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In this proceeding, we briefly highlight the contributions to the 6th International Symposium on High Energy Gamma-Ray Astronomy that were on behalf of the H.E.S.S. Collaboration, with particular focus given to those results shown publicly for the first time at this symposium. Many of these new results were made possible by the improved capabilities of the H.E.S.S. II telescope array, namely its increased sensitivity to γ-rays and lower energy threshold. Other important results capitalized on the very large datasets accumulated by H.E.S.S. I observations over the last 12 years. Prominent highlights cover a diverse range of topics and astronomical objects: the Galactic center, pulsars, pulsar wind nebulae, shell-type supernova remnants, γ-ray binaries, unidentified sources, flat-spectrum radio quasars, blazars, gamma-ray bursts, fast radio bursts, neutrino event follow-up, and Lorentz invariance violation. [ABSTRACT FROM AUTHOR]

Motivated by the need for megapixel high definition trace element imaging to capture intricate detail in natural material, together with faster acquisition and improved counting statistics in elemental imaging, a large energy-dispersive detector array called Maia has been developed by CSIRO and BNL for SXRF imaging on the XFM beamline at the Australian Synchrotron. A 96 detector prototype demonstrated the capacity of the system for real-time deconvolution of complex spectral data using an embedded implementation of the Dynamic Analysis method and acquiring highly detailed images up to 77 M pixels spanning large areas of complex mineral sample sections. [ABSTRACT FROM AUTHOR]

The H.E.S.S. (High Energy Stereoscopic System) Galactic plane survey (HGPS) was performed with the H.E.S.S. I Cherenkov telescope array in Namibia from 2004 to 2013. In total ~ 2700 hours of high-quality observations of the Galactic plane are available in the Galactic longitude range of 250° to 65° and Galactic latitude range of -3.5° < b < 3.5°. This is the first high-resolution (0.1°) and sensitive (1.5% Crab nebula point-source sensitivity) survey of the Milky Way in TeV gamma-rays. The HGPS has revealed a diverse population of cosmic accelerators in the Galaxy, from which we have compiled a catalog of 78 very-high-energy (E > 0.1 TeV) gamma-ray sources. In this contribution, we will show the latest survey maps, describe the source catalog construction method and further results from the upcoming HGPS paper such as source population statistics and the association of H.E.S.S. sources with known pulsar wind nebulae and highly energetic pulsars, supernova remnants, binary systems and GeV sources detected by the Fermi-LAT. [ABSTRACT FROM AUTHOR]

A hard x-ray micro-nanoprobe has commenced operation at the Australian Synchrotron providing versatile x-ray fluorescence microscopy across an incident energy range from 4 to 25 keV. Two x-ray probes are used to collect μ-XRF and μ-XANES for elemental and chemical microanalysis: a Kirkpatrick-Baez mirror microprobe for micron resolution studies and a Fresnel zone plate nanoprobe capable of 60-nm resolution. Some unique aspects of the beamline design and operation are discussed. An advanced energy dispersive x-ray fluorescence detection scheme named Maia has been developed for the beamline, which enables ultrafast x-ray fluorescence microscopy. [ABSTRACT FROM AUTHOR]

The Maia detector system is engineered for energy dispersive x-ray fluorescence spectroscopy and elemental imaging at photon rates exceeding 107/s, integrated scanning of samples for pixel transit times as small as 50μs and high definition images of 108 pixels and real-time processing of detected events for spectral deconvolution and online display of pure elemental images. The system developed by CSIRO and BNL combines a planar silicon 384 detector array, application-specific integrated circuits for pulse shaping and peak detection and sampling and optical data transmission to an FPGA-based pipelined, parallel processor. This paper describes the system and the underpinning engineering solutions. [ABSTRACT FROM AUTHOR]

This dedicated beamline will provide sub-micron spatial resolution with the highest flux possible and an energy tuning range of 4.7–25 keV using an in-vacuum undulator source. It will combine 2D mapping with μ-XRF, μ-XANES and μ-XAFS for elemental and chemical analysis to solve scientific problems that can only be understood using sub-micron resolutions. The primary beamline design goal is to achieve sub-micron spatial resolution, 100–200 nm, at energy resolutions approaching 1/10000. This spatial resolution will be achieved without a major compromise to the flux, as the beamline will simultaneously achieve detection sensitivities to sub-ppm levels. The beamline will have the flexibility to trade-off one parameter against gains in certain attributes, as dictated by the needs of the application. Fresnel zone plates are intended for the highest resolution applications, while the KB mirrors are shall be used for applications where achromatic focusing and high sensitivity are required. The beamline design will accommodate a diverse range of applications with greatly contrasting sample formats, sample composition and anticipated detector count rates. © 2007 American Institute of Physics [ABSTRACT FROM AUTHOR]