Introduction: Emergency department (ED) syncope management is extremely variable. We developed practice recommendations based on the validated Canadian Syncope Risk Score (CSRS) and outpatient cardiac monitoring strategy with physician input. Methods: We used a 2-step approach. Step-1: We pooled data from the derivation and validation prospective cohort studies (with adequate sample size) conducted at 11 Canadian sites (Sep 2010 to Apr 2018). Adults with syncope were enrolled excluding those with serious outcome identified during index ED evaluation. 30-day adjudicated serious outcomes were arrhythmic (arrhythmias, unknown cause of death) and non-arrhythmic (MI, structural heart disease, pulmonary embolism, hemorrhage)]. We compared the serious outcome proportion among risk categories using Cochran-Armitage test. Step-2: We conducted semi-structured interviews using observed risk to develop and refine the recommendations. We used purposive sampling of physicians involved in syncope care at 8 sites from Jun-Dec 2019 until theme saturation was reached. Two independent raters coded interviews using an inductive approach to identify themes; discrepancies were resolved by consensus. Results: Of the 8176 patients (mean age 54, 55% female), 293 (3.6%; 95%CI 3.2-4.0%) experienced 30-day serious outcomes; 0.4% deaths, 2.5% arrhythmic, 1.1% non-arrhythmic outcomes. The serious outcome proportion significantly increased from low to high-risk categories (p < 0.001; overall 0.6% to 27.7%; arrhythmic 0.2% to 17.3%; non-arrhythmic 0.4% to 5.9% respectively). C-statistic was 0.88 (95%CI0.86–0.90). Non-arrhythmia risk per day for the first 2 days was 0.5% for medium-risk, 2% for high-risk and very low thereafter. We recruited 31 physicians (14 ED, 7 cardiologists, 10 hospitalists/internists). 80% of physicians agreed that low risk patients can be discharged without specific follow-up with inconsistencies around length of ED observation. For cardiac monitoring of medium and high-risk, 64% indicated that they don't have access; 56% currently admit high-risk patients and an additional 20% agreed to this recommendation. A deeper exploration led to following refinement: discharge without specific follow-up for low-risk, a shared decision approach for medium-risk and short course of hospitalization for high-risk patients. Conclusion: The recommendations were developed (with online calculator) based on in-depth feedback from key stakeholders to improve uptake during implementation.

A number of laser facilities coming online all over the world promise the capability of high-power laser experiments with shot repetition rates between 1 and 10 Hz. Target availability and technical issues related to the interaction environment could become a bottleneck for the exploitation of such facilities. In this paper, we report on target needs for three different classes of experiments: dynamic compression physics, electron transport and isochoric heating, and laser-driven particle and radiation sources. We also review some of the most challenging issues in target fabrication and high repetition rate operation. Finally, we discuss current target supply strategies and future perspectives to establish a sustainable target provision infrastructure for advanced laser facilities.

With the explosive growth in the number of highly automated powder diffraction systems, many types of analyses which were previously considered a specialty analysis are now performed on a routine basis. Algorithms have been developed for measuring peak profiles from which crystallite sizes, residual microstrain, and X-ray crystal structure (Rietveld techniques for example) can be determined. However, these techniques require an instrumental peak profile calibration standard to correct the experimental data for instrumental broadening due to the system optics.

Significant problems are encountered when laboratories try to cross-correlate or reproduce published data due to the lack of a common reference material for instrumental calibration. This is particularly distressing in microstrain and crystallite size calculations which can be dramatically affected by a poor choice of standard materials. Microstrain and crystallite size measurement are becoming increasingly important for the characterization of advanced materials and catalysts.

An ordered oxygen-deficient tetragonal perovskite compound La1.67Sr0.33Cu205 has been synthesized by solid state reaction. X-ray powder diffraction was used to characterize the material. Unit cell parameters least-squares refined from non-overlapping diffraction peaks are a = 10.8696(9)Å, c = 3.8612(6)Å and V = 456.2(1)Å3. X-ray powder data have been obtained for the experimentally observed peak positions corrected for systematic errors, the relative intensities, values of dexp and the Miller indices of both resolved and overlapping reflections. The experimental diffraction pattern was compared to computer simulated patterns calculated from the neutron crystal structure parameters and the non-oxygen-deficient LaCuO3 compound. The figure of merit is F30 = 33.8 (0.018, 48).

The Ultra-Fast Flash Observatory (UFFO), which will be launched onboard theLomonosov spacecraft, contains two crucial instruments: UFFO BurstAlert & Trigger Telescope (UBAT) for detection and localization of Gamma-Ray Bursts(GRBs) and the fast-response Slewing Mirror Telescope (SMT) designed for the observationof the prompt optical/UV counterparts. Here we discuss the in-space calibrations of theUBAT detector and SMT telescope. After the launch, the observations of the standard X-raysources such as pulsar in Crab nebula will provide data for necessary calibrations ofUBAT. Several standard stars will be used for the photometric calibration of SMT. Thecelestial X-ray sources, e.g. X-ray binaries with bright optical sourcesin their close angular vicinity will serve for the cross-calibration of UBAT and SMT.

The Ultra-Fast Flash Observatory (UFFO) Pathfinder for Gamma-Ray Bursts (GRBs) consistsof two telescopes. The UFFO Burst Alert & Trigger Telescope (UBAT) handles thedetection and localization of GRBs, and the Slewing Mirror Telescope (SMT) conducts themeasurement of the UV/optical afterglow. UBAT is equipped with an X-ray detector, analogand digital signal readout electronics that detects X-rays from GRBs and determines thelocation. SMT is equipped with a stepping motor and the associated electronics to rotatethe slewing mirror targeting the GRBs identified by UBAT. First the slewing mirror pointsto a GRB, then SMT obtains the optical image of the GRB using the intensified CCD and itsreadout electronics. The UFFO Data Acquisition system (UDAQ) is responsible for theoverall function and operation of the observatory and the communication with the satellitemain processor. In this paper we present the design and implementation of the electronicsof UBAT and SMT as well as the architecture and implementation of UDAQ.

One of the unexplored domains in the study of gamma-ray bursts (GRBs) is the early timephase of the optical light curve. We have proposed Ultra-Fast Flash Observatory (UFFO) toaddress this question through extraordinary opportunities presented by a series of smallspace missions. The UFFO is equipped with a fast-response Slewing Mirror Telescope thatuses a rapidly moving mirror or mirror array to redirect the optical beam rather thanslewing the entire spacecraft or telescope to aim the optical instrument at the GRBposition. The UFFO will probe the early optical rise of GRBs with sub-second response, forthe first time, opening a completely new frontier in GRB and transient studies. Its fastresponse measurements of the optical emission of dozens of GRB each year will provideunique probes of the burst mechanism and test the prospect of GRB as a new standardcandle, potentially opening up the z > 10 universe. We describe the current limit inearly photon measurements, the aspects of early photon physics, our soon-to-be-launchedUFFO-pathfinder mission, and our next planned mission, the UFFO-100.

The Slewing Mirror Telescope (SMT) is the UV/optical telescope of UFFO-pathfinder. TheSMT optical system is a Ritchey-Chrétien (RC) telescope of 100 mm diameter pointed bymeans of a gimbal-mounted flat mirror in front of the telescope. The RC telescope has a17 × 17arcmin2 in Field of View and 4.3 arcsec resolution (full width halfmaximum of the point spread function) The beam-steering mirror enables the SMT to access a35 × 35degree region and point and settle within 1 sec. All mirrors were fabricated toabout 0.02 wavelengths RMS in wave front error (WFE) and 84.7% average reflectivity over200 nm ~ 650 nm. The RC telescope was aligned to 0.05 wavelengths RMS in WFE (testwavelength 632.8 nm). In this paper, the technical details of the RC telescope and slewingmirror system assembly, integration, and testing are given shortly, and performance testsof the full SMT optical system are reported.

The UFFO (Ultra-Fast Flash Observatory) is a GRB detector on board the Lomonosovsatellite, to be launched in 2013. The GRB trigger is provided by an X-ray detector,called UBAT (UFFO Burst Alarm & Trigger Telescope), which detects X-rays from the GRBand then triggers to determine the direction of the GRB and then alerts the Slewing MirrorTelescope (SMT) to turn in the direction of the GRB and record the optical photon fluxes.This report details the calibration of the two components: the MAPMTs and the YSO crystalsand simulations of the UBAT. The results shows that this design can observe a GRB within afield of view of ±35° and can trigger in a time scale as short as 0.2 – 1.0 safter the appearance of a GRB X-ray spike.

The Ultra-Fast Flash Observatory (UFFO) is a space observatory for optical follow-ups ofgamma ray bursts (GRBs), aiming to explore the first 60 seconds of GRBs optical emission.UFFO is utilized to catch early optical emissions from GRBs within few sec after triggerusing a Gimbal mirror which redirects the optical path rather than slewing entirespacecraft. We have developed a 15 cm two-axis Gimbal mirror stage for the UFFO-Pathfinderwhich is going to be on board the Lomonosov satellite which is to be launched in 2013. Thestage is designed for fast and accurate motion with given budgets of 3 kg of mass and 3Watt of power. By employing stepping motors, the slewing mirror can rotate faster than 15deg/sec so that objects in the UFFO coverage (60 deg × 60 deg) can be targeted in~1 sec. The obtained targeting resolution is better 2 arcmin using a close-loopcontrol with high precision rotary encoder. In this presentation, we will discuss detailsof design, manufacturing, space qualification tests, as well as performance tests.

The Ultra-Fast Flash Observatory (UFFO) aims to detect the earliest moment of Gamma-RayBursts (GRBs) which is not well known, resulting into the enhancement of GRB mechanismunderstanding. The pathfinder mission was proposed to be a scaled-down version of UFFO,and only contains the UFFO Burst Alert & Trigger Telescope (UBAT) measuring theX-ray/gamma-ray with the wide-field of view and the Slewing Mirror Telescope (SMT) with arapid-response for the UV/optical photons. Once the UBAT detects a GRB candidate with theposition accuracy of 10 arcmin, the SMT steers the UV/optical photons from the candidateto the telescope by the fast rotatable mirror and provides the early UV/optical photonsmeasurements with 4 arcsec accuracy. The SMT has a modified Ritchey-Chrètien telescopewith the aperture size of 10 cm diameter including the rotatable mirror and the imagereadout by the intensified charge-coupled device. There is a key board called the UFFOData Acquisition system (UDAQ) that manages the communication of each telescope and alsoof the satellite and the UFFO overall operation. This pathfinder is designed and builtwithin the limited size and weight of  ~20 kg and the low power consumption up to ~30 W. We will discuss the design and performance of the UFFO-pathfinder, and itsintegration to the Lomonosov satellite.

The crystal structure of type I clathrate Ba8Ni4Ge42 has been determined using neutron powder diffraction, transmission electron microscopy (TEM, for possible superlattice), and extended X-ray absorption fine structure (EXAFS) measurements. Ba8Ni4Ge42 is cubic with the space group Pmn and unit-cell parameter a = 10.6769(2) Å (Dx = 5.988 g cm−3). The structure combines two different types of polyhedra: the dodecahedron (Ge20, 20-atom cage with 12 pentagonal faces) and the tetrakaidecahedron (Ge24, 24-atom cage with 12 pentagonal and 2 hexagonal faces). Each unit cell contains two Ge20 dodecahedra and six Ge24 tetrakaidecahedra. The Ge20 dodecahedra are linked via the interstitial 6c positions. The framework structure is formed by a tetrahedrally bounded network of Ge atoms, whereas Ba atoms reside inside the Ge20 and Ge24 cavities at the 2a and 6d crystallographic positions, respectively. Ni atoms exclusively occupy the 6c positions located on the hexagonal faces of the larger tetrakaidecahedra; no Ni atoms are found in the smaller dodecahedra that consist of pentagonal faces. A local structure study using EXAFS supports the coexistence of Ge and Ni on the 6c site. Electron diffraction in TEM reveals no detectable Ge/Ni ordering.