The European Space Agency's Planck satellite, launched on 14 May 2009, is the third-generation space experiment in the field of cosmic microwave background (CMB) research. It will image the anisotropies of the CMB over the whole sky, with unprecedented sensitivity ( ΔT T ∼ 2 × 10 −6 ) and angular resolution (∼5 arcmin). Planck will provide a major source of information relevant to many fundamental cosmological problems and will test current theories of the early evolution of the Universe and the origin of structure. It will also address a wide range of areas of astrophysical research related to the Milky Way as well as external galaxies and clusters of galaxies. The ability of Planck to measure polarization across a wide frequency range (30−350 GHz), with high precision and accuracy, and over the whole sky, will provide unique insight, not only into specific cosmological questions, but also into the properties of the interstellar medium. This paper is part of a series which describes the technical capabilities of the Planck scientific payload. It is based on the knowledge gathered during the on-ground calibration campaigns of the major subsystems, principally its telescope and its two scientific instruments, and of tests at fully integrated satellite level. It represents the best estimate before launch of the technical performance that the satellite and its payload will achieve in flight. In this paper, we summarise the main elements of the payload performance, which is described in detail in the accompanying papers. In addition, we describe the satellite performance elements which are most relevant for science, and provide an overview of the plans for scientific operations and data analysis.

The high throughput X-ray spectroscopy mission XMM is the second cornerstone project in the European Space Agency (ESA) long-term program for space science. This observatory has at its heart three large X-ray telescopes, which will provide a large collecting area (1450 cm each at 1.5 keV and 600 cm2 each at 8.0 keV) with a spatial resolution around 15 arcesec. Five Flight models (including the two spare ones) of the XMM X-ray telescope have been delivered to ESA in 1998. They show optical performance. which is far better than the specifications, especially in terms of optical and X-ray stray light reduction. The low level of X-ray stray light will be an important benefit for the observation of the extended faint sources such as super nova . remnants or clusters of active galaxies. This reduction of X-ray stray light is due, in particular. to the implementation of a very complex and accurate X-ray baffle mounted at the entrance of the telescope.In this paper, we present first the need, the design. the , manufacturing and the integration of the X-ray baffle. Then, we concentrate on the verification of the performance of the baffle at ; the Centre Spatial de Liege. Finally, we will present the excellent results obtained with these baffles.1.

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The X-ray Multi-Minor Mission is one of the four "Cornerstone" projects in the ESA Long-Term Program for Space Science. Presently, five XMM Minor Modules (MM) (including one Qualification Model) have been tested in the FOCALX facility of CSL. The MMs are illuminated by a vertical EUV (58.4 nm) collimated beam allowing to get the optical performance in an effective flight configuration. To fully analyse the MM characteristics, reflectivity measurements are performed in X-ray thanks to a pencil beam. The reflectivity measurements of single shell are performed at Al, Au, Cu, Mo lines between 1 .5and 1 3 keV. This information is used to evaluate the effective area in X-rays. Wing scattering measurements are performed and show a good correlation with the Power Spectral Density measured with a PROMAP microscope interferometer during minor shell manufacturing. This paper deals first with the presentation and comparison of the results achieved on the five MMs. In a second step the results of complementary tests, performed to cross check the data and to get a better understanding of the MM behaviour, are discussed.

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In the frame of the XMM project, several test campaigns are accomplished to qualify the optical elements of the mission. The tests described in this paper are performed on a XMM Flight Model Mirror Module (FM MM) added with a Reflection Grating Assembly (RGA). The Mirror Module contains 58 X-ray optical quality shells, an X-ray baffle (XRB) to reduce the straylight. This complete XMM Flight Model Mirror Assembly (MA) is tested in a vertical configuration at CSL, in a full aperture or partial EUV collimated beam illumination, and with an X-ray pencil beam. One of the advantages of the EUV collimated beam is to verify the correct position of the RGA when integrated in flight configuration on the Mirror Module structure. This is not possible in X-ray with a fmite source distance. The partial EUV illumination is performed to verify the correct integration of the RGA grating stacks. The pencil beam allows to make an accurate metrology of the XRB position, and to verify the positions of the 0, 1 and 2 diffraction order foci.In this paper, the tested module is first exposed, and the approach to qualify the instrument is described. The analysis of the results achieved over the different test configurations is presented. The impact of the environmental tests on the Reflection Grating Box is also diagnosed.

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A BST RACT Ihe high throughput X-ray specuoscopv mission XMNI is the second cornerstone project in the European Space Agency (ESA) long-term program for space science. This observatory has at its heart three large X-ray telescopes, which iI1 provide a large collecting area (1430 cm each at 1.5 keV and 600 cm each at 8.0 kcV) with a spatial resolution better than 15 arcsec. ultra-thin mirror measured in the energy range 1.5-8.0 keV. This graph is also indicates the 2