'Flat field' diaporamas de présentation

Photometric Methods and Sources of Noise

Photometric Methods and Sources of Noise. CCD Detectors Photometric measurements Sources of Noise. Photometric detectors of the past: photomultipliers. Not good for transit work because you could only observe one star at a time.

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Forces cause changes in motion.

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Forces cause changes in motion.

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Resolution Specification

Definition of resolution In all cases the resolution is defined as l/Dl , where Dl is the FWHM of an emission line measured in pixels multiplied by the dispersion determined during wavelength calibration.

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PACS CQM/AVM ILT

PACS CQM/AVM ILT. Results of functional/performance/ calibration tests. Major (science) requirements on PACS. Detectors: Sensitivity, Detector/readout noise (NEP), Dynamic Range Image Quality: blur, distortion, misalignment

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Photometric Techniques I Preliminary reductions and calibrations Sergio Ortolani

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Ground-based observations of Kepler asteroseismic targets

Ground-based observations of Kepler asteroseismic targets. Joanna Molenda-?akowicz Instytut Astronomiczny Uniwersytetu Wroc?awskiego POLAND. Kepler asteroseismic targets. what are these objects? pulsating, preferably solar-type stars that will be observed by the Kepler space telescope

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COR1 CURRENT STATUS AND FUTURE PLANS

COR1 CURRENT STATUS AND FUTURE PLANS. Joseph Davila 1 , O. C. St. Cyr 1 William Thompson 2 1 NASA Goddard Space Flight Center, 2 Adnet Systems, Inc. COR1 Status. COR1-A and COR1-B are both observing regularly as part of the synoptic program Both are returning scientifically-useful images!

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COS Training Series IV: COS Post-observation

COS Training Series IV: COS Post-observation. M.E. Kaiser P. E. Hodge 28 February 2008. COS Spectrograph (Colorado, BASG). COS Pipeline Verification. STScI : Mary Elizabeth Kaiser Phil Hodge Tony Keyes Tom Ake Cristina Oliveira Dave Sahnow Brittany Shaw Alessandra Aloisi Rosa Diaz

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SIRTF-IRS software

SIRTF-IRS software. Fred Lahuis Leiden 18 Nov 2002. (presented by Ewine van Dishoeck and Adwin Boogert, c2d meeting Dec. 11, 2002). IRS Instrument. Low resolution R~60-120 imaging spectrograph 1 st and 2 nd order SL Si:As 5.3 - 14.2 micron LL Si:Sb 14.2 - 20.0 micron.

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The Status of COS Flat Fields

The Status of COS Flat Fields. Tom Ake TIPS 21 August 2008. Status of COS Flat Fields. Material covered today COS Description and Signal-to-Noise Requirements NUV Ground Calibration and SMOV4 Plans FUV Detector Characteristics FUV Ground Calibration and SMOV4 Plans

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A noiseless 512 x 512 detector for AO with kHz frame rates

A noiseless 512 x 512 detector for AO with kHz frame rates. John Vallerga, Jason McPhate, Anton Tremsin and Oswald Siegmund Space Sciences Laboratory, University of California, Berkeley Bettina Mikulec and Allan Clark University of Geneva. Future WFS Requirements*. High (~80%) optical QE

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Finderscopes Part I Optical Systems: Refractors and Eyepieces

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Introduction to Spitzer and some applications

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ACS WFC Flat-Field Changes

ACS WFC Flat-Field Changes. Temperature change from -77 C to -81 C on July 4, 2006 leads to expected changes for flat fields. Are L-flat measures stable before ?T, and is there a change after cooldown? (Yes/yes)

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AEOS Telescope + Image-Slicer/ Spectrograph

AEOS Telescope + Image-Slicer/ Spectrograph. Data Reduction and Results for June 8, 2006. AEOS + Image-Slicer Spectrograph: Observing parameters. 3.7-meter telescope with adaptive optics Scale: 0.5 arc-seconds per fiber 1-minute exposures Twilight not significant

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The Photometric Performance and Calibration of WFC3

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Photon Transfer Method 1.

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 exposures are required to remove the contribution of the PRNU and of small imperfections in the flat fields caused by uneven illumination.

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Testing and characterizing the CCDs of the OmegaCam wide-angle camera

F. Christen 2 , C. Cavadore 1 , B. Gaillard, O. Iwert 1 , K. Kuijken 2 , D. Baade 1 , S. Darbon 1. 1 : European Southern Observatory 2 : Kapteyn Instituut (Groningen).

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Background photo courtesy of NOAO. Taken with LBNL p-channel CCD with extended red sensitivity.

Pixel Area Variation in CCDs and Implications for Precision Photometry Roger Smith & Gustavo Rahmer (Caltech). Pixels change size ; centers may be displaced. %. %. Guider. 0.26%. 36 NIR Detectors 3 bandpasses. Spectrograph slit. 560mm diameter. 36 CCDs, 6 bandpasses. QE.

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