PPT-High finesse multi-mirror optical cavities

with feedback Fabry Perot cavity in cw mode feedback amp optical issues Comparison with Sapphire parameters Fabry Perot cavity in pulsed mode Comparison with Sapphire parameters Present . eROSITA. . Design . . Manufacturing. . Recent X-Ray tests. . Status. Vadim. . Burwitz. , Peter Friedrich on behalf of the . eROSITA. team. Mirror Design. From . ABRIXAS (ROSITA, DUO) . to . eROSITA. 2013.02.13-16. 경희대. 김은빈. 김민배. 천경원 . The GMT-. CfA. , . Carnagie. , . Catolica. , Chicago Large Earth Finder (G-CLEF). . A fiber fed, optical . echelle. spectrograph. Precision radial velocity capability (PRV. April 2012 High finesse optical cavities R. Martin, G. Mueller, and D.B. Tanner University of Florida Margot Phelps, Liyuan Zhang, G. Billingsley and D. Reitze Caltech Vistas in Axion Physics April 2 PDH . Modulation Frequency. Daisuke TATSUMI. National astronomical observatory of Japan. #-----------------------------------------------------------------------. # . pdh-signal.kat. test file for Finesse 1.1. OPTICAL STRAIN GAUGE. . Marten’s mirror extensometer. Tuckerman optical strain gauge. Marten’s mirror extensometer. Working Principle. To measure Elongation. Developed by Peterson and Wahl in 1936. OPTICAL STRAIN GAUGE. . Marten’s mirror extensometer. Tuckerman optical strain gauge. Marten’s mirror extensometer. Working Principle. To measure Elongation. Developed by Peterson and Wahl in 1936. Segment Optics and Space Instruments. 1 . Department of Electrical and Telecommunications Engineering, New York City College of Technology. 2. Instrument Systems and Technology, Optics Division, NASA Goddard Space Flight Center. pathfinder Dual-Mirror telescope for the CTA-SST array . Rodolfo . Canestrari. . for the . ASTRI. collaboration. INAF. -Astronomical Observatory of . Brera. An overview on the optical design, telescope structure & . MegaWatt. pulse powers. PI: Mark . Notcutt. Boulder Precision Electro-Optics. 5733 Central Ave. Boulder CO. Buildup of circulation Power in a cavity. Spacing between both laser and cavity modes. Equals the repetition rate of the laser 402.5 MHz. Joseph M. Howard, Garrett J. West. Optics Branch, Code 551, GSFC NASA. Agenda. Optical Design Lab (ODL). Optical Specifications. Refractive vs. Reflective. Freeform Optics. Examples. 2. Welcome to the ODL!!. Peter . Kneisel. Jefferson Lab. May 19, 2014. Since I believe that I am much better in talking about the past than “predicting” the future - my view is clouded by the past 47 years – I will start with some remarks about the past. The diagram below shows an easy to congure method for measuring the wavefront error (WFE) of a Schmidt- Cassegrain telescope using an Imagine Optic HASO-32 wavefront sensor equipped with a A perture is the main lens or mirror that gathers the light to a F/ number is a measure of the speed and clarity of the optical – An astronomer wants to design a telescope that takes up the beam. . power. 1979. What. do . we. . call. as High . Power. . Linac. ?. Beam. . power. . vs . Beam. . average. . power. I x E . x . duty. . cycle. but. . energy. . is. . measured. in .