Solar-B SOT/FPP 1 SOT-17 17-20 April 2006Ted Tarbell FPP CCD Camera Performance Ted Tarbell 17-Apr-2006.

Slides:

Advertisements

Similar presentations

Toolkit for testing CCD cameras

Advertisements

Area Detectors Like film can detect position Like scintillation detector can measure intensity With modern computers can assign hkl from unaligned crystal.

First results from the HEPAPS4 Active Pixel Sensor

1 Estimate on SOT light level in flight with throughput measurements in SOT sun tests T. Shimizu 1, T. Tarbell 2, T. Berger 2, Y. Suematsu 3, M. Kubo 1,

1 Estimate on SOT light level in flight with throughput measurements in SOT sun tests T. Shimizu 1, T. Tarbell 2, Y. Suematsu 3, M. Kubo 1, K. Ichimoto.

CHARGE COUPLING TRUE CDS PIXEL PROCESSING True CDS CMOS pixel noise data 2.8 e- CMOS photon transfer.

Astronomical Detectors

1 Lites FPP-SP Performance SOT #17 Meeting, NAOJ, April Solar-B FPP As-Built Performance of the FPP Spectro- Polarimeter October, 2004 FPP Team Bruce.

CCDs. CCDs—the good (+)  Linear response  photometry is “simple” +High efficiency, compared to other detectors +Sensitive to many wavelengths +2-D arrays.

SDW20051 Vincent Lapeyrère LESIA – Observatoire de Paris Calibration of flight model CCDs for CoRoT mission.

PLATO kick-off meeting 09-Nov-2010 PLATO Payload overall architecture.

From CCD to EMCCD Scientific imaging for today’s microscopy.

Charge-Coupled Device (CCD)

CCD testing Enver Alagoz 12 April CCD testing goals CCD testing is to learn how to – do dark noise characterization – do gain measurements – determine.

CCD Detectors in High- Resolution Biology Jian Guan

Overview of Scientific Imaging using CCD Arrays Jaal Ghandhi Mechanical Engineering Univ. of Wisconsin-Madison.

EMVA 1288 ITE 2008 M. Wäny CMOS IMAGE SENSORS Clear definitions for a clear VISION EMVA 1288 Standard for Measurement and Presentation of.

Different sources of noise in EM-CCD cameras

Agile: A Time-Series CCD Photometer to Study Variables Anjum Mukadam, Russell Owen, Ed Mannery University of Washington, Seattle.

A new idea of the vertex detector for ILC Y. Sugimoto Nov

Detecting Electrons: CCD vs Film Practical CryoEM Course July 26, 2005 Christopher Booth.

AST3 detector properties

Photon Transfer Method 1. Using two identical flat field exposures it is possible to measure the read noise of a CCD with the Photon Transfer method. Two.

D. Neff, expts done This report shows 2rh window origami (two rhodamine labeled staples/origami). Massud annealed and stored this origami at 4.

Low Light Level CCDs (LLLCCD) A new idea from Marconi (EEV) to reduce or eliminate CCD read-out noise.

SBIG ST-7XME CCD Presentation by Keith Rickard. And now for something completely different… What colour is a rainbow? It’s red!

CMOS Image Sensor Design. M. Wäny Nov EMVA Standard 1288 Standard for Measurement and Presentation of Specifications for Machine Vision Sensors and.

CCD Detectors CCD=“charge coupled device” Readout method:

Active Pixel Sensors for Direct Detection of Soft X-rays Andrew Blue* a, R. Bates a, A. Clark c, S. Dhesi b, D. Maneuski a, J. Marchal b, P. Steadman b,

NIRSpec Operations Concept Michael Regan(STScI), Jeff Valenti (STScI) Wolfram Freduling(ECF), Harald Kuntschner(ECF), Robert Fosbury (ECF)

10/26/20151 Observational Astrophysics I Astronomical detectors Kitchin pp

XRT’s Observational Parameters R. Kano (NAOJ). Contents FOV & Full Disk Imaging Time Cadence & Observation Table New Items as Solar X-ray Telescopes –Pre-flare.

CDE CDR, September 14, 2004 Your Position, Your Name 1 GATS AIM Science Team Meeting January 23-24, 2007 CIPS Calibration Review, Aimee Merkel, Bill McClintock.

Feb 4, 20034th Solar-B Science Meeting1 SOT Scientific Observations & Operations T. Shimizu (National Astronomical Observatory of Japan)

1 WB/lct CCD OVERVIEW Kepler will have 42 CCDs 2,200 column x 1,024 row full frame CCDs Field of View (FOV) > 100 square degrees (113 w/ vignetting)

Apr 17-22, NAOJ SOT optical performance Focus stability in orbit Y. Katsukawa (NAOJ) and SOT team.

First tests of CHERWELL, a Monolithic Active Pixel Sensor. A CMOS Image Sensor (CIS) using 180 nm technology James Mylroie-Smith Queen Mary, University.

ACS STATUS Linda Smith (thanks to David Golimowski for providing the slides)

Astronomical Institute University of Bern 31th IADC Meeting, April , 2013, ESOC, Darmstadt, Germany Improved Space Object Observation Techniques.

Observational Astrophysics I

1 SOT Polarization Calibration -- method and results for FG -- K.Ichimoto and SOT Team SOT#

1 Optical observations of asteroids – and the same for space debris… Dr. D. Koschny European Space Agency Chair of Astronautics, TU Munich Stardust school.

Choosing the Appropriate Camera “Resolving” the Application.

Human vision The image is formed on retina (sítnice) –The light is focused on retina by lens (čočka) –Retina contains two types of receptors: rods (tyčinky)

TIPS - Oct 13, 2005 M. Sirianni Temperature change for ACS CCDs: initial study on scientific performance M. Sirianni, T. Wheeler, C.Cox, M. Mutchler, A.

Physics 114: Lecture 8 Measuring Noise in Real Data Dale E. Gary NJIT Physics Department.

On the Evaluation of Optical Performace of Observing Instruments Y. Suematsu (National Astronomical Observatory of Japan) ABSTRACT: It is useful to represent.

1 Scientific Data from Solar-B Solar Optical Telescope (SOT) T.Shimizu (NAOJ) Solar-B MO&DA Working Group

STIS STATUS Charles Proffitt TIPs May 21, STIS Status - Status of Repair Results of FT Amp B Bias Anomaly Changes to SMOV Plan.

1 Performance of a CCD tracker at room temperature T. Tsukamoto (Saga Univ.) T. Kuniya, H. Watanabe (Saga Univ.); A. Miyamoto, Y. Sugimoto (KEK); S. Takahashi,

Plato Consortium Kickoff Meeting, Paris 1 09-Nov-2010 Plato CCD and Front-End Electronics Dave Walton UCL/MSSL

2006/4/17-20 Extended 17 th SOT meeting M. Kubo (JAXA/ISAS), K. Ichimito, Y. Katsukawa (NAOJ), and SOT-team Comparison of FG and SP data from Sun test.

IAS Hinode Data WorkshopThursday 15-November-2007 The Hinode Solar Optical Telescope Data & Calibration Dr. Thomas Berger Lockheed Martin Advanced Technology.

Cameras For Microscopy Ryan McGorty 26 March 2013.

Digital Cameras in Microscopy Kurt Thorn Nikon Imaging QB3/UCSF.

Comparison of a CCD and the Vanilla CMOS APS for Soft X-ray Diffraction Graeme Stewart a, R. Bates a, A. Blue a, A. Clark c, S. Dhesi b, D. Maneuski a,

CCD Calibrations Eliminating noise and other sources of error.

Announcements After a short lecture we will adjourn to the Farm. Tonight is a Dark Sky make-up night. Class will meet Thursday night. If clear: meet at.

Relative Spectral Response and Flat Fields with Internal Calibration Lamps Luisa M. Lara IAA-CSIC Granada (SPAIN)

Charge Transfer Efficiency of Charge Coupled Device

Chapter I, Digital Imaging Fundamentals: Lesson II Capture

Preliminary Design Review

Preliminary Design Review

SCIENTIFIC CMOS PIXELS

EPIC Calibration & Operations Meeting

Announcements HR Diagram lab will be extended for one week. I’ll talk about it today. Homework: Chapter 9 # 1, 2 & 3 Next week is a Dark Sky Night. If.

Measuring the Density of Laser-Cooled Atoms

Turning photons into bits in the cold

European Synchrotron Radiation Facility:

IN5350 – CMOS Image Sensor Design

Presentation transcript:

Solar-B SOT/FPP 1 SOT April 2006Ted Tarbell FPP CCD Camera Performance Ted Tarbell 17-Apr-2006

Solar-B SOT/FPP 2 SOT April 2006Ted Tarbell FPP CCD Detectors FG: 4096 x 2048 pixels, thinned, back-illuminated SP: two 24 x 1024 on the same chip, front-illuminated CT: 50 x 50, front-illuminated All have 12 micron square pixels FG CCD CT CCD SP CCD

Solar-B SOT/FPP 3 SOT April 2006Ted Tarbell FPP CCD Cameras All cameras: – Low power, radiation resistant, cooled electronics boxes –2.5 Mega-pixels/sec readout rate, with 12-bit A-D conversion –SP & FG detectors are cooled, CT at room temperature FG Camera –On-chip summing of 1x1, 2x2 or 4x4 pixels –Full frame readout in 3.75 sec (1x1) or 1.9 sec (2x2) –Full frame exposure with shutter or partial frame continuous exposure in shutterless frame transfer mode SP Camera –Continuous exposure, shutterless frame transfer mode –112 spectral x 1024 spatial pixels on each of 2 detectors –On-chip summing of 1x2 pixels possible (spatial summing)

Solar-B SOT/FPP 4 SOT April 2006Ted Tarbell Linearity & Noise from Light Transfer Linearity Plot Average intensity vs. exposure time for a constant source There is an electronic offset at exposure time = 0 Noise Plot Noise-squared vs. average intensity Straight line for an ideal camera Slope is square-root-of-N noise Value at electronic offset = read noise

Solar-B SOT/FPP 5 SOT April 2006Ted Tarbell FG Gains & Read Noise Levels GainElectrons/DNRead Noise (DN) Read Noise (e) Prime Prime Prime Prime Red Red Red Red Results from FPP Thermal/Vacuum Test, 27 Mar 2004 FG CCD –32 C SP CEB +5 C Darks

Solar-B SOT/FPP 6 SOT April 2006Ted Tarbell SP Gains & Read Noise Levels GainElectrons/DNRead Noise (DN) Read Noise (e) Prime Prime Prime Prime Red Red Red Red Results from FPP Thermal/Vacuum Test, 8 April 2004 SP CCD –38 C SP CEB 0 C Darks

Solar-B SOT/FPP 7 SOT April 2006Ted Tarbell CT Gains & Read Noise Levels GainElectrons/DNRead Noise (DN) Read Noise (e) Prime Prime Prime Prime Red Red Red Red Results from CT CEB Checkout, 26 Nov 2003 Room Temperature Light Transfer Curves

Solar-B SOT/FPP 8 SOT April 2006Ted Tarbell FG & SP have Additional “ADC” Noise Before Repair After Repair

Solar-B SOT/FPP 9 SOT April 2006Ted Tarbell Dark Current in FG Camera Dark Current is not measurable below about -30 deg C and is negligible below about 0 deg C Read noise does not depend on temperature

Solar-B SOT/FPP 10 SOT April 2006Ted Tarbell Orbital Temperature Variation

Solar-B SOT/FPP 11 SOT April 2006Ted Tarbell Conclusions Developing these cameras to meet the requirements of high readout rate, low noise, excellent linearity, low power, and radiation tolerance was a significant challenge FG and SP have ADC noise, and SP has more readout noise than desired Nevertheless, they meet their fundamental noise requirements –SP: 1000:1 polarimetric SNR in normal mode –FG: 200:1 SNR in single images, 500:1 pol. SNR in normal mode –CT: < arcsecond rms error per axis in image displacement The FG and SP cameras will be cold enough that dark current will be negligible