The first atmospheric Cherenkov telescope of VERITAS (the Very Energetic Radiation Imaging Telescope Array System) has been in operation since February 2005. We present here a technical description of the instrument and a summary of its performance. The calibration methods are described, along with the results of Monte Carlo simulations of the telescope and comparisons between real and simulated data. The analysis of TeV γ-ray observations of the Crab Nebula, including the reconstructed energy spectrum, is shown to give results consistent with earlier measurements. The telescope is operating as expected and has met or exceeded all design specifications.

LS I +61 303 is one of only a few high-mass X-ray binaries currently detected at high significance in very high energy -rays. The system was observed over several orbital cycles (between 2006 September and 2007 February) with the VERITAS array of imaging air Cerenkov telescopes. A signal of -rays with energies above 300 GeV is found with a statistical significance of 8.4 standard deviations. The detected flux is measured to be strongly variable; the maximum flux is found during most orbital cycles at apastron. The energy spectrum for the period of maximum emission can be characterized by a power law with a photon index of À ¼ 2:40 AE 0:16 stat AE 0:2 sys and a flux above 300 GeV corresponding to 15%-20% of the flux from the Crab Nebula.

We report the detection of pulsed gamma rays from the Crab pulsar at energies above 100 giga-electron volts (GeV) with the Very Energetic Radiation Imaging Telescope Array System (VERITAS) array of atmospheric Cherenkov telescopes. The detection cannot be explained on the basis of current pulsar models. The photon spectrum of pulsed emission between 100 mega-electron volts and 400 GeV is described by a broken power law that is statistically preferred over a power law with an exponential cutoff. It is unlikely that the observation can be explained by invoking curvature radiation as the origin of the observed gamma rays above 100 GeV. Our findings require that these gamma rays be produced more than 10 stellar radii from the neutron star.

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This paper reports on our experience with the implementation of the Real-time Specification for Java on the Ovm open source Java virtual machine. We describe the architecture and main design decisions involved in implementing real-time Java on Ovm. We present the first use of Real-time Java in avionics in the context of control software for a ScanEagle Unmanned Aerial Vehicle.

The intermediate-frequency peaked BL Lacertae (IBL) object 3C 66A is detected during [2007][2008] in VHE (very high energy; E > 100 GeV) γ rays with the VERITAS stereoscopic array of imaging atmospheric Cherenkov telescopes. An excess of 1791 events is detected, corresponding to a significance of 21.2 standard deviations (σ ), in these observations (32.8 hr live time). The observed integral flux above 200 GeV is 6% of the Crab Nebula's flux and shows evidence for variability on the timescale of days. The measured energy spectrum is characterized by a soft power law with photon index Γ = 4.1 ± 0.4 stat ± 0.6 sys . The radio galaxy 3C 66B is excluded as a possible source of the VHE emission.

SUMMARYJava is becoming a viable platform for real-time computing. There are production and research realtime Java VMs, as well as applications in both the military and civil sectors. Technological advances and increased adoption of real-time Java contrast significantly with the lack of benchmarks. Existing benchmarks are either synthetic micro-benchmarks, or proprietary, making it difficult to independently verify and repeat reported results. This paper presents the CD x benchmark, a family of open-source implementations of the same application that target different real-time virtual machines. CD x is, at its core, a real-time benchmark with a single periodic task, which implements an idealized aircraft collision detection algorithm. The benchmark can be configured to use different sets of real-time features and comes with a number of workloads. It can be run on standard Java virtual machines, on real-time and Safety Critical Java virtual machine, and a C version is provided to compare with native performance.

Max Wertheimer (1880-1943), the founder of the Gestalt School of Psychology, published a monograph on the perception of apparent motion in 1912, which initiated a new direction for a great deal of subsequent perceptual theory and research. Wertheimer's research was inspired by a serendipitous observation of a pure apparent movement, which he called the phi-phenomenon to distinguish it from optimal apparent movement (beta), which resembles real movement. Wertheimer called his novel observation 'pure' because it was perceived in the absence of any object being seen to change its position in space. The phi-phenomenon, as well as the best conditions for seeing it, were not described clearly in this monograph, leading to considerable subsequent confusion about its appearance and occurrence. We review the history leading to the discovery of the phi-phenomenon, and then describe: (i) a likely source for the confusion evident in most contemporary research on the phi-phenomenon; (ii) the best conditions for seeing the phi-phenomenon; (iii) new conditions that provide a particularly vivid phi-phenomenon; and (iv) two lines of thought that may provide explanations of the phi-phenomenon and also distinguish phi from beta.