Cryogenic Near-IR Spectro-Polarimeter (Cryo-NIRSP) Instrument Science Requirement Document
|
|
- Bruce Stone
- 5 years ago
- Views:
Transcription
1 Project Documentation Document SPEC-0056 Revision D Cryogenic Near-IR Spectro-Polarimeter (Cryo-NIRSP) Instrument Science Requirement Document M. Penn, J. Kuhn, D. Elmore * Instrument Group 28 July 2010 Prepared By: Name Signature Date David Elmore Instrument Scientist D. Elmore 10 Nov 2010 Approved By: Approved By: Approved By: Released By: Steve Hegwer Instrument Engineer Rob Hubbard Systems Engineer Thomas Rimmele Project Scientist Jeremy Wagner Project Manager S. Hegwer 10 Nov 2010 R. Hubbard 12 Nov 2010 T. Rimmele 22 Nov 2010 J. Wagner 10 Mar 2011 * Responsible author Advanced Technology Solar Telescope 950 N. Cherry Avenue Tucson, AZ Phone atst@nso.edu Fax
2 REVISION SUMMARY: 1. Date: 9/24/2001 Revision: A By: H. Lin, M. Collados (original authors) Changes: Initial version. 2. Date: 5/29/2003 Revision: B By: M. Penn Changes: Combine NIRHRS with NIRSP. 3. Date: 3/15/2006 Revision: C By: M. Penn Changes: Divide Nasmyth and Coudé instruments. 4. Date: 3/9/2009 Revision: C1 By: M. Penn Changes: Specify 1.0 arcsec/pixel, FOV 3 arcmin, thermal IR priority, re-examine science drivers. 5. Date: 3/13/2009 Revision: C2 By: M. Penn Changes: Change several requirements based on instrument group meeting. 6. Date: 4/23/2009 Revision: C3 By: M. Penn Changes: Incorporate changes from instrument group meetings; rename Cryo-NIRSP. 7. Date: 3/18/2010 Revision: C4 By: M. Penn Changes: Added responsible author (D. Elmore) 8. Date: 7/28/2010 Revision: D By: D. Elmore, J. Kuhn, D. Mickey Changes: Revised science, general features, requirements. WAIVERS: The following waivers are applicable to this specification: 1. RFW-0048: Field of View Vignetting (15-Nov-2013) SPEC-0056, Revision D Page ii
3 Table of Contents 1. Introduction PURPOSE SCOPE RESPONSIBLE AUTHOR APPLICABLE DOCUMENTS ABBREVIATIONS AND ACRONYMS Mission Example Science Cases General Features IMAGE STABILITY AND OCCULTING FLAT-FIELDING AND WAVELENGTH CALIBRATION POLARIZATION CALIBRATION CONTEXT IMAGER IMAGE SCANNING SAFETY MECHANISM DATA DISPLAYS Requirements SPECTRAL COVERAGE SPECTRAL RESOLUTION TOTAL TRANSMISSION OF THE INSTRUMENT THERMAL EMISSION POLARIZATION MODULATION POLARIMETRIC ACCURACY CALIBRATION OPTICS POLARIMETRIC ACCURACY TEMPORAL, SPATIAL AND SPECTRAL MODULATION SPATIAL SAMPLING SPATIAL FIELD OF VIEW MULTI-WAVELENGTH OBSERVATIONS IMAGE STABILITY REQUIREMENTS IMAGE ROTATION COMPENSATION CONTEXT IMAGING, REGISTRATION AND GUIDING OCCULTING ABSOLUTE PHOTOMETRIC AND SCATTERED LIGHT CALIBRATION... 9 SPEC-0056, Revision D Page iii
4 1. INTRODUCTION 1.1 PURPOSE This document defines the requirements for the Cryogenic Near-IR Spectro-Polarimeter. It is one of the first-light instruments for the ATST. 1.2 SCOPE This document covers all requirements of the Cryogenic Near-IR Spectro-Polarimeter (Cryo- NIRSP), including science requirements and some requirements derived from the science. Designers of the CRYO-NIRSP optical, mechanical, electronic, and software systems subsystems should use this document. 1.3 RESPONSIBLE AUTHOR Changes to this document are to be coordinated with the responsible author. 1.4 APPLICABLE DOCUMENTS [1] ATST Design and Development proposal [2] ATST Science Requirements Document, ATST SPEC-0001 [3] ATST ViSP Instrument Science Requirements Document, ATST SPEC-0055 [4] Collados, M. 1999, in ASP Conf. Ser. 184, Third Advances in Solar Physics Euroconference: Magnetic Fields and Oscillations, 3-22 [5] Penn, M.J., Lin, H., Tomczyk, S., Elmore, D., Judge, P. Background Induced Measurement Errors in the Coronal Intensity, Density, Velocity and Magnetic Field Solar Physics, 2004, 222, p61. [6] Penn, M. and the ATST Coronal Working Group, ATST Background Induced Measurement Errors in the Coronal Intensity, Density, Velocity and Magnetic Field, ATST RPT ABBREVIATIONS AND ACRONYMS ATST AO Cryo-NIRSP FOV GOS I c Advanced Technology Solar Telescope Adaptive optics Cryogenic Near-IR Spectro-Polarimeter Field Of View Gregorian Optical System Continuum intensity SPEC-0056, Rev D Page 1 of 9
5 2. MISSION The primary purpose of the Cryogenic Near-IR Spectro-Polarimeter (Cryo-NIRSP) is the study of solar coronal magnetic fields over a large field-of-view at near- and thermal-infrared wavelengths. Cryo-NIRSP will measure the full polarization state (Stokes I, Q, U and V) of spectral lines originating on the Sun at wavelengths from 1000 nm (500nm goal) to 5000 nm. It is the only ATST instrument with the capability of sensitively imaging the relatively faint infrared corona and the thermal infrared solar spectrum. Cryo-NIRSP depends on the full coronagraphic capabilities of ATST to observe both the near-limb (using ATST s prime-focus and secondary occulting) and the more distant corona and heliosphere. Its thermal infrared capabilities allow sensitive study of the solar disk in the CO lines. Near-limb capabilities allow unique observations of spicules, prominences, flares, and eruptive events in the low corona. SPEC-0056, Rev D Page 2 of 9
6 3. EXAMPLE SCIENCE CASES Some examples of the science topics to be addressed with Cryo-NIRSP are found in the ATST SRD and are listed below. The primary topic is listed in bold, while some predictable secondary topics, which will benefit from Cryo-NIRSP observations are listed in italics. Cryo-NIRSP and ATST in coronagraph mode are qualitatively new solar research capabilities that are not available anywhere -- we expect non-incremental, discovery science to result. SRD number Title Spatial res. (arcsec) Coronal Magnetic Fields Requirement (Goal) Spectral res. (λ/δλ) Requirement (Goal) Cadence (sec) 1.0 (0.5) 3x10 4 Few Coronal Velocity & Density in Loops Coronal Intensity Fluctuation Chromosphere heating and dynamics (CO observed on the disk) Prominence and spicule formation and evolution (Halpha and HeI near limb) 1.0 (0.5) 3x (0.5) 5 x (0.15) 1x10 5 (2x10 5 ) (0.5) 5x10 4 (1x10 5 ) 60 An instrument with a spatial pixel size of about 0.15 arc seconds and a spectral resolution of 1x10 5 will satisfy all science requirements. For the low-resolution coronal observations, requirements are appropriately met by binning by 2 or 3 in either or both dimensions. Stabilized images with image scanning and a slit spectrograph can meet temporal cadence requirements. SPEC-0056, Rev D Page 3 of 9
7 4. GENERAL FEATURES The CRYO-NIRSP will consist primarily of (a) a polarimeter, which performs the separation of the polarization state of the incident sunlight, (b) a spectrograph, which disperses the incident sunlight into a spectrum, (c) an IR camera, which records the polarized spectra provided by the polarimeter and the spectrograph and (d) an IR context camera, which images the infrared coronal emission surrounding the field-of-view of the spectro-polarimeter. Sensitive instrument performance depends on achieving a relatively low-emissivity background from the instrument surroundings and from low-emissivity ATST mirrors. Coronal performance depends on effective two-stage occulting of out-of-field light from the ATST optical train. 4.1 IMAGE STABILITY AND OCCULTING The Cryo-NIRSP requires image stabilization at the level of its 0.5 arcsec pixels. This is essential for useful long integrations and for scanning the image across the slit. Image stability is also essential for near-limb observations, as small image shifts with respect to the Gregorian occulter can produce large brightness variations from scattered light. Observations far into the corona must depend on the telescope tracking stability. We assume the near-limb stability will be achieved with a Gregorian light pick-off (or dichroic) that provides a stabilized image using M2 steering. At the Gregorian focus 0.1 arcsec tip-tilt image stability is desirable. In most circumstances the prime-focus occulter will reduce the total energy in this field to less than 0.1% of the unocculted field. An articulated secondary occulter must provide final occulting of the M2- stabilized image at the Gregorian focus. The final optical relay from the telescope into the spectrograph must present a stable, translatable, image to the Cryo-NIRSP. 4.2 FLAT-FIELDING AND WAVELENGTH CALIBRATION The flat-field calibration unit will produce a homogeneous illumination (i) by using continuum and fixed-wavelength lamps at selected wavelengths, and (ii) by moving the grating to remove solar spectral lines. Stable fixed-wavelength flat-field illumination will provide wavelength calibration over the full wavelength range of the Cryo-NIRSP 4.3 POLARIZATION CALIBRATION The Cryo-NIRSP requires a polarization calibration unit. Both the polarimeter and the calibration units will be located upstream near the telescope secondary focus, before most of the strong polarizing optical elements in the optical path. 4.4 CONTEXT IMAGER A context imager will be required to establish the spectrograph pointing relative to coronal or other solar structures, and is the only ATST coronal imaging instrument. The FOV should match the spectrograph FOV of 3 arcmin, and spatially oversample the image. The imager should have a filter system to observe specific coronal emission lines or continuum channels. 4.5 IMAGE SCANNING There must be control provisions in the optical relay between the telescope and the Cryo-NIRSP for steering the input beam so that the occulted field-of-view of the telescope can be scanned across the slit. SPEC-0056, Rev D Page 4 of 9
8 4.6 SAFETY MECHANISM The instrument must have a hardware safety mechanism that protects the context imager and spectrograph from sudden intensity increases associated with unexpected telescope re-pointing onto the disk. 4.7 DATA DISPLAYS The instrument must provide real-time user feedback in the form of graphic data displays, including context images, raw spectrograph images, Stokes parameter images, and maps of a scanned region at a selected Stokes parameter and wavelength. SPEC-0056, Rev D Page 5 of 9
9 5. REQUIREMENTS 5.1 SPECTRAL COVERAGE The Cryo-NIRSP will operate across the continuous spectrum from 1000nm (to observe the corona at 1075nm and the chromosphere at 1083nm.) to 5000 nm (e.g., molecular lines of CO 4666nm). Though subject to relatively higher levels of scattered light, useful science could be obtained at visible, nm and nm, emission lines. Requirement: Spectral coverage from 1000 nm to 5000nm Goal: 500nm to 5000nm Source: ATST Proposal 5.2 SPECTRAL RESOLUTION To properly resolve high temperature and low temperature spectral lines from the corona different spectral resolutions (and consequently dispersions) are needed. A single resolution of 30,000 combined with detector binning in the spectral dimension should provide a compromise, which will adequately address all main coronal science topics. For on-disk observations of the CO lines, resolution of at least 100,000 is required. Requirement: Spectral resolution 30,000 for coronal observations, 100,000 for disk observations Goal: Spectral resolution of 200,000 for on-disk observations Source: SRD 3.2.2, 3.2.4, 3.2.5, 3.2.7, TOTAL TRANSMISSION OF THE INSTRUMENT The coronal faintness makes it of primary importance to maximize the photon throughput of the instrument (telescope + polarimeter). As a guide, a total transmission larger than 10% is desirable Requirement: Total transmission of the instrument 10% Goal: Total transmission of the instrument 30% Source: SRD THERMAL EMISSION The thermal emission from the telescope and instrument combination detected by the instrument spectro-polarimetric camera must be minimized to low levels, below the level of a coronal emission intensity of 10 millionths of disk center brightness. Requirement: Low background emission at 3934nm (order 10 millionths disk brightness) 5.5 POLARIZATION MODULATION Polarization modulation must be provided ahead of the spectrograph slits. Provisions for geometric beam splitter image registration and calibration must be provided. Rotating wave plates as necessary to cover the operating wavelength range must be integrated into the telescope and system control. SPEC-0056, Rev D Page 6 of 9
10 5.6 POLARIMETRIC ACCURACY The amplitude of each element M ij of the overall Mueller matrix M (telescope plus polarimeter) must be calibrated to a relative accuracy ij at all time, i.e. M ij (1 ± ij), to get an absolute polarimetric accuracy of 5x10-4 I c, regardless of whether M is constant with time or not. The matrix gives the maximum absolute values of the relative uncertainties in M, 10 5x10 5x10 5x x10 5x x10 2 5x x10 5x Requirement: better than 5x10-4 Goal: 5x10-5 Source: SRD CALIBRATION OPTICS POLARIMETRIC ACCURACY The calibration optics should allow for accurate measurement of the polarization property of the telescope and the instrument to reach the polarimetric accuracy expressed by the error matrix shown above. Requirement: better than 5x10-4 Source: SRD 5.5 Requirement: 5x10-4 I c polarimetric accuracy of the calibration optics Goal: 5x10-5 Source: SRD 5.8 TEMPORAL, SPATIAL AND SPECTRAL MODULATION The modulation frequency requirement is largely determined by the design of the polarimeter. For a single beam system, the requirement for the modulation frequency is in the range of khz to tens of khz. In a dual beam system, however, this requirement can be relaxed considerably. The polarimeter thus should include a polarizing beam splitter that would provide two orthogonally polarized fields-of-view, and the instrument will provide for an optical swapping of these polarized fields, through the use of a polarization modulator such as a rotating retarder, to address seeing-induced and other systematic polarization crosstalk. In any case, the modulation frequency will be the highest possible depending on the technology development, not being less than 10 Hz (full images per second). Finally the instrument should be able to switch wavelength with the spectrograph within a period of about 10 seconds. This operation might include changing a grating angle or changing a blocking filter. Requirement: Polarimeter: Dual beam with 10 Hz frame rate; <10 sec wavelength change Goals: Change wavelengths in 1 second, 80Hz frame rate SPEC-0056, Rev D Page 7 of 9
11 5.9 SPATIAL SAMPLING The Cryo-NIRSP science topics present a variety of desired spatial resolutions. A spatial dispersion of 0.5 arc second/pixel will address most of the coronal science goals. Disk mode sampling should be at the diffraction limit for 4.7 micron wavelength. Requirement: 0.5 arc second/pixel size for coronal observations, 0.15 arc seconds sampling for disk observations (at 4.7 micron) Source: SRD 3.2.2, 3.2.4, 3.2.5, 3.2.7, SPATIAL FIELD OF VIEW The NIRSP will have the possibility to observe large fields of view, 4 arc minutes parallel to the limb and at least 3 arc minutes perpendicular to the limb. The goal is access to a full 5 arc minute FOV. Disk mode observation may be limited to 1.5 arc minutes FOV. Requirement: Coronal mode 4 arc minutes parallel to the limb, 3 arc minutes perpendicular to the limb. Disk mode, 1.5 arc minutes square. Goal: 5 arc minutes Source: SRD 3.2.2, 3.2.4, 3.2.5, 3.2.7, MULTI-WAVELENGTH OBSERVATIONS Some observations would require multiple wavelength regions to be observed with this instrument, such as 1075nm, 1080nm, 1431nm, and 3934nm coronal observations and 1565nm and 4666nm for disk observations. This instrument must have the ability to observe these different wavelength regions in succession (with about 10 sec cadence as discussed in 5.8 above). The spectrograph must be designed to efficiently access the highest priority emission lines. Requirement: Multiple wavelengths observable at high efficiency Priority: IMAGE STABILITY REQUIREMENTS The Cryo-NIRSP, with 0.5 arc second/pixel, requires image stabilization. The instrument should be provided with a tip-tilt corrected beam for both on-disk and near-limb observations. For nearlimb observations, the image stabilization should occur before the final occulting, which should be located at the Gregorian focus, and the solar limb may be used to provide a tracking signal. Requirement: Image stability with < 1.0 arc second root mean square Goal: image stability < 0.1 arc second root mean square Source: SRD 3.2.2, 3.2.4, 3.2.5, 3.2.7, IMAGE ROTATION COMPENSATION Image rotation compensation at the Coudé Lab is required. Requirement: Image rotation must be limited to less than 0.25 degrees peak-to-peak over one hour. Priority: 2 Source: Source: 3.2.2, 3.2.4, 3.2.5, 3.2.7, SPEC-0056, Rev D Page 8 of 9
12 5.14 CONTEXT IMAGING, REGISTRATION AND GUIDING In order to verify the observed field of view (and for some direct science observations) Cryo- NIRSP requires a mechanism for directing the light beam ahead of the slit or reflected from the slit to an IR sensitive imager. This imager should adequately sample the field of view of the spectrograph and should allow for filtered observations at the particular wavelengths of coronal emission lines contained within the wavelength range of the Cryo-NIRSP system. Requirement: Context imager will sample the coronal field of view with 0.5 arc seconds per pixel Goal: To achieve 0.15 arc seconds per pixel spatial sampling across the full field of view of disk observations Priority: 2 Source: 3.2.2, 3.2.4, 3.2.5, 3.2.7, OCCULTING Partial occulting will be provided by the limited field of view at the prime focus aperture. An additional occulter is required at the stabilized Gregorian image plane. The occulter will intercept a segment of the solar disk; the segment is to have a chord length of 4 arc minutes coincident with the long edge of the instrument field of view, and a radius of 16 arc minutes. The occulter must be capable of rotation about the center of view (optical axis) to provide access to any position on the solar limb. Requirement: Occulter at Gregorian image plane consisting of a circular segment with radius equivalent to 16 arc minutes on the sky and chord at least 4 arc minutes. Center of arc will be offset by 82.5 arc seconds from the optical axis, along any azimuth. It must be possible to underor over-occult by 5 arc seconds. Source: 3.2.4, 3.2.5, 3.2.7, ABSOLUTE PHOTOMETRIC AND SCATTERED LIGHT CALIBRATION Cryo-NIRSP needs to be able to observe stellar objects in order to calibrate the photometric and scattered light characteristics of the instrument. Requirement: Ability to observe stellar objects. Source: 3.2.4, 3.2.5, 3.2.7, SPEC-0056, Rev D Page 9 of 9
13 Request for Waiver RFW Number: 0048 Date Requested: 7-November-2013 RFW Title: Cryo-NIRSP field of view vignetting Contract No: 22023S Requestor: David Elmore WBS: Document/Drawing Infringed Upon: SPEC-0056 Cryo-NIRSP ISRD Summary of Issue: Unable to span full field without vignetting Next Higher Item Level Affected: N/A Items External to Contract Affected: Science performance Proposed Change and Justification: The Cryo-NIRSP ISRD requirement 5.10 calls for: Requirement: Coronal mode 4 arc minutes parallel to the limb, 3 arc minutes perpendicular to the limb. Disk mode, 1.5 arc minutes square. The modulator for the Cryo-NIRSP is in the converging beam about 550mm in front of the slit and outside the cryostat for thermal and mechanical reasons. A slightly undersized aperture vignettes the field of view while still permitting observations to the field edges. The clear aperture was originally specified to be 118mm to match the diameter of the calibration optics at the GOS. After the vendor informed us that the largest crystal optics they had ever fabricated at this thickness was 113mm clear aperture, the calibration optics were moved from the 'retarder' stage to the 'modulator' stage at the GOS since there are no longer have modulators at the GOS and thereby reduced the clear aperture to 105mm for the GOS optics. The Cryo team was asked to evaluate the consequence of a 105mm clear aperture in place of 118 for the Cryo-NIRSP modulator. Here is the response from 22 July. David and Tom, I didn't realize Don was out of Africa, but he's back and fired up zemax. With a 105mm CA modulator we'd see 50% vignetting at the edge of a 5' diameter field and 14% light loss at the 4' edge of our slit field. At 3' there is no vignetting loss. Thus, I find it hard to argue from a science requirements viewpoint that we will qualitatively suffer with your smaller (105mm) modulator. Jeff The SWG looked at this vignetting issue and concluded: the SWG does not anticipate that the proposed field of view and wavelength restrictions will have any negative impact on the critical first- instrument generation ATST science 1
14 Request for Waiver RFW Number: 0048 Corrective Actions Already Attempted: Moving the rotator into the cryostat has the consequence of a redesign of the rotator for vacuum operation, redesign of the cryostat to accommodate the rotator, and increased thermal pumping required of the Cryo-NIRSP. Documents Attached: Waiver, if granted, Adversely Affects: Performance: yes Reliability: Cost: Dimensions: Safety: Software: Weight: Maintenance: Other Risk: Impact if waiver not granted: The project would incur risk and cost increase due to the requirement of polishing crystals of an aperture larger than ever attempted. Concessions Offered: If optical technology permits, a full aperture modulator could be implemented in the future using the current rotator. Though the clear aperture fully meeting spec will be 105mm, the full aperture will be at least 10mm greater so that the light loss will be less than the estimate though polarization modulation performance may not meet specification. Please note: Both parties must sign to acknowledge acceptance of this waiver. Contractor Project Manager Work Package Manager Signature Date Signature Date Change Control Board Decision: APPROVED ADMINISTRATIVE USE ONLY Approval Date: Rejected Date: 15-November
Visible Spectro-Polarimeter (ViSP) Instrument Science Requirement
Project Documentation Document SPEC-0055 Revision D Visible Spectro-Polarimeter (ViSP) Instrument Science Requirement D. Elmore 1, H. Socas-Navarro, R. Casini 3 June 2014 Released By: Name Joseph McMullin
More informationCommon questions when planning observations with DKIST Jan 30, 2018
Common questions when planning observations with DKIST Jan 30, 2018 1. Can the DKIST instruments work together? All instruments except Cryo-NIRSP can work together and with Adaptive Optics (AO). All can
More informationNear Infrared Spectro-Polarimeter Use Case
Project Documentation RPT-0036 Revision A Near Infrared Spectro-Polarimeter Use Case S. Gibson, L. Fletcher, R. Hubbard, S. Keil, J. Kuhn, H. Lin, M. Penn Science Working Group May 2008 Approved for use:
More informationPolarimetry Working Group Recommendations on Telescope Calibration and Polarization Modulator Location
Project Documentation Document RPT-0046 Draft A3 Polarimetry Working Group Recommendations on Telescope Calibration and Polarization Modulator Location David Elmore ATST Instrument Scientist 1 November
More informationPolarization Calibration Plan
Project Documentation Document RPT-0055 Revision A Polarization Calibration Plan David Elmore Science Team 3 September 2015 Advanced Technology Solar Telescope 950 N. Cherry Avenue Tucson, AZ 85719 Phone
More informationMcMath-Pierce Adaptive Optics Overview. Christoph Keller National Solar Observatory, Tucson
McMath-Pierce Adaptive Optics Overview Christoph Keller National Solar Observatory, Tucson Small-Scale Structures on the Sun 1 arcsec Important astrophysical scales (pressure scale height in photosphere,
More informationFirst observations of the second solar spectrum with spatial resolution at the Lunette Jean Rösch
First observations of the second solar spectrum with spatial resolution at the Lunette Jean Rösch Malherbe, J.-M., Moity, J., Arnaud, J., Roudier, Th., July 2006 The experiment setup in spectroscopic mode
More informationNST Instrumentation and Data. Big Bear Solar Observatory
NST Instrumentation and Data 1.6 m Clear Aperture Off-Axis Telescope New Solar Telescope The New Solar Telescope Optical Configuration The NST configuration is a 1/5 scale copy of one segment of the
More informationpre Proposal in response to the 2010 call for a medium-size mission opportunity in ESA s science programme for a launch in 2022.
Solar magnetism explorer (SolmeX) Exploring the magnetic field in the upper atmosphere of our closest star preprint at arxiv 1108.5304 (Exp.Astron.) or search for solmex in ADS Hardi Peter & SolmeX team
More informationSouthern African Large Telescope. Prime Focus Imaging Spectrograph. Instrument Acceptance Testing Plan
Southern African Large Telescope Prime Focus Imaging Spectrograph Instrument Acceptance Testing Plan Eric B. Burgh University of Wisconsin Document Number: SALT-3160AP0003 Revision 1.0 18 February 2003
More informationPolarization Measurements at the Daniel K. Inouye Solar Telescope (formerly ATST) Valentin Martinez Pillet David Elmore
Polarization Measurements at the Daniel K. Inouye Solar Telescope (formerly ATST) Valentin Martinez Pillet David Elmore Summary Inouye Solar Telescope will observationally test models with spatial resolution
More informationInstrumental Polarization of Telescopes on Alt-Azimuth and Equatorial Mounts
Project Documentation Report #0009 Revision #A Instrumental Polarization of Telescopes on Alt-Azimuth and Equatorial Mounts Christoph U. Keller 4 December 2002 Advanced Technology Solar Telescope 950 N.
More informationAn eclipse experiment to study the solar chromosphere and spicules
An eclipse experiment to study the solar chromosphere and spicules Draft 1.2, P. G. Judge, 30 Dec 2010. An experiment is proposed to measure a critical part of the chromospheric flash spectrum during the
More informationSolar Magnetic Fields Jun 07 UA/NSO Summer School 1
Solar Magnetic Fields 2 12 Jun 07 UA/NSO Summer School 1 Solar Magnetic Fields 2 (12 June) An introduction to the instruments and techniques used to remotely measure the solar magnetic field Stokes Vectors
More informationA down-to-earth guide to high-resolution solar observations. Kevin Reardon National Solar Observatory
A down-to-earth guide to high-resolution solar observations Kevin Reardon kreardon@nso.edu National Solar Observatory Seeing Adaptive Optics Image Reconstruction Atmospheric Effects Spectral Lines Calibration
More informationVisible Spectro-Polarimeter Use Case
Project Documentation RPT-0032 Revision A Visible Spectro-Polarimeter Use Case Alexandra Tritschler, David Elmore, Craig DeForest, Peter Nelson, Rebecca Centeno-Elliot Science Working Group May 2008 Approved
More informationFIRS: A New Instrument for Multi-Wavelength Spectropolarimetry
: A New Instrument for Multi-Wavelength Spectropolarimetry Sarah Jaeggli, Haosheng Lin Institute for Astronomy, University of Hawai i is supported by the National Science Foundation Major Research Program,
More informationNICMOS Status and Plans
1997 HST Calibration Workshop Space Telescope Science Institute, 1997 S. Casertano, et al., eds. NICMOS Status and Plans Rodger I. Thompson Steward Observatory, University of Arizona, Tucson, AZ 85721
More informationExoplanets Direct imaging. Direct method of exoplanet detection. Direct imaging: observational challenges
Black body flux (in units 10-26 W m -2 Hz -1 ) of some Solar System bodies as seen from 10 pc. A putative hot Jupiter is also shown. The planets have two peaks in their spectra. The short-wavelength peak
More informationMulti-Application Solar Telescope Preliminary results
Preliminary results Shibu K. Mathew Udaipur Solar Observatory Past Present Future Telescope specs. and components Installation Optical alignment and tests Back-end instruments Preliminary observations
More informationCoronal magnetometry
Coronal magnetometry status report February 13, 2006 Philip Judge & Steven Tomczyk High Altitude Observatory, NCAR, Boulder CO, USA Coronal magnetometry p.1/21 The challenge we wish to measure coronal
More informationATST Science Requirements Document
Project Documentation Specification #0001 Revision B ATST Science Requirements Document Thomas Rimmele Science Team December 12, 2005 Advanced Technology Solar Telescope 950 N. Cherry Avenue Tucson, AZ
More informationSolar Optical Telescope onboard HINODE for Diagnosing the Solar Magnetic Fields
Solar Optical Telescope onboard HINODE for Diagnosing the Solar Magnetic Fields Kiyoshi Ichimoto 1) and HINODE/SOT-team 1) Solar-B Project Office National Astronomical Observatory /NINS 16 th International
More informationProposed National Large Solar Telescope. Jagdev Singh Indian Institute of Astrophysics, Bangalore , India.
J. Astrophys. Astr. (2008) 29, 345 351 Proposed National Large Solar Telescope Jagdev Singh Indian Institute of Astrophysics, Bangalore 560 034, India. e-mail: jsingh@iiap.res.in Abstract. Sun s atmosphere
More informationVector Magnetic Field Diagnostics using Hanle Effect
Meeting on Science with Planned and Upcoming Solar Facilities in the Country, Bangalore, India, November 2-3, 2011 Vector Magnetic Field Diagnostics using Hanle Effect M. Sampoorna Indian Institute of
More informationCASE/ARIEL & FINESSE Briefing
CASE/ARIEL & FINESSE Briefing Presentation to NRC Committee for Exoplanet Science Strategy including material from the ARIEL consortium Mark Swain - JPL 19 April 2019 2018 California Institute of Technology.
More informationGEMINI 8-M Telescopes Project
GEMINI 8-M Telescopes Project RPT-PS-G0065 The Gemini Instrumentation Program F. C. Gillett, D. A. Simons March 25, 1996 GEMINI PROJECT OFFICE 950 N. Cherry Ave. Tucson, Arizona 85719 Phone: (520) 318-8545
More informationAstronomy 203 practice final examination
Astronomy 203 practice final examination Fall 1999 If this were a real, in-class examination, you would be reminded here of the exam rules, which are as follows: You may consult only one page of formulas
More informationCoronal Magnetometry Jean Arnaud, Marianne Faurobert, Gérad Grec et Jean-Claude Vial. Jean Arnaud Marianne Faurobert Gérard Grec et Jean-Claude Vial
Coronal Magnetometry Jean Arnaud, Marianne Faurobert, Gérad Grec et Jean-Claude Vial Jean Arnaud Marianne Faurobert Gérard Grec et Jean-Claude Vial INTRODUCTION The solar corona is a high temperature and
More informationlinear polarization: the electric field is oriented in a single direction circular polarization: the electric field vector rotates
Chapter 8 Polarimetry 8.1 Description of polarized radiation The polarization of electromagnetic radiation is described by the orientation of the wave s electric field vector. There are two different cases
More informationUV spectro-polarimetry with CLASP & CLASP2 sounding rocket experiments
UV spectro-polarimetry with CLASP & CLASP2 sounding rocket experiments R. Ishikawa (1), R. Kano (1), A. Winebarger (2), D. E. McKenzie (2), F. Auchere (3), J. Trujillo Bueno (4), N. Narukage (1), K. Kobayashi
More informationExoplanets Direct imaging. Direct method of exoplanet detection. Direct imaging: observational challenges
Black body flux (in units 10-26 W m -2 Hz -1 ) of some Solar System bodies as seen from 10 pc. A putative hot Jupiter is also shown. The planets have two peaks in their spectra. The short-wavelength peak
More informationSpeckles and adaptive optics
Chapter 9 Speckles and adaptive optics A better understanding of the atmospheric seeing and the properties of speckles is important for finding techniques to reduce the disturbing effects or to correct
More informationAstro 500 A500/L-15 1
Astro 500 A500/L-15 1 Lecture Outline Spectroscopy from a 3D Perspective ü Basics of spectroscopy and spectrographs ü Fundamental challenges of sampling the data cube Approaches and example of available
More informationarxiv: v1 [astro-ph.im] 28 Jan 2017
Polarization Modeling and Predictions for DKIST Part 1: Telescope and example instrument configurations. David M. Harrington a and Stacey R. Sueoka b a National Solar Observatory, 8 Kiopa a Street, Ste
More informationIntensity Oscillations and coronal heating: ADITYA-1 Mission. Jagdev Singh, Indian Institute of Astrophysics, Bengaluru
Intensity Oscillations and coronal heating: ADITYA-1 Mission ARIES Jagdev Singh, Indian Institute of Astrophysics, Bengaluru Science with Planned and Upcoming Solar facilities Nov. 3, 2011. A low density
More informationSpectroscopy at 8-10 m telescopes: the GTC perspective. Romano Corradi GRANTECAN
Spectroscopy at 8-10 m telescopes: the GTC perspective Romano Corradi GRANTECAN Spectroscopy from large ground-based telescope At the vanguard of observational astronomy is a growing family of >8m telescopes:
More informationGoals of the meeting. Catch up with JWST news and developments: ERS and GO call for proposals are coming!!
Welcome Goals of the meeting Catch up with JWST news and developments: ERS and GO call for proposals are coming!! What is JWST capable of (focus on H 2 spectroscopy)? What do we need to do (models, lab)
More informationNIRSpec Performance Report NPR / ESA-JWST-RP Authors: T. Böker, S. Birkmann & P. Ferruit Date of Issue: 20.5.
NIRSpec Performance Report NPR-2013-011 / ESA-JWST-RP-19649 Authors: T. Böker, S. Birkmann & P. Ferruit Date of Issue: 20.5.2013 Revision: 1 estec European Space Research and Technology Centre Keplerlaan
More information1. Give short answers to the following questions. a. What limits the size of a corrected field of view in AO?
Astronomy 418/518 final practice exam 1. Give short answers to the following questions. a. What limits the size of a corrected field of view in AO? b. Describe the visibility vs. baseline for a two element,
More informationWebster Cash University of Colorado. X-ray Interferometry
Webster Cash University of Colorado X-ray Interferometry Co-Investigators Steve Kahn - Columbia University Mark Schattenburg - MIT David Windt - Lucent (Bell-Labs) Outline of Presentation Science Potential
More informationVenus 2012 transit: spectroscopy and high resolution observations proposals
IAP workshop France/Japan - March, 6th 2012 Venus 2012 transit: spectroscopy and high resolution observations proposals by Cyril Bazin, Serge Koutchmy et al. Institut d Astrophysique de Paris UMR 7095
More informationCanariCam-Polarimetry: A Dual-Beam 10 µm Polarimeter for the GTC
Astronomical Polarimetry: Current Status and Future Directions ASP Conference Series, Vol. 343, 2005 Adamson, Aspin, Davis, and Fujiyoshi CanariCam-Polarimetry: A Dual-Beam 10 µm Polarimeter for the GTC
More informationSolar Magnetic Fields Jun 07 UA/NSO Summer School 1
Solar Magnetic Fields 1 11 Jun 07 UA/NSO Summer School 1 If the sun didn't have a magnetic field, then it would be as boring a star as most astronomers think it is. -- Robert Leighton 11 Jun 07 UA/NSO
More informationNew insights from. observation. Hinode-VTT He Andreas Lagg (MPS) Saku Tsuneta (NAOJ) Ryohko Ishikawa (NAOJ/Univ. Tokyo)
New insights from Hinode-VTT He10830 observation Ryohko Ishikawa (NAOJ/Univ. Tokyo) Saku Tsuneta (NAOJ) Andreas Lagg (MPS) Hinode-VTT joint campaign (HOP71) (2008/04/29-2008/05/12) Purpose: Finding chromospheric
More informationSPITZER SPACE TELESCOPE
SPITZER SPACE TELESCOPE The Rationale for Infrared Astronomy reveal cool states of matter explore the hidden Universe provide access to many spectral features probe the early life of the cosmos WANT TO
More informationDirection - Conférence. The European Extremely Large Telescope
Direction - Conférence The European Extremely Large Telescope The E-ELT 40-m class telescope: largest opticalinfrared telescope in the world. Segmented primary mirror. Active optics to maintain collimation
More informationLecture 6: Polarimetry 2. Polarizers and Retarders. Polarimeters. Scattering Polarization. Zeeman Effect. Hanle Effect. Outline
Lecture 6: Polarimetry 2 Outline 1 Polarizers and Retarders 2 Polarimeters 3 Scattering Polarization 4 Zeeman Effect 5 Hanle Effect Christoph U. Keller, Utrecht University, C.U.Keller@uu.nl Solar Physics,
More informationOptical/IR Observational Astronomy Telescopes I: Telescope Basics. David Buckley, SAAO
David Buckley, SAAO 27 Feb 2012 1 Some other Telescope Parameters 1. Plate Scale This defines the scale of an image at the telescopes focal surface For a focal plane, with no distortion, this is just related
More informationReal Telescopes & Cameras. Stephen Eikenberry 05 October 2017
Lecture 7: Real Telescopes & Cameras Stephen Eikenberry 05 October 2017 Real Telescopes Research observatories no longer build Newtonian or Parabolic telescopes for optical/ir astronomy Aberrations from
More informationKeck Adaptive Optics Note 1069
Keck Adaptive Optics Note 1069 Tip-Tilt Sensing with Keck I Laser Guide Star Adaptive Optics: Sensor Selection and Performance Predictions DRAFT to be updated as more performance data becomes available
More informationThe Sun s Dynamic Atmosphere
Lecture 16 The Sun s Dynamic Atmosphere Jiong Qiu, MSU Physics Department Guiding Questions 1. What is the temperature and density structure of the Sun s atmosphere? Does the atmosphere cool off farther
More informationNAOYUKI TAMURA Subaru Instrument Astronomer Subaru Telescope, NAOJ
FMOS status tt report Science workshop 2011.02.2802 28-03.0202 NAOYUKI TAMURA Subaru Instrument Astronomer Subaru Telescope, NAOJ * Overview * Recent history & current status t * Schedule & future plan
More informationObserving with the Infrared Spectrograph
Observing with the Infrared Spectrograph C. Grillmair, L. Armus GO Workshop 21-22 November 2002 Outline 1) Meet the IRS IST 2) Basic IRS capabilities 3) Observing and readout modes 4) Data products and
More informationON THE POLARIZATION THE SOLAR CORONAL EMISSION LINES. E. MOGILEVSKY, B. IOSHPA, and V. OBRIDKO
ON THE POLARIZATION OF THE SOLAR CORONAL EMISSION LINES E. MOGILEVSKY, B. IOSHPA, and V. OBRIDKO Institute of Terrestrial Magnetism, Ionosphere and Radiowave Propagation, Academy of Sciences of the U.S.S.R.,
More informationHigh-Resolution Imagers
40 Telescopes and Imagers High-Resolution Imagers High-resolution imagers look at very small fields of view with diffraction-limited angular resolution. As the field is small, intrinsic aberrations are
More informationPhotometric Studies of GEO Debris
Photometric Studies of GEO Debris Patrick Seitzer Department of Astronomy, University of Michigan 500 Church St. 818 Dennison Bldg, Ann Arbor, MI 48109 pseitzer@umich.edu Heather M. Cowardin ESCG/Jacobs
More informationObservational programs at Istituto Ricerche Solari Locarno (IRSOL)
Observational programs at Istituto Ricerche Solari Locarno (IRSOL) Renzo Ramelli and IRSOL collaborators IRSOL Locarno, Switzerland Suzhou, China 24th July 2009 Scientific Collaborators affiliated to IRSOL
More informationToward Interplanetary Space Weather: Strategies for Manned Missions to Mars
centre for fusion, space and astrophysics Toward Interplanetary Space Weather: Strategies for Manned Missions to Mars Presented by: On behalf of: Jennifer Harris Claire Foullon, E. Verwichte, V. Nakariakov
More informationLCO Global Telescope Network: Operations and policies for a time-domain facility. Todd Boroson
LCO Global Telescope Network: Operations and policies for a time-domain facility Todd Boroson Network Concept Eighteen robotic telescopes ultimately ~27 2-meter, 1-meter, 40-cm Eight high-quality sites
More informationPolarimetry Techniques. K. Sankarasubramanian ISRO Satellite Centre Bangalore India
Polarimetry Techniques K. Sankarasubramanian ISRO Satellite Centre Bangalore sankark@isac.gov.in Outline Introduction Why Polarimetry? Requirements Polarization Basics Stokes Parameters & Mueller Matrices
More informationCalibration of an Ultra-High Accuracy Polarimeter at the Part-Per-Million Level
Calibration of an Ultra-High Accuracy Polarimeter at the Part-Per-Million Level Sloane J. Wiktorowicz The Aerospace Corporation Calcon Technical Meeting August 24, 2016 2016 The Aerospace Corporation Ultra-High
More informationLab 4: Stellar Spectroscopy
Name:... Astronomy 101: Observational Astronomy Fall 2006 Lab 4: Stellar Spectroscopy 1 Observations 1.1 Objectives and Observation Schedule During this lab each group will target a few bright stars of
More informationReduction procedure of long-slit optical spectra. Astrophysical observatory of Asiago
Reduction procedure of long-slit optical spectra Astrophysical observatory of Asiago Spectrograph: slit + dispersion grating + detector (CCD) It produces two-dimension data: Spatial direction (x) along
More informationOptics Optical Testing and Testing Instrumentation Lab
Optics 513 - Optical Testing and Testing Instrumentation Lab Lab #6 - Interference Microscopes The purpose of this lab is to observe the samples provided using two different interference microscopes --
More informationHERSCHEL/UVCI ALIGNMENT PLAN
DIPARTIMENTO DI ASTRONOMIA E SCIENZA DELLO SPAZIO HERSCHEL/UVCI ALIGNMENT PLAN M. Romoli (a), G. Corti (a), F. Landini (a) (a) Dipartimento di Astronomia e Scienza dello Spazio, Università di Firenze (Italy)
More informationNext Generation UV Coronagraph Instrumentation for Solar Cycle-24
J. Astrophys. Astr. (2008) 29, 321 327 Next Generation UV Coronagraph Instrumentation for Solar Cycle-24 John L. Kohl 1,, Rajmal Jain 2, Steven R. Cranmer 1, Larry D. Gardner 1, Anil K. Pradhan 3, John
More informationLecture 8: Polarimetry 2. Polarizers and Retarders. Polarimeters. Scattering Polarization. Zeeman Effect. Outline
Lecture 8: Polarimetry 2 Outline 1 Polarizers and Retarders 2 Polarimeters 3 Scattering Polarization 4 Zeeman Effect Christoph U. Keller, Utrecht University, C.U.Keller@uu.nl Observational Astrophysics
More informationChemistry 524--Final Exam--Keiderling May 4, :30 -?? pm SES
Chemistry 524--Final Exam--Keiderling May 4, 2011 3:30 -?? pm -- 4286 SES Please answer all questions in the answer book provided. Calculators, rulers, pens and pencils are permitted. No open books or
More informationAbsolute calibration in solar scattering polarization measurements with ZIMPOL
Absolute calibration in solar scattering polarization measurements with ZIMPOL Michele Bianda 1, Renzo Ramelli 1, Daniel Gisler 1,4, Jan Stenflo 1,2, Ivan Defilippis 3 1) IRSOL, Istituto Ricerche Solari
More informationGround and On-Orbit Characterization and Calibration of the Geosynchronous Imaging Fourier Transform Spectrometer (GIFTS)
Ground and On-Orbit Characterization and Calibration of the Geosynchronous Imaging Fourier Transform Spectrometer (GIFTS) John D. Elwell 1, Deron K. Scott 1 Henry E. Revercomb 2, Fred A. Best 2, Robert
More informationIntroduction to the Chinese Giant Solar Telescope
First Asia-Pacific Solar Physics Meeting ASI Conference Series, 2011, Vol. 2, pp 31 36 Edited by Arnab Rai Choudhuri & Dipankar Banerjee Introduction to the Chinese Giant Solar Telescope Y. Y. Deng (On
More informationGEMINI 8-M Telescopes Project
GEMINI 8-M Telescopes Project RPT-I-G0057 Principles Behind the Gemini Instrumentation Program M. Mountain, F. Gillett, D. Robertson, D. Simons GEMINI PROJECT OFFICE 950 N. Cherry Ave. Tucson, Arizona
More informationThe Austrian contribution to the European Extremely Large Telescope
The Austrian contribution to the European Extremely Large Telescope Werner W. Zeilinger consortium Evolution of Telescope Size Scientific American 2015 14/15.Dec.2015 From Ground to Space 2 Discoveries
More informationIntroduction to Daytime Astronomical Polarimetry
Introduction to Daytime Astronomical Polarimetry Sami K. Solanki Max Planck Institute for Solar System Research Introduction to Solar Polarimetry Sami K. Solanki Max Planck Institute for Solar System Research
More informationOptical/IR Observational Astronomy Spectroscopy. David Buckley, SALT
David Buckley, SALT 1 Background is really just monochromatic photometry History 1637 Descartes explained the origin of the rainbow. 1666 Newton s classic experiments on the nature of colour. 1752 Melvil
More informationSolar-B. Report from Kyoto 8-11 Nov Meeting organized by K. Shibata Kwasan and Hida Observatories of Kyoto University
Solar-B Report from Kyoto 8-11 Nov Meeting organized by K. Shibata Kwasan and Hida Observatories of Kyoto University The mission overview Japanese mission as a follow-on to Yohkoh. Collaboration with USA
More informationE-ELT Overview. Alistair McPherson Programme Manager
E-ELT Overview Alistair McPherson Programme Manager Science drivers Planets in other stellar systems Imaging and spectroscopy The quest for Earth-like exo-planets Stellar populations In galaxies inaccessible
More informationMERIS US Workshop. Instrument Characterization Overview. Steven Delwart
MERIS US Workshop Instrument Characterization Overview Steven Delwart Presentation Overview On-Ground Characterisation 1. Diffuser characterisation 2. Polarization sensitivity 3. Optical Transmission 4.
More informationIntroduction to SDSS -instruments, survey strategy, etc
Introduction to SDSS -instruments, survey strategy, etc (materials from http://www.sdss.org/) Shan Huang 17 February 2010 Survey type Status Imaging and Spectroscopy Basic Facts SDSS-II completed, SDSS-III
More informationSpitzer Space Telescope
Spitzer Space Telescope (A.K.A. The Space Infrared Telescope Facility) The Infrared Imaging Chain 1/38 The infrared imaging chain Generally similar to the optical imaging chain... 1) Source (different
More informationRobert Stobie Prime Focus Imaging Spectrograph Status. On-Sky Grating Spectroscopy Performance: Method
Board Papers: * * Robert Stobie Prime Focus Imaging Spectrograph Status On-Sky Performance/ Acceptance Data Package Throughput/ grating performance Still to complete: Fabry Perot, PSF, Polarimetry Fixes
More informationFORCAST: Science Capabili2es and Data Products. William D. Vacca
FORCAST: Science Capabili2es and Data Products William D. Vacca Faint Object infrared Camera for the SOFIA Telescope (FORCAST) SWC (blue) Light from telescope LWC (red) Facility Instrument PI: Terry Herter
More informationFMOS. A Wide-field Multi-Object Infra-red Spectrograph for the Subaru Telescope. David Bonfield, Gavin Dalton
FMOS A Wide-field Multi-Object Infra-red Spectrograph for the Subaru Telescope David Bonfield, Gavin Dalton David Bonfield Oxford University Wide Field NIR Spectroscopy WFCAM, VISTA are about to deliver
More informationPhase-Referencing and the Atmosphere
Phase-Referencing and the Atmosphere Francoise Delplancke Outline: Basic principle of phase-referencing Atmospheric / astrophysical limitations Phase-referencing requirements: Practical problems: dispersion
More informationSpectro polarimetry with liquid crystals
Mem. S.A.It. Vol. 78, 203 c SAIt 2007 Memorie della Spectro polarimetry with liquid crystals J.-M. Malherbe 1, Th. Roudier 2, J. Moity 1, P. Mein 1, J. Arnaud 3, and R. Muller 2 1 Observatoire de Paris,
More informationThermal And Near infrared Sensor for carbon Observation (TANSO) On board the Greenhouse gases Observing SATellite (GOSAT) Research Announcement
Thermal And Near infrared Sensor for carbon Observation (TANSO) On board the Greenhouse gases Observing SATellite (GOSAT) Research Announcement Appendix A Outlines of GOSAT and TANSO Sensor GOSAT (Greenhouse
More informationThe HST Set of Absolute Standards for the 0.12 µm to 2.5 µm Spectral Range
Instrument Science Report CAL/SCS-010 The HST Set of Absolute Standards for the 0.12 µm to 2.5 µm Spectral Range L. Colina, R. Bohlin, D. Calzetti, C. Skinner, S. Casertano October 3, 1996 ABSTRACT A proposal
More informationThe importance of ground-based observations of the solar corona
The importance of ground-based observations of the solar corona J. Burkepile 1, S. Tomczyk 1, P. Nelson 1, A.G. dewijn 1, S. Sewell 1, D. Elmore 2, L. Sutherland 1, R. Summers 1, D. Kolinski 1, L. Sitongia
More informationNEON Archive School 2006
NEON Archive School 2006 Introduction to Spectroscopic Techniques (low dispersion) M. Dennefeld (IAP-Paris) Outline Basic optics of gratings and spectrographs (with emphasis on long-slit spectroscopy)
More informationOptical/NIR Spectroscopy A3130. John Wilson Univ of Virginia
Optical/NIR Spectroscopy A3130 John Wilson Univ of Virginia Topics: Photometry is low resolution spectroscopy Uses of spectroscopy in astronomy Data cubes and dimensionality challenge Spectrograph design
More informationThe in-orbit wavelength calibration of the WFC G800L grism
The in-orbit wavelength calibration of the WFC G800L grism A. Pasquali, N. Pirzkal, J.R. Walsh March 5, 2003 ABSTRACT We present the G800L grism spectra of the Wolf-Rayet stars WR45 and WR96 acquired with
More informationLecture 4: Polarimetry 2. Polarizers and Retarders. Polarimeters. Scattering Polarization. Zeeman Effect. Outline
Lecture 4: Polarimetry 2 Outline 1 Polarizers and Retarders 2 Polarimeters 3 Scattering Polarization 4 Zeeman Effect Christoph U. Keller, Utrecht University, C.U.Keller@uu.nl Observational Astrophysics
More informationSeptember 14, Monday 4. Tools for Solar Observations-II
September 14, Monday 4. Tools for Solar Observations-II Spectrographs. Measurements of the line shift. Spectrograph Most solar spectrographs use reflection gratings. a(sinα+sinβ) grating constant Blazed
More informationAnnapurni Subramaniam IIA UVIT-PMB Meeting 08 June 2012
UVIT IN ORBIT CALIBRATIONS Annapurni Subramaniam IIA UVIT-PMB Meeting 08 June 2012 UVIT Telescope various components Calibrations are of two types: 1. Ground calibrations 2. In orbit calibrations In general,
More informationEPIC Straylight. telescopes/sieves/rga revisited. David Lumb, Athena Study Scientist
EPIC Straylight telescopes/sieves/rga revisited David Lumb, Athena Study Scientist Leicester BOC 7 Mar 2012 Topics Covered 1. The X-ray sieves 2. Initial in flight calibration (Crab ~Rev 54-56) 3. Sco
More informationEnd-to-end simulations of the Visible Tunable Filter for the Daniel K. Inouye Solar Telescope
End-to-end simulations of the Visible Tunable Filter for the Daniel K. Inouye Solar Telescope Wolfgang Schmidt, Matthias Schubert, Monika Ellwarth, Jörg Baumgartner, Alexander Bell, Andreas Fischer, Clemens
More informationA Large Coronagraph for Solar Coronal Magnetic Field Measurements
A Large Coronagraph for Solar Coronal Magnetic Field Measurements Steven Tomczyk HAO, NCAR High Altitude Observatory (HAO) National Center for Atmospheric Research (NCAR) The National Center for Atmospheric
More informationThe Sun. Never look directly at the Sun, especially NOT through an unfiltered telescope!!
The Sun Introduction We will meet in class for a brief discussion and review of background material. We will then go outside for approximately 1 hour of telescope observing. The telescopes will already
More informationSOLAR ADAPTIVE OPTICS SYSTEM FOR 1-M NEW VACUUM SOLAR TELESCOPE
Florence, Italy. May 2013 ISBN: 978-88-908876-0-4 DOI: 10.12839/AO4ELT3.13295 SOLAR ADAPTIVE OPTICS SYSTEM FOR 1-M NEW VACUUM SOLAR TELESCOPE Changhui Rao 1, Lei Zhu 1, Naiting Gu 1, Xuejun Rao 1, Lanqiang
More information