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    A Physical Model-based Correction for Charge Traps in the Hubble Space Telescope’s Wide Field Camera 3 Near-IR Detector and Its Applications to Transiting Exoplanets and Brown Dwarfs

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    Zhou_2017_AJ_153_243.pdf
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    FInal Published Version
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    Author
    Zhou, Yifan cc
    Apai, Dániel cc
    Lew, Ben W. P. cc
    Schneider, Glenn cc
    Affiliation
    Univ Arizona, Dept Astron, Steward Observ
    Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab
    Issue Date
    2017-05-04
    Keywords
    brown dwarfs
    instrumentation: detectors
    planets and satellites: atmospheres
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    A Physical Model-based Correction for Charge Traps in the Hubble Space Telescope’s Wide Field Camera 3 Near-IR Detector and Its Applications to Transiting Exoplanets and Brown Dwarfs 2017, 153 (6):243 The Astronomical Journal
    Journal
    The Astronomical Journal
    Rights
    © 2017. The American Astronomical Society. All rights reserved.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    The Hubble Space Telescope Wide Field Camera 3 (WFC3) near-IR channel is extensively used in time-resolved observations, especially for transiting exoplanet spectroscopy as well as. brown dwarf and directly imaged exoplanet rotational phase mapping. The ramp effect is the dominant source of systematics in the WFC3 for time-resolved observations, which limits its photometric precision. Current mitigation strategies are based on empirical fits and require additional orbits to help the telescope reach a thermal equilibrium. We show that the ramp-effect profiles can be explained and corrected with high fidelity using charge trapping theories. We also present a model for this process that can be used to predict and to correct charge trap systematics. Our model is based on a very small number of parameters that are intrinsic to the detector. We find that these parameters are very stable between the different data sets, and we provide best-fit values. Our model is tested with more than 120 orbits (similar to 40 visits) of WFC3 observations. and is proved to be able to provide near photon noise limited corrections for observations made with both staring and scanning modes of transiting exoplanets as well as for starting-mode observations of brown dwarfs. After our model correction, the light curve of the first orbit in each visit has the same photometric precision as subsequent orbits, so data from the first orbit no longer need. to. be discarded. Near-IR arrays with the same physical characteristics (e.g., JWST/NIRCam) may also benefit from the extension of this model if similar systematic profiles are observed.
    ISSN
    1538-3881
    DOI
    10.3847/1538-3881/aa6481
    Version
    Final published version
    Sponsors
    NASA Earth and Space Science Fellowship Program [NNX16AP54H]; Technology Research Initiative Fund (TRIF) Imaging Fellowship, University of Arizona; National Aeronautics and Space Administration [NNX15AD94G]; NASA through a grant from Space Telescope Science Institute [12314, 13418, 14241]; NASA [NAS5-26555]
    Additional Links
    http://stacks.iop.org/1538-3881/153/i=6/a=243?key=crossref.d8632f701456202d40ec5de454a41fff
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-3881/aa6481
    Scopus Count
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    UA Faculty Publications

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