![]() ![]() In theĭispersion direction, the aperture of RGS covers the entire FOV of the Largely determined by the imaging properties of the mirror. The CCDs (5 ), and the spatial resolution in this direction is In the cross-dispersionĭirection, the size of the field of view is determined by the width of In the dispersion direction at 5, 15 and 38 Å in first and secondīoth spectrometers cover the same field of view, with the dispersionĭirection along the spacecraft -Z axis. Size of one bin projected onto the sky is about 2”.5 in theĬross-dispersion direction, and roughly 3, 5 and 7” and 4, 6, and 9” In second order for wavelengths of 5, 15 and 38 Å, respectively. In the dispersion direction one bin corresponds toĪbout 7, 10, and 14 mÅ in first order, and about 4, 6, and 10 mÅ (81 ), which is sufficient to fully sample the RGS line spreadįunction (LSF). Performed in the default spectroscopy mode, leading to a bin size of During readout, pixel on-chip binning (OCB) is (27 ) pixels, half (1024x384) exposed to the sky and half usedĪs a storage area. Side in order to suppress optical and UV light. Maximise the soft energy response and aluminium-coated on the exposed ![]() The RGS MOS chips are back-illuminated in order to The EPIC MOS cameras, which are located along the dispersion direction The RFCs consist of linear arrays of 9 MOS CCD chips similar to those in Instrument is a slowly varying function of dispersion angle, and isĮqual to approximately 8.3 and 12.7 mm Å at 15 Å in first The grating plates in the RGAs have mean grooveĭensities of about 645.6 lines mm. Each RGA intercepts about 58% of the total light focused by the The two X-ray telescopes with EPIC MOS cameras at their primaryįocus. The RGAs are mounted in the light path of These consist of Reflection Grating Assemblies (RGAs) and RGS FocalĬameras (RFCs), see Fig. Two of the three XMM-Newton X-ray telescopes are equipped with RGS units. Physical conditions and chemical composition of the emitting material. Ni thus offering a large number of diagnostic tools to investigate the Mg and Si and the L-shell transitions of heavier elements like Fe and Transitions and He-like triplets of light elements, such as C, N, O, Ne, Particularly high density of X-ray emission lines including the K-shell The energy range covered by the RGS has a Spectral resolution (from 100 to 500, FWHM) X-ray spectroscopy in theĮnergy range 0.33-2.5 keV or 5-38 Å 4. 4 REFLECTION GRATING SPECTROMETER (RGS)Īmong the science instruments of XMM-Newton, the RGS is best suited for high Next: 3.4.1 Diffraction Geometry Up: 3 XMM-Newton - a concise overview Previous: 3.3.12.3 Count rate conversion from other X-ray satellite missionsģ. ![]()
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