30-meter cabin refurbishment for a large Field Of View: status of on-going study S.Leclercq 28/04/2008.

Slides:



Advertisements
Similar presentations
Software-supported Development of Optical Components Matthias Haupt Software-supported Development of Optical Components 2007 AutoOptics Short Course at.
Advertisements

Hall C SHMS Fringe Field Analysis Michael Moore Hall C Winter Meeting
Measuring film thickness using Opti-Probe
1 ATST Imager and Slit Viewer Optics Ming Liang. 2 Optical layout of the telescope, relay optics, beam reducer and imager. Optical Layouts.
LWIR FPA Mirror Image Problem & Recovery April 11, 2011 Roy W. Esplin Dave McLain.
LIGHT AND THE RETINAL IMAGE: KEY POINTS Light travels in (more or less) straight lines: the pinhole camera’s inverted image Enlarging the pinhole leads.
Practical Optics Class Opti696D, Fall Laser Bar Code Scanner Chunyu Zhao.
Myriam Newman April 13, 2007 Laser-Wire 1 Myriam Newman LC-ABD Meeting University of Oxford Thursday, April 13 Lens Performance Review Laser-Wire Team.
A Narrow Field Lobster Eye Telescope Dick Willingale – AXRO December 2014 A Narrow Field Lobster Eye Telescope (for SVOM and similar) Dick Willingale Adrian.
FDWAVE : USING THE FD TELESCOPES TO DETECT THE MICRO WAVE RADIATION PRODUCED BY ATMOSPHERIC SHOWERS Simulation C. Di Giulio, for FDWAVE Chicago, October.
SXC meeting SRON, July 19-20, SXC meeting 19-20/07/2007 Alignment Positioning of mirror with respect to detector (internal). Positioning of total.
SLAC National Accelerator Center
Keck I Cassegrain ADC: Preliminary Design Overview UCO/Lick Observatory 15 October 2003.
1 Laser Beam Coherence Purpose: To determine the frequency separation between the axial modes of a He-Ne Laser All sources of light, including lasers,
Chapter 16.3 – Reflection and Color
SIW 2003 The antenna element Ravi ATNF, Narrabri 1.The role of the antenna in a Fourier synthesis radio telescope 2.The Compact array antenna.
MAGIC II Mirrors and reflector M. Doro Udine. MAGIC Collaboration Meeting. 2006/05/10-13.
FLAO Alignment Procedures G. Brusa, S. Esposito FLAO system external review, Florence, 30/31 March 2009.
Chris A. Mack, Fundamental Principles of Optical Lithography, (c) Figure 3.1 Examples of typical aberrations of construction.
Doc.: IEEE /0630r0 Submission May 2015 Intel CorporationSlide 1 Verification of IEEE ad Channel Model for Enterprise Cubical Environment.
All these Sky Pixels Are Yours The evolution of telescopes and CCD Arrays: The Coming Data Nightmare.
Could CKOV1 become RICH? 1. Characteristics of Cherenkov light at low momenta (180 < p < 280 MeV/c) 2. Layout and characterization of the neutron beam.
Optical Alignment with Computer Generated Holograms
WFS Preliminary design phase report I V. Velur, J. Bell, A. Moore, C. Neyman Design Meeting (Team meeting #10) Sept 17 th, 2007.
NGAO Alignment Plan See KAON 719 P. Wizinowich. 2 Introduction KAON 719 is intended to define & describe the alignments that will need to be performed.
Wide-field, triple spectrograph with R=5000 for a fast 22 m telescope Roger Angel, Steward Observatory 1 st draft, December 4, 2002 Summary This wide-field,
COrE+ Optics options.
Tibor Agócs Purpose of the talk  Wide-field spectroscopy/imaging is the driver  MOS  IFU  NB/WB imager  Current FOV is 40 arcmin – it’s.
 Design  Manufacturing  Recent X-Ray tests  Status Vadim Burwitz, Peter Friedrich on behalf of the eROSITA team.
SOLAR TRACKING SYSTEM.
ASTRI SST-2M The Prototype monolithic 1.8 m
Integration and Alignment of Optical Subsystem Roy W. Esplin Dave McLain.
Ch. 14 Light and Reflection. Spherical aberrations – a blurred image produced from rays that reflect at points on a mirror far from the principle axis.
Axial color. Lateral color Plane parallel plate.
September 28, 2007LGS for SAM – PDR – Optics1 LGS for SAM Optical Alignment R.Tighe, A.Tokovinin. LGS for SAM Design Review September 2007, La Serena.
MCAO Adaptive Optics Module Subsystem Optical Designs R.A.Buchroeder.
COLD FRONT END Stephen Muchovej Caltech. CONSIDERATIONS RF System Itself Physical Considerations Packaging Mounting.
STATUS REPORT OF FPC SPICA Task Force Meeting March 29, 2010 MATSUMOTO, Toshio (SNU)
PACS IIDR 01/02 Mar 2001 FPFPU Alignment1 D. Kampf KAYSER-THREDE.
Geometric Optics. An object inside the focus casts a virtual image that is only focused by the eye.
Update to End to End LSST Science Simulation Garrett Jernigan and John Peterson December, 2004 Status of the Science End-to-End Simulator: 1. Sky Models.
SPIE Optics for EUV, X-Ray, and Gamma-Ray Astronomy VI
PACS SVR 22/23 June 2006 PACS FPU Subunits1 FM FPU Subunits A. Poglitsch.
ZTF Optics Design P. Jelinsky ZTF Technical Meeting 1.
Eusoballoon optics test Baptiste Mot, Gilles Roudil, Camille Catalano, Peter von Ballmoos Test configuration Calibration of the light beam Exploration.
September 16, 2008LSST Camera F2F1 Camera Calibration Optical Configurations and Calculations Keith Bechtol Andy Scacco Allesandro Sonnenfeld.
Zero field The 25 ‑ m f /0.7 primary mirror for the Giant Magellan Telescope (GMT) is made of seven 8.4 ‑ m segments in a close packed array. Each of the.
Absolute Calibration of Null Correctors Using Dual-Computer- Generated Holograms (CGHs) Proteep Mallik, Jim Burge, Rene Zehnder, College of Optical Sciences,
Welcome to the technical meeting on the future bolometer instrument for the IRAM 30m telescope Monday morning: presentations: context and site, 10 arcmin.
Binospec - Next Generation Optical Spectrograph for the MMT
Light, Polarization & Color. The nature of an object’s color What are examples of color? How can we tell one shade of a color from another? Do objects.
Plan in summer shutdown Magnet -SF1FF -Swap of QEA magnet - Multipole field of Final Doublet IP-BSM improvement.
Image at:
ZTF Optics Design ZTF Technical Meeting 1.
On the Evaluation of Optical Performace of Observing Instruments Y. Suematsu (National Astronomical Observatory of Japan) ABSTRACT: It is useful to represent.
14FEB2005/KWCAE2-UsersGroup Astro-E2 X-Ray Telescopes XRT Setup & Structure Performance Characteristics –Effective Area –Angular Resolution –Optical Axes.
Diamond Radiator Fabrication and Assessment Brendan Pratt Fridah Mokaya Richard Jones University of Connecticut GlueX Collaboration Meeting, Jefferson.
New emittance monitor beamline
Adaptive Optics in the VLT and ELT era Optics for AO
1 SuperCam Optics & Mount Design Dathon Golish 8/2/06 Zemax Optical Design: Converts the SMT f/13.8 beam to f/5 to match SuperCam Large Flat:.75 m x.55.
Compressor Helium filled optional equivalent plane imaging laser beam dump hole in mirror for e-beam SSA and more.
Lights, Mirrors, and Lenses Light is another type of wave that carries energy. A light ray is a narrow beam of light that travels in a straight line. Light.
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,
SWCam Project Status October 3, 2012 Gordon Stacey 1.
Lab 2 Alignment.
Internal CDR meeting December 20th, 2005
l 66TH MEETING OF THE ESRF l May 2014 l Author
Green Bank Telescope Sub-reflector Stabilization (Wind)
Intra-pixel Sensitivity Testing Preliminary Design Review
Technology deconstruction for optical contact angle meter — Do you need a contact angle meter as this? Have you ever found they faked on measuring contact.
Presentation transcript:

30-meter cabin refurbishment for a large Field Of View: status of on-going study S.Leclercq 28/04/2008

New Optics Specifications 1.FOV  10’ for bolometers, FOV  7’ for heterodynes. 2.Mirrors size < 1.6 m and surface accuracy  15  m RMS. 3.Optical systems fit in limited room (+ hardware & operator). 4.Number of optical elements as small as possible. 5.M3 rotating system efficient an simple. 6.Bolometer size  % & sample  HPBW = 1.03 /D  ’ on 8 inches wafer (  ImageSize ~ 5). 7.Smallest cryostat window possible for bolometers (D < 18 cm). 8.Minimum cost  no new M2 and all elements in receiver cabin.

Current optics versus proposition Current FOV = 4.5 arcmin available for both bolometers and heterodynes. 7 mirrors in cabin + 1 or 2 lens(es) for bolometers M  3 flat M3 elliptic contour = 1040×740 M4 elliptic contour = 920×650 M3 rotate on elevation axis (Nasmyth) M3-M4 = 700 mm Proposed FOV = 10 arcmin for bolometers, 7.4 arcmin for heterodynes. 2 mirrors in cabin + 2 lenses for bolometers Mh  3 flat, Mb>3 curved M3 elliptic contour = 1440×1200 M4h elliptic contour = 1170×810 M4b elliptic contour = 1070×990 M5b elliptic contour = 980×930 M3 Nasmyth for heterodyne, 2 axes of rotation for bolometers M3-M4h = 860 mm M3-M4b = 1500 mm

Reference frame for Zemax simulations Azimuth cabin (or Nasmyth cabin or receiver cabin) Elevation cabin M1 vertex Subreflector (M2) hyperbolic Main reflector (M1) parabolic Back view Profile view = Elevation axis Top view  Simulation of the whole telescope (not equivalent lens) Vertex window

Heterodynes optics: current vs proposed Current optics Proposed optics M3 Vertex window (tilt for anti-glint) Elevation cabin walls Azimuth cabin limit Azimuth cabin walls M4 Line symbolizing the position of the cabin roof beams new M3 M4h Elevation axis wall discs Top view at 0 degree elevation angle Focus proposed Focus current F M2 shifted +1.3 mm F M2 shifted -0.8 mm F best F M2 shifted +1.3 mm FOV 7.4 arcmin Blue rays = (+FOV/2;0), Green rays = (0;+FOV/2), Red rays = (–FOV/2;0), Yellow rays = (0;–FOV/2) FOV 4.8 arcmin (maximum possible)

Through focus spot diagram, heterodynes Current optics Proposed optics =0.87mm  foc=5cm circle = Airy disc FOV 4.8 arcmin (maximum possible) FOV 7.4 arcmin Blue = (+FOV/2;0), Green = (0;+FOV/2), Red = (–FOV/2;0), Yellow = (0;–FOV/2), Magenta = (0;0)

Current optics Proposed optics FOV ~4 arcmin FOV =10 arcmin Bolometers optics: Current Vs Proposed Top view at 0 degree elevation angle M3 M5 M6 Vertex window (tilt for anti-glint) Elevation cabin walls Azimuth cabin walls M4 Line symbolizing the position of the azimuth cabin bars M7 M3 M5b M4 bolometer M4 heterodyne Blue rays = (+FOV/2;0), Green rays = (0;+FOV/2), Red rays = (–FOV/2;0), Yellow rays = (0;–FOV/2) Elevation axis wall discs Fit mirrors in allocated place Minimize reflection angles Minimize window size Maximize FOV  Few possibilities  Outer spots diverge quickly

Profile view at 0 degree elevation angle M3 M4 M5 M6 Vertex window Elevation cabin floor Step at cabins interface Azimuth cabin limit Azimuth cabin - roof bar - tilted bar M3 M4 bolometer M5 bolometer bolts elevation axis lid wall disc M4h FOV ~4 arcmin FOV =10 arcmin Bolometers optics: current vs proposed Blue rays = (+FOV/2;0), Green rays = (0;+FOV/2), Red rays = (–FOV/2;0), Yellow rays = (0;–FOV/2) Current optics Proposed optics

Back view at 0 degree elevation angle M3 M5 M6 Vertex window Azimuth cabin walls M4 Azimuth cabin roof bars M7 M3 M5 bolometer M4 bolometer M4 heterodyne Elevation axis wall discs FOV ~4 arcmin FOV =10 arcmin Bolometers optics: current vs proposed Blue rays = (+FOV/2;0), Green rays = (0;+FOV/2), Red rays = (–FOV/2;0), Yellow rays = (0;–FOV/2) Current optics Proposed optics Optical surfaces flat and quadric surfaces Optical surfaces flat and quadric + Zernike aspheric corrections

Through focus spot diagram, bolometers Current optics (MAMBO 2)Proposed optics =0.87mm  foc=5cm circle = Airy disc FOV 3.5 arcmin FOV 10 arcmin Blue = (+FOV/2;0), Green = (0;+FOV/2), Red = (–FOV/2;0), Yellow = (0;–FOV/2), Magenta = (0;0) M2 shift = 0.9 mm M2 shift = 0 mm. Acceptable M2 shift =  0.8 mm   F ~ 15 mm 4  4 pixels to sample HPBW PSF = Airy * Aberration Elevation = 0 

Through focus spot diagram, bolometers Current optics (MAMBO 2)Proposed optics =0.87mm  foc=5cm circle = Airy disc FOV 3.5 arcmin FOV 10 arcmin Blue = (+FOV/2;0), Green = (0;+FOV/2), Red = (–FOV/2;0), Yellow = (0;–FOV/2), Magenta = (0;0) M2 shift = 0.9 mm M2 shift = 0 mm. Acceptable M2 shift =  0.8 mm   F ~ 15 mm 4  4 pixels to sample HPBW PSF = Airy * Aberration Elevation = 60 

Conclusion Heterodyne optics ready for realization phase. Bolometer optics need refinement, but is ready for approval. FOV significantly increased while keeping everything in the receiver cabin  efficient, cheap and secured solution. New M3 must be mounted on 2 rotating axes (its own azimuth and elevation)  electronics and software control, laser alignment. M4h must be mounted on translation rail. M4b, M5b, L6 and L7 have curved surfaces with complex aspheric corrections. To do: Solid Works ; M3 and M4h motorized mounts ; mechanical structure & support ; laser system ; electronics ; control software ; buy raw material ; chopper replacement ; machining ; mounting. Estimated budget ~ keuros. Estimated timing ~ if design approval in may  ready for winter 2009.

Extra slides

Short chronology of the study Late 90s: Astrophysics and technology  large Fields Of View (FOV) : Early concepts to increase the 30m FOV (S.Navarro)  new optics in receiver cabin, elements in main dish (M1) structure, new subreflector (M2). Fall 06: Optical software, current system in Optalix and Zemax, FOV study. May 07: 1 st proposition for a new optical design, all in “receiver cabin” with a non-Nasmyth motorized M3  14.5’ for low cost. Jan 08 : 3 rd proposition refining specifications  11.4’ for bolo, 7.4’ for hetero. Feb 08 : start optimization of designs based on 3 rd proposition. Apr 08 : 1 design meets specifications  10’ bolo, 7.4’ hetero. June 08 : start realization phase if proposed design is approved. Winter 09 : new optics in the 30m receiver cabin.

New bolo optics: multi fields shaded model, cryostat window, image spots,through-focus spot diagram

New bolo optics: behaviour with elevation change

New bolo optics: FFT PSF (linear and log), Wavelengths spots diagrams, FFT MTF

New bolo optics: RMS vs Focus, RMS vs wavelengths, Encircled energy, RMS vs Fields

Project planning