Max Mutchler

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We have studied the charge trapping problem in the WFPC2 CCDs by examining residual images in dark calibration exposures taken at various intervals after non-saturated planetary exposures. Charge is trapped during read-out of the planet image, followed by a slow release of charge during the dark frame, hence resulting in a residual image. Our results(More)
  • Michael A Dopita, William P Blair, Knox S Long, Max Mutchler, Bradley C Whitmore, Kip D Kuntz +14 others
  • 2010
We present Wide Field Camera 3 images taken with the Hubble Space Telescope within a single field in the southern grand design star-forming galaxy M83. Based on their size, morphology and photometry in continuum-subtracted Hα, [S II ], Hβ, [O III ] and [O II ] filters, we have identified 60 supernova remnant candidates, as well as a handful of young(More)
We present the results of over two years of inflight charge transfer efficiency (CTE) monitoring of the CCDs in the Advanced Camera for Surveys (ACS), based on two internal tests: Extended Pixel Edge Response (EPER), and First Pixel Response (FPR). In general, we find that CTE losses are worst at the lowest signal levels, and at each signal level, CTE(More)
The goal of SMOV proposal 7022 was to verify that there was no change in basic WFPC2 instrument health and internal calibrations. A variety of internal exposures were obtained in order to provide a monitor of the integrity of the CCD camera electronics in both bays (gain 7 and gain 15), a test for quantum efficiency in the CCDs, and an internal check on the(More)
  • Max Mutchler, Marco Sirianni, Doug Van Orsow, Adam Riess
  • 2004
We describe the routine production of the " superbias " and " superdark " reference files that are used to calibrate ACS science data in the pipeline (CALACS). These files are identified by the BIASFILE and DARKFILE keywords in the header of every ACS science image. We describe the primary bias and dark features contained in these files, and provide some(More)
We provide some background on pointing ACS, and present the dither and mosaic patterns that will be provided as a convenience for HST Cycle 11 Phase II proposal writers. This report supersedes any previous documents which describe specific ACS dither and mosaic patterns-namely, ACS Instrument Science Report 98-02 by Stiavelli, and the engineering versions(More)
Most inner main-belt asteroids are primitive rock and metal bodies in orbit about the Sun between Mars and Jupiter. Disruption, through high-velocity collisions or rotational spin-up, is believed to be the primary mechanism for the production and destruction of small asteroids and a contributor to dust in the Sun's zodiacal cloud, while analogous collisions(More)
(a) B-band (F435W) mosaic of M51 Abstract In January 2005, the Hubble Heritage Team obtained a large 4-color (B, V, I, and Hα) mosaic image of the Whirlpool Galaxy NGC 5194 (M51), and its companion NGC 5195, with the Advanced Camera for Surveys (ACS) onboard the Hubble Space Telescope (HST). The resulting color composite image was released to the community(More)
The Advanced Camera for Surveys (ACS), installed in the Hubble Space Telescope (HST) in March 2002, comprises three cameras: the Wide Field Camera (WFC), designed for deep near-IR survey imaging programs; the High Resolution Camera (HRC), a high angular resolution imager which fully samples the HST full spread function (PSF) in the visible; and the Solar(More)
The number of hot pixels on the Wide Field Channel of the Advanced Camera for Surveys will increase over the next few years as radiation damage accrues. A considerable reduction in dark rate and hence hot pixel counts should result from lowering the detector temperature. When the Aft Shroud Cooling System is installed in Servicing Mission 4, temperatures as(More)