The Canada.Fraxxe-Hawajj Telescope (GHT) is developing an Adaptive Optics Instrument Adaptor for general use at its 3.6 m telescope. It consists of a 19 electrode, bimcrph deformable mirror (1:6:12) used with a 19 sub-aperture, curvature wavefront sensor. The wavefront sensor optical gain is controlled by the amplitude of a vibrating membrane mirror, which produces a defocus in t1 pupil plane. The tip-tilt correction is accomplished separately from the high order correction by tI f/19.6 reimaging mirror of the adaptor. The optical design minimizes tI number of reflections by using off-axis mirrors. The whole assembly is contained in an aluminium casting 1 10 cm in diameter and 28 cm thick. The adaptive optics control system will provide a 90 Hz servo bandwidth and modal control. The Pegasus user interface will manage overall control of tl system by the observer. This user-friendly interface has been developed at FHT, tl goal being to allow non-specialists in adaptive optics to operate the instrument in an optimal fashion, given the numerous parameters such as: brightness of t.l reference source, iscplanatic angle between reference and scieree sources, speed of atmospheric turbuleixz, wavelength of observation etc. Various imaging detectors or more complex instruments can be mounted on this adaptive optics adaptor. in t1 initial stage, we plan to use a CU) camera and NICMOS (HgCdTe) array for imagery in tl visible and non-tlrmal infrared. An integral field spectrograph will be provided as well The latter will offer a great deal of observing mode flexibility; imagery and/or spectroscopy with various combinations ci spatial and spectral resolution. . PROJECF STATUSThe Canada-Fraixe-Hawajj Telescope has undertaken the development and fabrication of an Adaptive Optics Bxmnette (AOB) for its 3.6 m telescope on top of Mauna Kea (Hawaii). The "bomtte" will be installed at tl f/8 Cassegrain focus of tl telescope. Physically, the bonnette is an adaptor ring 1.1 m in diameter and 28 cm thick on which varions instruments (imagers, spectrographs) can be mounted. It will be a fiity instrument, offering varions backup modes to insure reliability frcxn an operational point of view. The user interface aims at being reasonably straightforward, offering a simple and restricted choice of parameters to tJ user.The design and fabrication tasks are shared between many institutes; the CFHT is managing tl project, issuing the specifications, supervising development and fabrication, performance modelling and realizing the general user interfe. The Dominion Astrophysical Observatory (DAO, Canada) has designed and is fabricating the opto-mechanical bench, and the wavefront sensor assembly (WFS). The optical design is from H. Richardson (U. of Victoria Canada) and DAO is subcontracting the fabrication of the optics to various companies in the US and Canada. The company Laserdot (Marcoussis, France) is providing the deformable mirror and the real-time control system. Laserdot is also providing some high level software tools. The fabrication o...

We present observations of the BL Lac object 1ES 0414+009 in the >200 GeV gamma-ray band by the VERITAS array of Cherenkov telescopes. 1ES 0414+009 was observed by VERITAS between 2008 January and 2011 February, resulting in 56.2 hr of good quality pointed observations. These observations resulted in a detection of 822 events from the source corresponding to a statistical significance of 6.4 standard deviations (6.4σ) above the background. The source flux, showing no evidence for variability, is measured as (5.2 ± 1.1 stat ± 2.6 sys)× 10 −12 photons cm −2 s −1 above 200 GeV, equivalent to approximately 2% of the Crab Nebula flux above this energy. The differential photon spectrum from 230 GeV to 850 GeV is well fit by a power law with a photon index of Γ = 3.4 ± 0.5 stat ± 0.3 sys and a flux normalization of (1.6 ± 0.3 stat ± 0.8 sys) × 10 −11 photons cm −2 s −1 at 300 GeV. We also present multiwavelength results taken in the optical (MDM), x-ray (Swift-XRT), and GeV (Fermi-LAT) bands and use these results to construct a broadband spectral energy distribution (SED). Modeling of this SED indicates that homogenous one-zone leptonic scenarios are not adequate to describe emission from the system, with a lepto-hadronic model providing a better fit to the data.

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