WFIRST-AFTA Exit Pupil Masks (Cycle 5) for the Wide Field Instrument Bert Pasquale Cathy Marx June 30, 2015.

Slides:



Advertisements
Similar presentations
1 AN ALIGNMENT STRATEGY FOR THE ATST M2 Implementing a standalone correction strategy for ATST M2 Robert S. Upton NIO/AURA February 11,2005.
Advertisements

NIR INSTRUMENT FOR GLAO Takashi Hattori, Iwata Ikuru (Subaru Telescope)
LWIR FPA Mirror Image Problem & Recovery April 11, 2011 Roy W. Esplin Dave McLain.
SXC meeting SRON, July 19-20, SXC meeting 19-20/07/2007 Alignment Positioning of mirror with respect to detector (internal). Positioning of total.
Head-Mounted Display Sherman & Craig, pp
Impact of Cost Savings Ideas on NGAO Instrumentation December 19, 2008 Sean Adkins.
NGAO Instrumentation Overview September 2008 Updated Sean Adkins.
Head-Mounted Display Sherman & Craig, pp
NGAO Instrumentation Cost Drivers and Cost Savings September 2008 Sean Adkins.
An Optimized Pupil Coronagraph: A New Way To Observe Extrasolar Planets This work was performed for the Jet Propulsion Laboratory, California Institute.
 Design  Manufacturing  Recent X-Ray tests  Status Vadim Burwitz, Peter Friedrich on behalf of the eROSITA team.
Integration and Alignment of Optical Subsystem Roy W. Esplin Dave McLain.
WFIRST Instrument reference information July 1, 2015.
A. Ealet Berkeley, december Spectrometer simulation Note in ● Why we need it now ● What should.
14 Sep 1998R D Ekers - Synth Image Workshop: INTRODUCTION 1 Synthesis Imaging Workshop Introduction R. D. Ekers 14 Sep 1998.
Masahiro Konishi (IoA, UTokyo), SWIMS Team S W I M S.
1 Korean Activities in IR Space Missions - Past, Current and Future - Woong-Seob Jeong 1 on behalf of Korean Infrared Astronomy Group 1 KASI, Korea Ramada.
Problem 1: Given the lens and the object, ray trace to find the image
A visible-light AO system for the 4.2 m SOAR telescope A. Tokovinin, B. Gregory, H. E. Schwarz, V. Terebizh, S. Thomas.
PACS IIDR 01/02 Mar 2001 FPFPU Alignment1 D. Kampf KAYSER-THREDE.
MIT 2.71/ /22/04 wk3-b-1 Imaging Instruments (part I) Principal Planes and Focal Lengths (Effective, Back, Front) Multi-element systems Pupils &
Herschel Space ObservatoryPACS Science Verification ReviewMPE 22/23 June 2006 GJ / MPE 1 PACS Test Facility Capabilities – Cryogenics and OGSE Gerd Jakob.
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.
Progress Report Geo-CAPE Coastal Ecosystem Dynamics Imager (CEDI) IRAD Repackaging Study Jason Budinoff / GSFC Cathy Marx / GSFC May 12, 2011.
INS NIRSpec, 12 May 2005 Introduction to NIRSpec Michael Regan.
MIRI Optical System CDR, 6 th & 7 th December 2006 Mid InfraRed Instrument 07-1 Optical System Critical Design Review (CDR) TIPS Presentation: Margaret.
Hubble Space Telescope Coronagraphs John Krist JPL.
WFIRST IFU -- Preliminary “existence proof” Qian Gong & Dave Content GSFC optics branch, Code 551.
イメージスライサー型可視光 面分光ユニットの開発 Development of an integral field unit (IFU) with an image slicer Shinobu Ozaki, Satoshi Miyazaki, Takuya Yamashita, Takashi Hattori,
Optimisation of the PACS Chopper Markus Nielbock Ulrich Klaas Jeroen Bouwman Helmut Dannerbauer Jürgen Schreiber Ulrich Grözinger.
WFIRST DRM2 candidate design – payload summary At SDT7 3/1-2/2012 consensus for concepts w/out overlap w/ other mission, aka “DRM2” was: 1.1m aperture,
Mechanical design meeting, IAG, Calibration Unit mechanical design Svend M. Bauer Andreas Kelz, Emil Popow, Martin M. Roth.
NIRSpec IFU Eric Prieto Final Presentation Definition Phase May, 11th – ESTEC.
Science with Giant Telescopes - Jun 15-18, Instrument Concepts InstrumentFunction range (microns) ResolutionFOV GMACSOptical Multi-Object Spectrometer.
Wide field telescope using spherical mirrors Jim Burge and Roger Angel University of Arizona Tucson, AZ Jim
On the Evaluation of Optical Performace of Observing Instruments Y. Suematsu (National Astronomical Observatory of Japan) ABSTRACT: It is useful to represent.
System Performance Metrics and Current Performance Status George Angeli.
IFS prototype – PM3 LAM, 13/06/2003 Prototype testing at CRAL Tests at room temperature in the visible.
Astronomical Observational Techniques and Instrumentation
RAW DATA BIAS & DARK SUBTRACTION PIXEL-TO-PIXEL DQE CORR. LOCATE EXTR. WINDOW THROUGHPUT CORRECTION (incl. L-flat, blaze function, transmission of optics,
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.
May 22, 2003WFC3 Report at the June 03 TIPS1 Optical alignment and image quality testing at GSFC Test lead: Bill Eichorn, GSFC Test conductors: George.
1 Airborne Science Program EMASHSI Kick Off Meeting Interfaces NASA Ames Research Center University of California Santa Cruz Airborne Science & Technology.
06 Oct 05Space Science & Technology Dept1 Solar Orbiter Consortium Meeting 03 Mar 06 Optical Design Of Solar Orbiter Normal Incidence Spectrometer KF Middleton.
PACS IIDR 01/02 Mar 2001 Optical System Design1 N. Geis MPE.
F. Pepe Observatoire de Genève Optical astronomical spectroscopy at the VLT (Part 2)
NIRSpec - the JWST Multi-Object Spectrograph P. Ferruit (ESA), S. Arribas (CSIS), S. Birkmann (ESA), T. Böker (ESA), A. Bunker (Oxford), S. Charlot (IAP),
Astronomical Spectroscopic Techniques. Contents 1.Optics (1): Stops, Pupils, Field Optics and Cameras 2.Basic Electromagnetics –Math –Maxwell's equations.
Spatially Resolved Spectroscopy ASTR 3010 Lecture 17 Textbook Ch. 11.
WFC3 SMOV UVIS and IR Geometric Distortion Calibration and Multidrizzle Vera Kozhurina-Platais and WFC3 team.
More Zemax screenshots of the optical setup of the NIKA prototype installed since June 2012 at its final permanent position at the 30m telescope. S. Leclercq,
B. Humensky 2/24/2012 CTA-SCT Mtg - SLAC
Astronomical Spectroscopic Techniques
Pyramid sensors for AO and co-phasing
Single Object & Time Series Spectroscopy with JWST NIRCam
NIRSpec pipeline concept Guido De Marchi, Tracy Beck, Torsten Böker
30-Nov-2006 Jean-Marc Defise - CSL
Spectrophotometric calibration of the IFU spectrograph
Summary Single Object & Time Series Spectroscopy Jeff Valenti JWST Mission Scientist Space Telescope Science Institute.
The Medium Resolution Spectrometer on behalf of the MRS team
SNAP spectrograph demonstrator : Test Plan
Integral Field Spectroscopy
GIFTS Blackbody Subsystem Critical Design Review Blackbody Requirements Flowdown Fred Best 9 March 2004.
Astronomical Observational Techniques and Instrumentation
He Sun Advisor: N. Jeremy Kasdin Mechanical and Aerospace Engineering
5018 Sensors Channels 420 at 150 V.
Modern Observational/Instrumentation Techniques Astronomy 500
The Image The pixels in the image The mask The resulting image 255 X
5018 Sensors Channels 420 at 150 V.
Presentation transcript:

WFIRST-AFTA Exit Pupil Masks (Cycle 5) for the Wide Field Instrument Bert Pasquale Cathy Marx June 30, 2015

Exit Pupil Masks Overview Purpose: Provide Science Team with Normalized Exit Pupil Masks to apply to WFIRST-AFTA wavefront data Wavefront Maps and Pupil Masks are provided for each WFIRST-AFTA Cycle 5 Optical Channels: – WFC (Wide Field Channel): WIM & WSM Longwave (Thermal) – Uses Pupil Mask (Lyot Stop) Shortwave (Non-Thermal, < ~1.6µm) - Uses only Telescope Structure – IFU (Integral Field Channel) Image slicer Image Final Sensor Image Wavefronts are given in Zernike sets (See appendix) Pupil Masks are given as High-Resolution (~2k x 2k pixels) image files with lossless compression (TIFF) Wavefront Pupil (Circle Unit 1) Overlays with Mask (Square Unit 1) 2

Entrance Pupil with Payload and Optical Clocking Marks 3

Entrance Pupil and FOV Axis Orientation 4 Note: WFI “Optical FOV” Axes are in angular space, and appear flipped when overlaid with the Entrance Pupil’s projected local X/Y Axes They require a 150° rotation to transform FOV.

Individual FOV & Entrance Pupil Projection 5

Entrance/Exit Pupil Simultaneous View 6

WFC Stop, Exit Pupil & FPA Axis Orientations 7 Something

Shortwave vs. Longwave Pupil Masks Longwave Filters H158 ( ) F184 ( ) W149 ( ) GRS ( ) – Require Lyot Stop – Stop is shaped to block emissions of all telescope structures for all fields – Vignetting of outer aperture Shortwave Filters Z087 ( ) Y106 ( ) J129 ( ) – Does not require Lyot Stop (but can be used if desired for pupil continuity) – Mask includes only telescope struts and COBS (No aperture vignetting) 8

Wide Field Channel Normalized Pupil Masks 9 AFTA WFC C5 Exit Pupil Mask Norm.tif – Lyot Projection, Some Vignetting

Wide Field Channel Shortwave Pupil Masks 10 AFTA WFC C5 Exit Pupil Shortwave Norm.tif – Telescope Structure, No Vignetting

Integral Field Unit Pupil Mask 11

IFU Image Slicer Exit Pupil Detail 12

IFU Intermediate & Exit Pupil Orientation 13 Spectrograph Pupil Relay

(Back) IFU Sensor & Pupil Orientation 14 Flipped to Match X/Y Axis

IFU Image Slicer and Sensor Normalized Pupil Mask 15 AFTA IFU C5 Exit Pupil Norm.tif – Lyot Projection, Some vignetting Same Mask: Slicer & Pupil

Pupil Summary The following WFIRST-AFTA Cycle 5 Wide Field Instrument Exit Pupil Masks have been produced with correct alignment and normalization to the Wavefront Data. – AFTA WFC C5 Exit Pupil Mask Norm.tif – AFTA WFC C5 Exit Pupil Shortwave Norm.tif (No vignetting, Tel structure only) – AFTA IFU C5 Exit Pupil Norm.tif (Applies to both Slicer and Sensor Exit Pupils) Wavefront Data Files (See File: AFTA Zernike Coefficients Use.docx) – AFTA C5 WFC Zernike and Field Data xlsx – AFTA C5 PSF-Zernike Cross-Check ppt – AFTA C5 IFU PSF Samples xlsx – AFTA C5 IFU Zernike Data xlsx 16