The European Photon Imaging Camera on XMM-Newton: The pn-CCD camera

By L. Strüder, U. Briel, K. Dennerl, R. Hartmann, E. Kendziorra, N. Meidinger, E. Pfeffermann, C. Reppin, B. Aschenbach, W. Bornemann and 48 more. 2001

2,268 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/2b1d6df4659ff8dd7a1c04a28e903b187c9fab4d

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Citations in the corpus

The mercury imaging X-ray spectrometer (MIXS) on BepiColombo (2010, background): “668 669 We have estimated the MIXS background at Mercury by scaling that experienced by the 670 XMM Newton X-ray observatory’s EPIC X-ray camera’s pn-CCDs (Strüder et al., 2001) 671 which are in a highly elliptical orbit around the Earth.”
OBSCURATION-DEPENDENT EVOLUTION OF ACTIVE GALACTIC NUCLEI (2015, methodology): “The first step is to produce event files from the Observation Data Files (ODF) using the epchain and emchain tasks of sas for the EPIC (European Photon Imaging Camera; Strüder et al. 2001; Turner et al. 2001) PN and MOS detectors respectively.”
Evidence of a high-velocity ionized outflow in a second narrow-line quasar PG 0844+349 (2003, methodology): “We use the full XMM–Newton X-ray data, including the EPIC pn camera (Strüder et al. 2001), C© 2003 RAS Downloaded from https://academic.oup.com/mnras/article-abstract/346/4/1025/1062121 by guest on 28 July 2018 which has the best sensitivity of any instrument flown to date in the ∼7–10 keV…”
The XMM-Newton Wide-Field Survey in the COSMOS Field: Statistical Properties of Clusters of Galaxies (2006, methodology): “In this paper we use the data collected by the European Photon Imaging Cameras (EPIC): the pn-CCD camera (Strüder et al. 2001) and the MOS-CCD cameras (Turner et al. 2001).”
Cosmic X-ray surveys of distant active galaxies (2015, methodology): “…rising background levels and dropping 2 Note that many X-ray detectors, including those used on Chandra and XMM-Newton to perform cosmic surveys, simultaneously obtain imaging, spectral, and timing data for the collected photons (e.g., Strüder et al 2001; Turner et al 2001; Garmire et al 2003).”
XMM–Newton observations of the brightest ultraluminous X-ray sources (2006, methodology): “In this work we have utilised data from the EPIC cameras on boardXMM-Newton (Turner et al. 2001; Strüder et al. 2001).”
The X-Ray Observatory Suzaku (2007, positive): “The X-ray Imaging Spectrometer (XIS) employs X-ray sensitive silicon charge-coupled devices (CCD), which are operated in a photon-counting mode, similar to that used in S4 K. Mitsuda et al. [Vol. 59, the ASCA SIS (Burke et al. 1994; Yamashita et al. 1997), Chandra ACIS (Garmire et al. 1992; Bautz et”
An XMM–Newton survey of broad iron lines in Seyfert galaxies (2007, methodology): “The observations described here were taken with the EPIC-pn CCD camera (Struder et al. 2001) on board XMM-Newton.”
The first XMM-Newton slew survey catalogue: XMMSL1 (2008, methodology): “…has been computed by adding the area contained in all of the images used in source searching with an exposure time greater than 1 s. b Flux limit, units of 10−11 ergs s−1 cm−2. long streaks in the MOS cameras but are well formed in the fast observing modes of the pn camera (Strüder et al. 2001).”
Highlights from the XMM-Newton Extended Survey of the Taurus Molecular Cloud (XEST) (2006, methodology): “The detection statistics of our EPIC (Strüder et al. 2001; Turner et al. 2001) X-ray survey is summarized in Table 1 separately for theXMM-Newton data, and for the combined XMM-Newton andChandra fields (in parentheses).”
The Compact, Conical, Accretion-Disk Warm Absorber of the Seyfert 1 Galaxy NGC 4051 and Its Implications for IGM-Galaxy Feedback Processes (2007, methodology): “The task epchain was used to obtain calibrated event lists for the EPIC-PN camera (Struder et al. 2001) which has a better calibration below 0.8 keV than EPIC-MOS3.”
An absorption origin for the X-ray spectral variability of MCG-6-30-15 (2008, methodology): “In this analysis we use data from the CCD detector (Strüder et al., 2001) in the energy range 0.4− 9.8 keV.”
The SRG/eROSITA all-sky survey (2024, positive): “The additional presence of a frame-store area in the CCD reduces substantially the amount of so-called out-of-time events, which are recorded during the CCD read-out, a significant improvement with respect to the EPIC-pn camera on XMM-Newton .”
A global look at X-ray time lags in seyfert galaxies (2016, methodology): “For this analysis, we use the data from the XMM-Newton EPIC-pn camera because of its higher effective area and fast readout (Strüder et al. 2001; Jansen et al. 2001).”
A Massive X-Ray Outflow from the Quasar PDS 456 (2003, methodology): “THE X-RAY OBSERVATIONS PDS 456 was observed byXMM-Newton on 2001 February 26 with a duration of 40 ks. Data were taken with the EPICpn detector (Struder et al. 2001) in full window mode and with the EPIC-MOS detector (Turner et al. 2001) in large window mode.”
BAT AGN Spectroscopic Survey. V. X-Ray Properties of the Swift/BAT 70-month AGN Catalog (2017, positive): “The source is instead more likely associated to the X-ray bright Seyfert 2 IGR J02164+5126/2MASSJ02162672+5125251, which is clearly detected in the 10.0 ks XMM-Newton EPIC/PN observation (see also Masetti et al. 2009).”