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[en] A third-generation VUV and soft X-ray ring (VSX ring in short) with a low emittance of several nm·rad is being designed at the Institute for Solid State Physics (ISSP) of the University of Tokyo, in close collaboration with the Photon Factory of KEK. The proposal for constructing the light source facility (VSX Light Source) is now in preparation for submission to the government. A brief description is presented on the facility storage ring and injectors as well as a newly organized body for construction and utilization of the facility. (J.P.N.)
[en] Swift is a first-of-its-kind multiwavelength transient observatory for gamma-ray burst astronomy. It has the optimum capabilities for the next breakthroughs in determining the origin of gamma-ray bursts and their afterglows, as well as using bursts to probe the early Universe. Swift will also perform the first sensitive hard X-ray survey of the sky. The mission is being developed by an international collaboration and consists of three instruments, the Burst Alert Telescope (BAT), the X-ray Telescope (XRT), and the Ultraviolet and Optical Telescope (UVOT). The BAT, a wide-field gamma-ray detector, will detect 3-7 gamma-ray bursts per week with a sensitivity 5 times that of BATSE. The sensitive narrow-field XRT and UVOT will be autonomously slewed to the burst location in 20 to 70 seconds to determine 0.3-5.0 arcsec positions and perform optical, UV, and X-ray spectrophotometry. Strong education/public outreach and follow-up programs will help to engage the public and astronomical community. The Swift launch is planned for September 2003
[en] We developed an off-axis-illuminated zone-plate-based hard x-ray Zernike phase-contrast microscope beamline at Pohang Light Source. Owing to condenser optics-free and off-axis illumination, a large field of view was achieved. The pinhole-type Zernike phase plate affords high-contrast images of a cell with minimal artifacts such as the shade-off and halo effects. The setup, including the optics and the alignment, is simple and easy, and allows faster and easier imaging of large bio-samples.
[en] The Hefei Light Source (HLS) is a VUV and soft X-ray synchrotron radiation source. The HLS was offcially put into operation in January 2015 after the upgrade project. The Alarm System is an important part of this upgrade project. This system is developed under BEAST for real-time monitoring equipment status and sending the alarm information to the relevant technical staff. The alarm information is acquired by Alarm Server, which is a component of BEAST. JSP is adopted to implement the alarm query system based on B/S. The way of SMS alarming is implemented by calling the interface of the commercial SMS platform. The way of Email alarming is implemented by calling the Linux mailing command. The operation indicates that the alarm system is configurable and reliable. The alarm system extends the information annunciation methods. The Web of the alarm query and the ways of SMS and Email alarming can effectively help the relevant technical staff deal with the alarm information. (authors)
[en] Intense, quasi-coherent photon pulses with pulse lengths on the order of 10 picoseconds will be available from future high-brilliance synchrotron-radiation sources. Photon energies will span the range from the VUV to soft x-rays
[en] A new type of small-dimensional plasma source with soft X radiation (SXR) concentration allowing one to obtain SXR flux density of up to 106 W/cm2 under the SXR pulse energy density of 15...30 mI/cm2 in 2...4 mm spot in spectral SXR range λ less than (0.9-1.0) nm is developed
[en] We present the general properties of the far-ultraviolet (FUV; 1370-1710 A) continuum background over most of the sky, obtained with the Spectroscopy of Plasma Evolution from Astrophysical Radiation (SPEAR) instrument (also known as FIMS), flown aboard the STSAT-1 satellite mission. We find that the diffuse FUV continuum intensity is well correlated with NHI, 100 μm, and Hα intensities but anti-correlated with soft X-ray intensity. The correlation of the diffuse background with the direct stellar flux is weaker than the correlation with other parameters. The continuum spectra are relatively flat. However, a weak softening of the FUV spectra toward some sight lines, mostly at high Galactic latitudes, is found not only in direct stellar but also in diffuse background spectra. The diffuse background is relatively softer than the direct stellar spectrum. We also find that the diffuse FUV background averaged over the sky has a bit softer spectrum compared to direct stellar radiation. A map of the ratio of 1370-1520 A to 1560-1710 A band intensity shows that the sky is divided into roughly two parts. However, this map shows a lot of patchy structures on small scales. The spatial variation of the hardness ratio seems to be largely determined by the longitudinal distribution of OB-type stars in the Galactic plane. A correlation of the hardness ratio with the FUV intensity is found at high intensities but an anti-correlation is found at low intensities. We also find evidence that the FUV intensity distribution is log-normal in nature.
[en] The monochromator is intended for radiation in the far UV or for soft X-rays. It consists of the following components, successively placed in the direction of the radiation: an entrance slit, a pair of curved mirrors, a disperging grating, a second pair of curved mirrors, and an exit slit. The position of the slits and the curved mirrors is fixed and between the curved mirrors at least one plane mirror is positioned. In the case of one plane mirror the positions of this and the disperging grating can be varied but the angle between their surfaces is fixed. In the case of two plane mirrors, these are coupled so that the rotation of one mirror causes rotation of the other in the opposite direction by the same angle. The grate is positioned between these two mirrors and is moveable parallel to itself in a plane perpendicular to the radiation plane. (Th.P.)