Development of the Extreme Ultraviolet Spectrometer: EXCEED
|
|
|
- Harvey Scot Black
- 8 years ago
- Views:
Transcription
1 Development of the Extreme Ultraviolet Spectrometer: EXCEED Go Murakami*, Kazuo Yoshioka, Atsushi Yamazaki, Tomoki Kimura Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency Ichiro Yoshikawa, Kentaro Uji Department of Earth and Planetary Science, the University of Tokyo Fuminori Tsuchiya, Masato Kagitani Department of Geophysics, Graduate School of Science Tohoku University Kazunori Uemizu National Astronomical Observatory of Japan ABSTRACT The extreme ultraviolet (EUV) telescope EXCEED (Extreme Ultraviolet Spectroscope for Exospheric Dynamics) onboard the Japan's small satellite SPRINT-A will be launched in August 0. The EXCEED instrument will observe tenuous gases and plasmas around the planets in the solar system (e.g., Mercury, Venus, Mars, Jupiter, and Saturn). One of the primary observation targets is Jupiter, whose magnetospheric plasma dynamics is dominated by planetary rotation. In the EUV range, a number of emission lines originate from plasmas distributed in Jupiter's inner magnetosphere. The EXCEED instrument is designed to have a wavelength range of -4 nm with a spectral resolution of nm. The spectrograph slits have a field of view of 400 x 40 arc-seconds (maximum), and the attitude fluctuations are stabilized within arc-seconds. The optics of the instrument consists of a primary mirror with a diameter of 0cm, a laminar type grating, and an EUV detector using microchannel plates (MCPs). The surfaces of the primary mirror and the grating are coated with CVD-SiC. We have finished the final integration and ground calibration of the EXCEED instrument. We performed optical tests of EXCEED and measured the following performances.. Quantum efficiency of the detector: >0%. : 0. nm (0 slit) and.0 nm (60 slit). Spatial resolution: 6-0 We have confirmed that all of these results satisfied the specifications. Now EXCEED is ready for launch.
2 0 Feb Tohoku University Symposium on Planetary Science 0 Development of the Extreme Ultraviolet Spectrometer: EXCEED Go Murakami, K. Yoshioka, A. Yamazaki, T. Kimura (ISAS/JAXA) I. Yoshikawa, K. Uji (Univ. Tokyo) F. Tsuchiya, M. Kagitani (Tohoku Univ.) K. Uemizu (NAOJ) Overview of the EXCEED mission (EXtreme ultraviolet spectroscope for ExosphEric Dynamics) An earth-orbiting Extreme Ultraviolet (EUV) spectroscopic mission The first mission of the ISAS/JAXA small scientific satellite series (Sprint-A) EXCEED measures EUV emissions from tenuous gases and plasmas around the planets Observation targets : Mercury, Venus, Mars, Jupiter, and Saturn Major specifications - Launching : August 0 - Weight:0kg -Size:m m 4m -Orbit:90km 0km (LEO) - Inclination: deg ± a few deg. - Mission life :> year - Pointing accuracy : ± arc-min (improved to ±arc-sec by FOV camera) Buffle EUV spectrometer FOV camera (Yoshikawa et al. AdGeo 00,0) Project scientist : I. Yoshikawa (The Univ. of Tokyo) SPRINT-A/EXCEED Instrument overview Specifications Wavelength range 60 4 nm Spatial resolution 0 arc-sec Field of view 400 arc-sec. (FWHM) nm (depends on slit) Primary mirror 0 cm diameter, f = 60 cm (F/8) Optical layout EUV spectrometer. Selectable by stepping motor, types of shape, types of filter + blank. Laminar type, toroidal, CVD-SiC coated, D = 0 mm, f ~ 400 mm. EUV detector -stage microchannel plate (MCP) + resistive anode encoder (RAE), CsI coated Actuator MCPs Vacuum chamber Slit Move: = 9 positions Blank In CaF (Dambbel) Opening window Vacuum pipe MCPs should be kept under vacuum -> The window must be opened after launch 4 Sensitivity - (reflectivity) - (diffraction efficiency) -Filter (transmittance) (quantum efficiency) - (spectral and spatial resolution) EUV spectrometer (spectral and spatial resolution) and slit (spatial resolution) Sensitivity (quantum efficiency) 6
3 Quantum efficiency of the detector -Set the flight detector (MCP with CsI photocathode) and a calibrated detector (MCP without photocathode) on a rotation gimbal -Compare the quantum efficiencies at various wavelengths -Light source: hollow cathode lamp + monochromator (Gas: He, Ne, Ar, and O) -Open and close the window under vacuum Vacuum chamber Flight MCP Calibrated lab-mcp Incident light Rotate Monochromator Hollow cathode lamp 7 Quantum detection efficiency [%] Quantum efficiency of the detector Spectral range: 60-4 nm Requirement FM MCP Lab MCP Flight MCP Lab MCP Flight MCP achieved ~00 times higher efficiency than Lab-MCP Quantum efficiency: 0~0% Counts per photon Total sensitivity Spectral range: 60-4 nm Blank slit Requirement W/O CsI Total sensitivity: ~% (-> Effective area: ~ cm ) 8 EUV spectrometer (spectral and spatial resolution) -EUV spectrometer and the flight mirror are set on a dummy structure -Incident light: F/8 -Light source: hollow cathode lamp We have obtained spectrums of various gases and measured the spectral and spatial resolution Vacuum chamber Flight mirror Hollow cathode lamp Collimator mirror EUV spectrometer Dummy structure 9 0 Source: Ar Source: Ne Slit: 0 Slit: 0
![Rotate Monochromator Hollow cathode lamp 7 Quantum detection efficiency [%] Quantum efficiency of the detector Spectral range: 60-4 nm 00](/docs-images/43/16202938/images/page_3.jpg "0 0 0. 0. Requirement FM MCP Lab MCP Flight MCP Lab MCP 60 80 00 0 40 Flight MCP achieved ~00 times higher efficiency than Lab-MCP Quantum efficiency: 0~0% Counts per photon 0-0 - 0-0 -4 Total")
4 Source: O Source: He Slit: 0 Slit: 0 4 We measured the FWHM of each line 000 Argon Neon Oxygen Helium 000 ArII 46Å Spectra from pinhole slit (after VT) OI 6Å OI 04Å(M) OII 4Å(M) OII Å(M) ArI 067Å ArI 048Å OI 06Å(M) OI 989Å(M) OI 949Å ArII 9Å ArII 90Å OII 84Å NeI 744Å NeI 76Å NeI 60Å HeI 84Å Spatial resolution -We used a pinhole instead of a slit (included in the flight slit plate) -The FWHM for the spatial axis was measured at each wavelength FWHM (FWHM) [nm] " slit 60" slit X-axis [0bits] Wavelength vs. Pixel 0 slit: FWHM < 0.4 nm 60 slit: FWHM <.0 nm Linear!! Pixel (0~0) Spatial resolution for point source [arc-sec.] Test pinhole (size: 40 um = ) Spatial resolution of 0 is achieved!! 6 Optical test of the whole instrument EXCEED (after final integ.) Collimator and slit (spatial resolution) Collimated light FOV camera 7 -Input collimated light (visible) to whole EXCEED D = 0 cm -Take a slit image by FOV -Measure the FWHM of the pinhole image on the slit -Before/after vibration test Pinhole Collimating mirror 8 0 cm
5 Optical test of the whole instrument Pinholes Spatial resolution at the slit: FWHM = 4.9 FWHM: 4.9 Slit image by FOV camera Spatial resolution of whole instrument: FWHM < 0 is achieved!! 9 Summary EXCEED will be soon launched in August 0! We have finished the final integration and ground calibrations of EXCEED Quantum efficiency of the detector: >0% -> Total sensitivity: ~% (effective area ~ cm ) : 0. nm (0 slit).0 nm (60 slit) Spatial resolution: 6~0 0 よくわかるEXCEED 測 Thank you!
Fig.1. The DAWN spacecraft
Introduction Optical calibration of the DAWN framing cameras G. Abraham,G. Kovacs, B. Nagy Department of Mechatronics, Optics and Engineering Informatics Budapest University of Technology and Economics
SOLSPEC MEASUREMENT OF THE SOLAR ABSOLUTE SPECTRAL IRRADIANCE FROM 165 to 2900 nm ON BOARD THE INTERNATIONAL SPACE STATION
SOLSPEC MEASUREMENT OF THE SOLAR ABSOLUTE SPECTRAL IRRADIANCE FROM 165 to 2900 nm ON BOARD THE INTERNATIONAL SPACE STATION G. Thuillier1, D. Bolsee2 1 LATMOS-CNRS, France 2 Institut d Aéronomie Spatiale
ATOMIC SPECTRA. Apparatus: Optical spectrometer, spectral tubes, power supply, incandescent lamp, bottles of dyed water, elevating jack or block.
1 ATOMIC SPECTRA Objective: To measure the wavelengths of visible light emitted by atomic hydrogen and verify the measured wavelengths against those predicted by quantum theory. To identify an unknown
WELCOME to Aurorae In the Solar System. J.E. Klemaszewski
WELCOME to Aurorae In the Solar System Aurorae in the Solar System Sponsoring Projects Galileo Europa Mission Jupiter System Data Analysis Program ACRIMSAT Supporting Projects Ulysses Project Outer Planets
Yukikatsu Terada (Saitama Univ, Japan), on behalf of the Astro-H Software Calibration board
Yukikatsu Terada (Saitama Univ, Japan), on behalf of the Astro-H Software Calibration board SKIP (Rob Introduction) The sixth series of the Japanese X-ray satellite. Collaboration with JAXA, NASA, and
THE BOHR QUANTUM MODEL
THE BOHR QUANTUM MODEL INTRODUCTION When light from a low-pressure gas is subject to an electric discharge, a discrete line spectrum is emitted. When light from such a low-pressure gas is examined with
Experiment #5: Qualitative Absorption Spectroscopy
Experiment #5: Qualitative Absorption Spectroscopy One of the most important areas in the field of analytical chemistry is that of spectroscopy. In general terms, spectroscopy deals with the interactions
Geol 116 The Planet Class 7-1 Feb 28, 2005. Exercise 1, Calculate the escape velocities of the nine planets in the solar system
Exercises/Discussions Atmospheric Composition: Escape Velocities and Surface Temperature Objectives Escape velocity and the mass and size of a planetary body The effect of escape velocity and surface temperature
O6: The Diffraction Grating Spectrometer
2B30: PRACTICAL ASTROPHYSICS FORMAL REPORT: O6: The Diffraction Grating Spectrometer Adam Hill Lab partner: G. Evans Tutor: Dr. Peter Storey 1 Abstract The calibration of a diffraction grating spectrometer
Overview of NASA s Laser Communications Relay Demonstration
Overview of NASA s Laser Communications Relay Demonstration April 2012 Bernard Edwards NASA Goddard Space Flight Center (301) 286-8926 Bernard.L.Edwards@nasa.gov 1 LCRD Demonstration Scenarios Mission
ID Objective Requirements Description of Test Date & Examiner 15 Verify that the optics?? OMC
NAOMI OMC/NCU Acceptance Tests at the University of Durham ATC Document number AOW/GEN/RAH/15.0/06/00 OMC/NCU acceptance tests DRAFT (Version date: 2 nd June 2000) wht-naomi-44 The ID numbers are those
High resolution images obtained with Solar Optical Telescope on Hinode. SOLAR-B Project Office National Astronomical Observatory of Japan (NAOJ)
High resolution images obtained with Solar Optical Telescope on Hinode SOLAR-B Project Office National Astronomical Observatory of Japan (NAOJ) Temperature stratification of solar atmosphere G-band Ca
WAVELENGTH OF LIGHT - DIFFRACTION GRATING
PURPOSE In this experiment we will use the diffraction grating and the spectrometer to measure wavelengths in the mercury spectrum. THEORY A diffraction grating is essentially a series of parallel equidistant
SGS: Das Scanning Grating Spektrometer Ein kleines, günstiges Spektrometermodul auf Basis eines dispersiven Mikrosystems
the leading supplier of Micro Scanning Devices Your Micro Optical Solution IPHT-Workshop 11.-12.03.08 We move the light for you! SGS: Das Scanning Grating Spektrometer Ein kleines, günstiges Spektrometermodul
NASA s Dawn Mission Journey to the Asteroid Frontier
NASA s Dawn Mission Journey to the Asteroid Frontier Dawn Lucy McFadden, Co-Investigator University of Maryland College Park, MD January 12, 2009 SBAG update 9 th Discovery Mission Dawn Explores the Earliest
Spectral Measurement Solutions for Industry and Research
Spectral Measurement Solutions for Industry and Research Hamamatsu Photonics offers a comprehensive range of products for spectroscopic applications, covering the, Visible and Infrared regions for Industrial,
3 - Atomic Absorption Spectroscopy
3 - Atomic Absorption Spectroscopy Introduction Atomic-absorption (AA) spectroscopy uses the absorption of light to measure the concentration of gas-phase atoms. Since samples are usually liquids or solids,
Efficiency, Dispersion and Straylight Performance Tests of Immersed Gratings for High Resolution Spectroscopy in the Near Infra-red
Changing the economics of space Efficiency, Dispersion and Straylight Performance Tests of Immersed Gratings for High Resolution Spectroscopy in the Near Infra-red J. Fernandez-Saldivar 1, F. Culfaz 1,
Project 2B Building a Solar Cell (2): Solar Cell Performance
April. 15, 2010 Due April. 29, 2010 Project 2B Building a Solar Cell (2): Solar Cell Performance Objective: In this project we are going to experimentally measure the I-V characteristics, energy conversion
x Distance of the Sun to planet --------------------------------------------------------------------
Solar System Investigation 26C 26C Solar System How big is the solar system? It is difficult to comprehend great distances. For example, how great a distance is 140,000 kilometers (the diameter of Jupiter)
GRID AND PRISM SPECTROMETERS
FYSA230/2 GRID AND PRISM SPECTROMETERS 1. Introduction Electromagnetic radiation (e.g. visible light) experiences reflection, refraction, interference and diffraction phenomena when entering and passing
Science Focus 9 Space Exploration Topic Test
SPACE EXPLORATION UNIT TEST ASSESSMENT Student Name Class 1. The axis for the frame of reference to identify locations on the earth are A. Equinox and Solstice B. Ecuador and Madagascar C. Equator and
Electromagnetic Radiation (EMR) and Remote Sensing
Electromagnetic Radiation (EMR) and Remote Sensing 1 Atmosphere Anything missing in between? Electromagnetic Radiation (EMR) is radiated by atomic particles at the source (the Sun), propagates through
Exoplanet and Solar System Synergy with Future Missions
Exoplanet and Solar System Synergy with Future Missions Britney Schmidt Georgia Tech OPAG Steering Committee Steve Vance, Jet Propulsion Lab Kunio Sayanagi, Hampton University Solar System Targets for
THE SOLAR SYSTEM - EXERCISES 1
THE SOLAR SYSTEM - EXERCISES 1 THE SUN AND THE SOLAR SYSTEM Name the planets in their order from the sun. 1 2 3 4 5 6 7 8 The asteroid belt is between and Which planet has the most moons? About how many?
7. Our Solar System. Planetary Orbits to Scale. The Eight Planetary Orbits
7. Our Solar System Terrestrial & Jovian planets Seven large satellites [moons] Chemical composition of the planets Asteroids & comets The Terrestrial & Jovian Planets Four small terrestrial planets Like
Observing Lake Erie Algae Blooms via. Hyper Spectral Imaging on CubeSat
Observing Lake Erie Algae Blooms via Hyper Spectral Imaging on CubeSat Chris Emr, Department of Physics Advisor: Professor Paul Barnhart, Department of Aerospace Engineering Case Western Reserve University
How To Understand Light And Color
PRACTICE EXAM IV P202 SPRING 2004 1. In two separate double slit experiments, an interference pattern is observed on a screen. In the first experiment, violet light (λ = 754 nm) is used and a second-order
ILLUSTRATIVE EXAMPLE: Given: A = 3 and B = 4 if we now want the value of C=? C = 3 + 4 = 9 + 16 = 25 or 2
Forensic Spectral Anaylysis: Warm up! The study of triangles has been done since ancient times. Many of the early discoveries about triangles are still used today. We will only be concerned with the "right
Laboratory #3 Guide: Optical and Electrical Properties of Transparent Conductors -- September 23, 2014
Laboratory #3 Guide: Optical and Electrical Properties of Transparent Conductors -- September 23, 2014 Introduction Following our previous lab exercises, you now have the skills and understanding to control
An Airborne A-Band Spectrometer for Remote Sensing Of Aerosol and Cloud Optical Properties
An Airborne A-Band Spectrometer for Remote Sensing Of Aerosol and Cloud Optical Properties Michael Pitts, Chris Hostetler, Lamont Poole, Carl Holden, and Didier Rault NASA Langley Research Center, MS 435,
Atoms Absorb & Emit Light
Atoms Absorb & Emit Light Spectra The wavelength of the light that an element emits or absorbs is its fingerprint. Atoms emit and absorb light First Test is Thurs, Feb 1 st About 30 multiple choice questions
Probing for Information
Name Class Date Inquiry Lab Probing for Information Using Scientific Methods Information about planets in our solar system has been collected by observation from Earth and from probes, or scientific instruments,
Introduction to reflective aberration corrected holographic diffraction gratings
Introduction to reflective aberration corrected holographic diffraction gratings By Steve Slutter, Wu Jiang, and Olivier Nicolle The reflective diffraction grating is the heart of most spectroscopy systems
Chapter 6 Telescopes: Portals of Discovery. How does your eye form an image? Refraction. Example: Refraction at Sunset.
Chapter 6 Telescopes: Portals of Discovery 6.1 Eyes and Cameras: Everyday Light Sensors Our goals for learning:! How does your eye form an image?! How do we record images? How does your eye form an image?
Laser Ranging to Nano-Satellites
13-0222 Laser Ranging to Nano-Satellites G. Kirchner (1), Ludwig Grunwaldt (2), Reinhard Neubert (2), Franz Koidl (1), Merlin Barschke (3), Zizung Yoon (3), Hauke Fiedler (4), Christine Hollenstein (5)
Raman spectroscopy Lecture
Raman spectroscopy Lecture Licentiate course in measurement science and technology Spring 2008 10.04.2008 Antti Kivioja Contents - Introduction - What is Raman spectroscopy? - The theory of Raman spectroscopy
Anna Serdyuchenko, Victor Gorshelev, Mark Weber John P. Burrows University of Bremen, Institute for Environmental Physics
Anna Serdyuchenko, Victor Gorshelev, Mark Weber John P. Burrows University of Bremen, Institute for Environmental Physics 3-5 June 2013 ACSO meeting WMO Geneva, Switzerland 1 Graphics: DLR-IMF 3-5 June
How Does One Obtain Spectral +Imaging Data
How Does One Obtain Spectral +Imaging Data What we observe depends on the instruments that one observes with! In x and γ-ray spectroscopy we have a wide variety of instruments with different properties
High Resolution Imaging of Satellites with Ground-Based 10-m Astronomical Telescopes
UCRL-TR-227709 High Resolution Imaging of Satellites with Ground-Based 10-m Astronomical Telescopes C. Marois February 2, 2007 Disclaimer This document was prepared as an account of work sponsored by an
Building your own Spectroscope
Building your own Spectroscope 0-0.341-0.445-0.606-0.872-1.36 Lyman Balmer Paschen n=4 n=8 n=7 n=6 n=5 n=4 ENERGY/10-19 J -2.42-5.45 E 5 2 E 4 2 E 3 2 E E 5 3 4 3 n=3 n=2 (Many other transitions beyond
Reflectance Measurements of Materials Used in the Solar Industry. Selecting the Appropriate Accessories for UV/Vis/NIR Measurements.
T e c h n i c a l N o t e Reflectance Measurements of Materials Used in the Solar Industry UV/Vis/NIR Author: Dr. Jeffrey L. Taylor PerkinElmer, Inc. 710 Bridgeport Avenue Shelton, CT 06484 USA Selecting
Earth Is Not the Center of the Universe
Earth Is Not the Center of the Universe Source: Utah State Office of Education Introduction Have you ever looked up at the night sky and wondered about all the pinpoint lights? People through the ages
A STEP 400 Technical development status
A STEP 400 Technical development status ARENA workshop, Catania, 17 sept 08 Authors: J.B. Daban (1), C. Gouvret (1), A. Agabi (1), T. Guillot (2), F. Fressin (2), L. Abe (1), N. Crouzet (2), Y. Fanteï-Caujolle
High Resolution Planetary Imaging Workflow
High Resolution Planetary Imaging Workflow Fighting the Atmosphere Getting out of the Atmosphere Adaptive Optics Lucky Imaging Lucky Imaging is the process of capturing planets using a CCD video camera.
Copyright 1999 2010 by Mark Brandt, Ph.D. 12
Introduction to Absorbance Spectroscopy A single beam spectrophotometer is comprised of a light source, a monochromator, a sample holder, and a detector. An ideal instrument has a light source that emits
Planetary Imaging Workshop Larry Owens
Planetary Imaging Workshop Larry Owens Lowell Observatory, 1971-1973 Backyard Telescope, 2005 How is it possible? How is it done? Lowell Observatory Sequence,1971 Acquisition E-X-P-E-R-I-M-E-N-T-A-T-I-O-N!
Grazing incidence wavefront sensing and verification of X-ray optics performance
Grazing incidence wavefront sensing and verification of X-ray optics performance Timo T. Saha, Scott Rohrbach, and William W. Zhang, NASA Goddard Space Flight Center, Greenbelt, Md 20771 Evaluation of
Name: João Fernando Alves da Silva Class: 7-4 Number: 10
Name: João Fernando Alves da Silva Class: 7-4 Number: 10 What is the constitution of the Solar System? The Solar System is constituted not only by planets, which have satellites, but also by thousands
Synthetic Sensing: Proximity / Distance Sensors
Synthetic Sensing: Proximity / Distance Sensors MediaRobotics Lab, February 2010 Proximity detection is dependent on the object of interest. One size does not fit all For non-contact distance measurement,
astronomy 2008 1. A planet was viewed from Earth for several hours. The diagrams below represent the appearance of the planet at four different times.
1. A planet was viewed from Earth for several hours. The diagrams below represent the appearance of the planet at four different times. 5. If the distance between the Earth and the Sun were increased,
Robotic Pre-Cursor Contribution to Human NEA Mission. H. Kuninaka JSPEC/JAXA
Robotic Pre-Cursor Contribution to Human NEA Mission H. Kuninaka JSPEC/JAXA Asteroid Explorer Hayabusa Dimensions 1.0m x 1.6m x 1.1m Weight : 380kg(Dry) Chemical Fuel 70kg Xe Propellant 60kg Total 510kg
Theremino System Theremino Spectrometer Technology
Theremino System Theremino Spectrometer Technology theremino System - Theremino Spectrometer Technology - August 15, 2014 - Page 1 Operation principles By placing a digital camera with a diffraction grating
Physics 30 Worksheet # 14: Michelson Experiment
Physics 30 Worksheet # 14: Michelson Experiment 1. The speed of light found by a Michelson experiment was found to be 2.90 x 10 8 m/s. If the two hills were 20.0 km apart, what was the frequency of the
How To Make A Plasma Control System
XXII. Erfahrungsaustausch Mühlleiten 2015 Plasmaanalyse und Prozessoptimierung mittels spektroskopischem Plasmamonitoring in industriellen Anwendungen Swen Marke,, Lichtenau Thomas Schütte, Plasus GmbH,
A high accuracy, small field of view star guider with application to SNAP.
A high accuracy, small field of view star guider with application to SNAP. Aurélia Secroun and Michael Lampton Space Sciences Laboratory, U.C. Berkeley Michael Levi Lawrence Berkeley National Laboratory,
A.4 The Solar System Scale Model
CHAPTER A. LABORATORY EXPERIMENTS 25 Name: Section: Date: A.4 The Solar System Scale Model I. Introduction Our solar system is inhabited by a variety of objects, ranging from a small rocky asteroid only
An Introduction to the MTG-IRS Mission
An Introduction to the MTG-IRS Mission Stefano Gigli, EUMETSAT IRS-NWC Workshop, Eumetsat HQ, 25-0713 Summary 1. Products and Performance 2. Design Overview 3. L1 Data Organisation 2 Part 1 1. Products
- the. or may. scales on. Butterfly wing. magnified about 75 times.
Lecture Notes (Applications of Diffraction) Intro: - the iridescent colors seen in many beetles is due to diffraction of light rays hitting the small groovess of its exoskeleton - these ridges are only
ING LA PALMA TECHNICAL NOTE No. 130. Investigation of Low Fringing Detectors on the ISIS Spectrograph.
ING LA PALMA TECHNICAL NOTE No. 130 Investigation of Low Fringing Detectors on the ISIS Spectrograph. Simon Tulloch (ING) June 2005 Investigation of Low Fringing Detectors on the ISIS Spectrograph. 1.
Angular Velocity vs. Linear Velocity
MATH 7 Angular Velocity vs. Linear Velocity Dr. Neal, WKU Given an object with a fixed speed that is moving in a circle with a fixed ius, we can define the angular velocity of the object. That is, we can
The Solar System. Unit 4 covers the following framework standards: ES 10 and PS 11. Content was adapted the following:
Unit 4 The Solar System Chapter 7 ~ The History of the Solar System o Section 1 ~ The Formation of the Solar System o Section 2 ~ Observing the Solar System Chapter 8 ~ The Parts the Solar System o Section
The Spacewire interface for HERSCHEL/SCORE suborbital mission
The Spacewire interface for HERSCHEL/SCORE suborbital mission International Spacewire Conference, Dundee, 19 Sept. 2007 Session: SpaceWire missions and applications Pancrazzi Maurizio e Scienza dello Spazio
Nederland België / Belgique
Cronus Brochure 2 Introduction Cronus: The first spectrometer and colorimeter in one The Cronus is world s first spectrocolorimeter combining a high en VIS spectrometer with a high speed XYZ colorimeter.
The Optical Design of the High Resolution Imaging Channel for the SIMBIO-SYS experiment on the BepiColombo Mission to Mercury
Mem. S.A.It. Suppl. Vol. 12, 77 c SAIt 2008 Memorie della Supplementi The Optical Design of the High Resolution Imaging Channel for the SIMBIO-SYS experiment on the BepiColombo Mission to Mercury G. Marra
Large FOV Mobile E-O Telescope for Searching and Tracking Low-orbit Micro-satellites and Space Debris
Large FOV Mobile E-O Telescope for earching and Tracking Low-orbit Micro-satellites and pace Debris WANG Jian-li 1, GAO Xin, TANG Jia, HAN Chang-yuan 1, ZHAO Jin-yu 1 1 Changchun Institute of Optics, Fine
Helium-Neon Laser. Figure 1: Diagram of optical and electrical components used in the HeNe laser experiment.
Helium-Neon Laser Experiment objectives: assemble and align a 3-mW HeNe laser from readily available optical components, record photographically the transverse mode structure of the laser output beam,
Solar System Overview
Solar System Overview Planets: Four inner planets, Terrestrial planets Four outer planets, Jovian planets Asteroids: Minor planets (planetesimals) Meteroids: Chucks of rocks (smaller than asteroids) (Mercury,
The Sino-French Gamma-Ray Burst Mission SVOM (Space-based multi-band astronomical Variable Objects Monitor)
The Sino-French Gamma-Ray Burst Mission SVOM (Space-based multi-band astronomical Variable Objects Monitor) Didier BARRET on behalf of the SVOM collaboration didier.barret@cesr.fr Outline SVOM background
MY FIRST STEPS IN SLIT SPECTROSCOPY
MY FIRST STEPS IN SLIT SPECTROSCOPY Andrew Wilson BAAVSS Spectroscopy Workshop Norman Lockyer Observatory October 2015 Overview My choice of spectrograph, camera and telescope Getting started and basic
The Field Camera Unit project for the WSO-UV space telescope
Mem. S.A.It. Vol. 78, 697 c SAIt 2007 Memorie della The Field Camera Unit project for the WSO-UV space telescope S. Scuderi 1, I. Pagano 1, M. Fiorini 2, L. Gambicorti 3, A. Gherardi 3, F. Gianotti 4,
16th International Toki Conference on Advanced Imaging and Plasma Diagnostics
16th International Toki Conference on Advanced Imaging and Plasma Diagnostics Temperature Diagnostics for Field-Reversed Configuration Plasmas on the Pulsed High Density (PHD) Experiment Hiroshi Gota,
16 th IOCCG Committee annual meeting. Plymouth, UK 15 17 February 2011. mission: Present status and near future
16 th IOCCG Committee annual meeting Plymouth, UK 15 17 February 2011 The Meteor 3M Mt satellite mission: Present status and near future plans MISSION AIMS Satellites of the series METEOR M M are purposed
Raman Spectroscopy Basics
Raman Spectroscopy Basics Introduction Raman spectroscopy is a spectroscopic technique based on inelastic scattering of monochromatic light, usually from a laser source. Inelastic scattering means that
UV/VIS/IR SPECTROSCOPY ANALYSIS OF NANOPARTICLES
UV/VIS/IR SPECTROSCOPY ANALYSIS OF NANOPARTICLES SEPTEMBER 2012, V 1.1 4878 RONSON CT STE K SAN DIEGO, CA 92111 858-565 - 4227 NANOCOMPOSIX.COM Note to the Reader: We at nanocomposix have published this
ShindaiSat : A Visible Light Communication Experimental Micro-Satellite
ShindaiSat : A Visible Light Communication Experimental Micro-Satellite Atsushi Nakajima, Nobutada Sako, Masato Kamemura, Yuuki Wakayama, Arata Fukuzawa, Hironori Sugiyama and Naoki Okada Graduate School
Optical laser beam scanner lens relay system
1. Introduction Optical laser beam scanner lens relay system Laser beam scanning is used most often by far in confocal microscopes. There are many ways by which a laser beam can be scanned across the back
VIETNAM ACADEMY OF SCIENCE AND TECHNOLOGY VIETNAM NATIONAL SATELLITE CENTER CUBESAT PICO DRAGON. Presenter Name: Do Xuan Phong
VIETNAM ACADEMY OF SCIENCE AND TECHNOLOGY VIETNAM NATIONAL SATELLITE CENTER CUBESAT PICO DRAGON Presenter Name: Do Xuan Phong Co-authors: Vu Viet Phuong, Truong Xuan Hung, Le Xuan Huy, Bui Nam Duong, Do
Solar System Fundamentals. What is a Planet? Planetary orbits Planetary temperatures Planetary Atmospheres Origin of the Solar System
Solar System Fundamentals What is a Planet? Planetary orbits Planetary temperatures Planetary Atmospheres Origin of the Solar System Properties of Planets What is a planet? Defined finally in August 2006!
Solar System Facts & Fun
Solar System Facts & Fun Space is such a fascinating place. God put the Earth in just the right place so everything was just right for life as we know it. Have you ever wondered about the other planets
Realization of a UV fisheye hyperspectral camera
Realization of a UV fisheye hyperspectral camera Valentina Caricato, Andrea Egidi, Marco Pisani and Massimo Zucco, INRIM Outline Purpose of the instrument Required specs Hyperspectral technique Optical
Problem Set 6 UV-Vis Absorption Spectroscopy. 13-1. Express the following absorbances in terms of percent transmittance:
Problem Set 6 UV-Vis Absorption Spectroscopy 13-1. Express the following absorbances in terms of percent transmittance: a 0.051 b 0.918 c 0.379 d 0.261 e 0.485 f 0.072 A = log P o /P = log1/t = - log T
Status of the FERMI@Elettra Free Electron Laser
Status of the FERMI@Elettra Free Electron Laser E. Allaria on behalf of the FERMI team Work partially supported by the Italian Ministry of University and Research under grants FIRB-RBAP045JF2 and FIRB-RBAP06AWK3
Passive Remote Sensing of Clouds from Airborne Platforms
Passive Remote Sensing of Clouds from Airborne Platforms Why airborne measurements? My instrument: the Solar Spectral Flux Radiometer (SSFR) Some spectrometry/radiometry basics How can we infer cloud properties
What s in the Mix? Liquid Color Spectroscopy Lab (Randy Landsberg & Bill Fisher)
What s in the Mix? Liquid Color Spectroscopy Lab (Randy Landsberg & Bill Fisher) Introduction: There is more to a color than a name. Color can tell us lots of information. In this lab you will use a spectrophotometer
CBERS Program Update Jacie 2011. Frederico dos Santos Liporace AMS Kepler liporace@amskepler.com
CBERS Program Update Jacie 2011 Frederico dos Santos Liporace AMS Kepler liporace@amskepler.com Overview CBERS 3 and 4 characteristics Differences from previous CBERS satellites (CBERS 1/2/2B) Geometric
FTIR Instrumentation
FTIR Instrumentation Adopted from the FTIR lab instruction by H.-N. Hsieh, New Jersey Institute of Technology: http://www-ec.njit.edu/~hsieh/ene669/ftir.html 1. IR Instrumentation Two types of instrumentation
A Guide to Modern Planetary Imaging. Christopher Go
A Guide to Modern Planetary Imaging Christopher Go Fighting the Atmosphere Getting out of the Atmosphere Adaptive Optics Speckle/Lucky Imaging Speckle Imaging: Feeling Lucky Speckle or Lucky Imaging is
Jr. Edition. Solar System. Trading Cards. Solar System Trading Cards, Jr. Edition. Learn more about the solar system on these websites:
Solar System Trading Cards, Jr. Edition To use these cards: Print out onto card stock or heavy paper. Cut out and fold in half along dotted line; glue or tape each card together. FOLD National Aeronautics
Dawn - Overview, Science Objectives, Mission Progress. Hap McSween For PI Chris Russell
Dawn - Overview, Science Objectives, Mission Progress Hap McSween For PI Chris Russell Presentation to Decadal Survey Primitive Bodies Panel, Washington, DC, Sep 2009 Spacecraft configuration, assembly
Science Standard 4 Earth in Space Grade Level Expectations
Science Standard 4 Earth in Space Grade Level Expectations Science Standard 4 Earth in Space Our Solar System is a collection of gravitationally interacting bodies that include Earth and the Moon. Universal
THE GOCI INSTRUMENT ON COMS MISSION THE FIRST GEOSTATIONARY OCEAN COLOR IMAGER
THE GOCI INSTRUMENT ON COMS MISSION THE FIRST GEOSTATIONARY OCEAN COLOR IMAGER Topic 1 - Optical instruments for Earth / Planets surface and atmosphere study François FAURE, Astrium SAS Satellite, Toulouse,
Short overview of TEUFEL-project
Short overview of TEUFEL-project ELAN-meeting may 2004 Frascati (I) Contents Overview of TEUFEL project at Twente Photo cathode research Recent experience Outlook Overview FEL Drive laser Photo cathode
HIGH RESOLUTION IMAGING X RAY SPECTROSCOPY OF MARS
High resolution X-ray spectroscopy: towards XEUS and Con-X MSSL, 7-8 March 6 HIGH RESOLUTION IMAGING X RAY SPECTROSCOPY OF MARS K. Dennerl a a Max Planck Institut für extraterrestrische Physik, Giessenbachstraße,
CSSAR Space Science Cooperation
CSSAR Space Science Cooperation WANG Shuzhi Center for Space Science and Applied Research Chinese Academy of Science(CSSAR) Table of Contents Brief History of CSSAR International Cooperation CAS Strategic
Powerful Analytics based on Modern Spectrometers
Powerful Analytics based on Modern Spectrometers Gerhard Schlemmer Analytik Jena AG, Konrad- Zuse- Str. 1, 07745 Jena g.schlemmer@analytik-jena.de 1 1 Powerful Analytics based on Modern Spectrometers Optimizing
Archival Science with the ESAC Science Archives and Virtual Observatory
Archival Science with the ESAC Science Archives and Virtual Observatory Deborah Baines Science Archives and VO Team Scientist European Space Agency (ESA) European Space Astronomy Centre (ESAC) Science
Are We Alone?! Exoplanet Characterization and Direct Imaging!
From Cosmic Birth to Living Earths A Vision for Space Astronomy in the 2020s and Beyond Are We Alone?! Exoplanet Characterization and Direct Imaging! A Study Commissioned by the Associated Universities
Modern Classical Optics
Modern Classical Optics GEOFFREY BROOKER Department of Physics University of Oxford OXPORD UNIVERSITY PRESS Contents 1 Electromagnetism and basic optics 1 1.1 Introduction 1 1.2 The Maxwell equations 1
Austin Peay State University Department of Chemistry Chem 1111. The Use of the Spectrophotometer and Beer's Law
Purpose To become familiar with using a spectrophotometer and gain an understanding of Beer s law and it s relationship to solution concentration. Introduction Scientists use many methods to determine