Chang,Liang YNAO,CAS July 09-10,2011 Fore Parts of Optical Design Scheme of FASOT (from telescope to spectrograph)

Slides:



Advertisements
Similar presentations
GLAO instrument specifications and sensitivities
Advertisements

MCAO Laser Launch Telescope and Periscope Celine d’Orgeville and Jim Catone.
1 ATST Imager and Slit Viewer Optics Ming Liang. 2 Optical layout of the telescope, relay optics, beam reducer and imager. Optical Layouts.
Cavity length alignement 1.Two alignement mirrors -> symmetric beam image 2.PZT sweeping with an amplitude = several FSR 3.Shift two plane mirrors (in.
Light and Telescopes Please pick up your assigned transmitter
Udo Schühle 5. Solar Orbiter EUS Consortium Meeting RAL, 3. March 2006 EUS NI spectrograph design constraints EUS NI spectrograph design constraints Udo.
Udo Schühle 5. Solar Orbiter EUS Consortium Meeting RAL, 3. March 2006 EUS NI spectrograph design constraints EUS NI spectrograph design constraints Udo.
PACS IIDR 01/02 Mar 2001 Baffle and Straylight1 D. Kampf KAYSER-THREDE.
Measures of Source Intensity 1. Radiant Flux, Φ Rate of transfer of energy Φ = δQ/δt (W)
Telescope Tear-Down Anatomy of a 114mm f/8 Newtonian Reflector.
Designing a High Resolution Fiber-Fed Spectrograph for Solar Observations Edmond Wilson Brennan Thomason Stephanie Inabnet Tamara Reed Harding University.
The Origin of Modern Astronomy Chapter 4:. Isaac Newton 1689.
IRMS Optical Subsystem Review. The Charter Confirm that the MOSFIRE design is a feasible baseline for IRMS (yes) Verify that the MOSFIRE design can achieve.
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,
Fiber Optics Defining Characteristics: Numerical Aperture Spectral Transmission Diameter.
Slide 1 Light and telescopes Just by analyzing the light received from a star, astronomers can retrieve information about a star’s 1.Total energy output.
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.
BSRT Optics Design BI Days 24 th November 2011 Aurélie Rabiller BE-BI-PM.
Optical characteristics of the EUV spectrometer for the normal-incidence region L. Poletto, G. Tondello Istituto Nazionale per la Fisica della Materia.
2.4m Telescope Group Yunnan Observatory of CAS Status of LiJET Project & The Coude Echelle Spectrograph for the Lijang 1.8m Telescope China-Japan Collaboration.
8 September Observational Astronomy TELESCOPES, Active and adaptive optics Kitchin pp
Visual Angle How large an object appears, and how much detail we can see on it, depends on the size of the image it makes on the retina. This, in turns,
D EDICATED S PECTROPHOTOMETER F OR L OCALIZED T RANSMITTANCE A ND R EFLECTANCE M EASUREMENTS Laetitia ABEL-TIBERINI, Frédéric LEMARQUIS, Michel LEQUIME.
MCAO Adaptive Optics Module Subsystem Optical Designs R.A.Buchroeder.
B.Delabre November 2003ANGRA DOS REIS - BRAZIL ESO 2 nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS ESO VLT SECOND GENERATION INSTRUMENTATION Optical.
Notre Dame extended Research Community NANOWeek: The Power of Microscopes Optics Visible light Optical microscopes and telescopes Scanning electron microscope.
ZTFC 12-segment field flattener (and related) options R. Dekany 07 Aug 2012.
Jason Kuhn 12/12/12.  Two numbers are always specified i.e  The first number specifies the scratch number, which is an indication of its severity.
The Observations of LAMOST Jianrong Shi NAOC 1/
High Resolution Echelle Spectrograph for Chinese Weihai 1m Telescope. Leiwang, Yongtian Zhu, Zhongwen Hu Nanjing institute of Astronomical Optics Technology.
Austin Roorda, Ph.D. University of Houston College of Optometry
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.
An IFU for IFOSC on IUCAA 2m Telescope
NORDFORSK Summer School, La Palma, June-July 2006 NOT: Telescope and Instrumentation Michal I. Andersen & Heidi Korhonen Astrophysikalisches Institut Potsdam.
Optical Subsystem Roy Esplin Dave McLain. Internal Optics Bench Subassembly 2 Gut Ray Dichroic Beamsplitter (MWIR reflected, LWIR transmitted) LWIR Lens.
NEXT GENERATION OPTICAL SPECTROGRAPH FOR NOAO Samuel Barden, Charles Harmer, Taft Armandroff, Arjun Dey, and Buell Jannuzi (National Optical Astronomy.
Pg 1 Spherical Grating Spectrographs CALSYS Upgrade Darragh O’Donoghue Why? Unacceptably low light throughput resulting in loss of science time while getting.
WFIRST IFU -- Preliminary “existence proof” Qian Gong & Dave Content GSFC optics branch, Code 551.
Notre Dame extended Research Community NANOWeek: The Power of Microscopes Optics Visible light Optical microscopes and telescopes Scanning electron microscope.
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 t e g r a t e d D e s i g n C a p a b i l i t y / I n s t r u m e n t S y n t h e s i s & A.
Image at:
Solar orbiter_______________________________________________.
Preliminary Foreoptics Design for FASOT of 2nd Generation L. Chang, X.M Cheng
Prof. Charles A. DiMarzio Northeastern University Fall 2003 July 2003
Wide field telescope using spherical mirrors Jim Burge and Roger Angel University of Arizona Tucson, AZ Jim
Telescopes Resolution - Degree to which fine detail can be distinguished Resolution - Degree to which fine detail can be distinguished Fundamentally an.
14FEB2005/KWCAE2-UsersGroup Astro-E2 X-Ray Telescopes XRT Setup & Structure Performance Characteristics –Effective Area –Angular Resolution –Optical Axes.
Notre Dame extended Research Community NANOWeek: The Power of Microscopes Optics/Use of light Optical microscopes and telescopes Scanning electron microscope.
Visible Spectro-polarimeter (ViSP) Conceptual Design David Elmore HAO/NCAR
Compressor Helium filled optional equivalent plane imaging laser beam dump hole in mirror for e-beam SSA and more.
Performance and sensitivity of Low Resolution Spectrographs for LAMOST Zhu Yongtian, Hou Yonghui, Hu Zhongwen Wang Lei, Wang Jianing.
Topic report C. C. Tsai Speaker: C. C. Tsai Adviser: Dr. S. L. Huang 2011/12/29 Specification of handheld probe for dermatology 2016/6/111.
Astronomical Spectroscopic Techniques. Contents 1.Optics (1): Stops, Pupils, Field Optics and Cameras 2.Basic Electromagnetics –Math –Maxwell's equations.
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.
Sasha GilevichDrive Laser Meeting December Launch System Outline General Layout Incidence Angle Effect of the broad bandwidth.
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,
July © Chuck DiMarzio, Northeastern University ECEG105/ECEU646 Optics for Engineers Course Notes Part 4: Apertures, Aberrations Prof.
Integral Field Spectrograph Eric Prieto LAM. How to do 3D spectroscopy.
Jeffrey R. Regester Physics Department High Point University
Astronomical Spectroscopic Techniques
SEMICAPS DIFFRACTIVE SIL
Interference Requirements
Observational Astronomy
Performance of Fibers in IFU
EUS NI spectrograph design constraints
Fraunhofer diffraction from Circular apertures:
The optical layout of future WFCT
Fig. 1 Experimental setup.
star 2004 june 26 nelson, Na footprints Zenith, 90 km Na layer
Presentation transcript:

Chang,Liang YNAO,CAS July 09-10,2011 Fore Parts of Optical Design Scheme of FASOT (from telescope to spectrograph)

o-beam e-beam 1. Optical Configurations Telescope Diameter:800mm,Focal ratio:F/10, FOV:1.5arcmin(30 arcsec?? or 22.5arcsec??),0.75 arcsec/fiber Ordinary beam 1600 fibers/4 units, each unit:400 fibers Extraordinary beam 1600 fibers/4 units, every unit:400 fibers Monitor system

2. Telescope Diameter: 800mm Thickness of primary mirror: 80mm Clear Aperture of secondary mirror:230mm , Thickness of secondary mirror :23mm , Focal ratio: F/10, FOV, 1.5arcmin, (The first phase of the project is 30 arcsec or 22.25arcsec??) Image size on telescope focal plane: 1.5 arc min: 3.45mm , 30arcsec:1.163mm Wavelength Range: nm , Windows material: K9 or N-BK7 Primary/Secondary mirror: zerodur with aluminum coating Airy disc

2. Amplifying System Amplifying System??=Collimator+Image Lens

For 0.75 ”,telescope image size is umSingle Lenslet size is 200um Magnification times=6.875,(200/29.089) Collimator: f=240mm, Clear 30 ” ; ’ Image lens: f= mm , Clear 30 ” ; 1.5 Image quality at Lenslet ” is 0.31 ”, better than 0.6 ” at 850nm;(80% energy in 0.6 ” ) Actual design is 0.75 ” should continue to be optimized Angle between o-beam and e-beam is 10° , Polarimeter clear apture: 1.5 ’ ” ,

LASFN9 Length:0.5019mm Fiber diameter?? 60um or 30um or 24um

THE END Thanks