P3K WFS development meeting #3 V VelurCaltech Optical Observatories Pasadena, CA 91125. 02/09/2007.

Slides:



Advertisements
Similar presentations
EIS Design Optimization Criteria Overall Length < 3 meters Overall Width < 0.5m Telescope Mirror Diameter 150mm Plate scale 1 arc-sec/pixel spatial –13.5.
Advertisements

30-meter cabin refurbishment for a large Field Of View: status of on-going study S.Leclercq 28/04/2008.
1 ATST Imager and Slit Viewer Optics Ming Liang. 2 Optical layout of the telescope, relay optics, beam reducer and imager. Optical Layouts.
C. Beichman, Dimitra Touli, Gautam Vasisht, Roger Smith Tom Greene
Demetrio Magrin INAF – Astronomical Observatory of Padova Optical Design Catania, 11/06/2014.
LBT AO Progress Meeting, Arcetri Walter Seifert (ZAH, LSW) The LBT AO System and LUCIFER 1.Requirements for the commissioning of LUCIFER:
Trade Study Report: Fixed vs. Variable LGS Asterism V. Velur Caltech Optical Observatories Pasadena, CA V. Velur Caltech Optical Observatories Pasadena,
Impact of Cost Savings Ideas on NGAO Instrumentation December 19, 2008 Sean Adkins.
Low order wavefront sensor trade study Richard Clare NGAO meeting #4 January
1 NGAO Instrumentation Studies Overview By Sean Adkins November 14, 2006.
LGS WFS Design Status & Issues Dekany, Delacroix, & Velur Caltech Optical Observatories.
1 Laser Guide Star Wavefront Sensor Mini-Review 6/15/2015Richard Dekany 12/07/2009.
Object selection ideas for NGAO NGAO Meeting #6 Anna Moore April 26, 2007.
PALM-3000 HOWFS Design Update 2/27/08 C. Baranec Pasadena, CA February 27 th 2008.
Keck Next Generation Adaptive Optics Team Meeting 6 1 Optical Relay and Field Rotation (WBS , ) Brian Bauman April 26, 2007.
LO WFS Summit 6/19/2015Richard Dekany A Joint Meeting of the NGAO, IRIS, and K1 LO WFS Teams 12/15/2009.
WFS Preliminary design phase report I V. Velur, J. Bell, A. Moore, C. Neyman Design Meeting (Team meeting #10) Sept 17 th, 2007.
PHARO (2?) James Lloyd (Cornell). PHARO is the Palomar Workhorse AO Instrument Commissioned in early 1998 Built at Cornell: Tom Hayward/Bernhard Brandl.
NGAO Instrumentation Cost Drivers and Cost Savings September 2008 Sean Adkins.
NGAO Science Instruments Build to Cost Status February 5, 2009 Sean Adkins.
NGAO NGS WFS design review Caltech Optical Observatories 31 st March 2010.
NGAO NGS WFS design review Caltech Optical Observatories 1 st April NGAO WFS design, Caltech Optical Observatories.
P3K WFS development meeting #2 V Velur Caltech Optical Observatories Pasadena, CA
LGS wavefront sensor : Type and number of sub-apertures NGAO Team Meeting #4 V. Velur Caltech Optical Observatories 01/22/2007.
NGAO NGS WFS design review Caltech Optical Observatories 1 st April NGAO WFS design, Caltech Optical Observatories.
Performance analysis of NGAO NGSWFS with and without the IF dichroic Caltech Optical Observatories 6 th April, 2010.
1 NGAO Science Instrument Reuse Part 1: NIRC2 NGAO IWG December 12, 2006.
NGAO NGS WFS design review Caltech Optical Observatories 1 st April NGAO WFS design, Caltech Optical Observatories.
NGAO Laser Guide Star wavefront sensor Optical Design 17/16/2015Caltech Optical Observatories PD Phase LGS WFS Mini-Review.
MCAO Adaptive Optics Module Subsystem Optical Designs R.A.Buchroeder.
A visible-light AO system for the 4.2 m SOAR telescope A. Tokovinin, B. Gregory, H. E. Schwarz, V. Terebizh, S. Thomas.
STATUS REPORT OF FPC SPICA Task Force Meeting March 29, 2010 MATSUMOTO, Toshio (SNU)
MIRHES (Mid-IR high-resolution echelle spectrometer) MIRHES team.
AO for ELT – Paris, June 2009 MAORY Multi conjugate Adaptive Optics RelaY for the E-ELT Emiliano Diolaiti (INAF–Osservatorio Astronomico di Bologna)
15 October Observational Astronomy Direct imaging Photometry Kitchin pp ,
1 Palomar Tomograph V. Velur 1, B. Platt 2, M. Britton 1, R. Dekany 1 1 Caltech Optical Observatories, California Institute of Technology 2 Interferometry.
The Second International Workshop on Ultra-high-energy cosmic rays and their sources INR, Moscow, April 14-16, 2005 from Extreme Universe Space Observatory.
DL – IFU (Prieto/Taylor) Slicer: –25mas sampling … 0.9mm slices ~f/250 (assuming no anamorphism) Detector = 2k array of 18um pixels –Slit subtends 1-pixel.
Lyot Stop Focal Plane Mask OAP3 Out of plane spherical mirror.
NORDFORSK Summer School, La Palma, June-July 2006 NOT: Telescope and Instrumentation Michal I. Andersen & Heidi Korhonen Astrophysikalisches Institut Potsdam.
Simple Double Beam Spectrometer
IRIS OIWFS Concept Study D. Loop1, M. Fletcher1, V. Reshetov1, R
ATLAS The LTAO module for the E-ELT Thierry Fusco ONERA / DOTA On behalf of the ATLAS consortium Advanced Tomography with Laser for AO systems.
MIRI Optical System CDR, 6 th & 7 th December 2006 Mid InfraRed Instrument 07-1 Optical System Critical Design Review (CDR) TIPS Presentation: Margaret.
September 16, 2008LSST Camera F2F1 Camera Calibration Optical Configurations and Calculations Keith Bechtol Andy Scacco Allesandro Sonnenfeld.
WFIRST IFU -- Preliminary “existence proof” Qian Gong & Dave Content GSFC optics branch, Code 551.
The Active Optics System S. Thomas and the AO team.
March 31, 2000SPIE CONFERENCE 4007, MUNICH1 Principles, Performance and Limitations of Multi-conjugate Adaptive Optics F.Rigaut 1, B.Ellerbroek 1 and R.Flicker.
Wide field telescope using spherical mirrors Jim Burge and Roger Angel University of Arizona Tucson, AZ Jim
System Performance Metrics and Current Performance Status George Angeli.
Astronomical Observational Techniques and Instrumentation
N A S A G O D D A R D S P A C E F L I G H T C E N T E R I n s t r u m e n t S y n t h e s i s a n d A n a l y s i s L a b o r a t o r y APS Formation Sensor.
François Rigaut, Gemini Observatory GSMT SWG Meeting, LAX, 2003/03/06 François Rigaut, Gemini Observatory GSMT SWG Meeting, LAX, 2003/03/06 GSMT AO Simulations.
Transmission Measurement Basic Outline. Transmission Curve Describes the percentage of a signal that is transmitted through an object (filter) over a.
Introduction of RAVEN Subaru Future Instrument Workshop Shin Oya (Subaru Telescope) Mitaka Adaptive Optics Lab Subaru Telescope Astronomical.
Astronomical Spectroscopic Techniques. Contents 1.Optics (1): Stops, Pupils, Field Optics and Cameras 2.Basic Electromagnetics –Math –Maxwell's equations.
3 rd March 2006EUS Consortium meeting EUS Instrument Overview Eric Sawyer RAL.
Date of download: 6/21/2016 Copyright © 2016 SPIE. All rights reserved. AO corrected average Strehl ratios at different field positions and Sun elevations.
Date of download: 6/23/2016 Copyright © 2016 SPIE. All rights reserved. Conventional spin-scan mode reticle seeker with a single element detector. Figure.
Integral Field Spectrograph Eric Prieto LAM. How to do 3D spectroscopy.
Jeffrey R. Regester Physics Department High Point University
Astronomical Spectroscopic Techniques
Jeffrey R. Regester Greensboro Day School Greensboro NC
An Act of Kindness -
GIFTS Blackbody Subsystem Critical Design Review Blackbody Requirements Flowdown Fred Best 9 March 2004.
Astronomical Observational Techniques and Instrumentation
Resolution.
Trade Study Report: Fixed vs. Variable LGS Asterism
Observational Astronomy
NGAO Trade Study GLAO for non-NGAO instruments
Presentation transcript:

P3K WFS development meeting #3 V VelurCaltech Optical Observatories Pasadena, CA /09/2007

Agenda TT sensor design. Multiple TT stars? - RTC issues, WFE budget. Truth sensor (for focus and astigmatism) - what kind? what band?

Plate scale selection for TT sensor: Native PALAO plate scale = 381  /arcsec. HgCdTe detector has 18  pixels i.e. raw plate scale = 47 mas/pixel H-band ( =1.65mm) spot size = /D = 68 mas So for a simple 2x2 quadcell this will work for I, J and H bands. The sensitivity goes up (at the cost of dynamic range) with wavelength. The idea is to see if we can use the whole chip mmx36.8 mm = 97 arcsec.

TT sensor concept The #s on the previous page suggest that it may be a possibility to go directly onto the chip and use the entire chip to acquire stars over a ~ 90 arcsec FoV. In principle we could use multiple TT stars if the RTC would allow it.

Zemax design (90” FoV)

Spot diagram