Focalpoint newton
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The four individual quadrants each having three pn-CCD subunits with a format 200 x 64 pixels are operated in parallel. In case of the pn camera, the spatially uniform detector quality over the entire FOV is realized by the monolithic fabrication of twelve 3 x 1 cm pn-CCDs on a single wafer. The CCDs of the pn camera: The picture shows the twelve chips mounted and the connections to the integrated preamplifiers. This means that the 300 micron gaps between the outer CCDs in one camera are covered by their opposite numbers in the other camera. The two MOS cameras are arranged on the spacecraft focal plane bulkhead so that the CCDs are orthogonal.
#Focalpoint newton full#
The full CCD image can be read out using either node, or read out using both nodes simultaneously, to halve the readout time. The readout register is split into two sections, ending in a readout node. The imaging section has 600 x 600, 40 micron square, pixels one pixel covers 1.1 x 1.1 arcsec on the FOV 15 pixels cover the mirror PSF half energy width of 15 arcsec. The imaging area is ~2.5 x 2.5 cm, so that a mosaic of seven covers the focal plane 62 mm in diameter, equivalent to 28.4 arcmin. The CCDs are buttable with a dead region of less than 300 microns wide on three sides to minimise the dead space, adjacent CCDs are stepped by about 1 mm to overlap by 300 microns. The central CCD is at the focal point on the optical axis of the telescope while the outer six are stepped towards the mirror by 4.5 mm to follow approximately the focal plane curvature, and improve the focus for off-axis sources. There are seven EEV type 22 front-illuminated CCDs in the focal plane of each MOS camera. The CCDs of one of the MOS cameras in the cryostat. In addition, the ERM provides detailed monitoring of the space radiative environment constituting a reference for the development of detectors to be used in futures missions. The main function of the ERM is the detection of the radiative belts and solar flares in order to supply particle environment information for the correct operation of the EPIC camera. This does not only hold for the geometry of the CCD arrays and the instrument design but also for other properties, like e.g., their readout times.Īnother experiment on board of XMM-Newton is the EPIC Radiation Monitor (ERM). The two types of EPIC, however, differ in some major aspects. tables with one entry line per received event, listing (among others) attributes of the events such as the position at which they were registered, their arrival time and their energies. The EPIC cameras offer the possibility to perform extremely sensitive imaging observations over the telescope's field of view (FOV) of 30 arcmin and in the energy range from 0.15 to 15 keV with moderate spectral (E/Delta E ~ 20-50) and angular resolution (PSF, 6 arcsec FWHM).Īll EPIC CCDs operate in photon counting mode with a fixed, mode dependent frame read-out frequency, producing event lists, i.e. The third X-ray telescope has an unobstructed beam the EPIC instrument at the focus of this telescope uses pn CCDs and is referred to as the pn camera. The gratings divert about half of the telescope incident flux towards the RGS detectors such that (taking structural obscuration into account) about 44% of the original incoming flux reaches the MOS cameras.
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They are installed behind the X-ray telescopes that are equipped with the gratings of the Reflection Grating Spectrometers (RGS). Two of the cameras are MOS (Metal Oxide Semi-conductor) CCD arrays (referred to as the MOS cameras). The XMM-Newton spacecraft is carrying a set of three X-ray CCD cameras, comprising the European Photon Imaging Camera (EPIC). 2001, A&A 365, L27.Īdditional information can be obtained from the XMM-Newton Users' Handbook.
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This description is mostly based on the information contained in the papers The European Photon Imaging Camera (EPIC) onboard XMM-Newton