Proposal for a research project to be carried. out in Physics 400 (Senior Research) and. IDIS 493 (Honors Thesis).
|
|
- Solomon Day
- 5 years ago
- Views:
Transcription
1 Proposal for a research project to be carried out in Physics 400 (Senior Research) and IDIS 493 (Honors Thesis). Variable Star CCD Photometry and Analysis Amber L. Stuver Submitted in fulfillment of requirements for Physics 491. December 16, 1998
2 Abstract My research will focus initially on the techniques required to properly observe and analyze a variable star. The technique as planned includes selecting a variable star to observe and selecting a constant magnitude star in the same star field as the variable star, and observing the frequency of the variable star by taking CCD (charge-coupled device) images though the CCD camera. The software that accompanies the camera I plan to use has utilities that will assign the variable star a comparive magnitude with respect to the constant magnitude star I select as my reference. First, a short period star (preferably a member of the Cepheid populations) will be observed and its light curve will be plotted in order to refine my photometry techniques. A longer period variable star (perhaps of the Beta Canis Majois group) and/or an eclipscing binary system will be observed, weather permitting. Once the observations are complete, a Fourier analysis of the light curve will be performed in order to reveal any periodicities that are not obvious from the light curve and a hypothesis formation will be attempted in respect to what is causing the varying luminosity of the variable star.
3 Stuver 1 Introduction Variable stars are stars that vary in luminosity over a period of time which can range from several hours to many days and each star has its own characteristic period. 1 The purpose for the research being proposed here is to observe a variable star and analyze the luminosity variation over the star s period. CCD photometry will be implemented due to its sensitivity and convenient digital format. The data collected will be processed first by the CCD camera s software in order to plot the star s light curve and then this light curve will undergo a Fourier analysis to analyze the periodicities of the light curve. From this Fourier analysis, a hypothesis will be attempted in order to account for the luminosity variations. Background A CCD camera detects photons and these photons induce a charge which is then recorded and then interpreted by the camera to produce a digital image. The quantum efficiency (the photoelectric effects that induce a charge on the CCD) of CCD cameras is extremely high and thus makes the camera extraordinarily sensitive to the few photons that have traversed the light years and penetrated the earth s atmosphere. Along with the camera s sensitivity, CCD cameras are very linear and, by this, can measure light intensity accurately. 2 These two features make CCD astrophotography preferable over traditional silver astrophotography. Figure 1 illustrates the power of the CCD camera by
4 Stuver 2 showing an image of the horse-head nebula which is very faint but this 900 second exposure can resolve the nebula and stars around it well. Procedure Since a CCD camera is an area detector, it can cover a decent fraction of the telescope s field of view and can therefore observe more than one star. Therefore, a choice field of view would be one that contains a variable star and a constant magnitude star so that both are visible in the image. Using this comparative method allows for atmospheric variations from one night to another to be all but eliminated. Since the CCD has an intrinsic noise involved with it, a dark frame (a frame that is the same temperature and exposure time as the image being processed but not exposed to any photons) must be digitally subtracted from the actual raw image in order to eliminate the noise in the picture. This is done using the software that accompanied the CCD camera through a process called dark subtraction. It has also been determined that the most efficient temperature to take exposures at is approximately 25 o centigrade (since the intrinsic noise is temperature dependent). This was determined by plotting the average pixel value of ten second dark frames against the temperature, ranging from 40 o centigrade to room temperature, of the respective dark frames as illustrated in Figure 2. As shown there, reducing the temperature to below 25 o centigrade reduced the efficiency of the camera since it takes a great deal more energy to only decrease the noise marginally after that point.
5 Stuver 3 The software mentioned previously interprets the input data from the camera and has a utility that allows a star to be assigned a unit magnitude and every other star in that same image can be compared to that magnitude. 3 The numerical values from these comparative magnitudes are displayed through this utility and a light curve will be developed from these magnitudes. The observing techniques will first be tested by plotting a light curve for a short period variable star, possibly a member of the Dwarf Cepheids or the Beta Canis Majoris stars. Members of these groups have characteristic periods of between two to five hours, respectively, on average. Once the technique has been refined, a longer period variable star, perhaps a population I or population II Cepheid which have characteristic periods of between 5-10 days and days, respectively, will be observed. 4 As of this point in time, I plan to begin my prototype curve with β Canis Majoris which has a characteristic period of 5 approximately hours. Once the data has been gathered, a Fourier analysis will be carried out in order to detect any periodicities that are not obvious from the star s light curve. Further analysis of the Fourier analysis will lead to a formulation of a hypothesis as to what is causing the variation in the luminosity of the variable star observed. Resources The primary piece of apparatus will be a CCD (charged-coupled device) camera (specifically a model ST-6 CCD imaging camera manufactured by the Santa Barbara Instrument Group). Along with the CCD camera, a telescope around 6 inches in diameter
6 Stuver 4 and between 50 to 100 inches in focal length will be needed, a laptop computer to receive the data input from the CCD camera, and Fourier analysis software. The budget is therefore minimal since all of the equipment is already possessed by Frostburg State University and can be provided.
7 Figure 1 Stuver 5
8 Stuver 6 Figure 2 Temperature vs. Average Pixel Value for a 10 Second Dark Exposure Average pixel value Temperature (degrees C)
9 Stuver 7 Figure Captions: Figure 1: This is a CCD image of the horse-head nebula which is very difficult to resolve with moderate sized telescopes. This image was taken by the manufactures of the camera and is a 900 second exposure. Figure 2: This average pixel value for a 10 second dark frame vs. temperature plot shows how lowering the temperature below 25 o centigrade reduces the efficiency of the camera since it takes a great deal more energy to only to decrease the noise marginally. Works Cited 1. Pasachoff, Jay M., Donald H. Menzel, Stars and Planets, (New York: Houghton Mifflin, 1992), pp Zelik, Michael, Elske v. P. Smith. Introductory Astronomy and Astrophysics, (Philadelphia: Saunders, 1987), p Model ST-6 Professional CCD Imaging Camera, (California: Santa Barbara Instrument Group, n.d). p Reference 2, pp
Term Paper for PHYS 490. Special Topics. Fall CCD Astrophotography. Amber L. Stuver. Performed under the supervision of: Dr.
Term Paper for PHYS 490 Special Topics Fall 1998 CCD Astrophotography Amber L. Stuver Performed under the supervision of: Dr. Gregory Latta December 16, 1998 Table of Contents Basic CCD Camera Operation.1
More informationAstronomy 341 Fall 2012 Observational Astronomy Haverford College. CCD Terminology
CCD Terminology Read noise An unavoidable pixel-to-pixel fluctuation in the number of electrons per pixel that occurs during chip readout. Typical values for read noise are ~ 10 or fewer electrons per
More informationINTRODUCTION TO CCD IMAGING
ASTR 1030 Astronomy Lab 85 Intro to CCD Imaging INTRODUCTION TO CCD IMAGING SYNOPSIS: In this lab we will learn about some of the advantages of CCD cameras for use in astronomy and how to process an image.
More informationIntroduction, & Teaching Strategies
Introduction, Curriculum Links & Teaching Strategies Author: David Bowdley & Daniel Duggan This project has been funded with support from the European Commission. This publication reflects the views only
More informationRHO CCD. imaging and observa3on notes AST aug 2011
RHO CCD imaging and observa3on notes AST 6725 30 aug 2011 Camera Specs & Info 76 cm Telescope f/4 Prime focus (3.04 m focal length) SBIG ST- 8XME CCD Camera Kodak KAF- 1603ME Class 2 imaging CCD Built-
More informationCCD reductions techniques
CCD reductions techniques Origin of noise Noise: whatever phenomena that increase the uncertainty or error of a signal Origin of noises: 1. Poisson fluctuation in counting photons (shot noise) 2. Pixel-pixel
More informationCHARGE-COUPLED DEVICE (CCD)
CHARGE-COUPLED DEVICE (CCD) Definition A charge-coupled device (CCD) is an analog shift register, enabling analog signals, usually light, manipulation - for example, conversion into a digital value that
More informationAstrophotography. Playing with your digital SLR camera in the dark
Astrophotography Playing with your digital SLR camera in the dark Lots of objects to photograph in the night sky Moon - Bright, pretty big, lots of detail, not much color Planets - Fairly bright, very
More informationThe 0.84 m Telescope OAN/SPM - BC, Mexico
The 0.84 m Telescope OAN/SPM - BC, Mexico Readout error CCD zero-level (bias) ramping CCD bias frame banding Shutter failure Significant dark current Image malting Focus frame taken during twilight IR
More informationThe Noise about Noise
The Noise about Noise I have found that few topics in astrophotography cause as much confusion as noise and proper exposure. In this column I will attempt to present some of the theory that goes into determining
More informationAstro-photography. Daguerreotype: on a copper plate
AST 1022L Astro-photography 1840-1980s: Photographic plates were astronomers' main imaging tool At right: first ever picture of the full moon, by John William Draper (1840) Daguerreotype: exposure using
More informationErrata to First Printing 1 2nd Edition of of The Handbook of Astronomical Image Processing
Errata to First Printing 1 nd Edition of of The Handbook of Astronomical Image Processing 1. Page 47: In nd line of paragraph. Following Equ..17, change 4 to 14. Text should read as follows: The dark frame
More informationPhotometry. La Palma trip 2014 Lecture 2 Prof. S.C. Trager
Photometry La Palma trip 2014 Lecture 2 Prof. S.C. Trager Photometry is the measurement of magnitude from images technically, it s the measurement of light, but astronomers use the above definition these
More informationPhotometry, PSF Fitting, Astrometry. AST443, Lecture 8 Stanimir Metchev
Photometry, PSF Fitting, Astrometry AST443, Lecture 8 Stanimir Metchev Administrative Project 2: finalized proposals due today Project 3: see at end due in class on Wed, Oct 14 Midterm: Monday, Oct 26
More informationCCD vs CMOS for Video Astronomy by Jim Thompson, P.Eng Test Report November 20 th, 2017
CCD vs CMOS for Video Astronomy by Jim Thompson, P.Eng Test Report November 20 th, 2017 Introduction: Video Astronomy (VA), the method of observing the night sky through a video camera instead of an eyepiece,
More informationPhotometry of the variable stars using CCD detectors
Contrib. Astron. Obs. Skalnaté Pleso 35, 35 44, (2005) Photometry of the variable stars using CCD detectors I. Photometric reduction. Š. Parimucha 1, M. Vaňko 2 1 Institute of Physics, Faculty of Natural
More informationPhotometry. Variable Star Photometry
Variable Star Photometry Photometry One of the most basic of astronomical analysis is photometry, or the monitoring of the light output of an astronomical object. Many stars, be they in binaries, interacting,
More informationTHE CALIBRATION OF THE OPTICAL IMAGER FOR THE HOKU KEA TELESCOPE. Jamie L. H. Scharf Physics & Astronomy, University of Hawai i at Hilo Hilo, HI 96720
THE CALIBRATION OF THE OPTICAL IMAGER FOR THE HOKU KEA TELESCOPE Jamie L. H. Scharf Physics & Astronomy, University of Hawai i at Hilo Hilo, HI 96720 ABSTRACT I have been calibrating the science CCD camera
More informationEvaluation of the Foveon X3 sensor for astronomy
Evaluation of the Foveon X3 sensor for astronomy Anna-Lea Lesage, Matthias Schwarz alesage@hs.uni-hamburg.de, Hamburger Sternwarte October 2009 Abstract Foveon X3 is a new type of CMOS colour sensor. We
More information"Internet Telescope" Performance Requirements
"Internet Telescope" Performance Requirements by Dr. Frank Melsheimer DFM Engineering, Inc. 1035 Delaware Avenue Longmont, Colorado 80501 phone 303-678-8143 fax 303-772-9411 www.dfmengineering.com Table
More informationAstronomical Detectors. Lecture 3 Astronomy & Astrophysics Fall 2011
Astronomical Detectors Lecture 3 Astronomy & Astrophysics Fall 2011 Detector Requirements Record incident photons that have been captured by the telescope. Intensity, Phase, Frequency, Polarization Difficulty
More informationCousins/Bessell vs. Johnson Filter Standards
Cousins/Bessell vs. Johnson Filter Standards by Gerald Persha President, Optec, Inc. [Also available in Adobe PDF Format: filter monograph.pdf] Identifying broad band "standard" photometric filters for
More informationCCD Characteristics Lab
CCD Characteristics Lab Observational Astronomy 6/6/07 1 Introduction In this laboratory exercise, you will be using the Hirsch Observatory s CCD camera, a Santa Barbara Instruments Group (SBIG) ST-8E.
More informationFeasibility and Design for the Simplex Electronic Telescope. Brian Dodson
Feasibility and Design for the Simplex Electronic Telescope Brian Dodson Charge: A feasibility check and design hints are wanted for the proposed Simplex Electronic Telescope (SET). The telescope is based
More informationWEBCAMS UNDER THE SPOTLIGHT
WEBCAMS UNDER THE SPOTLIGHT MEASURING THE KEY PERFORMANCE CHARACTERISTICS OF A WEBCAM BASED IMAGER Robin Leadbeater Q-2006 If a camera is going to be used for scientific measurements, it is important to
More informationAstraLux SNR and DR considerations
AstraLux SNR page 1 AstraLux SNR and DR considerations Stefan Hippler, hippler@mpia.de, March 2008 AstraLux Homepage: http://www.mpia.de/astralux Contents 1 Signal to Noise (SNR) considerations for AstraLux
More informationThe Design and Construction of an Inexpensive CCD Camera for Astronomical Imaging
The Design and Construction of an Inexpensive CCD Camera for Astronomical Imaging Mr. Ben Teasdel III South Carolina State University Abstract The design, construction and testing results of an inexpensive
More information1.6 Beam Wander vs. Image Jitter
8 Chapter 1 1.6 Beam Wander vs. Image Jitter It is common at this point to look at beam wander and image jitter and ask what differentiates them. Consider a cooperative optical communication system that
More informationElectron Multiplying Charge Coupled Devices. Craig Mackay, Institute of Astronomy, University of Cambridge.
Electron Multiplying Charge Coupled Devices Craig Mackay, Institute of Astronomy, University of Cambridge. Outline Introduction to EMCCDs: General Characteristics Applications of EMCCDs: Current and Potential
More informationModel ST-9XE CCD Imaging Camera SBIG ASTRONOMICAL INSTRUMENTS
Model ST-9XE CCD Imaging Camera.. SBIG ASTRONOMICAL INSTRUMENTS 1... Model ST-9XE Dual CCD Self-Guiding Camera The ST-9XE is identical to the ST-7/8/10/2000 cameras with the exception of the imaging CCD.
More informationObservation Data. Optical Images
Data Analysis Introduction Optical Imaging Tsuyoshi Terai Subaru Telescope Imaging Observation Measure the light from celestial objects and understand their physics Take images of objects with a specific
More informationCMOS sensor for TAOS 2
CMOS sensor for TAOS 2 Shiang-Yu Wang ( 王祥宇 ) Academia Sinica, Institute of Astronomy & Astrophysics Taiwan American Occultation Survey Institute of Astronomy & Astrophysics, Academia Sinica, Taiwan Sun-Kun
More informationAperture Photometry with CCD Images using IRAF. Kevin Krisciunas
Aperture Photometry with CCD Images using IRAF Kevin Krisciunas Images must be taken in a sensible manner. Ask advice from experienced observers. But remember Wallerstein s Rule: Four astronomers, five
More informationYou, too, can make useful and beautiful astronomical images at Mees: Lesson 1
You, too, can make useful and beautiful astronomical images at Mees: Lesson 1 Useful references: The Mees telescope startup/shutdown guide: http://www.pas.rochester.edu/~dmw/ast142/projects/chklist.pdf
More informationThe New. Astronomy. 2 Practical Focusing
The New 2 Practical Focusing Astronomy CCD cameras represent some pretty fancy technology, but in some ways they are just like ordinary cameras. As with a traditional film camera, the difference between
More informationProblems with filters can have the strangest causes
Problems with filters can have the strangest causes If you switch from simple astrophotography to more difficult fields of activity and start working with different filters, correctors and systems, you
More informationDETECTORS Important characteristics: 1) Wavelength response 2) Quantum response how light is detected 3) Sensitivity 4) Frequency of response
DETECTORS Important characteristics: 1) Wavelength response 2) Quantum response how light is detected 3) Sensitivity 4) Frequency of response (response time) 5) Stability 6) Cost 7) convenience Photoelectric
More informationStellar Photometry: I. Measuring. Ast 401/Phy 580 Fall 2014
What s Left (Today): Introduction to Photometry Nov 10 Photometry I/Spectra I Nov 12 Spectra II Nov 17 Guest lecture on IR by Trilling Nov 19 Radio lecture by Hunter Nov 24 Canceled Nov 26 Thanksgiving
More informationDSLR Photometry. Part 1. ASSA Photometry Nov 2016
DSLR Photometry Part 1 ASSA Photometry Nov 2016 Because of the complexity of the subject, these two sessions on DSLR Photometry will not equip you to be a fully fledged DSLR photometrists. It is hoped
More informationLight gathering Power: Magnification with eyepiece:
Telescopes Light gathering Power: The amount of light that can be gathered by a telescope in a given amount of time: t 1 /t 2 = (D 2 /D 1 ) 2 The larger the diameter the smaller the amount of time. If
More informationHASP SPARTAN V Optical Subsystem
HASP SPARTAN V Optical Subsystem Anthony Cangelosi Chris Nie Colorado Space Grant Consortium Academic Advisor: Kendra Kilbride Anthony.Cangelosi@Colorado.edu March 29 th, 2010 Abstract With the high cost
More informationCharge-Coupled Device (CCD) Detectors pixel silicon chip electronics cryogenics
Charge-Coupled Device (CCD) Detectors As revolutionary in astronomy as the invention of the telescope and photography semiconductor detectors a collection of miniature photodiodes, each called a picture
More informationIntroduction to CCD camera
Observational Astronomy 2011/2012 Introduction to CCD camera Charge Coupled Device (CCD) photo sensor coupled to shift register Jörg R. Hörandel Radboud University Nijmegen http://particle.astro.ru.nl/goto.html?astropract1-1112
More informationASTRO 1050 MicroObservatory RGB Image (if cloudy)
ASTRO 1050 MicroObservatory RGB Image (if cloudy) ABSTRACT For this assignment, you will be using the MicroObservatory Robotic Telescope Network, run by the Harvard-Smithsonian Center for Astrophysics
More informationProperties of a Detector
Properties of a Detector Quantum Efficiency fraction of photons detected wavelength and spatially dependent Dynamic Range difference between lowest and highest measurable flux Linearity detection rate
More informationTIRCAM2 (TIFR Near Infrared Imaging Camera - 3.6m Devasthal Optical Telescope (DOT)
TIRCAM2 (TIFR Near Infrared Imaging Camera - II) @ 3.6m Devasthal Optical Telescope (DOT) (ver 4.0 June 2017) TIRCAM2 (TIFR Near Infrared Imaging Camera - II) is a closed cycle cooled imager that has been
More informationAnnual Report on CCD Imaging at the OAN-SPM 2007
Annual Report on CCD Imaging at the OAN-SPM 2007 Michael Richer & Alan Watson November 2007 1 Introduction This is a report on the state of CCDs and small telescopes of the OAN-SPM. It is based on measurements
More informationWhat an Observational Astronomer needs to know!
What an Observational Astronomer needs to know! IRAF:Photometry D. Hatzidimitriou Masters course on Methods of Observations and Analysis in Astronomy Basic concepts Counts how are they related to the actual
More informationChapter 34 The Wave Nature of Light; Interference. Copyright 2009 Pearson Education, Inc.
Chapter 34 The Wave Nature of Light; Interference 34-7 Luminous Intensity The intensity of light as perceived depends not only on the actual intensity but also on the sensitivity of the eye at different
More informationPixel Response Effects on CCD Camera Gain Calibration
1 of 7 1/21/2014 3:03 PM HO M E P R O D UC T S B R IE F S T E C H NO T E S S UP P O RT P UR C HA S E NE W S W E B T O O L S INF O C O NTA C T Pixel Response Effects on CCD Camera Gain Calibration Copyright
More information3/5/17. Detector Basics. Quantum Efficiency (QE) and Spectral Response. Quantum Efficiency (QE) and Spectral Response
3/5/17 Detector Basics The purpose of any detector is to record the light collected by the telescope. All detectors transform the incident radiation into a some other form to create a permanent record,
More informationAstrophotography. An intro to night sky photography
Astrophotography An intro to night sky photography Agenda Hardware Some myths exposed Image Acquisition Calibration Hardware Cameras, Lenses and Mounts Cameras for Astro-imaging Point and Shoot Limited
More informationAbstract. Preface. Acknowledgments
Contents Abstract Preface Acknowledgments iv v vii 1 Introduction 1 1.1 A Very Brief History of Visible Detectors in Astronomy................ 1 1.2 The CCD: Astronomy s Champion Workhorse......................
More informationObservational Astronomy
Observational Astronomy Instruments The telescope- instruments combination forms a tightly coupled system: Telescope = collecting photons and forming an image Instruments = registering and analyzing the
More informationHIGH SPEED CCD PHOTOMETRY
Baltic Astronomy, vol.j, 519-526, 1995. HIGH SPEED CCD PHOTOMETRY D. O'Donoghue Department of Astronomy, University of Cape Town, Rondebosch 7700, Cape Town, South Africa. Received November 23, 1995. Abstract.
More informationCCD User s Guide SBIG ST7E CCD camera and Macintosh ibook control computer with Meade flip mirror assembly mounted on LX200
Massachusetts Institute of Technology Department of Earth, Atmospheric, and Planetary Sciences Handout 8 /week of 2002 March 18 12.409 Hands-On Astronomy, Spring 2002 CCD User s Guide SBIG ST7E CCD camera
More informationCross-Talk in the ACS WFC Detectors. II: Using GAIN=2 to Minimize the Effect
Cross-Talk in the ACS WFC Detectors. II: Using GAIN=2 to Minimize the Effect Mauro Giavalisco August 10, 2004 ABSTRACT Cross talk is observed in images taken with ACS WFC between the four CCD quadrants
More informationSingle Photon Interference Katelynn Sharma and Garrett West University of Rochester, Institute of Optics, 275 Hutchison Rd. Rochester, NY 14627
Single Photon Interference Katelynn Sharma and Garrett West University of Rochester, Institute of Optics, 275 Hutchison Rd. Rochester, NY 14627 Abstract: In studying the Mach-Zender interferometer and
More informationThe DSI for Autostar Suite
An Introduction To DSI Imaging John E. Hoot President Software Systems Consulting 1 The DSI for Autostar Suite Meade Autostar Suite Not Just A Project, A Mission John E. Hoot System Architect 2 1 DSI -
More informationMASSACHUSETTS INSTITUTE OF TECHNOLOGY Mechanical Engineering Department. 2.71/2.710 Final Exam. May 21, Duration: 3 hours (9 am-12 noon)
MASSACHUSETTS INSTITUTE OF TECHNOLOGY Mechanical Engineering Department 2.71/2.710 Final Exam May 21, 2013 Duration: 3 hours (9 am-12 noon) CLOSED BOOK Total pages: 5 Name: PLEASE RETURN THIS BOOKLET WITH
More informationPresented by Jerry Hubbell Lake of the Woods Observatory (MPC I24) President, Rappahannock Astronomy Club
Presented by Jerry Hubbell Lake of the Woods Observatory (MPC I24) President, Rappahannock Astronomy Club ENGINEERING A FIBER-FED FED SPECTROMETER FOR ASTRONOMICAL USE Objectives Discuss the engineering
More informationGetting started with Digital Astrophotography - Part II Rodger King - Dec 2016
Getting started with Digital Astrophotography - Part II Rodger King - Dec 2016 RECAP Getting started with Digital Astrophotography - Part I Rodger King - May 2016 Visual Astronomy Equipment Telescope Tripod
More information10/25/2017. Light and Telescope. Reflector - Mirror. Refractor - Lens. PHYS 1411 Introduction to Astronomy. Topics for Today s class
PHYS 1411 Introduction to Astronomy Light and Telescope Chapter 6 Reminders Homework on Chapter 4, 5 and 6 due November 1 st. No extensions. Lab 8 handout is on class web page. Due Week of November 27
More informationGetting started with Digital Astrophotography - Part I Rodger King - May 2016
Getting started with Digital Astrophotography - Part I Rodger King - May 2016 Flame Nebula orsehead Nebula. Question Astronomy Which type of Telescope is better - A Lens or Mirror? 500-900 More compact
More informationLecture 5. Telescopes (part II) and Detectors
Lecture 5 Telescopes (part II) and Detectors Please take a moment to remember the crew of STS-107, the space shuttle Columbia, as well as their families. Crew of the Space Shuttle Columbia Lost February
More informationTelescope Basics by Keith Beadman
Telescope Basics 2009 by Keith Beadman Table of Contents Introduction...1 The Basics...2 What a telescope is...2 Aperture size...3 Focal length...4 Focal ratio...5 Magnification...6 Introduction In the
More informationAIR FORCE INSTITUTE OF TECHNOLOGY
DETECTING NEAR-EARTH OBJECTS USING CROSS-CORRELATION WITH A POINT SPREAD FUNCTION THESIS Anthony O'Dell, Captain, USAF AFIT/GE/ENG/09-30 DEPARTMENT OF THE AIR FORCE AIR UNIVERSITY AIR FORCE INSTITUTE OF
More informationStretching Your Photons
Stretching Your Photons Advanced Imaging Conference November 10-12, 2006 San Jose, California by R. Jay GaBany www.cosmotography.com 2006 Please do not reproduce or distribute without permission. We work
More informationHotech SCA Field Flattener
Hotech SCA Field Flattener A Non-reducing Field Flattener that Works! By Alan Smallbone We are lucky enough to live in times when affordable refractors can be had for a reasonable price. This has made
More informationDesign and test of a high-contrast imaging coronagraph based on two. 50-step transmission filters
Design and test of a high-contrast imaging coronagraph based on two 50-step transmission filters Jiangpei Dou *a,b, Deqing Ren a,b,c, Yongtian Zhu a,b, Xi Zhang a,b,d, Xue Wang a,b,d a. National Astronomical
More informationGlobal Erratum for Kepler Q0-Q17 & K2 C0-C5 Short-Cadence Data
Global Erratum for Kepler Q0-Q17 & K2 C0-C5 Short-Cadence Data KSCI-19080-002 23 March 2016 NASA Ames Research Center Moffett Field, CA 94035 Prepared by: Date Douglas Caldwell, Instrument Scientist Prepared
More informationDESIGNING AND IMPLEMENTING AN ADAPTIVE OPTICS SYSTEM FOR THE UH HOKU KE`A OBSERVATORY ABSTRACT
DESIGNING AND IMPLEMENTING AN ADAPTIVE OPTICS SYSTEM FOR THE UH HOKU KE`A OBSERVATORY University of Hawai`i at Hilo Alex Hedglen ABSTRACT The presented project is to implement a small adaptive optics system
More informationImplementation of a waveform recovery algorithm on FPGAs using a zonal method (Hudgin)
1st AO4ELT conference, 07010 (2010) DOI:10.1051/ao4elt/201007010 Owned by the authors, published by EDP Sciences, 2010 Implementation of a waveform recovery algorithm on FPGAs using a zonal method (Hudgin)
More informationSecrets of Telescope Resolution
amateur telescope making Secrets of Telescope Resolution Computer modeling and mathematical analysis shed light on instrumental limits to angular resolution. By Daniel W. Rickey even on a good night, the
More informationThe Imaging Chain in Optical Astronomy
The Imaging Chain in Optical Astronomy Review and Overview Imaging Chain includes these elements: 1. energy source 2. object 3. collector 4. detector (or sensor) 5. processor 6. display 7. analysis 8.
More informationThe Imaging Chain in Optical Astronomy
The Imaging Chain in Optical Astronomy 1 Review and Overview Imaging Chain includes these elements: 1. energy source 2. object 3. collector 4. detector (or sensor) 5. processor 6. display 7. analysis 8.
More informationDigital camera. Sensor. Memory card. Circuit board
Digital camera Circuit board Memory card Sensor Detector element (pixel). Typical size: 2-5 m square Typical number: 5-20M Pixel = Photogate Photon + Thin film electrode (semi-transparent) Depletion volume
More informationCombining Images for SNR improvement. Richard Crisp 04 February 2014
Combining Images for SNR improvement Richard Crisp 04 February 2014 rdcrisp@earthlink.net Improving SNR by Combining Multiple Frames The typical Astro Image is made by combining many sub-exposures (frames)
More informationApplications of Optics
Nicholas J. Giordano www.cengage.com/physics/giordano Chapter 26 Applications of Optics Marilyn Akins, PhD Broome Community College Applications of Optics Many devices are based on the principles of optics
More informationPHYSICS. Chapter 35 Lecture FOR SCIENTISTS AND ENGINEERS A STRATEGIC APPROACH 4/E RANDALL D. KNIGHT
PHYSICS FOR SCIENTISTS AND ENGINEERS A STRATEGIC APPROACH 4/E Chapter 35 Lecture RANDALL D. KNIGHT Chapter 35 Optical Instruments IN THIS CHAPTER, you will learn about some common optical instruments and
More informationLA SILLA OBSERVATORY
EUROPEAN SOUTHERN OBSERVATORY Organisation Européenne pour des Recherches Astronomiques dans l Hémisphère Austral Europäische Organisation für astronomische Forschung in der südlichen Hemisphäre LA SILLA
More informationRobo-AO Network. Reed L. Riddle. Workshop on Astronomy with Adaptive Optics on Moderate Sized Telescopes IUCAA, Pune, India August 24, 2011
Robo-AO Network Reed L. Riddle Workshop on Astronomy with Adaptive Optics on Moderate Sized Telescopes IUCAA, Pune, India August 24, 2011 Collaborative groups Can only do science Astronomy Networks - With
More informationDepartment of Mechanical and Aerospace Engineering, Princeton University Department of Astrophysical Sciences, Princeton University ABSTRACT
Phase and Amplitude Control Ability using Spatial Light Modulators and Zero Path Length Difference Michelson Interferometer Michael G. Littman, Michael Carr, Jim Leighton, Ezekiel Burke, David Spergel
More informationPUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC. Vol. XLm San Francisco, California, August, 1931 No. 254
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC Vol. XLm San Francisco, California, August, 1931 No. 254 RECENT PHOTOGRAPHIC OBSERVATIONS OF THE PLANETS* By E. C. Slipher This note deals with recent
More informationExtreme Astrophotography How Amateurs compete with the Pro s. Johannes Schedler CEDIC-09 Linz,
Extreme Astrophotography How Amateurs compete with the Pro s Johannes Schedler CEDIC-09 Linz, 04.04.2009 http://panther-observatory.com Professional Observatories Apertures of 8-10 m in operation Huge
More informationAstronomy and Image Processing. Many thanks to Professor Kate Whitaker in the physics department for her help
Astronomy and Image Processing Many thanks to Professor Kate Whitaker in the physics department for her help What is an image? An image is an array, or a matrix, of square pixels (picture elements) arranged
More informationYour Complete Astro Photography Solution
Your Complete Astro Photography Solution Some of this course will be classroom based. There will be practical work in the observatory and also some of the work will be done during the night. Our course
More informationPhotometry using CCDs
Photometry using CCDs Signal-to-Noise Ratio (SNR) Instrumental & Standard Magnitudes Point Spread Function (PSF) Aperture Photometry & PSF Fitting Examples Some Old-Fashioned Photometers ! Arrangement
More informationRaw Material Assignment #4. Due 5:30PM on Monday, November 30, 2009.
Raw Material Assignment #4. Due 5:30PM on Monday, November 30, 2009. Part I. Pick Your Brain! (40 points) Type your answers for the following questions in a word processor; we will accept Word Documents
More informationProcessing ACA Monitor Window Data
Processing ACA Monitor Window Data CIAO 3.4 Science Threads Processing ACA Monitor Window Data 1 Table of Contents Processing ACA Monitor Window Data CIAO 3.4 Background Information Get Started Obtaining
More informationSetting GAIN and OFFSET on cold CMOS camera for deep sky astrophotography
English Version Dr. Q on astrophotography: Setting GAIN and OFFSET on cold CMOS camera for deep sky astrophotography First of all, because of some characteristics of the current CMOS cameras like insufficient
More informationMY ASTROPHOTOGRAPHY WORKFLOW Scott J. Davis June 21, 2012
Table of Contents Image Acquisition Types 2 Image Acquisition Exposure 3 Image Acquisition Some Extra Notes 4 Stacking Setup 5 Stacking 7 Preparing for Post Processing 8 Preparing your Photoshop File 9
More informationMONS Field Monitor. System Definition Phase. Design Report
Field Monitor System Definition Phase Design Report _AUS_PL_RP_0002(1) Issue 1 11 April 2001 Prepared by Date11 April 2001 Chris Boshuizen and Leigh Pfitzner Checked by Date11 April 2001 Tim Bedding Approved
More informationarxiv: v1 [astro-ph.im] 11 Oct 2016
Techniques And Results For The Calibration Of The MST Prototype For The Cherenkov Telescope Array arxiv:1610.03347v1 [astro-ph.im] 11 Oct 2016 L. Oakes 1,a), M. Garczarczyk 2, S. Kaphle 1, M. Mayer 1,
More informationSTIS First Order Spectroscopic PSF s. Ted Gull, Don Lindler Nick Collins Don Tennant Bob S. Hill Eliot Malumuth
STIS First Order Spectroscopic PSF s Ted Gull, Don Lindler Nick Collins Don Tennant Bob S. Hill Eliot Malumuth Example: Eta Carinae Balmer Alpha 150 s Eta Carinae and Ejecta 52 x0.2 F1 (0.5 ) 10 s 0.3
More informationLocally Optimized Combination of Images (LOCI) Algorithm
Locally Optimized Combination of Images (LOCI) Algorithm Keck NIRC2 Implementation using Matlab Justin R. Crepp 1. INTRODUCTION Of the myriad post-processing techniques used to reduce highcontrast imaging
More informationHello, welcome to the video lecture series on Digital Image Processing.
Digital Image Processing. Professor P. K. Biswas. Department of Electronics and Electrical Communication Engineering. Indian Institute of Technology, Kharagpur. Lecture-33. Contrast Stretching Operation.
More informationNPOI Visible Light Combiners
NPOI Visible Light Combiners 16 March 2016 Gerard van Belle NPOI Beam Combiners New Fringe Engine for NPOI Classic beam combiner NSF funded (NMT) Data capture all of 3 spectrometers, all night long Currently
More informationChasing Faint Objects
Chasing Faint Objects Image Processing Tips and Tricks Linz CEDIC 2015 Fabian Neyer 7. March 2015 www.starpointing.com Small Objects Large Objects RAW Data: Robert Pölzl usually around 1 usually > 1 Fabian
More informationSelecting the NIR detectors for Euclid
National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Selecting the NIR detectors for Euclid Stefanie Wachter Michael Seiffert On behalf of the Euclid
More information