Class Note for ASTR 518 with Professor Rieke at UA
Class Note for ASTR 518 with Professor Rieke at UA
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This 27 page Class Notes was uploaded by an elite notetaker on Friday February 6, 2015. The Class Notes belongs to a course at University of Arizona taught by a professor in Fall. Since its upload, it has received 18 views.
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Date Created: 02/06/15
Xray spectrum Wavelength 1pm 100nm 10nm 1nm 01 nm1A 1 1 1 cum vuv Son Xray 2ao UVi Extreme Ultraviolet 1 Hard X rays i 3 Cr 3 3 9W 1 eV 10 eV 100 eV 1 keV 10 keV Photon energy Material re ectivity for Xrays WaveIengIIn 1130 nm 10 nm I nm M nnI I I I I MgFngll EL Q Manna crysIIaIls NonnaI incidence reIIIeciivity E U I 1 Windt E11 Steams J Konright 10 an Inn an I KEV In New PnnIInn energy Bragg condition for Xray diffraction f quotdent I xx39 x igfne wa we xxxV no x I r 1 df39 Him quotjj figl ffjr Ezrsin H Rwy I I I i l l I l 1 sin 3 i I I i I i Constructive interference when mi 2d sin6 d 2A ZIA 10 keV m1 yields lt9 15O Re ection by multiple layers m7t2d sine he W Si LN dSI Mo TSi Mo Si l e A a For normal incidence e m2 rst order m 1 re ection 392d 1J2 it the two layers are approximately equal AI 114 a quarterwave plate coating Example for the EUV 90 eV 08 MoB4CSi 70 at 135 nm 06 FWHM 055 nm 50 bilayers 07 05 04 Reflectivity 03 02 P 0 c5 o 1 o I o I 0 1 9 0 01 00 120 125 130 135 140 145 Wavelength nm Bulk material re ection for Xrays The index of refraction at Xray wavelengths may be written n 1 5 i 0 1 00000 010000 001000 000100 000010 000001 01 100 Bulk material re ection for Xrays 39 For 6 gt O and 0 and if incident X rays are in vacuum I 1 then by Snell39s law Xrays will undergo total external re ection for angles measured om the surface 6 lt 66 where cos 6 1 5 Using 1st two terms of Taylor expansion 23 12 6 and for 1o4 Scanning Xray mappers Cenum elecuonlcs Gas Smrage Inlevmedial gas Svswm Conuo cuumer 1 x 2 v Commamr Propomnna coumer Xray sky from HEAOI Imaging Xray telescopes Modern mirror designs pioneered by EINSTEIN INCIDENT PARAXIIIL RADIATION Y FOCA L HYPERBOLOD SURFACE 1 1 Wolter type1 optics geometry Welter Xray telescope designs CDHFOEM WPEREOLOIU39 xmplamemoln M 2 3 IE E Type I an quot x39 quotquotM ALP REFLECTING SURF CES 1 H39r39F39ERBOLDIEIpquot x famaomlu 9 h F 39 F Type II 4 git2 quot REFLECTING EUFF39JCES Iquot Pm E ULDID i Jun 39 ELLIF39SDIE Modern Xray observatories xemy Telescope Mirrurs Mmercneraeterisne Einstein EXOSAT ROSAT EBXRTASCA Chandra XMM aperture diameter 58 em 23 em 33 em 12 d is 1 2 m 0722de mums 4 95M 2 nested 4 nested 3 95M 4 nested 5x nested one module me module geometric area 350 80 1140 13310de 1100 SEEM d 135 yang 195 4070 90110 233135 2145 2751 1840 axcmm focal ength m 3 45 1 09 2 4 3 s 10 7 5 minor coating Ni Au Au Au 1r An highest energy focused kev 5 2 2 12 10 10 on axis reselutmn aresee 4 1x 4 75 0 5 20 Chandra design donly veuecled second SCI 0 Your X rays nested muruvs J vocal 7 plane I 1 X mys f fnsrselof X rays tour nested rrlrroys Mirror elements are 08 m long and from 0 6 m to L2 rn in diammc39 Performance of CHANDRA optics I A 50 85 EE diameter seconds of arc o N o 0 AR Lac HRC I In O 0277 kev simulation H 1490 keV simuIaIion A a 4950 keV Simulation N n A 9150 keV Simulation 539 a l l I I 0 5 10 15 Off Axis Angle minutes of arc Chandra s View of M83 Chandra 038 keV The giant collection area of XMMNewton 3X58 concentric Woltertype P mirrors lt30 arcmin grazing gt v incidence angles to achieve high throughput at high energies Xray detectors Proportional counter awards preampli er u r muming wire U pulsa mV quot 39 hrgm entrance window H Xrays high uhage supply on rm ntng wire mun ult1snn Vnn Voltage spike proportional to hv eg IPC on EINSTEIN HEA02 5mm m r a m m mmm w muan Large Area Xenon lled 0 Pro rtionalCo 39 LKXPC 001 Counters 3 E 39ecu39ve area 6000c 2 FOV 1x1 deg Range 27100 keV Xray detectors Scintillation detector encapsulamd Dynaaes mummy thl caupllng Iayevi Fholnmulllplmr cmm X ray Ann vv tho czmude Elecrons mun volume Typically Nal or CSI Voltage spike s or nspropor1ional to hv Xray detectors Microchannel plates MCP Electron Gain lncidenl erzy Phnlnn ELECYROD NG Accelerating anlzge MICRDCHANNEL PLATE Secnndzly Ele rnns A ems smucmRE CHANNELS ouwm mums U3 J Xray detectors CCDs ACIS 10x1024x1024 CCDs for imaging and spectroscopy Integration time 02 to 3 sec Readout time 41 ms to avoid pileup Energy resolution given by number of electronhole pairs created with 36eV per pair Can suffer radiation damage ACIS on CHANDRA ConstellationX Xray lg x observatory 0f the future f Atlas V551 Stable and Quasistable orbital locations I 15 um I Mann39s Orbit Tn Sun Euquot Looking Dawn on m Edipric Mm Characteristics of ConX Baseline Mission Characteristics Overall Band Pass I13 to 4D ke u Effective 35 1 one on2 over 323 1 o ke u39 15 cm2 at1IJ1IleV 1 anon cm2 at 125 kev enun emz at an new Spectral resolving power 125 over 03 1 ke d F39a iI HlilE 39IlEu SDI over 110 liequot in central 35 aremin only 2400 at El lushr in central 2 5 arcmin only 3910 over 1U 4IZI he Angular resolution 3915 arose over I13T lze v 30 arose over T 4IJ lie vf Field of u iew IjFCl IJ El aromin on a side Mission lifetime l5 years oonsu maoles for 1 El yea rs Projected launch date 2015 funding dependent Anticipated sensitivity of Con X 7 I I Callor39irriefei I 397 10000 E Egon X HXT NE Gratings o 1000 3 7 as E E E lt 100 XMM gratings Chandra gratings 0 a E l E a 7 w t o i i 9 7 N Lu 10 2 539 K 73 E II quot39x E T 1 I L 025 10 ll Energy keV Optical arrangement for low medium energy ConX telescopes i Transition edge sensor microcalorimeters TES of XMS 3 I Operated at mum wunu Hbit tKi F H 1444 mquot We superconductor V n tummy 1 ultra transrtlon z n IIauInuIInuuuuuuuna mmugmqu temperature 1 f E I Remmee mOhm 96 98 100 102 104 Temperature mK detected FWHM 235 4kTEmaX12 14ev for 01 10 keV Hard Xray telescopes HXT aboard ConX 640 keV 40 cm 474 M NH Mirror 3 i 1 J I 1 J 1 39 j 10M i Focal Length 1 I gt 1 31 39 39 1 dezTeiarrays 121 39 quot1 5 Hard X ray Imaging Camera
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