image stability
DESCRIPTION
Image Stability. ACS SMOV image stability test (prop 9017) went from a cold soak (anti-solar pointing) for 8 orbits to a hot attitude (including off-nominal roll) Nominal jitter (typically about 3 mas RMS and 10 mas peak-to-peak) - PowerPoint PPT PresentationTRANSCRIPT
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Image StabilityImage StabilityImage StabilityImage Stability
ACS SMOV image stability test (prop 9017) went from a cold soak (anti-solar pointing) for 8 orbits to a hot attitude (including off-nominal roll)– Nominal jitter (typically about 3 mas RMS
and 10 mas peak-to-peak) – Smooth drift at rates up to about 6 mas/hr in
both the HRC and WFC (same direction). – Drift may be due to FGS's or to rigid body
movement of the ACS wrt the OTA– Similar to image drift rates for other SIs.
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Calibration – Flat FieldsCalibration – Flat FieldsCalibration – Flat FieldsCalibration – Flat Fields
L-flat for the F555W filter, the plot is a 4th order least-squares fit to the stellar photometry. – ~10% gradient from upper left to lower
right– (Mack, van der Marel, Bohlin, Blakeslee,
Cox)
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Flat field – Sanity ChecksFlat field – Sanity ChecksFlat field – Sanity ChecksFlat field – Sanity Checks
Ratio of the F555W photometry in the CRJ to the DRZ image, corrected for distortion. – White is 1.10 and black is 0.93.
Pixel Map from Geometricdistortion – ratio produces 1% residual
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SensitivitySensitivitySensitivitySensitivity
0.8 0.85 0.9 0.95 1 1.05 1.1 1.15 1.2
F220W
F250WF330W
F344N
F435WF475W
F502N
F550M
F555WF606W
F625W
F658NF660N
F775W
F814WF850LP
F892N
• Inflight sensitivity vs prediction from components
0.85 0.95 1.05 1.15 1.25
F435W
F475W
F502N
F550M
F555W
F606W
F625W
F658N
F660N
F775W
F814W
F850LP
F892N
HRC WFC
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WFC Distortion CalibrationWFC Distortion CalibrationWFC Distortion CalibrationWFC Distortion Calibration
• 4th order 2D polynomial fit matches observed distortion well - RMS residual 1.1 mas (.02 px) - peak deviation ~ .2 px
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WFC CCD Amplifier Cross-talkWFC CCD Amplifier Cross-talkWFC CCD Amplifier Cross-talkWFC CCD Amplifier Cross-talk
• Low-level “ghosts” of extended objects mirrored in alternate quadrants• Slight “droop” (fractional e-) in bias level of all 3 alternate amps• Ghosts do not appear to be proportional to target signal
Hard (2 e-) stretch ofWFC UGC10214 image
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WFC: Long wave haloWFC: Long wave haloWFC: Long wave haloWFC: Long wave halo
B acks id e i llu m in ate d,th in n ed C C D (~1 5 m )
S od a g lass h ead er200 0 m
He ad er m eta liz atio n
CC D Pac kage Cro ss -se ction
Al metal layer reflects long- photons
F814w F850LP
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WFC: Long wave haloWFC: Long wave haloWFC: Long wave haloWFC: Long wave halo
F775W F850LP FR1016N - 996
FILTER ETC Measured 80%5x5 px 5x5 px Ensq (px)
F775W (I) 0.8 0.79 5.2F850LP (z) 0.76 0.68 7.1FR1016N-996 0.73 0.49 15
IR Encircled Energy Performance
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Optical “Ghosts”Optical “Ghosts”Optical “Ghosts”Optical “Ghosts”
Two ghost features have been identified with >0.1% of target energy:
WFC CCD to window reflection produces pairs of elliptical ghosts with ~ 0.2% integrated energy
F660N [NII] filter produces halos with ~2% of integrated energy due to reflection between its surfaces
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Cats-Eye Nebula
NGC 6543 (HRC)
[OII] 3727 [OIII] 5007 H
Ramp filter
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Coronagraph performanceCoronagraph performanceCoronagraph performanceCoronagraph performance
• Target acquisition functions• executed proposal second time with dithering to determine optimum location under each occulting spot
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Coronagraph Dither Coronagraph Dither ResultsResults
Coronagraph Dither Coronagraph Dither ResultsResults
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Coronagraph PerformanceCoronagraph PerformanceCoronagraph PerformanceCoronagraph Performance
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SBC – First Light ImageSBC – First Light ImageSBC – First Light ImageSBC – First Light Image
Globular star cluster NGC6681. This cluster, with [Fe/H] = -1.5, is rich in Blue Horizontal Branch stars.The image combines first light data taken with three filters F125LP, F150LP, and F165LP.
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Solar Blind ChannelSolar Blind ChannelSolar Blind ChannelSolar Blind Channel
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CALACSCALACSCALACSCALACS
• First generation updates to CALACS & PyDrizzle are complete, software is frozen for distribution in next STSDAS
•Includes ST-ECF AXE software for grism/prism
Mosaic generated from 18 images of 47 Tuc
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HDF-N: i+ z & grism HDF-N: i+ z & grism HDF-N: i+ z & grism HDF-N: i+ z & grism
WFC - 2x i- 3x z orbits - “HDF overlay”
Grism: 3 orbits
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HDF-N ACS Grism HDF-N ACS Grism examplesexamples
HDF-N ACS Grism HDF-N ACS Grism examplesexamples
Emission-line galaxy with continuum and knots - [OIII] 5007 and H 6563
Redshift z = 0.319 F814AB = 22.5
(WFC 2x i + 3x z orbits, 3 grism orbits)
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HDF-N SN2002dc HDF-N SN2002dc HDF-N SN2002dc HDF-N SN2002dc
WFC 2x i + 3x z orbits, 3 grism orbits
Galaxy & SN z=0.475
• Identified from difference imaging with WFPC2 HDFN
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HDF-N SN2002dcHDF-N SN2002dcHDF-N SN2002dcHDF-N SN2002dc
• Galaxy and SN at z=0.48
• SN mag. is 22.7 (i)
• Type I (probably Ia)
Galaxy & SN z=0.475
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SN2002dd SN2002dd SN2002dd SN2002dd
Galaxyz=0.79
• Identified from extracted spectra !
SnIaz=1.06
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HDF-N SN2002ddHDF-N SN2002ddHDF-N SN2002ddHDF-N SN2002dd
• Follow-up with DD proposal
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Cool Image – A1689Cool Image – A1689Cool Image – A1689Cool Image – A1689
CourtesyACS Science Team
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Image StabilityImage StabilityImage StabilityImage Stability