The Near-Infrared Spectrometer and Photometer (NISP) is one of the key instruments on-board the Euclid satellite, one of the major mission of ESA’s 2015 Cosmic Vision program. The instrument is located at the payload of the Euclid satellite, and it is initially planned to be operated at ∼135 K, except the detectors that are cooled to about 90 K. The NISP instrument will perform spectroscopic observations and photometric imaging in 3 near-infrared bands (Y, J, H) covering a wavelength range from 0.92 μm – 2.0 μm over a field of view (FoV) of ∼0.5 deg2.
The Near Infrared Spectro-Photometer Optical assembly (NIOA) of EUCLID satellite requires high precision large lens holders with different lens materials, shapes and diameters. The aspherical lenses are glued into their separate CTE matched lens holder. The gluing of the lenses in their holder with 2K epoxy is selected as bonding process to minimize the stress in the lenses to achieve the required surface form error (SFE) performance (32nm) and lens position stability (±10μm) due to glue shrinkage. Adhesive shrinkage stress occurs during the glue curing at room temperature and operation in cryogenic temperatures, which might overstress the lens, cause performance loss, lens breakage or failure of the gluing interface.
The selection of the suitable glue and required bonding parameters, design and qualification of the gluing interface, development and verification of the gluing process was a great challenge because of the low TRL and heritage of the bonding technology. The different material combinations (CaF2 to SS316L, LF5G15 and S-FTM16 to Titanium, SUPRASIL3001 to Invar M93), large diameter (168mm) and thin edge of the lenses, cryogenic nonoperational temperature (100K) and high performance accuracy of the lenses were the main design driver of the development. The different coefficients of thermal expansion (CTE) between lens and lens holder produce large local mechanical stress. As hygroscopic crystal calcium fluoride (CaF2) is very sensitive to moisture therefore an additional surface treatment of the gluing area is necessary.
Extensive tests e.g glue handling and single lap shear tests are performed to select the suitable adhesive. Interface connection tests are performed to verify the feasibility of selected design (double pad design), injection channel, the roughness and treatment of the metal and lens interfaces, glue thickness, glue pad diameter and the gluing process. CTE and dynamic measurements of the glue, thermal cycling, damp- heat, connection shear and tension tests with all material combinations at RT and 100K are carried out to qualify the gluing interface. The gluing interface of the glued lenses in their mounts is also qualified with thermal cycling, 3D coordinate measurements before and after environmental tests, Polarimetry and vibration test of the lens assemblies.
A multi-function double pad gluing tool and lens mounting tool is designed, manufactured and verified to meet the lens positioning and alignment performance of the lens in the holder which provides the possibility to glue lenses, filters, mirrors with different diameters, shapes and thickness with ±10μm accuracy in plane, out of plane and ±10 arcsec in tip/tilt with respect to the lens holder interface. The paper presents the glue interface qualification results, the qualification/verification methods, the developed ground support equipment and the gluing process of the EUCLID high precision large cryogenic lens mounts. Test results achieved in the test campaign demonstrate the suitability of the selected adhesive, glue pad design, interface parameters and the processes for the precise gluing of the lenses in lens holders for all lenses. The qualification models of the NIOA are successfully glued and qualified. The developed process can also be used for other glass materials e.g. MaF2 and optical black coated metallic surfaces.
eROSITA (extended ROentgen Survey with an Imaging Telescope Array) is the core instrument on the Russian
Spektrum-Roentgen-Gamma (SRG) mission which is scheduled for launch in 2013. eROSITA will perform an all-sky
survey lasting four years, followed by a phase of three years for pointed observations. eROSITA consists of seven
identical Mirror Modules, each equipped with 54 Wolter-I shells with an outer diameter of 360 mm. This would provide
an effective area of ~1500 cm2 at 1.5 keV and an on axis PSF HEW of 15 arcsec resulting in an effective angular
resolution of 28 arcsec averaged over the field of view. In the focus of each mirror module, a fast frame-store pn-CCD
provides a field of view of 1°in diameter. In this paper we report on the instrument development and its status only.
The mirrors of the International X-ray Observatory (IXO) consist of a large number of high quality segments delivering
a spatial resolution better than 5 arcsec. A study concerning the slumping of thin glass foils for the IXO mirrors is under
development in Europe, funded by ESA and led by the Brera Observatory. We are investigating two approaches, the
"Direct" and "Indirect" slumping technologies, being respectively based on the use of convex and concave moulds. In
the first case during the thermal cycle the optical surface of the glass is in direct contact with the mould surface, while in
the second case it is the rear side of the foil which touches the master. Both approaches present pros and cons and aim of
this study is also to make an assessment of both processes and to perform a trade-off between the two. The thin plates are
made of D263glass produced by Schott. Each plate is 0.4 mm thick, with a reflecting area of 200 mm x 200 mm; the
mould are made of Fused Silica. After the thermal cycle the slumped MPs are characterized to define their optical
quality and microroughness. The adopted integration process foresees the bonding of the slumped foils to a rigid
backplane by means of reinforcing ribs. During the bonding process the plates are constrained to stay in close contact to
the surface of the master (i.e. the same mould used for the hot slumping process) by the application of a vacuum pump
suction. In this way spring-back deformations and low frequency errors still present on the foil profile after slumping can
be corrected. In this paper we present the preliminary results concerning achieved during the first part of the project.
Future X-ray observatory missions, such as IXO or Gen-X, require grazing incidence optics of large collecting area in
combination with a very good angular resolution. Wolter type I X-ray telescopes made of slumped glass segments could
be a possible alternative to silicon pore optics. To achieve these requirements we develop slumping methods for high
accuracy segments by experimental means. In particular, we follow the approach of indirect slumping and aim to
produce parabola and hyperbola in one piece. In order to avoid internal stress in the glass segments the thermal
expansion coefficient of the glass should closely match the thermal expansion of the mould material. Currently we focus
on a combination of the alloy KOVAR for the mould and D263 for the glass; additionally a platinum-coated silica as
mould material is studied. We investigate the behaviour of both materials during slumping in order to obtain the ideal
environment for the slumping process. Additionally we report on the design of different metrology methods to measure
the figure and thickness variations of the glass segments in visual light, e.g. interference, and on bearings used for shape
measurements and integration.
eROSITA (extended ROentgen Survey with an Imaging Telescope Array) is the core instrument on the Russian Spektrum-Roentgen-Gamma (SRG) mission which is scheduled for launch in late 2012. eROSITA is fully approved and funded by the German Space Agency DLR and the Max-Planck-Society. The instrument development is in phase C/D since fall 2009. The design driving science is the detection 100.000 Clusters of Galaxies up to redshift z ~1.3 in order to study the large scale structure in the Universe and test cosmological models, especially Dark Energy. This will be accomplished by an all-sky survey lasting for four years plus a phase of pointed observations. eROSITA consists of seven Wolter-I telescope modules, each equipped with 54 Wolter-I shells having an outer diameter of 360 mm. This would provide an effective area of ~1500 cm2 at 1.5 keV and an on axis PSF HEW of 15 arcsec resulting in an effective angular resolution of 28 - 30 arcsec, averaged over the field of view. In the focus of each mirror module, a fast frame-store pn-CCD provides a field of view of 1° in diameter.
Wolter type I X-ray telescopes made of slumped glass could be a light-weight alternative to nickel replica
optics. We are following the goal to develop the slumping methods for high accuracy glass segments with an
angular resolution of a few arcseconds by experimental means.
The development of segmented glass optics falls into three distinct areas: slumping process, metrology and
optics assembly. We report on our results in studying the sequence of the slumping process. By observing the
effects of different parameters we got a fine grasp on the process itself. The design of different metrology
methods to measure the figure of the glass segments both in visual and X-ray wavelengths were under way.
Integrating the segments into a structure became a main part in our development. We report on first results.
X-ray mirrors made of slumped glass could be a light-weight solution for large segmented
X-ray telescopes. Our goal is the development of a slumping process for high accuracy
glass segments with an angular resolution of a few arcseconds. In our studies we try to
understand the influence of the process by experimental means. We have recently built a
new experimental set-up which allows us to study the sequence of the slumping methods.
We report on our laboratory experiments and on the development of metrology methods to
measure the figure of the glass segments.
In our ongoing studies of high precision glass slumping we have successfully formed the first Wolter-I X-ray mirror
segments with parabola and hyperbola in one piece. It could be demonstrated that the excellent surface roughness of the
0.55 mm thick display glass chosen is conserved during the slumping process. The influence of several parameters of the
process, such as maximum temperature, heating and cooling rates etc. have to be measured and controlled with adequate
metrology. Currently, we are optimizing the process to reduce the figure errors down to 1 micrometer what will be the
starting point for further, final figure error corrections. We point out that metrology plays an important role in achieving a
high precision optics, i.e. an angular resolution of a few arcsec. In this paper we report on the results of our studies and
discuss them in the context of the requirements for future X-ray telescopes with large apertures.
Light sources, focusing elements and detectors working at wavelengths from 5nm to 40nm, so called EUV, are of increasing interest for the semiconductor industry, especially for lithography. A metrology has been developed to characterize modified nested Wolter grazing incidence optics which act as the condenser optic. It consists of a monochromatic EUV source and a MCP detector. The EUV source is designed to emit radiation at a wavelength of 13.5nm into a solid angle of up to 1.8sr, which is realized by a silicon-zirconium target used in transmission. Detector and EUV source have been calibrated. In particular, the angular dependences of the source radiation and the detector efficiency have been investigated. The calibrated metrology could be used for measuring the imaging properties of modified nested Wolter optics revealing the point-spread function (psf), the focal length and the effective collecting area. In this paper we will report on experimental setup in the X-ray test facility "PUMA," developing the EUV source, multi-channel plate detector properties, and the results of testing a modified EUV optics.
While investigating the feasibility of the accommodation of X-ray instrumentations on the International Space Station (ISS) a major question remained still open, i.e. the unknown extent of degradation of X-ray mirror surfaces and X-ray detector material caused by contamination in the ISS environment. Therefore, a sample expose experiment has been started in 2001 to investigate these effects in detail using the Russian expose facility provided by the Russian space industry company RKK Energia. While Kayser-Threde GmbH was responsible to organize and coordinate the experiment, gold-coated Zerodur and silicon samples have been provided by the Max-Planck-Institute (MPE). In total 5 samples were flown with the expose facility and have been exposed to the ISS environment for a total duration of 756 days. The analyses of 4 of them are presented in this paper. X-ray reflection measurements before and after the experiment at MPE's PANTER X-ray test facility and microscopy inspections revealed a thin structured surface layer which reduced the X-ray reflection of the exposed mirror samples dramatically. In addition, the samples have been analyzed with a scanning electron microscope, an energy dispersive X-ray spectrometer, and electron spectroscopy for chemical analysis. The results of all these measurements revealing the degradation of the X-ray mirrors and polished silicon detector surfaces are presented.
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