Swift Solar Activity X-ray Image (SSAXI-Rocket), mounted on the High-Resolution Coronal Imager (Hi-C) as a sub-payload, is a wide field solar X-ray imager designed to image Solar X-ray flares at high cadence (>5 Hz). SSAXI-Rocket consists of a Wolter-I optic with a focal length of 1 m, coupled with a monolithic CMOS X-ray sensor at the focal plane. The optics for SSAXI-Rocket were fabricated using the Electroformed Ni Replication (ENR) technique at Center for Astrophysics, Harvard-Smithsonian. Each optic has both parabolic and hyperbolic sections with 62 mm diameter at the inflection plane with a total optic length of 18 cm. The performance of the flight and flight spare optic mounted on a spider was measured at the Marshall Space Flight Center (MSFC) Stray Light Testing Facility (SLTF) to characterize the Point Spread Function (PSF) and Effective Area (EA). The flight optic selected for SSAXI-Rocket shows on-axis 16′′ Half Power Diameter (HPD) and 5′′ Full Width Half Maximum (FWHM) at 4.5 keV, exceeding the 23′′ HPD and 9′′ FWHM requirement. The effective area is about 0.64 cm2 at 4.5 keV. Coupled with the fast readout of an X-ray CMOS sensor, this optic enables rapid high-resolution X-ray imaging over a wide field of view (> 20′ x 20′). Here we review the design, fabrication and testing of the SSAXI-Rocket optic and summarize its performance.
The Swift Solar Activity X-ray Imager (SSAXI-Rocket) is a ride-along instrument to the High-Resolution Coronal Imager (Hi-C) Flare NASA sounding rocket launch campaign scheduled for the Spring 2024. In the short 5- minute rocket flight, SSAXI-Rocket will measure the soft X-ray near-peak emission phase of a large solar flare of GOES C-class or greater. The SSAXI-Rocket instrument has peak sensitivity to 10 MK solar plasma, similar to the current Hi-C flare extreme ultraviolet instruments, providing the exploration of the variability in heating and energy transport of solar flares. SSAXI-Rocket combines small X-ray focusing optic (Wolter-I) with onaxis imaging resolution of 9 arcseconds or better and high-speed readout CMOS detector, to image the flare soft X-rays at 5 hertz or faster, with minimized image saturation and pixel signal blooming. These high-time cadence measurements can help uncover the soft X-ray intensity variations which can provide constraints on the intermittent heating processes in the flare magnetic loops. SSAXI-Rocket is the testbed for technology that is planned for future heliophysics and astronomy SmallSat, CubeSat, and large satellite X-ray observatories.
The Swift Solar Activity X-Ray Imager (SSAXI-Rocket) sounding rocket experiment is a direct-imaging, soft Xray telescope optimized for the observation of large (GOES C class-X class) solar flares. SSAXI-Rocket has high temporal sampling cadence (> 5 Hz) enabled by a fast-readout CMOS detector. A single Wolter-1 optic focuses light onto the detector plane. The optic has a 15.8′′ half-power diameter (HPD) angular resolution on-axis and an effective area of 0.64 cm2 at 4.5 keV. The SSAXI-Rocket camera reads out a spectrally integrated signal, and the system spatial resolution is designed to be < 16′′ HPD over the instrument field of view (> 55′ × 55′). The detector is a back-illuminated delta doped CMOS (2048 × 2048 pixels) with 10 μm pitch pixels. This manuscript details our instrument design, and overviews the processes employed in telescope alignment, testing, delivery, and integration onto the Hi-C Sounding Rocket. We present the “as-built” projected flight performance of the delivered SSAXI-Rocket flight system, obtained by synthesizing the results of pre-flight subsystem testing and measurements performed during system integration and alignment.
We are developing Wolter X-ray optics compatible with the short focal length and small size suitable for SmallSat missions. These X-ray Optics are compact lightweight Wolter-I X-ray optics which are affordable for low cost future missions. We are leveraging the recent and on-going development to build lightweight Wolter-I X-ray optics based on the electroformed nickel replication (ENR) technique. Recent results will be presented.
Imaging of x-rays with energies >15 keV is a necessity for several applications in high-energy density physics experiments. Multilayer-coated, Wolter-type glancing-incidence optics offer higher collection efficiency than pinhole cameras or Kirkpatrick-Baez style mirrors, and can achieve spatial resolution of 10-100um over 1-8 mm fields of view with throughput ~ 1-10%. Designing the multilayer coating is a complex optimization problem, involving multiple tradeoffs. A narrow energy bandwidth (~1keV) is desirable to exclude background, but a broad angular acceptance is desirable for the optic to image a large field (~1-8 mm). A Wolter optic’s net reflectivity is two-bounce R2 = R1*R2 for a wide range of pairs of incidence angles θ1, θ 2. In addition, the multilayer coating can be modified in several ways, such as varying the period thickness through the stack, and along the length of the optic. Parallelized searches using ordinary gradient-descent and Markov-Chain Monte Carlo (MCMC) have been applied to design an optic to image Z-pinch plasmas on the Z Machine at Sandia National Laboratories. Methods are tested to design an appropriate cost function for this search, and to reduce computational cost to search the parameter space efficiently.
Versatile Optics for X-ray Imaging (VOXI) is a technology that enables a wide range of missions and opens up new opportunities for scientific research over multiple disciplines including fundamental physics, heliophysics, astrophysics, lunar and planetary science, and laboratory physics. VOXI is well-suited to SmallSats, which have become powerful platforms from which to conduct leading scientific investigations and cutting-edge technology developments at low cost with rapid turn-arounds. At the Center for Astrophysics | Harvard and Smithsonian, in collaboration with other institutions, we have developed VOXI, a Wolter-I Xray telescope with a focal length of < 1.5 m. In this paper we describe the potential of these optics, and the applications for VOXI optics considered to date.
It has been known for some time that sputtered low-density coatings deposited under vacuum (e.g. carbon or B4C), applied on top of high-density metallic coatings, can enhance the reflectivity in the soft x-ray band (below ~5 keV). In the last years, we experimented with novel carbonated coatings obtained by dip-liquid deposition, in which a thin film is formed on the surface of a mirror by immersion in a suitable precursor solution. After several attempts with different chemical compounds, we found an optimal candidate both for the reflectivity performance and for the convenience of the deposition process, which is much simpler and inexpensive compared to conventional processes. In particular, such coatings can enhance the soft x-ray response at the reflection angles employed in future telescopes, like ATHENA (ESA), Lynx (NASA) and eXTP (CAS). In this paper we consider the application of dip-liquid overcoatings on conventional coatings (Au, Ir) or in combination with recently proposed chromium overcoatings and their possible uses to enhance the reflectivity of x-ray mirrors at low, medium or higher energies, presenting the first experimental results of x-ray tests on these coatings.
The University of Colorado led Extreme-ultraviolet Stellar Characterization for Atmospheric Physics and Evolution (ESCAPE) small explorer mission concept is designed to measure the extreme- and far-ultraviolet (EUV; 80 - 560 A, 600 - 825 A, FUV; 1280 - 1650 A) irradiance and are activity of exoplanet host stars; essential measurements for assessing the stability of rocky planet atmospheres in the liquid-water habitable zone. The ESCAPE design consists of a fixed optical configuration with a grazing incidence Gregorian, or "Hetterick- Bowyer", telescope feeding grazing and normal incidence spectroscopic channels. The telescope is provided by a joint NASA Marshall Space Flight Center and Smithsonian Astrophysics Observatory team. The grazing incidence gratings have a radial profile and are ruled into single-crystal silicon using electron-beam lithography in the nanofabrication laboratory at Pennsylvania State University. Normal incidence gratings have aberration correcting holographic solutions and are supplied by Horiba Jobin Yvon. Spectra are imaged onto a curved microchannel plate detector supplied by the University of California, Berkeley. ESCAPE utilizes the Ball Aerospace BCP spacecraft. The simple, fixed configuration design of ESCAPE is projected to exceed the effective area of the last major EUV astrophysics spectrograph, EUV E-DS/S, by more than a factor of 50, providing unprecedented sensitivity in this essential bandpass for exoplanet host-star characterization. We report on the ESCAPE design, projected performance and mission implementation plan, as well as the trade studies carried out over Phase A to scope the first NASA EUV astrophysics mission in nearly 30 years. If selected, ESCAPE will launch in Fall 2025.
Wolter-I Optics for SmallSat Astronomy Mission (WOSAM) are a highly adaptable option for SmallSat missions for a number of astronomical uses. These compact Wolter-I optics with focal lengths on the order of 0.5 - 1 m are able to fit within strict mass and volume constraints and can be designed to fit the scientific requirements of exoplanet, solar, and lunar missions. In order to maximize Effective Area the telescope’s collecting area, graze angle, and vignetting need to be balanced. These factors are primarily affected by the optics’ focal length, outer diameter, shell length, and shell spacing. We show the modeling results of three SmallSat missions, the SmallSat Exosphere Explorer of hot Jupiters (SEEJ), the SmallSat Solar Axion and Activity X-ray Imager (SSAXI), and the Lunar X-ray Imaging Spectrometer (LuXIS). These missions have a range of Effective Area, Energy band, and Field of View requirements that can all be met with WOSAM telescopes.
Metallic coatings made of precious metals (e.g. Ir, Pt or Au) with high atomic number Z have been traditionally employed at grazing incidence for X-rays reflection and focalization. These materials offer a range of reflection extended to higher energies, but also present a series of absorption edges, which limit the reflectivity in the 2-4 keV band and below. Therefore the search for alternative coatings, able to improve the reflection in the soft energy range, is particularly relevant for the development of future telescopes, like ATHENA (ESA), Lynx (NASA) and eXTP (CAS). Low-Z overcoatings (e.g. carbon or B4C), applied on top of the high-Z metallic layer, can enhance the reflectivity in the softer band (mainly below 2 keV), but conventional deposition methods for these materials are not easily compatible with some of the mainstream technologies for mirror fabrication (notably, the silicon pore optics that will be used for the ATHENA X-ray mission which is being implemented by ESA). In this work we discuss novel solutions (carbon-like overcoatings realized by dip coating or vapor phase deposition), which can be particularly convenient for the application to ATHENA and to future telescopes.
We are developing Wolter-I X-ray optics for use in SmallSat missions. These optics are being designed for telescope focal lengths on the order of 0.5 - 1 m, much shorter than typical Astrophysics missions. The various parameters of the optics module: diameter, length, number nested shells, coatings, etc., depend partly on the spacecraft bus but the final design is driven by the science and instrument requirements of the mission (effective area, resolution, and energy band of interest). Ray trace software was developed and used to project the performance of several optics configurations, which, designed for SmallSat missions, meet the instrument requirements for the SmallSat Exosphere Explorer of hot Jupiters (SEEJ) . Results of this modeling is presented.
Axion is a promising dark matter candidate as well as a solution to the strong charge-parity (CP) problem in quantum chromodynamics (QCD). We describe a new concept for SmallSat Solar Axion and Activity X-ray Telescope (SSAXI) to search for solar axions or axion-like particles (ALPs) and to monitor solar activity over a wide dynamic range. SSAXI aims to unambiguously identify X-rays converted from axions in the solar magnetic field along the line of sight to the solar core, effectively imaging the solar core. SSAXI employs Miniature lightweight Wolter-I focusing X-ray optics (MiXO) and monolithic CMOS X-ray sensors in a compact package. The wide energy range (0.5 - 5 keV) of SSAXI can easily distinguish spectra of axion-converted X-rays from solar X-ray spectra, while encompassing the prime energy band (3 - 4.5 keV) of axion-converted X-rays. The high angular resolution (30 arcsec) and large field of view (40 arcmin) in SSAXI will easily resolve the enhanced X-ray flux over the 3 arcmin wide solar core while fully covering the X-ray activity over the entire solar disc. The fast readout in the inherently radiation tolerant CMOS X-ray sensors enables high resolution spectroscopy over a wide dynamic range with a broad range of operational temperatures. We present multiple mission implementation options for SSAXI under ESPA class. SSAXI will operate in a Sun-synchronous orbit for 1 yr preferably near a solar minimum to accumulate sufficient X-ray photon statistics.
The first detected exoplanets found were "hot Jupiters"; these are large Jupiter-like planets in close orbits with their host star. The stars in these so-called "hot Jupiter systems" can have significant X-ray emission and the X-ray flux likely changes the evolution of the overall star-planetary system in at least two ways: (1) the intense high energy flux alters the structure of the upper atmosphere of the planet - in some cases leading to significant mass loss; (2) the angular momentum and magnetic field of the planet induces even more activity on the star, enhancing its X-rays, which are then subsequently absorbed by the planet. If the alignment of the systems is appropriate, the planet will transit the host star. The resulting drop in flux from the star allows us to measure the distribution of the low-density planetary atmosphere. We describe a science mission concept for a SmallSat Exosphere Explorer of hot Jupiters (SEEJ; pronounced "siege"). SEEJ will monitor the X-ray emission of nearby X-ray bright stars with transiting hot Jupiters in order to measure the lowest density portion of exoplanet atmospheres and the coronae of the exoplanet hosts. SEEJ will use revolutionary Miniature X-ray Optics (MiXO) and CMOS X-ray detectors to obtain sufficient collecting area and high sensitivity in a low mass, small volume and low-cost package. SEEJ will observe scores of transits occurring on select systems to make detailed measurements of the transit depth and shape which can be compared to out-of-transit behavior of the target system. The depth and duration of the flux change will allow us to characterize the exospheres of multiple hot Jupiters in a single year. In addition, the long baselines (covering multiple stellar rotation periods) from the transit data will allow us to characterize the temperature, flux and flare rates of the exoplanet hosts at an unprecedented level. This, in turn, will provide valuable constraints for models of atmospheric loss. In this contribution we outline the science of SEEJ and focus on the enabling technologies Miniature X-ray Optics and CMOS X-ray detectors.
The long-term stability of exoplanetary atmospheres depends critically on the extreme-ultraviolet (EUV) flux from the host star. The EUV flux likely controls the demographics of the short-period planet population as well the ability for rocky planets to maintain habitable environments long enough for the emergence of life. We present the Extreme-ultraviolet Stellar Characterization for Atmospheric Physics and Evolution (ESCAPE) mission, an astrophysics Small Explorer proposed to NASA. ESCAPE employs extreme- and far-ultraviolet spectroscopy (70 - 1800 Α) to characterize the highenergy radiation environment in the habitable zones (HZs) around nearby stars. ESCAPE provides the first comprehensive study of the stellar EUV environments that control atmospheric mass-loss and determine the habitability of rocky exoplanets. The ESCAPE instrument comprises an EUV grazing incidence telescope feeding four diffraction gratings and a photon-counting detector. The telescope is 50 cm diameter with four nested parabolic primary mirrors and four nested elliptical secondary mirrors, fabricated and aligned by NASA Marshall Space Flight Center and the Smithsonian Astrophysical Observatory. The off-plane grating assemblies are fabricated at Pennsylvania State University and the ESCAPE detector system is a micro-channel plate (MCP; 125mm x 40mm active area) sensor developed by the University of California, Berkeley. ESCAPE employs the versatile and high-heritage Ball Aerospace BCP-100 spacecraft.
The New Hard X-ray Mission (NHXM) project will be operated by 2017 and is currently undergoing a Phase B study, under the coordination of the Italian Space Agency (ASI). The project is being proposed by an international team in the context of the ESA Call CV M3 as a Small Mission program, with a large Italian participation. It is based on 4 hard X-ray optics modules, each formed by 60 evenly spaced multilayer coated Wolter I mirror shells. An extensible bench is used to reach the 10 m focal length. The Wolter I monolithic substrates with multilayer coating are produced in NiCo by electroforming replication. Three of the mirror modules will host in the focal plane a hybrid a detector system (a soft X-ray Si DEPFET array plus a high energy CdTe detector). The detector of the fourth telescope will be a photoelectric polarimeter with imaging capabilities, operating from 2 up to 35 keV. The total on axis effective area of the three telescopes at 1 keV and 30 kev is of 1500 cm2 and 350 cm2 respectively, with an angular resolution of 20 arcsec HEW at 30 keV. In this paper we report on the design and development of the multilayer coated X-ray mirrors based on NiCo shells.
We have developed a process for indirectly coating arbitrarily small diameter electroformed nickel replicated optics with multilayers to increase their response at high energy (i.e. >10 keV). The ability to fabricate small diameter multilayer coated full shell Wolter X-ray optics with narrow bandpass opens the door to several applications within astronomy and also provides a path for cross-fertilization to other fields. We report on the characterization and evaluation of the first two prototype X-ray Wolter optics to be delivered to the Z Pulsed Power Facility at Sandia National Laboratories. The intent is to develop and field several optics as part of an imaging system with targeted spectral ranges.
In order to advance significantly scientific objectives, future x-ray astronomy missions will likely call for x-ray telescopes
with large aperture areas (≈ 3 m2) and fine angular resolution (≈ 12). Achieving such performance is programmatically
and technologically challenging due to the mass and envelope constraints of space-borne telescopes and to the need for
densely nested grazing-incidence optics. Such an x-ray telescope will require precision fabrication, alignment, mounting,
and assembly of large areas (≈ 600 m2) of lightweight (≈ 2 kg/m2 areal density) high-quality mirrors, at an acceptable cost
(≈ 1 M$/m2 of mirror surface area). This paper reviews relevant programmatic and technological issues, as well as possible
approaches for addressing these issues-including direct fabrication of monocrystalline silicon mirrors, active (in-space
adjustable) figure correction of replicated mirrors, static post-fabrication correction using ion implantation, differential
erosion or deposition, and coating-stress manipulation of thin substrates.
Adjustable X-ray optics represent a potential enabling technology for simultaneously achieving large effective area and high angular resolution for future X-ray Astronomy missions. The adjustable optics employ a bimorph mirror composed of a thin (1.5 μm) film of piezoelectric material deposited on the back of a 0.4 mm thick conical mirror segment. The application of localized electric fields in the piezoelectric material, normal to the mirror surface, result in localized deformations in mirror shape. Thus, mirror fabrication and mounting induced figure errors can be corrected, without the need for a massive reaction structure. With this approach, though, film stresses in the piezoelectric layer, resulting from deposition, crystallization, and differences in coefficient of thermal expansion, can distort the mirror. The large relative thickness of the piezoelectric material compared to the glass means that even 100MPa stresses can result in significant distortions. We have examined compensating for the piezoelectric processing related distortions by the deposition of controlled stress chromium/iridium films on the front surface of the mirror. We describe our experiments with tuning the product of the chromium/iridium film stress and film thickness to balance that resulting from the piezoelectric layer. We also evaluated the repeatability of this deposition process, and the robustness of the iridium coating.
NASA’S future X-ray astronomy missions will require X-ray optics that have large effective area while remaining lightweight, and cost effective. Some X-ray missions, such as XMM-Newton[1] , and the upcoming Spectrum-Röntgen- Gamma[2] mission use an electroformed nickel replication (ENR) process[3] to fabricate the nested grazing incidence X-ray telescope mirror shells for an array of moderate resolution, moderate effective area telescopes. We are developing a process to fabricate metal-ceramic replicated optics which will be lighter weight than current nickel replicated technology. Our technology development takes full advantage of the replication technique by fabricating large diameter mirrors with thin cross sections allowing maximum nesting and increase in collecting area. This will lead to future cost effective missions with large effective area and lightweight optics with good angular resolution. Recent results on fabrication and testing of these optics is presented.
Over the last few decades, grazing incidence X-ray optics have been a pivotal tool for advances in X-ray astronomy. They have been successfully employed in many great observatories such as ROSAT, Chandra X-ray Observatory and XMM-Newton. In planetary science, X-ray observations of Solar system objects are a great tool to understand the nature of the target bodies and the evolutionary history of the Solar system as a whole. To date, X-ray observations in near-target planetary missions have been limited to collimator-based instruments due to tight mass and volume constraints, arising from the multi-instrument nature of planetary missions. In addition, unlike observations of astrophysical sources at virtually infinite distances, near-target observations of planetary bodies introduce a unique set of challenges. While true focusing X-ray optics can overcome these challenges, a practical implementation of focusing X-ray optics for planetary missions depends on the feasibility of compact lightweight X-ray optics. We review scientific motivations for X-ray observations of planetary bodies and illustrate the unique challenges encountered in planetary missions through a few examples. We introduce a new metal-ceramic hybrid technology for X-ray mirrors that can enable compact lightweight Wolter-I X-ray optics suitable for resource limited planetary missions.
Nearly all X-ray astronomy missions of the past 25 years have utilized grazing incidence telescopes which use the
principle of nested shells to maximize the collecting area. Most of these missions have had multiple X-ray telescopes,
e.g. ASCA1, Beppo-SAX2, Suzaku3, XMM-Newton4, NuStar5, and also upcoming missions Astro-H6 and Spectrum-Röentgen-Gamma7. Multiple telescopes, which favor replication, may continue to be the appropriate architecture of some future missions. XMM-Newton and the upcoming Spectrum-Röentgen-Gamma mission use an electroformed nickel replication (ENR) process to fabricate their X-ray telescope mirror shells, a process which has achieved the best angular resolution to date for replicated telescopes. We are developing a process to fabricate metal-ceramic replicated
optics which will be lighter weight than current nickel replicated technology. They will be stiffer than the XMM mirrors,
which we expect will result in better angular resolution. Recent results on fabrication and testing of these optics is
presented.
The Extreme Physics Explorer (EPE) is a concept timing/spectroscopy mission that would use micro-channel plate
optics (MCPO) to provide 4m2 effective area focused to ~1 arc-min onto an X-ray calorimeter. We describe science
drivers for such a mission, possible designs for the large area MCPO needed for EPE, and the challenges of the large
area MCPO design.
X-ray astronomy grazing incidence telescopes use the principle of nested shells to maximize the
collecting area. Some of the more recent missions, such as XMM-Newton [1], have used an
electroformed nickel replication (ENR) process [2] to fabricate the mirror shells. Upcoming
missions, such as Spectrum-Röntgen-Gamma [3] and Focusing Optics X-ray Solar Imager [4], also
use the electroforming process to fabricate nested shell grazing incidence X-ray telescopes.
We present recent results on fabrication of replicas with multilayer coatings from Wolter-1 mandrels
using a new hardcoat release material to simplify and improve this electroforming process.
In the case of neutrons the refractive index is slightly less than unity for most elements and their isotopes [1].
Consequently, thermal and cold neutrons can be reflected from smooth surfaces at grazing-incidence angles. Hence, the
optical technologies developed for x-ray astronomy can be applied for neutron focusing. The focusing capabilities of
grazing incidence neutron imaging optics have been successfully demonstrated using nickel mirrors. The mirrors were
fabricated using an electroformed nickel replication process at Marshall Space Flight Center. Results of the neutron
optics experiments and current status of the multilayer coating replication technique development are presented.
Platinum is being explored as an alternative to the sprayed boron nitride mandrel release coating under study at GSFC
for the International X-ray Observatory (IXO). Two and three inch diameter, polished (PFS) and superpolished (SPFS)
fused silica flat mandrels, were used for these tests. Pt was applied to the mandrels by DC magnetron sputtering. The
substrate material was 400 micron thick D263 glass, the material which has been proposed for the IXO segmented
optics. These substrates were placed on the mandrels and thermally cycled with the same thermal profile being used at
GSFC in the development of the BN slumping for IXO. After the thermal cycle was complete, the D263 substrates were
removed; new D263 substrates were placed on the mandrels and the process was repeated. Four thermal cycles have
been completed to date. After initially coating the mandrels with Pt, no further conditioning was applied to the mandrels
before or during the thermal cycles. The microroughness of the mandrels and of the D263 substrates was measured
before and after thermal cycling. Atomic force microscopy (AFM) and 8 keV X-ray reflectivity data are presented.
The New Hard X-ray Mission (NHXM) has been designed to provide a real breakthrough on a number of hot
astrophysical issues that includes: black holes census, the physics of accretion, the particle acceleration mechanisms, the
effects of radiative transfer in highly magnetized plasmas and strong gravitational fields. NHXM combines fine imaging
capability up to 80 keV, today available only at E<10 keV, with sensitive photoelectric imaging polarimetry. It consists
of four identical mirrors, with a 10 m focal length, achieved after launch by means of a deployable structure. Three of the
four telescopes will have at their focus identical spectral-imaging cameras, while a X-ray imaging polarimeter will be
placed at the focus of the fourth. In order to ensure a low and stable background, NHXM will be placed in a low Earth
equatorial orbit. Here we will provide an overall description of this mission and of the developments that are currently
occurring in Italy. In the meanwhile we are forming an international collaboration, with the goal to have a consortium
of leading Institutes and people that are at the forefront of the scientific and technological developments that are
relevant for this mission.
The New Hard X-ray Mission (NHXM) project will be operated by 2016 and is currently undergoing the Phase B study.
It is based on 4 hard X-ray optics modules, each formed by 60 evenly spaced multilayer coated Wolter I mirror shells.
An extensible bench is used to reach the 10 m focal length. The Wolter I monolithic substrates with multilayer coating
are produced in NiCo by electroforming replication. Three of the mirror modules will host in the focal plane a hybrid a
detector system (a soft X-ray Si DEPFET array plus a high energy CdTe detector). The detector of the fourth telescope
will be a photoelectric polarimeter with imaging capabilities, operating from 2 up to 35 keV. The total on axis effective
area of the three telescopes at 1 keV and 30 kev is of 1500 cm2 and 350 cm2 respectively, with an angular resolution of
20 arcsec HEW at 30 keV. In this paper we report on the design and development of the multilayer optics of the mission,
based on thin replicated Ni mirror shells.
The International X-ray Observatory (IXO) is designed to conduct spectroscopic, imaging, and timing studies
of astrophysical phenomena that take place as near as in the solar system and as far as in the early universe. It
is a collaborative effort of ESA, JAXA, and NASA. It requires a large X-ray mirror assembly with an
unprecedented X-ray collection area and a suite of focal plane detectors that measure every property of each
photon. This paper reports on our effort to develop the necessary technology to enable the construction of the
mirror assembly required by IXO.
The use of depth-graded multilayer coatings is foreseen in several future X-ray telescopes (e.g. Hexit-Sat/NHXT, NuSTAR, IXO, NeXT), in order to extend to higher energies (up to 80 keV) the focusing capabilities of present day telescopes, like Chandra and XMM/Newton, that are operative in the soft X-ray band (0.1-10 keV).
The deposition of multilayer coatings is a difficult process, in which a good control of the individual layer thickness is required. The process must also be stable for the long time needed (several hours).
The main issues are the accuracy of the film (stability of the process), interfacial and surface roughness, the lateral homogeneity and the long-term stability of the film. Physical properties of the film, like the density or the crystallicity are also important.
The analysis of reflectivity measurements is an important tool to study the structure of multilayer samples, investigating in a non-destructive way the whole properties of the film down to the deepest layers. Nevertheless the analysis of data is not easy, neither standardized.
Two samples were realized using different materials (Pt/C and W/Si). The film structures were designed to be representative of broad angular/energy band multilayer coatings foreseen in hard X-ray focusing telescopes. Their reflectivity was measured for several energies in the 40-130 keV range as a function of the reflection angle. The High energy reflectivity data are compared with the theoretical expectations derived from low-energy (8.04 keV) measures acquired after the deposition.
X-ray astronomy grazing incidence telescopes use the principle of nested shells to
maximize the collecting area. Some of the more recent missions, such as XMM-Newton,
have used an electroformed nickel replication process to fabricate the mirror shells. We
have been developing coatings to simplify and improve this electroforming process.
This paper discusses our most recent results from studies using TiN as a mandrel
hardcoat in the electroforming process of fabricating nickel shell optics. The results
indicate that nickel replicas separate easily from the TiN coated mandrel, and little (if
any) degradation of the mandrel occurs after more than 20 replications. AFM
characterization of the mandrel and replica surfaces is shown. Preliminary results are also
included from studies which use this same process to replicate multilayer coatings; these
results indicate no change in the multilayer stack after separation from the mandrel.
The Constellation-X Observatory is currently planned as NASA's next major X-ray observatory to be launched towards
the end of the next decade. The driving science goals for the mission are to: 1) Trace the evolution of Black Holes with
cosmic time and determine their contribution to the energy output of the Universe; 2) Observe matter spiraling into
Black Holes to test the predictions of General Relativity; 3) Use galaxy clusters to trace the locations of Dark Matter and
follow the formation of structure as a function of distance; 4) Search for the missing baryonic matter; 5) Directly observe
the dynamics of Cosmic Feedback to test models for galaxy formation; 6) Observe the creation and dispersion of the
elements in supernovae; and 7) Precisely constrain the equation of state of neutron stars. To achieve these science goals
requires high resolution (R > 1250) X-ray spectroscopy with 100 times the throughput of the Chandra and XMMNewton.
The Constellation-X Observatory will achieve this requirement with a combination of four large X-ray
telescopes on a single satellite operating in the 0.25 to 10 keV range. These telescopes will feed X-ray micro-calorimeter
arrays and grating spectrometers. A hard X-ray telescope system will provide coverage up to at least 40 keV. We
describe the mission science drivers and the mission implementation approach.
Future astrophysics missions operating in the hard X-ray/Soft Gamma ray range is slated to carry novel focusing
telescopes based on the use of depth graded multilayer reflectors. Current design studies show that, at the foreseen focal
lengths, it should be feasible to focus X-rays at energies as high as 300 keV. These designs use extrapolations of
theoretical and experimentally determined optical constants below 100 keV. We have previously shown that
determining the optical constants from traditional single layer film above 40 keV is very difficult. One needs to have
substrates which are very flat and it is very important to know the exact flatness. In this paper we report on the
experimental determination of optical constants up to and above 130 keV using substrates with sub arcsecond flatness.
We present these results as obtained at the National Synchrotron Light Source in Brookhaven and compare these to
theoretically calculated values and previous experiments.
X-ray Wolter focusing telescopes concentrate the light by means of reflection on smooth surfaces at small grazing
angle (below a couple of degrees). The traditional coatings for these kind of applications are heavy materials
that, due to their high density, present a high critical energy for total reflection. Recent works have shown how a
thin layer of a light material, like carbon, on top of a traditional reflecting coating, can enhance the reflectivity in
soft x-ray spectral region (below 5 keV), without degrading the performances for higher energies. We presented
at SPIE 2007 some experimental results about the reflectivity measurement at very low energies (200 eV) and
rather large angles (1-2 deg). In the present work we extend the former study, by the realization of a new set of
samples with coatings made of different materials (Pt, Au, W, Ir) and the measurement of their reflectivity for
the typical angles (< 1°) and energies (1-10 keV) employed in astronomical grazing incidence telescopes.
The Constellation-X mission concept has been streamlined to a single Atlas V 551 configuration. This decision was reached by the project team after considering the increases in launch costs announced in 2006 coupled with the constrained budget environment apparent with the release of the NASA 2007 budget. Along with the Spectroscopy X-ray Telescopes, this new configuration continues to carry a Hard X-ray Telescope (HXT) component, with some modifications to the original requirements to adjust to the new configuration. The total effective area requirement in the 7 - 40 keV band has been reduced, but at the same time the angular resolution requirement has been increased from 1 arcmin to 30 arcsec. The Smithsonian Astrophysical Observatory, Marshall Space Flight Center and Brera Observatory (Italy) have been collaborating to develop and HXT which meets the requirements of Constellation-X. The development work we have been engaged in to produce multilayer coated Electroformed-Nickel-Replicate (ENR) shells is well suited for this new configuration. We report here on results of fabrication and testing of a prototyped optic for the HXT. Full beam illumination X-ray tests, taken at MPE-Panter Test Facility, show that these optics meet the new requirement of 30 arcsec for the streamlined Constellation-X configuration. This report also presents preliminary results from studies using titanium nitride as a release agent to simplify and improve the nickel electroforming replication process.
Future Astrophysics missions operating in the hard X-ray/Soft Gamma ray range is slated to carry novel focusing
telescopes based on the use of depth graded multilayer reflectors. Current design studies show that, at the foreseen focal
lengths, it should be feasible to focus X-rays at energies as high as 300 keV. These designs use extrapolations of
theoretical and experimentally determined optical constants from below 200 keV. In this paper we report on the first
experimental determination of optical constants up to and above 200 keV. We present these first results as obtained at
the National Synchrotron Light Source in Brookhaven and compare these to results obtained previously up to 180 keV of some of the same materials at the European Synchrotron Radiation Facility in Grenoble.
Depth graded multilayer designs for hard x-ray telescopes in the 10 keV to 70-80 keV energy range have had either W or
Pt as the heavy element. These materials have been chosen because of reasonable optical constants, the possibility to
grow smooth interfaces with the spacer material, and the stability over time. On the flip side both W and Pt have an
absorption edge -- 69.5 keV (W) and 78.4 keV (Pt) -- which is very close to the two 44Ti lines at 67.9 keV and 78.4 keV
that are produced in the envelope of a super nova explosion. Other materials have better optical constants and no
absorption edges in this energy range, for example Ni0.93V0.07, but are not used because of high interface roughness. By
using a WC/SiC multilayer for the bottom and a Ni0.93V0.07/SiC multilayer for the thicker top layers of a depth graded
multilayer we have made a reflector that doesn't have a clear absorption edge. This reflector has been measured at
energies between 8 keV and 130 keV. At a graze angle of 0.11 degree there is still nearly the same reflectivity below the
W absorption edge as for a traditional W based coating, and above the W absorption edge there is still 48% reflection at 80 keV.
In X-ray astronomical telescopes, the focalization of the radiation is achieved by means of grazing incidence Wolter I
(parabola + hyperbola) optics in total reflection regime. In general, high density materials (e.g. Au, Pt, Ir, W) are used as
reflecting coatings, in order to increase as much as possible the cut-off angles and energies for total reflection. However
these materials present an important reduction of the reflectivity between 0.2 and 5 keV, due to the photoabsorption, and
this phenomenon is particularly enhanced in correspondence of the M absorption edges (between 2 and 3.5 keV). In
general, this determines a strong decrease of the telescope effective area. To overcome the problem we suggested in
previous works the coating of the mirror surface by a low-density material such as carbon. Mirror samples with different
coatings made by high density materials: Au, Ir, Pt, and W with a carbon overcoating were manufactured and reflectivity
data in the soft X-ray band (100-2000 eV), performed both at the XACT facility in Palermo (Italy) and at BSRF
synchrotron in Beijing (China), are showed. In this paper we present some of the first results concerning the
measurements carried out at the photon energies of 200 eV (i.e. below the carbon K absorption edge) and 1280 eV (i.e.
the region just below the heavy material M absorption edge).
The Constellation-X mission planned for launch in 2015-2020 timeframe, will feature an array of Hard X-ray telescopes (HXT) with a total collecting area greater than 1500 cm2 at 40 keV. Two technologies are being investigated for the optics of these telescopes, one of which is multilayer-coated Electroformed-Nickel-Replicated (ENR) shells. The attraction of the ENR process is that the resulting full-shell optics are inherently stable and offer the prospect of better angular resolution which results in lower background and higher instrument sensitivity. We are building a prototype HXT mirror module using an ENR process to fabricate the individual shells. This prototype consists of 5 shells with diameters ranging from 15 cm to 28 cm with a length of 42.6 cm. The innermost of these will be coated with iridium, while the remainder will be coated with graded d-spaced W/Si multilayers. The assembly structure has been completed and last year we reported on full beam illumination results from the first test shell mounted in this structure. We have now fabricated and coated two (15 cm and 23 cm diameter) 100 micron thick shells which have been aligned and mounted. This paper presents the results of full beam illumination X-ray tests, taken at MPE-Panter. The HEW of the individual shells will be discussed, in addition to results from the full two shell optic test.
The Constellation-X (Con-X) mission planned for launch in 2015, will feature an array of Hard X-ray telescopes (HXT) with a total collecting area greater than 1500 cm2 at 40 keV. Two technologies are being investigated for the optics of these telescopes, including multilayer coated Electroformed-Nickel-Replicated (ENR) shells. The attraction of the ENR process is that the resulting full-shell optics are inherently stable and offer the prospect of better angular resolution which results in lower background and higher instrument sensitivity. We are building a prototype HXT mirror module using an ENR process to fabricate the individual shells. This prototype consists of 5 shells with diameters ranging from 150 mm to 280 mm with a length of 426 mm. The innermost of these will be coated with iridium, while the remainder will be coated with graded d-spaced W/Si multilayers. Parts I and II of this work were presented at the SPIE meetings in 2003 and 2004. This paper presents a progress update and focuses on accomplishments during this past year. In particular, we will present results from full illumination X-ray tests of multilayer coated shells, taken at the MPE-Panter X-ray facility.
We have identified an inexpensive, readily available, mechanically stable, extremely smooth, elastic, and mechanically uniform plastic suitable for thin film X-ray optics. Polyethylene terephthalate (PET) is easily deformed without losing its elastic properties or surface smoothness. Most important, PET can be coated with mono- or multilayers that reflect X-rays at grazing incidence. We have used these properties to produce X-ray optics made either as a concentric nest of cylinders or as a spiral. We have produced accurately formed shells in precisely machined vacuum mandresl or used a pin and wheel structure to form a continuously wound spiral. The wide range of medical, industrial and scientific applications for our technology includes: a monochromatic X-ray collimater for medical diagnostics, a relay optic to transport an X-ray beam from the target in a scanning electron microscop0e to a lithium-drifted silicon and microcalorimeter detectors and a satellite mounted telescope to collect celestial X-rays. A wide variety of mono- and multilayer coatings allow X-rays up to ~100 keV to be reflected. Our paper presents data from a variety of diagnostic measurements on the properties of the PET foil and imaging results form single- and multi-shell lenses.
The Constellation-X mission, planned for launch in 2013, will feature an array of hard-x-ray telescopes (HXT) with a total collecting area of greater than 1500 cm2 at 40 keV. Two technologies are currently being investigated for the optics of these telescopes including multilayer-coated Eletroformed-Nickel-Replicated (ENR) shells. The attraction of the ENR process is that the resulting full-shell optics are inherently stable and offer the prospect of better angular resolution which results in lower background and higher instrument sensitivity. The challenge for this process is to meet a relatively tight weight budget with a relatively dense material (ρnickel = 9 g/cm3.) To demonstrate the viability of the ENR process we are fabricating a prototype HXT mirror module to be tested against a competing segmented-glass-shell optic. The ENR prototype will consist of 5 shells of diameters from 150 mm to 280 mm with a length of 426 mm. To meet the stringent weight budget for Con-X, the shells will range in thickness from 100 microns to 150 microns. The innermost of these will be coated with Iridium, while the remainder will be coated with graded-dspaced W/Si multilayers. Mandrels for these shells are in the fabrication stage, the first test shells have been produced and are currently undergoing tests for figure and microroughness. A tentative date of June '04 has been set for the prototype X-ray testing at MSFC. Issues currently being addressed are the control of stresses in the multiplayer coating and ways of mitigating their effects on the figure of the necessarily thin shells. The fabrication, handling and mounting of these shells must be accomplished without inducing permanent figure distortions. A full status report on the prototype optic will be presented along with test results as available.
B-MINE is a concept for a balloon mission designed to probe the
deepest regions of a supernova explosion by detecting 44Ti emission at 68 keV with spatial and spectral resolutions that are sufficient to determine the extent and velocity distribution of the 44Ti emitting region. The payload introduces the concept of focusing optics and microcalorimeter spectroscopy to nuclear line emission astrophysics. B-MINE has a thin, plastic foil telescope multilayered to maximize the reflectivity in a 20 keV band centered at 68 keV and a microcalorimeter array optimized for the same energy band. This combination provides a reduced background, an energy resolution of 50 eV and a 3F sensitivity in 106 s of 3.3 10-7 ph cm-2 s-1 at 68 keV.
During the course of a long duration balloon flight, B-MINE could
carry out a detailed study of the 44Ti emission line centroid and
width in CAS A.
The NASA's Constellation X-Ray Mission consists of a Soft X-Ray Telescope (SXT) based on large collecting area optics plus a focusing Hard X-Ray Telescope (HXT) operating between 8 and 70 keV and possibly at even higher energy. The Con-X HXT will have a focal length of 10 m and graze angles are small (0.25 - 0.1 deg). The substrates will be coated with multilayers to enhance the reflectivity but single heavy element coatings are an alternative for the small diameter substrates of the set. Twelve copies of the HXT are distributed evenly among the four Con-X spacecrafts. With multiple telescopes it is appropriate to consider electroforming, the replication process used successfully by Beppo-SAX, JET-X/SWIFT, and XMM-Newton, to produce their substrates. The important feature of the technique is that for mirrors with aperture diameters less than 40 cm also with thin substrates it is possible to achieve good angular resolution, which is important for obtaining high signal-to-noise ratios in deep observations and imaging extended sources. We review the main results of our development study devoted to proving the feasibility of the process for the Con-X/HXT, with particular stress on demonstrating, not only by theoretical considerations but also presenting an important experimental proof, that we can satisfy the severe mass constraints of the mission still maintaining good imaging capabilities.
We present new results from a program to develop large area X-ray telescopes that are made from thin plastic shells. We use multi-shell cylindrical lenses in a point-to-point configuration to form full aperture images of the small focal spot in a an X-ray tube on a microchannel plate detector. The image data are analyzed to yield radial profiles and encircled energy curves. The derived parameters can be extrapolated to the case of a telescope that is a conical approximation to Wolter 1 optics. The plastic shells can be coated with suitable mono- or multilayers that allow for a wideband coverage of X-ray energies. Our current program is focused on the development of a large area, hard X-ray telescope for a balloon payload.
We report the results obtained during the second phase of a program which consists of comparing the performance of different multilayer material combinations. These coatings will be used to extend the bandpass of current hard X-ray optics toward 100 keV, an order of magnitude higher than present technology. The materials studied here are W/Si, Pt/C, and W/C. A comparison of the performance of depth graded multilayers of these different materials at energies 30-80 keV was undertaken. Specular reflectivity data were acquired at 30-80 keV using the X17B1 beamline of the National Synchrotron Light Source. Reflectivity versus energy plots showed a high enough reflectivity for the bandpass of interest at grazing angles typical for hard x-ray telescope mirror shells. The next phase of our program will continue with similar high-energy pencil beam measurements on multilayer coated telescope prototype shells.
We present results from a program to develop an X-ray telescope made from thin plastic shells. Our initial results have been obtained from multi-shell cylindrical lenses that are used in a point-to-point configuration to image the small focal spot of a an X-ray tube on a microchannel plate detector. We describe the steps that led up to the present design and present data from the tests that have been used to identify the properties of the plastic material that make it a suitable X-ray reflector. We discuss two applications of our technology to X-ray missions that are designed to address some of the scientific priorities set forth in NASA's long term plans for high energy astrophysics. One mission will observe in the 1- 10 keV band, the other will extend up to ca. 100keV.
We discuss technology that will produce a wide angle monochromatic beam of X-rays that appears to diverge from a virtual point source. Although our ideas are discussed in the context of dual energy subtraction angiography (DESA) that we are developing to operate in a clinical setting, they are widely adaptable to all applications of x-ray radiography. The best DESA analysis is obtained from X-ray images made in narrow energy bands just below and just above the I K-absorption edge. Our monochromator will be used to isolate these narrow bands to produce high contrast, high spatial resolution, ECG gated angiographic images. Emission lines, that have X-ray energies below (E-) and above (E+) the I K-absorption edge at 33.2 keV, are readily available. We have deposited variable d-spacing artificial crystals, called multilayers, on optically flat, very smooth substrates, to create narrow pass band X-ray monochromators centered on La and Ba K-emission lines. We will record (E-) and (E+) exposures on either photographic plates or, in the future, with energy sensitive pixelated arrays of solid state detectors. After a suitable normalization, the exposures will be subtracted to yield a high resolution, high contrast image of the I filled arteries. Although initial results will be obtained with conventional X-ray tubes, our goal is to couple the monochromators to a high intensity, laser produced, X-ray plasma. We will present early test data that shows the multilayer performance.
We present the results of a study of the influence of the deposition process parameters on the X-ray reflectivity of multilayer mirrors for applications at energies above 10 keV. The coating process used is DC magnetron sputtering and we have begun an optimization analysis for two material combinations: W/Si and Pt/C. The following process parameters were considered: argon pressure, distance between cathodes and substrate, and sputtering cathode currents. The samples are coated on 2' polished silicon wafers and their X-ray reflectivity is measured by performing a specular scan with an 8.05 keV (Cu K-alpha) X-ray beam. The reflectivity scans were analyzed with the IMD software and the fitted interface roughness values were correlated with the deposition parameters. The analysis of variance (ANOVA) statistical treatment of the data allows the determination of the contribution of each process parameter to the reflectivity and establishes which of the parameters need tighter control.
Multilayer structures with depth-graded spacing can show a high reflectivity in a broad energy passband for hard X-rays if the interface roughness/diffuseness is controlled and minimized. We present a study of several multilayer systems deposited by DC magnetron sputtering on <111> silicon wafers and superpolished fused silica substrates. The material combinations discussed are W/Si, WSi2/Si, W/C, Pt/C, Ni/C, Ni/B4C, and Mo/Si. The deposition method used was DC magnetron sputtering at low argon pressures (1.5 to 5 mT). The characterization methods used were: Atomic Force Microscopy in tapping mode, stylus profilometry, Rutherford backscattering, cross sectional TEM, and specular X-ray reflectivity (XRR) scans at 8.05 keV. Different process parameters were varied in order to optimize the interface roughness/diffuseness (sigma) that was measured by XRR scans.
Estimates of background in CZT detectorsi indicate that even with the beneficial concentration of a focussing telescope measurements in the 20 to 100 keV band of the Constellation X-ray Mission's HXT will become background limited after several thousand seconds of observing. This time is less than the expected exposure of most measurements. Consequently the sensitivity of most if not all observations of the HXT will be background limited. Therefore, the angular resolution should be as good as possible as long as the effective area remains high. We are pursuing a method for fabricating telescopes for thetwelve units of HXT that consists of electroforming integral shell substrates, a process that has been highly developed for XMM. We are attempting to adapt this method to higher energy X-rays by employing multilayer coatings, and smaller graze angles, and also reduce the mass of the telescopes from the XMM prescription by employing stronger, lighter alloys. The resolution that XMM has achieved, 15" HPW is an indication of the resolution we can expect.
We are engaged in a program to develop focusing hard X-ray optics for future X-ray astronomy missions (such as the Hard X-ray Telescope of Constellation-X) and have built a DC magnetron sputtering system to deposit multilayers on candidate substrates for future telescopes. Although our emphasis is on the multilayer coating of integral cylindrical optics which will provide the highest spatial resolution, other types of substrates can easily be coated in this system. We present specular reflectivity data (using CuKα X- rays) of W/Si constant d and depth graded-d multilayer depositions on substrates such as thermally formed DESAG glass and Duran glass cylinders. We will present data to show both azimuthal and linear uniformity of these coatings.
We present the results from a systematic study of several different material combinations for multilayer coatings on flat silicon and fused silica substrates. To obtain high reflectivity in a broad energy bandpass for hard X-rays (greater than 10 keV), a graded d-spacing multilayer structure must satisfy a set of conditions, e.g., low surface and interface roughness/diffuseness, good layer thickness uniformity, low residual stresses, etc. The coating process must be stable and accurately controlled over long deposition times, and allow good reproducibility from one run to another. The deposition method used was DC magnetron sputtering at low argon pressures (1.5 to 3.5 mT). The materials selected for the reflector/spacer pair were W/Si, W/C, Ni/C, and Pt/C. The initial work consisted in calibrating the deposition rate and optimizing the process parameters (argon backpressure, target to substrate distance, and cathode current). The main characterization methods used were: Atomic Force Microscopy in tapping mode, stylus profilometry, and specular X-ray reflectivity. In the next stage of the study, constant and graded d-spacing multilayers were deposited on Si and float glass substrates, with the design structure based on a computer modeling of the X-ray reflectivity dependence with grazing angle and energy. A specular reflectivity scan was performed for each sample at 8.05 keV (and also at higher energies for some samples) and was fitted using the IMD software. Cross-sectional TEM was performed on a limited number of samples to offer additional information. The analyses completed for W/Si, W/C, Pt/C, and Ni/C show for the best samples good uniformity and high reflectivity at 8.05 keV. The work in progress for Cu/Si and Mo/Si will be presented at the conference and will conclude this study of candidate materials and optimized designs for hard X-ray multilayer optics.
In addition to high resolving power in the traditional x-ray band, the Constellation X-ray scientific goals require broad bandpass, with response extending to E >= 40 keV. To achieve this objective, Constellation-X will incorporate a hard x-ray telescope (HXT) based on depth graded multilayer- coated grazing incidence optics and position-sensitive solid state detectors. This paper describes the HXT performance requires, provides an overview of the HXT optics and detector technology development efforts, and present example designs.
New design concepts and materials can be used to produce very lightweight, thin foil approximations, to Wolter I and other x-ray optics. Structures are designed around a central hub and spacers that connect one spoked wheels. Figure defining, thin pins span the distance between the wheels. Thin, metal coated or multilayered, plastic foils can be formed into cones, cylinders or spirals for x-ray telescopes or lenses. Imaging and spectroscopic data obtained with x- ray lenses are presented and they indicate that a 60 cm diameter, 4.65 m focal length x-ray telescope can have a half power diameter of < 2 arcmin.
The Multilayer Facility at the Center for Astrophysics is involved in developing graded-d spacing multilayers for coating X-ray optics for hard x-ray focusing telescopes. Graded d spacing W/C multilayers have been fabricated on flat substrates of silicon and characterized using specular x-ray reflectivity, AFM, and TEM. Results are presented and compared with theoretical models.
Studies are being carried out to compare the performance of several different separation materials used in the replication process. This report presents the results obtained during the second year of a program which consists of replicating smooth, thin substrates, depositing multilayer coatings upon them, and evaluating their performance. Replication smooth, thin substrates, depositing multilayer coatings upon them, and evaluating their performance. Replication and multilayer coatings are both critically important to the development of focussing hard x- ray telescopes that function up to 100 keV. The activities of the current year include extending the comparison between sputtered amorphous carbon and evaporated gold to include sputtered as well as evaporated gold. The figure of merit being the smoothness of the replica which has a direct effect on the specular reflectivity. These results were obtained with epoxy replication, but they should be applicable to electroformed nickel, the process we expect to use for the ultimate replicated optics.
We are engaged in a program to develop focusing hard x-ray optics for future x-ray astronomy missions. Optics are being developed to focus x-rays up to and beyond 80 keV. Emphasis is on the multilayer coating of integral cylindrical optics which will provide the highest spatial resolution. A chamber geometry has been designed to allow the uniform coating of the inside surface of integral cylinders. The building and testing of this system has taken place over the past year. Linear DC magnetron cathodes are used to sputter the multilayer films. Initial results from both longitudinal and azimuthal uniformity coating tests are presented.
AXAF telescope witness mirror calibrations have been carried out on ALS Beamline 6.3.2 in July 1997 and Jan-Feb 1998 to ascertain whether sufficient beam purity and signal to noise were available over the energy range 50-1000 eV. An overall accuracy of 1 percent is necessary on reflectivities to meet AXAF program requirements. Some beamline variations were incorporated - based on two previous test runs. Various filter/order-sorter combinations were used to control beam purity. A test involving strength of the N-edge dips in reflectivity versus sample angle to the beam showed the NVII, NVI, NIII, NII, and NI edges in roughly expected proportions. This verified adequate purity in all filter/order-sorter channels except the 260-454 eV channel that includes the NV and NIV edges just above the carbon K- edge. We discuss a future solution of this puzzle by other test for evaluation of the carbon contamination layer. Oxygen contamination is also ubiquitous on Ir mirrors and foils. These problems can also be handled through optimization of the data acquisition and use of control samples. In reflection Ir NIII appears out of the noise as two doublet-like bumps. Ir NII has so far been observed near the noise level < 2 percent. Averaged over many scans it too appears to be doublet-like. Scans through the NI edge near the noise level are compatible with a doublet-like or broad feature from 685-707 eV. transmission data give the NI and NIII edges better. Ir NIV and NV edges are not yet measurable for systematic reasons. NVI and NVII appear to be normal edges. Angle scans to derive the Ir and Cr layer thicknesses are feasible at approximately 900-920 eV. Reflectivities can be reliably measured at small angles to 1300 eV. This will be useful for overlap with measurements at NSLS. Optical constants derived from reflectivities in most segments of this energy range will meet requirements for AXAF. Transmission measurements are being pursued in addition, for confirmation and to augment some segments.
We are engaged in a program to develop focusing hard x-ray telescopes in a double conical or Wolter 1 geometry that function up to 100 keV by employing small graze angles and multilayer coatings. Directly polished substrates are not an option because they are too thick to be nested efficiently. The only alternative is to fabricate the very thin substrates by replication. Our objective is the production of integral cylindrical substrates because they should result in better angular resolution than segmented foil geometries. In addition, integral cylinders would be more resistant to possible stress from deep multilayer coatings than segmented ones. Both electroforming of nickel (method of SAX, JET-X, and XMM) and epoxy replication are under consideration. Both processes can utilize the same types of mandrels and separation agents. While electroforming can produce substrates that are thin, the high density of the nickel may result in high weight optics for some missions. For convenience, experimentation with replication and coating is being carried out initially on flats. Our replication studies include trials with gold and carbon separation agents. This paper reports on our efforts with epoxy replicated optics.
KEYWORDS: Multilayers, Sputter deposition, X-ray telescopes, Information operations, Hard x-rays, Atomic force microscopy, Space telescopes, X-ray characterization, Nickel, Transmission electron microscopy
The influence of varying the Ar-pressure in the process of depositing Ni/C multilayers by dc-magnetron sputtering has been studied, and atomic force microscopy (AFM) measurements, x-ray characterization results and transmission electron microscopy (TEM) results are presented. Single Ni and C films and Ni/C multilayers were deposited at Ar-pressures of 1.5, 3, 5 and 7 mTorr. The one-dimensional power spectral density data from the AFM measurements clearly indicate that the best densities and thin film qualities for both materials are obtained at lower Ar-pressure, i.e. 1.5 mTorr.
The Hard X-Ray Telescope was selected for study as a possible new intermediate size mission for the early 21st century. Its principal attributes are: (1) multiwavelength observing with a system of focussing telescopes that collectively observe from the UV to over 1 MeV, (2) much higher sensitivity and much better angular resolution in the 10 - 100 keV band, and (3) higher sensitivity for detecting gamma ray lines of known energy in the 100 keV to 1 MeV band. This paper emphasizes the mission aspects of the concept study such as the payload configuration and launch vehicle. An engineering team at the Marshall Space Center is participating in these two key aspects of the study.
Suzanne Romaine, Ricardo Bruni, Anna Clark, William Podgorski, D. Schultz, Daniel Schwartz, Leon Van Speybroeck, Ying Zhou, Robert Hahn, George Johnston, Andrew Longmire, J. Humphreys, Alan Shapiro, R. Tjulander, E. Barinek
The Mission Support Team SAO Reflectivities studies laboratory was responsible for the verification of the coating performance specification during the coating of the eight AXAF flight optics. Prior to the start of the coating of the flight optics, it was necessary to verify the scaleup of the coating chamber parameters from the test chamber to the flight optic coating chamber as well as to verify repeatability of coating quality. Immediately prior to the coating of each flight optic, witness samples were coated to verify the coating specification for each particular geometry. Similar witness samples were coated to verify the coating specification for each particular geometry. Similar witness samples were also coated with each flight optic. An overview of this monitoring program is presented along with a description of how the measurements are made, what tests are used to verify performance and a description of the witness sample deployment. Preliminary data on coating uniformity will also be presented.
One of the specifications used to polish the AXAF witness samples was that the rms surface roughness be <EQ 5 angstrom as measured by optical profilometry. This specification was chosen based on the cost of polishing and the necessity to keep scatter to a minimum. However, it is not necessarily the best indication of the expected performance of the soft x-ray reflectivity of the surfaces. In particular, the reflectivity data from the AXAF flight optic witness samples indicate sample to sample differences of a few percent which do not correlate with the optical profilometry results for these samples. Further investigations were carried out to measure rms surface roughness using atomic force microscopy (AFM). The differences shown by AFM surface roughness measurements correlates to differences found in reflectivity for these same samples. One-dimensional power spectral density data is presented from both AFM and WYKO measurements along with the reflectivity results at 8 keV for the AXAF witness samples. The results indicate that to obtain accurate prediction of x-ray performance it is necessary to look at the scanning probe metrology data provided by the AFM, in addition to the optical profilometry data.
The iridium coating of the AXAF flight optics by Optical Coating Laboratories, Inc. (OCLI) has taken place over the past eight months. During the coating effort, it was necessary to verify the performance of the coatings continually as deposition parameters were changed to accommodate the different geometry of each optic. In addition, quick look reflectivity measurements have been completed for witness samples coated during each run. The minimum reflectivity to be met was 82 percent at 20 arcminutes grazing angle and 50 percent at 34 arcminutes grazing angle. THis can be compared with a theoretical reflectivity, based on the Henke coefficients, of 88 percent and 62 percent at 20 and 34 arcmin respectively. Previous measurements by P. Slane, et al., gave mean values of 84 percent at 20 arcmin and 51 percent at 34 arcmin grazing angle. Measurements reported here were carried out by the SAO reflectivity laboratory, which is part of the AXAF mission support team. The quick look results of both the qualification samples and the production samples are presented along with the test results from the scaleup and verification runs that were used to set the coating parameters.
In recent years there has been an increased interest in the possible use of Ir as the reflecting surface in X-ray telescope programs. An X-ray study of such surfaces produced by sputtering of Ir on highly polished Zerodur flats is presented here. The study was performed using Fe K(alpha) 1 (6.404 Kev) and Cu K(alpha) 1 (8.048 keV) and includes measurement of total external reflection and scattering. The scattering measurement was made with three different instruments arrangements; one employed a 1D position sensitive detector for low resolution studies giving approximately 30 arcsec resolution (FWHM), and the other two arrangements employed channel cut crystals providing resolutions (FWHM) of 5 arcsec and 1 arcsec, respectively at Cu K(alpha) 1. The reflectivity study revealed a very close correspondence with a theoretical model based on recently published optical constants. This important result shows that an Ir coating can be produced with nominal bulk density.
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