Unlocking the Capabilities of Future High-Resolution X-ray Spectroscopy Missions Through Laboratory Astrophysics (original) (raw)
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Laboratory Astrophysics Needs for X-ray Grating Spectrometers
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The current generation of X-ray grating spectrometers on Chandra and XMM-Newton has modest sensitivity, largely due to a combination of modest resolution (typically 300-1000) and low efficiency (≲ 10%). The next generation of X-ray gratings, however, has already demonstrated far higher resolution and efficiency, capabilities that will transform the field. These gratings are planned for use on Explorers, Probes, and Flagship missions, so the time is right to prepare for the high-quality spectral data that will be returned by these missions. The highest-resolution grating data available, from the Chandra gratings, have already shown the limitations of existing atomic data for modeling; improvements are needed in laboratory measurements of wavelengths, radiative and collisional transition rates, as well as ionization and recombination crosssections. To prepare for these proposed missions, significant progress needs to be made in understanding the theoretical atomic physics as well. This white paper, in concert with a paper focusing on microcalorimeter missions, will summarize the work that has been done thus far in the field of laboratory X-ray astrophysics, with the goal of identifying the most critical tasks that are still outstanding. This includes tracing science requirements from missions such as Arcus, XGS-P, and Lynx and identifying the laboratory measurements needed to achieve them. We discuss long-term methods to prioritize these needs, along with our initial assessments, and indicate new facilities that will be required.
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A multi-faceted, multi-institutional laboratory astrophysics program is carried out at the Livermore electron beam ion trap facility, which is a mature spectroscopic source with unsurpassed controls and capabilities, and an unparalleled assortment of spectroscopic equipment, including a full complement of grating and crystal spectrometers and a 6x6 micro-calorimeter array. Recent results range from the calibration of x-ray diagnostics, including the Fe XVII and Fe XXV emission lines, extensive lists of L-shell ions, the first laboratory simulation and fit of a cometary x-ray emission spectrum, and the discovery of new spectral diagnostics for measuring magnetic field strengths.
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We present a new technique for determining the quantity and composition of dust in astrophysical environments using < 6 keV X-rays. We argue that high resolution X-ray spectra as enabled by the Chandra and XMM-Newton gratings should be considered a powerful and viable new resource for delving into a relatively unexplored regime for directly determining dust properties: composition, quantity, and distribution. We present initial cross-section measurements of astrophysically likely iron-based dust candidates taken at the Lawrence Berkeley National Laboratory Advanced Light Source synchrotron beamline, as an illustrative tool for the formulation of our technique for determining the quantify and composition of interstellar dust with X-rays. (Cross sections for the materials presented here will be made available for astrophysical modelling in the near future.) Focused at the 700 eV Fe L III and L II photoelectric edges, we discuss a technique for modeling dust properties in the soft X-rays using L-edge data, to complement K-edge X-ray absorption fine structure analysis techniques discussed in . This is intended to be a techniques paper of interest and usefulness to both condensed matter experimentalists and astrophysicists. For the experimentalists, we offer a new prescription for normalizing relatively low S/N L-edge cross section measurements. For astrophysics interests, we discuss the use of X-ray absorption spectra for determining dust composition in cold and ionized astrophysical environments, and a new method for determining speciesspecific gas-to-dust ratios. Possible astrophysical applications of interest, including relevance to Sagittarius A * are offered. Prospects for improving on this work in future X-ray missions with higher throughput and spectral resolution are also presented in the context of spectral resolution goals for gratings and calorimeters, -3for proposed and planned missions such as Astro-H and the International X-ray Observatory.
XEUS: The x-ray evolving universe spectroscopy mission
Space Telescopes and Instrumentation II: Ultraviolet to Gamma Ray, 2006
XEUS is the potential successor to ESA's XMM-Newton X-ray observatory and is being proposed in response to the Cosmic Vision 2015-2025 long term plan for ESA's Science Programme. Novel light-weight optics with an effective area of 5 m 2 at 1 keV and 2 m 2 at 7 keV and 2-5" HEW spatial resolution together with advanced detectors will provide much improved imaging, spectroscopic and timing performances and open new vistas in X-ray astronomy in the post 2015 timeframe. XEUS will allow the study of the birth, growth and spin of the super-massive black holes in early AGN, allow the cosmic feedback between galaxies and their environment to be investigated through the study of inflows and outflows and relativistic acceleration and allow the growth of large scale structures and metal synthesis to be probed using the hot X-ray emitting gas in clusters of galaxies and the warm/hot filamentary structures observable with X-ray absorption spectroscopy. High time resolution studies will allow the Equation of State of supra-nuclear material in neutron stars to be constrained. These science goals set very demanding requirements on the mission design which is based on two formation flying spacecraft launched to the second Earth-Sun Lagrangian point by an Ariane V ECA. One spacecraft will contain the novel high performance optics while the other, separated by the 35 m focal length, will contain narrow and wide field imaging spectrometers and other specialized instruments.
Status of x-ray imaging and spectroscopy mission (XRISM)
Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray, 2020
The X-Ray Imaging and Spectroscopy Mission (XRISM) is the successor to the 2016 Hitomi mission that ended prematurely. Like Hitomi, the primary science goals are to examine astrophysical problems with precise highresolution X-ray spectroscopy. XRISM promises to discover new horizons in X-ray astronomy. XRISM carries a 6 x 6 pixelized X-ray micro-calorimeter on the focal plane of an X-ray mirror assembly and a co-aligned X-ray CCD camera that covers the same energy band over a large field of view. XRISM utilizes Hitomi heritage, but all designs were reviewed. The attitude and orbit control system were improved in hardware and software. The number of star sensors were increased from two to three to improve coverage and robustness in onboard attitude determination and to obtain a wider field of view sun sensor. The fault detection, isolation, and reconfiguration (FDIR) system was carefully examined and reconfigured. Together with a planned increase of ground support stations, the survivability of the spacecraft is significantly improved.
High-Resolution X-ray Spectroscopy of the Interstellar Medium
2010
Aims. The interstellar medium (ISM) has a multiphase structure characterized by gas, dust and molecules. The gas can be found in different charge states: neutral, low-ionized (warm) and high-ionized (hot). It is possible to probe the multiphase ISM through the observation of its absorption lines and edges in the X-ray spectra of background sources. Methods. We present a high-quality RGS spectrum of the low-mass X-ray binary GS 1826−238 with an unprecedent detailed treatment of the absorption features due to the dust and both the neutral and ionized gas of the ISM. We constrain the column density ratios within the different phases of the ISM and measure the abundances of elements such as O, Ne, Fe and Mg. Results. We found significant deviations from the proto-Solar abundances: oxygen is over-abundant by a factor 1.23 ± 0.05, neon 1.75 ± 0.11, iron 1.37 ± 0.17 and magnesium 2.45 ± 0.35. The abundances are consistent with the measured metallicity gradient in our Galaxy: the ISM appears to be metal-rich in the inner regions. The spectrum also shows the presence of warm/hot ionized gas. The gas column has a total ionization degree less than 10%. We also show that dust plays an important role as expected from the position of GS 1826−238: most iron appears to be bound in dust grains, while 10−40% of oxygen consists of a mixture of dust and molecules.
O ct 2 01 2 The ASTRO-H X-ray Observatory
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The joint JAXA/NASA ASTRO-H mission is the sixth in a series of highly successful X-ray missions initiated by the Institute of Space and Astronautical Science (ISAS). ASTRO-H will investigate the physics of the high-energy universe via a suite of four instruments, covering a very wide energy range, from 0.3 keV to 600 keV. These instruments include a high-resolution, high-throughput spectrometer sensitive over 0.3-2 keV with high spectral resolution of Delta E < 7 eV, enabled by a micro-calorimeter array located in the focal plane of thin-foil X-ray optics; hard X-ray imaging spectrometers covering 5-80 keV, located in the focal plane of multilayer-coated, focusing hard X-ray mirrors; a wide-field imaging spectrometer sensitive over 0.4-12 keV, with an X-ray CCD camera in the focal plane of a soft X-ray telescope; and a non-focusing Compton-camera type soft gamma-ray detector, sensitive in the 40-600 keV band. The simultaneous broad bandpass, coupled with high spectral resolution...