The calibration database implemented for the Chandra X-ray Observatory is the most detailed and extensive CalDB of
its kind to date. Built according to the NASA High Energy Astrophysics Science Archive Research Center (HEASARC)
CalDB prescription, the Chandra CalDB provides indexed, selectable calibration data for detector responses, mirror
effective areas, grating efficiencies, instrument geometries, default source aim points, CCD characteristics, and quantum
efficiencies, among many others. The combined index comprises approximately 500 entries. A standard FTOOLS
parametric interface allows users and tools to access the index. Unique dataset selection requires certain input
calibration parameters such as mission, instrument, detector, UTC date and time, and certain ranged parameter values.
The goals of the HEASARC CalDB design are (1) to separate software upgrades from calibration upgrades, (2) to allow
multi-mission use of analysis software (for missions with a compliant CalDB) and (3) to facilitate the use of multiple
software packages for the same data. While we have been able to meet the multivariate needs of Chandra with the
current CalDB implementation from HEASARC, certain requirements and desirable enhancements have been identified
that raise the prospect of a developmental rewrite of the CalDB system. The explicit goal is to meet Chandra's specific
needs better, but such upgrades may also provide significant advantages to CalDB planning for future missions. In
particular we believe we will introduce important features aiding in the development of mission-independent analysis
software. We report our current plans and progress.
We present optical constants derived from synchrotron reflectance measurements of iridium-coated X-ray witness mirrors over 0.05-12 keV, relevant to the Chandra X-ray Observatory effective area calibration. In particular we present for the first time analysis of measurements taken at the Advanced Light Source Beamline 6.3.2 over 50-1000 eV, Chandra's lower-energy range. Refinements to the currently tabulated iridium optical constants (B. L. Henke et al., At. Data Nucl. Data Tables 54, 181-343, 1993 and on the Web at http://www-cxro.lbl.gov/optical_constants/) will become important as the low-energy calibration of Chandra's X-ray detectors and gratings are further improved, and as possible contaminants on the Chandra mirror assembly are considered in the refinement of the in-flight Ir absorption edge depths. The goal of this work has been to provide an improved tabulation of the Ir optical constants over the full range of Chandra using a self-consistent mirror model, including metallic layers, interface roughness, contaminating overlayer, and substrate. The low-energy data present us with a considerable challenge in the modeling of the overlayer composition, as the K-absorption features of C, O, and N are likely to be present in the ~10A overlayer. The haphazard contamination and chemical shifts may significantly affect optical constants attributed to this overlayer, which will distort the iridium optical constants derived. Furthermore, the witness mirror contamination may be considerably different from that deposited on the flight optics. The more complex modeling required to deal with low-energy effects must reduce to the simpler model applied at the higher energies, which has successfully derived optical constants for iridium in the higher energy range, including the iridium M-edges, already used in the Chandra calibration. We present our current results, and the state of our modeling and analysis, and our approach to a self-consistent tabulation.
We present optical constants derived from synchrotron reflectance measurements of iridium-coated X-ray witness mirrors over 0.05-12 keV, relevant to the Chandra X-ray Observatory effective area calibration. In particular we present for the first time analysis of
measurements taken at the Advanced Light Source Beamline 6.3.2 over 50-1000 eV, Chandra's lower-energy range. Refinements to the currently tabulated iridium optical constants (B. L. Henke et al., At. Data Nucl. Data Tables 54, 181-343, 1993 and on the Web at
http://www-cxro.lbl.gov/optical_constants/) will become important as the low-energy calibration of Chandra's X-ray detectors and gratings are further improved, and as possible contaminants on the Chandra
mirror assembly are considered in the refinement of the in-flight Ir absorption edge depths. The goal of this work has been to provide an improved tabulation of the Ir optical constants over the full range of Chandra using a self-consistent mirror model, including metallic layers, interface roughness, contaminating overlayer, and substrate. The low-energy data present us with a considerable challenge in the modeling of the overlayer composition, as the K-absorption features of C, O, and N are likely to be present in the ~10A overlayer. The haphazard contamination and chemical shifts may significantly affect optical constants attributed to this overlayer, which will distort the iridium optical constants derived. Furthermore, the witness mirror contamination may be considerably different from that deposited on the flight optics. The more complex modeling required to deal with low-energy effects must reduce to the simpler model applied at the higher energies, which has successfully derived optical constants for iridium in the higher energy range, including the iridium M-edges, already used in the Chandra calibration. We present our current results, and the state of our modeling and
analysis, and our approach to a self-consistent tabulation.
The Chandra X-ray Observatory was launched in July 1999, and is returning exquisite sub-arc second X-ray images of star groups, supernova remnants, galaxies, quasars, and clusters of galaxies. In addition to being the premier X-ray observatory in terms of angular and spectral resolution, Chandra is the best calibrated X-ray facility ever flown. We discuss here the calibration of the on-axis effective area of the High Resolution Mirror Assembly. Because we do not know the absolute X-ray flux density of any celestial source, this must be based primarily on ground measurements and on modeling. We use celestial sources which may be assumed to have smoothly varying spectra, such as the BL Lac object Markarian 421, to verify the continuity of the area calibration as a function of energy across the Ir M-edges. We believe the accuracy of the HRMA area calibration is of order 2%.
We report on the use of Na-(beta) alumina crystals in a synchrotron soft x-ray monochromator. With a grating spacing of 22.53 A, Na-(beta) alumina allows coverage of the .6 - 2 keV energy region not available to high resolution Si or Ge crystals. The crystal is shown to have an intrinsic energy resolving power E/(Delta) E of 800 - 1300 in first order with relatively high throughput. Second order (2d equals 11.26 A) is also strong, with a potential resolving power E/(Delta) E of 5000. The refractory nature of the crystal allows it to survive synchrotron heat loading without the damage experienced by organic long grating spacing crystals. The crystal is readily cleaved simplifying fabrication, alignment and mounting. Drawbacks include strong second order harmonics and strong anomalous dispersion effects from Na and Al.
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.
As calibrations of AXAF mirrors in the 2-12 keV range are near completion, we can report that the archive is complete for the scheduled number of mirrors over the 5-12 keV range, and also over the 2010-6200 eV range. Analysis of the results for optical constants and coating layer parameters is now proceeding rapidly. To date, we have derived optical constants from 39 mirrors over 5-12 keV using our existing Fresnel Equation model, with uniform layers of Ir, Cr, and Zerodur, and the roughness algorithm of Nevot and Croce. The analysis method has been presented in our earlier papers, but its application has been expanded to all three varieties of witness mirrors use in AXAF's qualification and production coating runs. For the first and most consistent variety, which have 1 angstrom roughness, reflectances are indistinguishable from mirror to mirror save for thickness variations between coating runs. Residuals of the fits for optical constants become large when reflectance values below 18 percent are included in the fits. If such data points are ignored, values of (delta) (E) and (beta) (E) very much like those of Henke et al. over 5-11 keV are obtained. Residuals are at the 0.6-0.8 percent level, which meets calibration requirements but exceeds experimental noise. For the second variety of witness mirror, polished to obtain roughness specification similar to the flight mirrors, fits approximately within the noise level of the measurements may be obtained over 5-11 keV, for reflectance values down to 5 percent. The (delta) (E) is essentially the same as that obtained from the 1 angstrom flats; however (beta) (E) is higher by approximately 3-4 percent systematically, and the mirror-to-mirror variation is larger. The third variety of mirror was obtained with 5-7 angstrom nominal roughness. Residuals to the fits are large for the entire range of angles, in some case exceeding 2 percent with a sinusoidal character through the critical angle. Coating layer depths are similar to those found for the other mirror types, with good precision. We discuss results along with possible improvements to the model and experiments to verify it.
We discuss the development of beamline U3A at NSLS for AXAF telescope witness mirror reflectivity calibrations in the 1- 2 keV energy range. The beamline was originally constructed as a white light beamline and has been upgraded with the addition of a monochromator to meet the needs of the AXAF calibration program. The beamline consists of an upstream horizontally focussing gold coated elliptical mirror, a differential pumping section, a sample/filter chamber, a monochromator and a downstream filter set. The mirror is set at a 2 degree incident angle for a nominal high energy cutoff at 2 keV. The monochromator is a separated element, scanning, double crystal/multilayer design having low to moderate energy resolution. A fixed exit beam is maintained through the 7-70 degree Bragg angle range by longitudinal translation of the second scanning crystal. Tracking is achieved by computer control of the scan motors with lookup table positioning of the crystal rotary tables. All motors are in vacuum and there are no motional feedthroughs. Several different multilayer or crystal pairs are co-mounted on the monochromator crystal holders and can be exchanged in situ. Currently installed are a W/Si multilayer pair, beryl, and Na-(beta) alumina allowing energy coverage from 180 eV to 2000 eV. Measurements with Na-(beta) alumina and beryl show that beam impurity less than 0.1 percent can be achieved in the 1-2 keV energy range. Measured resolving powers are E/(Delta) E equals 60 for W/Si, 500-800 for (beta) alumina and 1500 to 3000 for beryl. Initial results suggest that signal to noise and beam purity are adequate in the 1-2 keV region to achieve the 1 percent calibration accuracy required by AXAF. This allows overlap of Ir MV edge data taken on x-ray beamline X8A and with low energy data taken on ALS beamline 6.3.2.
The AXAF X-ray mirrors underwent thorough calibration using the X-ray Calibration Facility (XRCF) at the Marshall Space Flight Center in Huntsville, AL from late 1996 to early 1997. The x-ray calibration made novel use of the x-ray continuum from a conventional electron-impact source. Taking advantage of the good spectral resolution of solid-state detectors, continuum measurements proved advantageous in calibration the effective area of AXAF's High-Resolution Mirror Assembly (HRMA) for the entire AXAF energy band. The measurements were made by comparing the spectrum detected by a SSD at the focal plane with the spectrum detected by a beam normalization SSD. The HRMA effective area was calibrated by comparing the measurements with the HRMA raytrace model. The HRMA on-orbit performance predictions are made using the calibration results.
We discuss calibration of the Advanced X-ray Astrophysics Facility (AXAF) high resolution mirror assembly (HRMA) through the use of surrogate coating process witness flats. Reflectance measurements of representative witness flats have been made at the Advanced Light Source (ALS) Synchrotron Facility over an energy range of 60 - 940 eV. We discuss the procedures used for these measurements and some preliminary results of our studies. The initial results show, for some energy regions, a reduction in reflectance expected from a pure iridium coating layer. The observed decrease in mirror reflectance is believed to be the combined result of the presence of an organic thin film on the mirror surfaces, plus the effects of carbon on the ALS beamline optics. It appears that the tested mirror surfaces have a maximum level of molecular contamination amounting to an effective carbon thickness of from 5 - 10 angstroms. The source of this contamination is not identified, although this amount is not surprising.
We report iridium optical constants fitted from synchrotron reflectance data. Specifically, we have used the NKFIT algorithm of D. L. Windt to derive (delta) (E) and (beta) (E) from 2 - 12 keV reflectance calibrations of AXAF witness mirrors. The model is applied at each energy separately, to fit four to nine data points from reflectance-versus-energy scans at selected grazing angles. The stability of the model in the presence of Gaussian noise has been tested extensively. We report the results of several bias studies, involving the generation and analysis of artificial data. Bias studies have been used to determine the optimal grazing angles to be scanned in the various x-ray energy ranges to condition the optical constants. They have also been used to investigate the effects of individual errant data points on the resulting fits and derived optical constants. The results will aid in eliminating systematic errors in the derived optical constants. We also present results of our investigation of the Debye-Waller and Nevot-Croce roughness correction algorithms as applied to our measurements. The Nevot-Croce method gives a much better representation of the data, however its rigorous justification in this experiment is lacking, and the roughness parameter derived is not constant with energy. A more self- consistent model for roughness correction is sought.
We have completed another full year of reflectance calibrations of AXAF witness mirrors at the National Synchrotron Light Source. At the NSLS, we have used beamlines X8C (5 - 12 keV) and X8A (2 - 6 keV), sponsored by Los Alamos National Laboratory. All of the flats have been calibrated in the 5 - 12 keV range, and approximately 1/4 of all our flats have been calibrated in the 2 - 6.2 keV range. The repeatability in the coating processes reported in Denver has continued with the measurement of additional mirrors. Optical constants from reflectances have been derived for six of the eight AXAF mirror elements, and a degree of spatial uniformity information exists for three of these six. The addition of a semitransparent monitor has markedly increased efficiency of measurements in the 5 - 12 keV range, and efforts are being made to provide such a monitor detector for the lower energy ranges. We report the progress in reflectance data acquisition and optical constant derivations, and discuss implications of the results for the AXAF program.
In order to characterize the instrumentation on AXAF, each of the science instrument teams carries out sub-assembly calibrations. For the high energy transmission grating (HETG) group, this means individual measurements of the diffraction efficiencies of each of the 336 grating elements that goes into the completed HETG assembly. Measurements are made at a number of energies (corresponding to x-ray emission lines) which fix the parameters of a model. This model is determined from first principles and verified by extensively testing sample grating elements at synchrotron radiation facilities. Here we present new synchrotron radiation (SR) data obtained at the national Synchrotron Light Source (NSLS) and at the radiometry laboratory of the Physikalisch-Technische Bundesanstalt (PTB) using the electron storage ring BESSY in Berlin. The gratings are from AXAF flight lots, and we apply an improved data reduction technique which builds on our experience from last year (Markert et al., SPIE Proceedings 2518, 424, 1995). Our analysis takes into account the effects of small extended wings in the diffraction of the various orders in the NSLS data. Our goal is to obtain efficiencies in the 0th and plus/minus 1st diffraction orders which are accurate in the 1% level, except near absorption edges, where accuracies in the 5% to 10% level are required. With a few exceptions (discussed here) our new data/improved model meets these goals.
Measurements of the transmission properties of the AXAF CCD imaging spectrometer (ACIS) UV/optical blocking filters were performed at the National Synchrotron Light Source at Brookhaven Laboratories. The X-ray transmissions of two Al:Si/LEXAN/Al:Si three layer filters were measured between 260 and 3000 eV. The main purpose of the calibration was to determine a model transmission function with an accuracy of better than 1 percent. We present results from fits of model transmission functions to the measured x-ray transmission data. Detailed fine energy scans above the Al-K and C-K absorption edges revealed the presence of fine oscillations of the x-ray transmission. These features are most likely extended x-ray absorption fine structures (EXAFS). The amplitude of the EXAFS oscillations above the Al absorption edge is about 5 percent of the mean value of the x-ray transmission. EXAFS theory predicts a temperature dependence on the amplitude of the EXAFS oscillations. This dependence arises from the fact that thermal vibrations of the atoms in a solid produce a phase mismatch of the backscattered electron wave function. Since the ACIS filters will be at a much lower temperature on orbit we provide a prediction of the EXAFS component for the expected on orbit temperature of the ACIS filters.
For the best flexibility in ground and on-orbit calibration modeling of the AXAF telescope over its entire field of view, including off-axis calibration evaluations, AXAF synchrotron reflectance calibrations require that the measured reflectance data be reduced to optical parameters analogous to n and k. We have developed a method for AXAF witness mirror analysis which is a modification of the NKFIT optical constants algorithm published by D.L. Windt. The algorithm assumes uniform layer thicknesses using a recursive, exact formation of Fresnel's equations, with a modified Debye-Waller roughness correction factor. The recursion formula has been modified to include an explicit double-precision formulation. The results of most of the fits of AXAF calibration measurements yield residuals less than 1 percent of the reflectance value levels down to R approximately .03. The precision of the measurements is smaller still, which compromises the (chi) 2 fitting algorithm; however, the results will most likely prove adequate for AXAF witness mirrors calibrated in the 5-12 keV range. Coating density determined from the refractive index n is approximately 98.5 percent of the bulk for iridium. Derived coating thicknesses are extremely consistent with the photon energy, giving still more significant calibration information to the program.
For the past six years, a high-accuracy reflectance calibration system has been under development at the National Synchrotron Light Source at Brookhaven National Laboratory. The system utilizes Los Alamos National Laboratory's Beamlines X8A and X8C. Its purpose is to calibrate the reflection efficiencies of witness coupons associated with the coating of the eight mirror elements composing the High Resolution Mirror Assembly for NASA's Advanced X-ray Astrophysics Facility (AXAF). During the past year, measurements of reflectances of numerous iridium- coated witness flat mirrors have been obtained to a relative statistical precision of 0.4 percent, and an overall repeatability within 0.8 percent in the overlapping energy regions. The coating processes are strikingly repeatable, with reflectances in the 5-10 keV range for off-end witness flats nearly always being within 1 percent of one another, excluding interference fringes. The comparison reflectances between flats obtained from qualification coating runs and production runs of the Wolter Type I mirror elements are in turn nearly equal, indicating that the qualification run witness flats provide a good representation of the flight optics. Results will produce a calibration of AXAF with extremely good energy detail over the 2-12 keV range, which includes details of the M-absorption edge region for Ir. Development of the program to cover 0.05-2 keV continues.
Precise transmission measurements of free standing iridium foils and of iridium coatings supported on thin polyimide film have been made at the X8 beamline of the National Synchrotron Light Source, at energies from 2 to 12 keV. These measurements were conducted to provide iridium optical constants in support of NASA's Advanced X-ray Astrophysics Facility (AXAF). Transmission data were collected at small energy increments across iridium M and L absorption edges to study detailed edge structures. From these data, the imaginary components of the index of refraction were computed. The data also allows computation of the real parts, using the Kramers-Kronig dispersion integral. Preliminary results indicate a measurement accuracy of better than one percent for transmission. Absorption coefficients deviate by varying amounts from values predicted from Henke data table, which is consistent with the accuracy claimed for those table.s Nonuniform thickness in our iridium foils may be a source of errors in our analysis and improved foils are being sought. Additional measurements will also be needed with foils of different thickness to account and correct for possible effects of sample thickness on the determination of absorption edge fine structure. To our knowledge, transmission measurements of this degree of accuracy and precision have not been previously reported in the literature for iridium in the 2- 12 keV energy range.
The high energy transmission grating spectrometer (HETGS) for the Advanced X-ray Astrophysics Facility (AXAF) uses transmission gratings of period 2000 and 4000 angstrom to diffract x rays in the energy range 400 - 9000 eV. The gratings are so-called phased gratings, where the phase shift of x rays through the grating bars causes constructive interference at some wavelengths, thereby increasing the efficiency (in first order) to a level higher than would be expected for an opaque grating. AXAF has a program goal of calibrating the efficiencies (or effective areas) of the various spectrometers and imaging detectors (including the contribution of the x-ray mirrors) to an accuracy of a few percent. The HETGS group has elected to attempt a calibration at the sub-assembly level (i.e., the grating elements only, independent of the detectors and mirrors) at the 1% level. Since it is impossible (in practice) to measure grating efficiencies for all of the AXAF grating elements (336 elements in the flight assembly) at all energies, we have chosen instead to develop a model of the diffraction efficiency in all orders, and determine the parameters of the model by measuring the diffraction efficiencies at a few x ray energies. We verify the model by detailed studies of a few gratings made at the National Synchrotron Light Source. To date, we believe that we have an HETG model which is nearly accurate enough in the range 2200 - 9000 eV. At the lower energies of interest (400 eV - 2200 eV), however, the best fit grating model deviates from the synchrotron data by more than a few percent on average. In this paper we describe the model, the synchrotron tests that verify it, the discrepancies that we find at lower energies, and our plan to resolve the problems.
We have completed extensive synchrotron reflectivity measurements on several iridium mirrors which were intentionally coated with thin layers (100 angstroms or less) of polyethylene, a hydrocarbon contaminant. The purpose was to verify theoretical predictions of alterations in reflection efficiency of an iridium surface for various thicknesses of hydrocarbon contamination, and to evaluate the acceptability of attainable upper limits of such contamination for the mirrors aboard NASA's Advanced X-ray Astrophysics Facility (AXAF). Although the deposition of such thin layers is problematic with no systematic guarantee of uniform thickness or density, successful analysis by modeling the contaminant as a uniform surface layer may be done, within a limited X-ray energy range. The M-edges of iridium are significantly affected by the polyethylene layers. For the most part, contamination increases the reflectance in the M-edge range over that of bare iridium, although cross-over points between contaminated and uncontaminated mirrors occur at several angles relevant to AXAF. However, calibratability of the reflectance is a more significant issue than X-ray mirror efficiency. We present the modeling results for three thicknesses of polyethylene, and discuss the implications for the performance of AXAF mirrors and their calibratability.
As part of the calibration for the High Energy Transmission Grating Spectrometer (HETGS) on AXAF, we conducted several studies at synchrotrons in an effort to measure the resolving power and the quantum efficiency of gratings over a range of x- ray energies. Gratings that have been thoroughly studied can be used as calibration transfer standards at MIT to evaluate the quality and repeatability of our testing procedures. Synchrotron studies also enable us to evaluate our theoretical prediction of grating performance and thereby obtain a more accurate model of the gratings. In this paper we discuss studies made of 0.2 micrometers and 0.4 micrometers period gratings with gold grating bars supported by thin polyimide films. The goal of this experiment was to measure and accurately model the efficiencies of several grating facets over much of the energy range for which they would be used in space. Our tests were performed in January and July of 1994 at the National Synchrotron Light Source at Brookhaven National Laboratory. We used beam line X8A to illuminate sample gratings that were inserted in the UC/SAO Reflectometer Test Station (the same device that is used to study witness samples for the AXAF mirrors). A double crystal monochromator was used to select narrow energy bands over the range 0.6-6 keV. We measured the diffraction efficiencies as a function of energy for the first order x-rays. Results are in good agreement with predicted efficiencies calculated using gold optical constants that we recently measured, and confirm the energy shift of the MIV and MV edges from the standard values, as measured by Blake et al. (J. X-ray Sci. Technol., in press).
The Advanced X-ray Astrophysics Facility (AXAF) is one of NASA's 'great observatories' (launch 1998). One of its two focal plane detectors is the High Resolution Camera (HRC) assembly consisting of two microchannel Plate (MCP) based detectors. Key components of the two HRC detectors are UV/Ion shields consisting of metalized sub-micron plastic membranes, designed to prevent UV light and positive ions from reaching the detectors' sensitive surfaces. We discuss results from transmission measurements that have been conducted at the National Synchrotron Light Source (NSLS), on sample plastic membranes and the baseline design HRC-I UV/Ion shield.
Improved mirror reflectivity measurement techniques have been introduced to permit more accurate determinations of optical constants delta and beta in the complex index of refraction n = 1 - delta - i(beta) over the energy range 50 to 5000 eV. When the density has been determined by X-ray or other means, one can calculate the real and imaginary parts, f-prime and f-double prime, of the complex atomic scattering factor f = f(o) + f-prime + if-double prime from delta and beta. Preliminary results are given for the Ni LIII edge around 852 eV, and the Au M edge region from 2150 to 3500 eV. Since these are the first experimental evaluations of delta for these element edges, they are compared with appropriate reservations to semiempirical tabulations. There is much potential for this technique applied to synchrotron sources.
We are developing a system to calibrate reflectances of witness coupons to the AXAF flight mirrors at the National Synchrotron Light Source over the 0.05-12 keV energy range. These witness coupons will be coated in the same process as the AXAF mirror elements. One of the key issues is the accurate determination of mirror efficiencies across the absorption edges of the mirror coating elements. We present a series of reflectance measurements with 2 eV resolution of a nickel-coated flat mirror in the region of the Ni L-II (870 eV) and L-III (853 eV) absorption edges. Scans of reflectance versus grazing angle at fixed energies in this region show distinct interference fringes at grazing angles larger than the critical angle which are extinguished as the photon energy is increased beyond the low point of the L-III edge, indicating total absorption of the evanescent wave within the Ni film. At 51 arc minutes grazing angle, measured reflectance decreases smoothly by 35 percent and then recovers in an 8 eV band at the L-III edge. We have also measured reflectances in the M absorption edge region for gold, platinum, and iridium coated mirrors. We derive optical parameters n and k specific to the film for comparison to the existing data tables.
The study measures the X-ray reflectivity of the AXAF VETA-I optic and compares it with theoretical predictions. Measurements made at energies of 0.28, 0.9, 1.5, 2.1, and 2.3 keV are compared with predictions based on ray trace calculations. Results on the variation of the reflectivity with energy as well as the absolute value of the reflectivity are presented. A synchrotron reflectivity measurement with a high-energy resolution over the range 0.26 to 1.8 keV on a flat Zerodur sample is also reported. Evidence is found for contamination of the flat by a thin layer of carbon on the surface, and the possibility of alteration of the surface composition of the VETA-I mirror, perhaps by the polishing technique. The overall agreement between the measured and calculated effective area of VETA-I is between 2.6 and 10 percent. Measurements at individual energies deviate from the best-fitting calculation to 0.3 to 0.8 percent, averaging 0.6 percent at energies below the high energy cutoff of the mirror reflectivity, and are as high as 20.7 percent at the cutoff.
The 1-percent calibration accuracy goal of the Advanced X-ray Astrophysics Facility is being approached by way of an experiment at the National Synchrotron Light Source that will demonstrate the accuracy achievable in reflectance measurements conducted on coated flat mirrors in the 50 eV-12 keV energy range. The coatings will be of commercially produced Au, Ni, and Ir, deposited either by sputtering or by e-beam deposition. Optical constants will be estimated via the reflectance vs. angle-of-incidence method.
The reflectivity versus angle for a variety of molybdenum mirrors has been measured for both hard and soft x rays in an attempt to deduce any variation in performance between single crystal, polycrystalline, and evaporated mirrors. A fitting technique has been used to arrive at the roughness of the mirrors. An approach to utilize such measurements to characterize mirrors and derive low energy optical constants for many elements is outlined.
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