliability Requirements Purpose A process should take place to confirm that the NGAO system will provide a high level of reliability for a 10 year lifetime. Scope Unless otherwise indicated all of the requirements of this section apply to all components of NGAO. Performance System downtime should be minimized by a combination of component reliability, ease of repair, maintenance and appropriate sparing. Table 39. Reliability Performance Requirements #Reliability Performance RequirementDiscussionBased on39.1d" 5% of observing time lost to problemsThis includes any loss to an exposure in progress and the time to start the next exposure after recovering from a faultScience Case target sample size and survey durations ( HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/NGAO_SCRD_Release2_v10a_sm.pdf" KAON 455). Analysis of current LGS system efficiency ( HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON463.pdf" KAON 463).39.2The median time between faults during observing time should be e" 3 hrs Frequent short duration faults are not acceptable since they have a high impact on science productivityScience Case target sample size and survey durations ( HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/NGAO_SCRD_Release2_v10a_sm.pdf" KAON 455). Analysis of current LGS system efficiency ( HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/KAON463.pdf" KAON 463). Spares Requirements TBD Service and Maintenance Requirements TBDRefer to Instrument Baseline Requirements,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 572. Documentation Requirements The documentation requirements are defined in the Instrumentation Baseline Requirements Document.,  HYPERLINK "http://www.oir.caltech.edu/twiki_oir/pub/Keck/NGAO/NewKAONs/Baseline_Requirements_Document.doc" KAON 572 Documentation Package Drawings Electrical/Electronic Documentation Software Glossary  REF _Ref47412256 \h Table 2Table 2 defines the acronyms and specialized terms used in this document. Table  SEQ Table \* ARABIC 2 Glossary of Terms TermDefinitionACSActive Control SystemANSIAmerican National Standards InstituteAOAdaptive OpticsDCSDrive and Control SystemDSMDual Star ModuleFAAFederal Aviation AdministrationFOVField Of ViewFWHMFull Width at Half Maximum. IFUIntegral Field UnitKAONKeck Adaptive Optics NoteKIKeck InterferometerLGSLaser Guide StarMTBFMean Time Between FailuresNGAONext Generation Adaptive OpticsNGSNatural Guide StarNIRNear InfraRedNIRC2NIR Camera 2NIRSPECNIR SPECtrometerOHANAOptical Hawaiian Array for Nanoradian AstronomyOSHAOccupational Safety and Health AdministrationOSIRISOH-Suppression InfraRed Integral field SpectrographTBCTo Be CompletedTBDTo Be DeterminedWMKOW.M. Keck Observatory  Note that z band (central wavelength 912 nm) and Y band (central wavelength 1020 nm) are of interest as well, since Ha falls in z (Y) band for redshift 0.4 (0.55). The importance of including these two bands in addition to J, H, K is currently being assessed.  Note that z band (central wavelength 912 nm) and Y band (central wavelength 1020 nm) are of interest as well, since Ha falls in z (Y) band for redshift 0.4 (0.55). The importance of including these two bands in addition to J, H, K is currently being assessed.  Accuracy required needs to be determined  Accuracy required needs to be determined  Non-redundant aperture masking is an interesting approach for this, limits currently unknown, probably requires low read noise in science detector.  Non-redundant aperture masking is an interesting approach for this, limits currently unknown, probably requires low read noise in science detector.      California Association for Research in Astronomy NGAO System Requirements Document  FILENAME KAON456_NGAO_SRD_v1.16.docKAON456 NGAO SRD v1.11.docKAON456 NGAO SRD v1.10.doc  FILENAME KAON456_NGAO_SRD_v1.16.docKAON456 NGAO SRD v1.113.docKAON456 NGAO SRD v1.10.doc  NGAO System Requirements Document Table of Contents  NGAO System Requirements Document Figures and Tables  NGAO System Requirements Document - PAGE 73-  FILENAME KAON456_NGAO_SRD_v1.16.docKAON456 NGAO SRD v1.11.docKAON456 NGAO SRD v1.10.doc The TOC should display 4 levels. I couldnt get it to do this. PAGE \# "'Page: '#' '"  Work out how many nearby AGNs are available for this project from Keck. Need to consider tip-tilt star availability. PAGE \# "'Page: '#' '"  Work out how many nearby AGNs are available for this project from Keck. Need to consider tip-tilt star availability.  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