1 WFC3 Science Data Volume  Data Volume Estimates for WFC3 Operations ISR WFC3 2001-02; Lisse, Henry, Knezek, Hanley; 3/27/2001 ISR WFC3 2001-02; Lisse,

Slides:



Advertisements
Similar presentations
XRT Instrument Capabilities Ed DeLuca, Leon Golub & Jay Bookbinder SAO.
Advertisements

A NEW CTE PHOTOMETRIC CORRECTION FORMULA FOR ACS Marco Chiaberge TIPS meeting 05/16/2012.
1 WFC3 UVIS Shutter Blade Kailash C. Sahu STScI STScI Calibration Workshop August 13, 2014 With thanks to Sylvia Baggett and Megan Sosey.
Return to Hubble: Servicing Mission 4 Dr. Frank Summers Space Telescope Science Institute April 2, 2009.
The Status of the Hubble Space Telescope 2014 STScI Calibration Workshop Helmut Jenkner.
Proposed CalJWST Structure M. Robberto. Cross-Instrument Rationale 2 level processing  CALinsA: from RAMP to calibrated images  CALinsB: associated.
SDW Marco Sirianni Marco Sirianni (ESA/STScI) Max Mutchler (STSci) Radiation Damage in HST Detectors.
Following the Photons… Empirical, Pixel-Based Corrections for CTE Jay Anderson STScI October 12, 2011 Back-Tracking the Electrons.
How Does WFC3 Geometric Distortion Vary with Time ? Kozhurina-Platais.
Page 1 9/4/01 SMS Test Phase 2 & 3 WFC3 FSW and STScI Development Flow through SMGT 4/1/02-6/30/02 FSW 2.1 C&UT 7/8/01-8/15/01 FSW 2.2 C&UT - WFC3 Software.
SECCHI – Sun-Earth Connections Coronal and Heliospheric Investigation SECCHI Synoptic and Special Observing Programs Simon Plunkett SECCHI Operations Lead.
We have the first, direct measure of photometric loss due to imperfect CTE on ACS.
S. Baggett, J. Anderson, K. S. Long, J. W. MacKenty, K. Noeske, J. Biretta, and the WFC3 team (STScI) WFC3 : Understanding and mitigating UVIS charge.
1 TIPS 2011 May Persistence in the WFC3 IR detector Knox S. Long.
AST3 detector properties
ZTF Server Architecture Roger Smith Caltech
NGC 6217 in DSI mode with F658N Mosaic before new superbias why we don’t release images until after SMOV! ACS CCD monitoring and pipeline calibration review.
Printed by ACS 2 Gyro Mode Data Analysis Cheryl Pavlovsky, Marco Sirianni, Ken Sembach, ACS Instrument Team and the 2 Gyro Mode Team.
Introduction to and methods of SPACE-based observational astronomy 1 st MAGPOP School (Budapest, Aug ) Armando Gil de Paz (Universidad Complutense.
File FormatsFile Formats File Name ConventionsFile Name Conventions File ContentsFile Contents Association Contents & RulesAssociation Contents & Rules.
Page 1. Page 2 SMOV Status SMOV is proceeding on-track Key programs executed –ERO program –Geometric distortion program completed –ACS to FGS alignment.
N A S A G O D D A R D S P A C E F L I G H T C E N T E R I n s t r u m e n t S y n t h e s i s a n d A n a l y s i s L a b o r a t o r y Earth Atmosphere.
Science with the new HST after SM4 WFC3 slitless spectroscopy Harald Kuntschner Martin Kümmel, Jeremy R. Walsh (ST-ECF) WFC3-team at STScI and NASA.
NIRSpec Operations Concept Michael Regan(STScI), Jeff Valenti (STScI) Wolfram Freduling(ECF), Harald Kuntschner(ECF), Robert Fosbury (ECF)
Tutorial T-10 Amber Data Reduction (practical point of view) EuroSummer School Observation and data reduction with the Very Large Telescope Interferometer.
May 21, 2009John MacKenty, STScI1 WFC3 SM4 Events and Current Status.
High Precision Astrometry and Parallax from Spatial Scanning Part 2 Adam Riess and Stefano Casertano.
TIPS COS Overview - Keyes : 18 May 2000 COS Overview v CDR: April 2000 v FUV delivery: January 2001 v Environmental (Thermal-Vac): spring 2002 v Launch:
FTS Test Definition Summary Kaley Walker Test Readiness Review January 29, 2003.
The Status of HST/WFC3 John W. MacKenty Space Telescope Science Institute 12 August 2014 Calibration Workshop.
Observational Astrophysics I
SPACE TELESCOPE SCIENCE INSTITUTE Operated for NASA by AURA COS Pipeline Calibration Goals of CALCOS Association Table Input and Output Files High Level.
SNAP Collaboration meeting / Paris 10/20071 SPECTROMETER DETECTORS From science requirements to data storage.
COS Training Series II. Optimizing Observations --- David Sahnow February mm.
1 ACS Press Releases Science  Grism spectroscopy of UDF galaxies  Mass of the MACHO-LMC-5 lens  Earliest star-forming galaxies in UDF  Kepler’s SNR.
START NICMOS COOLING SYSTEM ACTIVITY SUMMARY. 1/25/01Ken Pulkkinen2 START NCS ACTIVITY Applicable SMOV Requirements: J NICMOS Cooling System.
Overall ArchitectureOverall Architecture Use of AssociationsUse of Associations Outline of ProcessingOutline of Processing Reuse of CALACS and CALNIC CodeReuse.
Calibration of the ACS Emission-Line Filters. C. R. (Bob) O’Dell Vanderbilt University.
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.
1 Hubble Science Operations Status Rodger Doxsey 18 November 2004.
Overall ArchitectureOverall Architecture Outline of ProcessingOutline of Processing Reuse of CALACS and CALNIC CodeReuse of CALACS and CALNIC Code Processing.
NICMOS Calibration Challenges in the Ultra Deep Field Rodger Thompson Steward Observatory University of Arizona.
The European Hubble Space Telescope Legacy Archive Wolfram Freudling.
Astronomical Observational Techniques and Instrumentation
SPACE TELESCOPE SCIENCE INSTITUTE Operated for NASA by AURA COS Monthly Status Review 17 September 2002.
APT Overview for Transiting Exoplanet Proposals Chris Moriarty – APT Developer.
Venus Observations HST Program Objectives v Explain Venus observing strategy. v Review areas of special concern with Venus observations and explain.
Basic Detector Measurements: Photon Transfer Curve, Read Noise, Dark Current, Intrapixel Capacitance, Nonlinearity, Reference Pixels MR – May 19, 2014.
Click to Change Title Here is a text box to present information in paragraph format, instead of bulleted lists. We’ve left space to the right for an image.
WFC3 SMOV Report for TIPS 16 July 2009 John MacKenty This presentation contains material that is embargoed until after the SM4 ERO press conference. Images/spectra.
Introduction NICMOS (Near-Infrared Camera and Multi-Object Spectroscopy) was installed on the Hubble Space Telescope during SM2 in 1997 and has been the.
1 WFC3 – Critical Science Review Science Driven CEIs Requirements.
CCD Image Processing: Issues & Solutions. CCDs: noise sources dark current –signal from unexposed CCD read noise –uncertainty in counting electrons in.
Status of PREMOS data SOLID Workshop 14th October 2013 G. Cessateur for the PREMOS team PMOD/WRC, Switzerland.
Installation of the ACS Guido De Marchi – TIPS meeting – Guido De Marchi - ESA/STScI - ACS Group The ACS was installed on board the HST on the.
WFC3 slitless spectroscopy
 Average – mean, median and mode are three “kinds” of average (commonly used to describe the mean).  Mean temperature – average temperature of the air.
Introducing the INS Master Schedule Wayne Baggett.
STIS Status TIPS, September 17, 2009 Charles Proffitt for the STIS team.
HST Cal Conf -- Oct 27, Calibration Status and Results for Wide Field Camera 3 – R. Kimble/GSFC, Calibration Status and Results.
July 25th, 2000WFC3 Critical Science Review1 Performance Summary in Key Science Areas Verify that WFC3 as designed is capable of carrying out the WFC3.
CCD Calibrations Eliminating noise and other sources of error.
OSIRIS operation summary
JWST Science Policy & Science Parallels
Observing Strategies and Constraints
Imaging with the James Webb Space Telescope
GPI Astrometric Calibration
LRO Mission Operations Concept
Observing with Modern Observatories (the data flow)
MDP / DHU - DR Usage vs downlinks -
Presentation transcript:

1 WFC3 Science Data Volume  Data Volume Estimates for WFC3 Operations ISR WFC ; Lisse, Henry, Knezek, Hanley; 3/27/2001 ISR WFC ; Lisse, Henry, Knezek, Hanley; 3/27/2001  Data Volume per WFC3 exposure UVIS Channel Full frame image = 4140 x 4206 pixels (including overscan) = 266 Mbits/exposure IR Channel Full frame image = 1024 x 1024 pixels (including reference pixels) = 16 Mbit/image

2 WFC3 Primary Data Volume  Observing time allocation assumptions One third of orbits are used for spectroscopy and two thirds for imaging Imaging is divided evenly between WFC3 and ACS (5 orbits/day each) 60% of WFC3 primary orbits will use the UVIS channel (3 orbits/day) 40% of WFC3 primary orbits will use the IR channel (2 orbits/day)  WFC3 ETC was used to determine the number of exposures per orbit for each filter used in 41 DRM proposals UVIS exposures assumed CRSPLIT = 2 Number of exposures per orbit was limited to 10 for UVIS and 17 for IR based on the transfer rate out of the WFC3 data buffer and a 60 minute visibility period

3 WFC3 Primary Data Volume  Summary of exposure statistics UVISIR Total number of exposures42,36129,053 Total number of orbits9,7395,140 Average exposures/orbit  Primary UVIS data volume 266 Mbits/exp * 4.4 exp/orbit * 3 orbits/day = 3461 Mbits/day  Primary IR data volume Average number of nondestructive readouts = 10 Average data volume per exposure = 16 Mbits/image * 10 images/exp 160 Mbits/exp * 5.7 exp/orbit * 2 orbits/day = 1808 Mbits/day

4 WFC3 Parallel Data Volume  Assume WFC3 is in parallel for all non-prime orbits 30% of WFC3 parallel orbits will use the UVIS channel (3 orbits/day) 70% of WFC3 primary orbits will use the IR channel (7 orbits/day) Assume an average of 2 exposures per parallel orbit for UVIS and IR  Parallel UVIS data volume 266 Mbits/exp * 2 exp/orbit * 3 orbits/day = 1596 Mbits/day  Parallel IR data volume Average number of nondestructive readouts = 16 Average data volume per exposure = 16 Mbits/image * 16 images/exp 256 Mbits/exp * 2 exp/orbit * 7 orbits/day = 3584 Mbits/day

5 WFC3 Calibration Data Volume  Routine calibration exposures performed during occultations UVIS IR Internal Flats Earth Flats Dark Frames Bias Frames 104 Total per cycle Exposures/day  Calibration UVIS data volume 266 Mbits/exp * 3.6 exp/day = 950 Mbits/day  Parallel IR data volume 256 Mbits/exp * 2.2 exp/day = 568 Mbits/day

6 WFC3 Average Data Volume UVISIR Exp/dayMbits/dayExp/dayMbits/day Primary Parallel Calibration Total  Combined WFC3: 50 Exp/day11.7 Gbits/day

7 Post SM4 Average Data Volume PrimaryParallelCalibrationTotal WFC ACS COS STIS Total Average daily data volume in Gbits without overheads Average daily data volume in Gbits without overheads

8 Average Data Volume Trend (Gbit) PrimeParCalDailyWeekly (w overheads) SM SM SM  190 Gbit/week is 80% of the 245 Gbit maximum using one transmitter  Test SMSs with 150 Gbit of science data have shown the feasibility of scheduling at 60% of TDRSS capacity using both HST SSRs to buffer data (High data Volume SMSs and TDRS Contact Usage, Patterson et al, 5/18/200)  Using two HST transmitters raises maximum weekly downlink to 440 Gbit but transmitter lifetime concerns make operating in this mode undesirable.