Karl D. Gordon & the
JWST Efficiency WG
15 Aug 2012
TIPS/JIM
STScI
SODRM 2012
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SODRM = Science Operations Design Reference Mission
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Goal is to generate a realistic estimate of the 1st year of JWST observations for
subsequent studies to improve efficiencies and other operations studies
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Not used for efficiency requirement
More realistic than SODRM 2005
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Observing and Engineering Templates
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Target acquisition
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Defined dither patterns
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Broader, more realistic science
Major effort by STScI and wider JWST community
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JWST Efficiency WG: K. Gordon (lead), V. Balzano, W. Blair, H. Ferguson, W. Kinzel, J.
Lotz, J. Rigby, G. Sonneborn, & J. Tumlinson
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Total of 56 scientists contributing directly
112 programs → 1.78 years total time
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70 science, 42 calibration
JWST-STScI-CI-000045, Revision C
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Undergoing final review in SOCCER
SODRM 2012 Program Information
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Every program had a coordinator (most from STScI)
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Responsible for making sure the program material is submitted
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Working with others was encouraged, especially those outside of STScI
Program nominal allocation given
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Provided an approximate guideline and breakdown between the major science
categories
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Actual program times were driven by the science needs
1-2 page description of each program
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APT/spreadsheet file
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Details that define the exposures (e.g., filling out the options in an observing
template)
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APT [19.4]: NIRCam, NIRSpec, MIRI
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Spreadsheet: NIRISS
Programs are an approximation of the cycle 1 JWST observations
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Science summary and outline of targets and observational strategies
Not allocations or reservations of observing time
Expect that the SODRM will be revised a few more times before launch
Example
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Imaging of resolved stellar populations (ID: 94010, lead: Gordon)
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The goal is to investigate the stellar populations in nearby galaxies
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AGB & YSO stars are of particular interest in the MIR
Targets
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4 positions in M31 (nucleus to 10 kpc star forming ring)
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3 positions each in LMC, SMC, & NGC 6822 (metallicity range)
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2 positions each in M33, M51, M81, & M82 (sample center and disk)
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1 position each in NGC 925, 1097, 3351, 4125, 4594, 5866, & 6946 (samples a
range of galaxy types)
MIRI & NIRCam Imaging
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MIRI (4x4 mosaic w/ Reuleaux dithering at each point)
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NIRCam (4x1 mosaic w/ full dithers [3 primary & 2 subpixel])
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F560W, F770W, F1000W, F1500W, F2100W
F115W, F356W
Total time required (w/ direct overheads): 494.2 hours
Example Program Description
Distribution of all Sources (Galactic Coordinates)
Circle sizes are proportional to the total exposure time per target per instrument
Colors are: Exoplanets, Galactic, Nearby Galaxies, Distant Galaxies & Cosmology,
& Calibration. No Solar System as moving targets are not shown.
Distribution of all Sources (Celestial Coordinates)
Circle sizes are proportional to the total exposure time per target per instrument
Colors are: Exoplanets, Galactic, Nearby Galaxies, Distant Galaxies & Cosmology,
& Calibration. No Solar System as moving targets are not shown.
Distribution of Total Exposure Times
per target per instrument
Cumulative Histrogram. Median exp. = 0.38 hours. Mean exp. = 1.84 hours.
Colors are: Solar System, Exoplanets, Galactic, Nearby Galaxies,
Distant Galaxies & Cosmology, & Calibration.
Solar System
Calibration
SODRM 2012 by
Category
Exoplanets
Distant Galaxies &
Cosmology
Galactic
Nearby Galaxies
SODRM 2012 by Instrument
MIRI
NIRSpec
NIRISS
NIRCam
NIRISS
NIRCam
Cor
SODRM by
Template
AMI
IFU
NIRSpec
Imaging
Fixed Slit
MSA
Cor
IFU
Imaging
LRS
MIRI
Thanks
This SODRM would not have been possible without the effort of a large group of people.
We thank all those that contributed.
Special thanks to the science program leads (J. Anderson, T. Beck, W. Blair, T. Brown,
C. Chen,J. Debbes, H. Ferguson, S. Friedman, K. Gordon, P. Goudfrooij, D. Hines, J.
Kalirai, T. Keyes, A. Koekemoer, D. Lafrenière, D. Lennon, C. Lisse, J. Lotz, R.
Maiolino, M. Meixner, J. Muzerolle, K. Pontoppidan, M. Regan, A. Rest, J. Rigby, M.
Robberto, K. Sahu, J. Stansberry, R. Soummer, J. Tumlinson, & J. Valenti) and
calibration program leads (H. Ferguson, K. Gordon, A. Koekemoer, J. Muzerolle, & M.
Perrin).
Thanks to all the others that have contributed to the creating the SODRM programs but
were not leads (R. Abraham, S. Arribas, T. Boker, M. Boyer, A. Bunker, N. Chanover,
S. Charlot, C. Engelbracht, C. Evans, P. Ferruit, M. Franx, T. Greene, H. Hammel, B.
Hansen, P. Jakobsen, W. Kinzel, D. Karakla, K. Noll, H. Richer, H.-W. Rix, J. Seale,
D. Soderblom, K. Uckert, C. Willott, M. Wolff).
Backup Slides
SODRM 2012: Future
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Direct interests of the JWST Efficiency WG
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Use to determine the current JWST observing efficiency
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Quantify the contribution each overhead makes
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Identify overheads for further study and potential reduction in size
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Interactions with the scheduling software
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Potential gains from science parallel observations
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Look at ways to efficiently implement them (limited parallels?)
Other planned SODRM 2012 studies
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Data volume, Mechanism usage, Momentum and propellant management
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Visit scheduling, Slew distribution, Test scheduling algorithms and constraints
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Provide early testing and feedback on the ground system (APT, ETC, operations,
etc.)
Post SODRM 2012 publicly
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Assumes the current JWST operations strategy
Invite the community to provide comments/updates
Next SODRM update in 2013/2014