Very-High Energy (VHE) gamma-ray astroparticle physics is a relatively young field, and observations over the past decade have surprisingly revealed almost two hundred VHE emitters which appear to act as cosmic particle accelerators. These sources are an important component of the Universe, influencing the evolution of stars and galaxies. At the same time, they also act as a probe of physics in the most extreme environments known -such as in supernova explosions, and around or after the merging of black holes and neutron stars. However, the existing experiments have provided exciting glimpses, but often falling short of supplying the full answer. A deeper understanding of the TeV sky requires a significant improvement in sensitivity at TeV energies, a wider energy coverage from tens of GeV to hundreds of TeV and a much better angular and energy resolution with respect to the currently running facilities. The next generation gamma-ray observatory, the Cherenkov Telescope Array Observatory (CTAO), is the answer to this need. In this talk I will present this upcoming observatory from its design to the construction, and its potential science exploitation. CTAO will allow the entire astronomical community to explore a new discovery space that will likely lead to paradigm-changing breakthroughs. In particular, CTA has an unprecedented sensitivity to short (sub-minute) timescale phenomena, placing it as a key instrument in the future of multi-messenger and multi-wavelength time domain astronomy. I will conclude the talk presenting the first scientific results obtained by the LST-1, the prototype of one CTA telescope type -the Large Sized Telescope, that is currently under commission.
We present results from simulations of the extragalactic polarized sky at 1.4 GHz. As the basis for our polarization models, we use a semi-empirical simulation of the extragalactic total intensity (Stokes I) continuum sky developed at the University of Oxford (http://scubed.physics.ox.ac.uk) under the European SKA Design Study (SKADS) initiative, and polarization distributions derived from analysis of polarization observations. By considering a luminosity dependence for the polarization of AGN, we are able to fit the 1.4 GHz polarized source counts derived from the NVSS and the DRAO ELAIS N1 deep field survey down to approximately 1 mJy. This trend is confirmed by analysis of the polarization of a complete sample of bright AGN. We are unable to fit the additional flattening of the polarized source counts from the deepest observations of the ELAIS N1 survey, which go down to ∼ 0.5 mJy. Below 1 mJy in Stokes I at 1.4 GHz, starforming galaxies become an increasingly important fraction of all radio sources. We use a spiral galaxy integrated polarization model to make realistic predictions of the number of polarized sources at µJy levels in polarized flux density and hence, realistic predictions of what the next generation radio telescopes such as ASKAP, other SKA pathfinders and the SKA itself will see.
The planned upgrade of the LHC to the High-Luminosity-LHC will push the luminosity limits above the original design values. Since the current detectors will not be able to cope with this environment ATLAS and CMS are doing research to find more radiation tolerant technologies for their innermost tracking layers. Chemical Vapour Deposition (CVD) diamond is an excellent candidate for this purpose. Detectors out of this material are already established in the highest irradiation regimes for the beam condition monitors at LHC. The RD42 collaboration is leading an effort to use CVD diamonds also as sensor material for the future tracking detectors. The signal behaviour of highly irradiated diamonds is presented as well as the recent study of the signal dependence on incident particle flux. There is also a recent development towards 3D detectors and especially 3D detectors with a pixel readout based on diamond sensors.
important resource for the international research community. Currently there are two operational undulator beamlines: 24ID-C-fully tunable in the energy range from 6 to 22keV (cover most element edges for phasing) and 24ID-E-fixed energy at ~12.66keV (optimized for Se SAD experiments). These operational beamlines are currently open to NE-CAT members and general APS users. Both undulator beamlines are fully equipped with state-of-theart instrumentation for its users. MD2 microdiffractometers installed at both the beamlines provide very clean beams from 5 microns to 100 microns in diameter and have exceptional sample visualization systems capable of visualizing micron-sized crystals with extreme clarity. Large-area CCD-based ADSC Quantum 315 detectors at both beamlines not only provide the best diffraction data, but also make it possible to resolve large unit cell dimensions. Both beamlines are equipped with ALS style robotic sample mounting systems, thereby making screening of large numbers of crystals much faster and less effort intensive. A new software suite RAPD provides data collection strategies and quasi-real time data integration and scaling through 128 core computing cluster. A simple automated MR/SAD pipeline for rapid structure solution is implemented. Users of the beamlines are supported by experienced resident crystallographers and have access to a full suite of data processing and structure analysis. A fully equipped chemistry laboratory and cold-room are also available for users. NE-CAT facility is used to focus on NE-CAT research on structural studies involving technically challenging crystallographic projects. In order to meet these needs several novel hardware and software ideas are implemented. A summary of beamline capabilities, technology, scientific highlights and details of availability will be presented. NE-CAT maintains a website at http://necat.chem.cornell.edu/.
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