Event Pileup in Charge-coupled Devices

By John E. Davis. 2001

321 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Radiation

View Paper: https://www.semanticscholar.org/paper/beea8d56874e26dc2b3fe420992f006e6c133e83

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Citations in the corpus

The Ultraluminous X-Ray Source Population from the Chandra Archive of Galaxies (2004, methodology): “Sources with detected count rates in excess of 0.1 c frame−1 were treated for effects of pileup following the procedures described in Davis (2002) and using the event pileup model of Davis (2001).”
The Chandra High‐Energy Transmission Grating: Design, Fabrication, Ground Calibration, and 5 Years in Flight (2005, methodology): “The HETGS effective area or ARF (Davis 2001a) for a given grating set or part, indicating HEG or MEG, and diffraction order m may be expressed in simplified form as: AP,m(λ) = MP(λ) gP,m(λ) Q(λ, ~σ) (8) where λ denotes the dependence on photon wavelength (or energy) and the three contributing terms ”
Constraining the mass and radius of neutron stars in globular clusters (2017, background): “Pileup occurs at relatively high count rates, when the energy deposited from two photons is incorrectly recorded as coming from one photon (Davis 2001); some combined photons are interpreted as signals from cosmic rays, and rejected.”
Magnetic Field Strengths in the Hot Spots and Lobes of Three Powerful Fanaroff-Riley Type II Radio Sources (2002, methodology): “Following Davis (2001) we fix the grade correction parameterḡ0 to 1 and allow only the grade morphing parameter to vary.3 We find the best fit (Table 8) to haveα = 0.75 ± 0.06 (since the slope and normalization are strongly correlated in this model, the error quoted is1σ for two interesting…”
Radiative efficiency, variability and Bondi accretion on to massive black holes: the transition from radio AGN to quasars in brightest cluster galaxies (2012, background): “Pile up occurs whenever two or more photons, arriving in the same detector region and within a single ACIS frame int- gration time, are detected as a single event (Davis 2001).”
High-Resolution Chandra HETGS and Rossi X-Ray Timing Explorer Observations of GRS 1915+105: A Hot Disk Atmosphere and Cold Gas Enriched in Iron and Silicon (2001, methodology): “We extract a separate set of HEG and MEG Ðrst-order spectra to be used with the HETGS pile-up model as implemented in ISIS8 (see Davis 2001 ; Houck & DeNicola 2000).”
A COMPLETE SAMPLE OF ULTRALUMINOUS X-RAY SOURCE HOST GALAXIES (2011, methodology): “The effects of pile-up of sources with detected count rates in excess of 0.1 counts frame−1 in Chandra/ACIS observations were treated following the procedures described by Davis (2001) using the multiplicative XSPEC model pileup.”
Cooling neutron star in the Cassiopeia A supernova remnant: evidence for superfluidity in the core (2010, result): “We exclude the subarray observation of Cas A (Pavlov & Luna 2009), since the pileup properties (Davis 2001) of this spectrum differ from the others, and those observations in which the Cas A NS dithered over bad pixels (most of the 2004 observations).”
MEASUREMENT OF THE RADIUS OF NEUTRON STARS WITH HIGH SIGNAL-TO-NOISE QUIESCENT LOW-MASS X-RAY BINARIES IN GLOBULAR CLUSTERS (2012, methodology): “For completeness, and to confirm this observation, a spectral analysis combining X7 to the other five qLMXBs of this work is performed in XSPEC in order to determine RNS. Note that the MCMC approach is not used and is not necessary here since this additional analysis is simply a consistency check to”
A new bound on axion-like particles (2017, background): “Pile-up occurs when multiple photons arrive in the same detector region within the same frame integration time and are therefore detected as a single photon event [33].”
Chandra Orion Ultradeep Project: Observations and Source Lists (2004, methodology): “While statistical reconstruction treatments of ACIS pile-up have been developed (Davis 2001; Kang et al. 2003), the approach adopted here is to discard events at the core of the point spread function, which are both spatially and spectrally distorted, and to use only ordinary, pile-up-free events…”
A Hydrogen Atmosphere Spectral Model Applied to the Neutron Star X7 in the Globular Cluster 47 Tucanae (2005, methodology): “Pileup occurs when two X-ray photons, arriving at the detector during one frame time, are erroneously identified as a single photon with the sum of the two photon energies, or else discarded (see Davis 2001).”
DIRECT OBSERVATION OF THE COOLING OF THE CASSIOPEIA A NEUTRON STAR (2010, methodology): “…similar spectral fit to that in Ho & Heinke (2009), a model containing photoelectric absorption (with abundances from Wilms et al. 2000), an unmagnetized carbon NS atmosphere, and scattering by interstellar dust (Predehl et al. 2003), all convolved with the Davis pileup model (Davis 2001) in XSPEC.”
THE CHANDRA SOURCE CATALOG (2009, methodology): “Instrumental response functions (Davis 2001a) define the mappings between physical (source) space and detector space.”
The SRG/eROSITA all-sky survey (2024, unknown): “This is mainly due to the pile-up effect (Ballet 1999; Davis 2001; Tamba et al. 2022), which occurs if two or more photons hit the same CCD pixel in the same (50 ms) read-out cycle and the A34, page 8 of 38 sum of the charges created will enter the event analyser (“energy pile-up”).”