The drive beam pulse compression system for the CLIC RF power source

The Compact LInear Collider (CLIC) is a high energy (0.5 to 5 TeV) e ± linear collider that uses a high- current electron beam (the drive beam) for 30 GHz RF power production by the Two-Beam Acceleration (TBA) method. Recently, a new cost­effective and efficient generation scheme for the drive beam has been developed. A fully­loaded normal­conducting linac operating at lower frequency (937 MHz) generates and accelerates the drive beam bunches, and a compression system composed of a delay­line and two combiner rings produces the proper drive beam time structure for RF power generation in the drive beam decelerator. In this paper, a preliminary design of the whole compression system is presented. In particular, the fundamental issue of preserving the bunch quality along the complex is studied and its impact on the beam parameters and on the various system components is assessed. A first design of the rings and delay­line lattice, including path length tuning chicanes, injection and extraction regions is also presented together with the simulation results of the beam longitudinal dynamics

Overview of CLIC and CTF3

The CLIC study aims at the design of a high-energy (0.5-5 TeV), high luminosity e+e- linear collider, as a possible facility for the post-LHC era. The beams are accelerated using high-frequency (30 GHz) normal-conducting structures operating at high accelerating gradients to reduce the length and, in consequence, the cost of the linac. The RF power for these structures is generated using the so-called Two-Beam Acceleration (TBA) scheme, where a low-energy, high-intensity electron beam (drive beam) runs parallel to the main linacs and is decelerated in resonant structures, which extract RF power from the drive beam. The drive beam is first accelerated in a low-frequency fully-loaded normal-conducting linac. Its time structure is then obtained by funneling in isochronous rings using transverse RF deflectors. CTF3, a new generation CLIC Test Facility, is being built at CERN to demonstrate the technical feasibility of this novel drive beam generation and RF power production scheme, albeit on a much smaller scale. CTF3 will also constitute a 30 GHz source with the CLIC nominal peak power and pulse length, for RF component testing. In this paper we give an overview of the CLIC study, focusing on the most recent progress and describe the CTF3 status

CLIC Drive Beam and LHC Based Fel-Nucleus Collider

The feasibility of a CLIC-LHC based FEL-nucleus collider is investigated. It is shown that the proposed scheme satisfies all requirements of an ideal photon source for the Nuclear Resonance Fluorescence method. The physics potential of the proposed collider is illustrated for a beam of Pb nuclei.Comment: Presented at PAC05, 16-20 May 2005, Knoxville, TN, US

Beam transverse stability in the CLIC combiner rings

The Compact Linear Collider (CLIC) RF power source is based on a new scheme of electron pulse compression and bunch frequency multiplication. In this scheme the drive beam time structure is obtained by the combination of electron bunch trains in isochronous rings using RF deflectors. One of the potential problems is the drive beam transverse stability in the rings, arising from beam resonant excitation of the electric field in the RF deflectors. In this paper numerical simulations are used to evaluate the effect and to show that the instability can be minimised by a proper choice of the tune of the ring, and of the parameters of the deflector and of the injection region lattice

An Overview of the New CLIC Test Facility (CTF3)

The CLIC (Compact Linear Collider) RF power source is based on a new scheme of electron pulse compression and bunch frequency multiplication, in which the drive beam time structure is obtained by the combination of electron bunch trains in isochronous rings. The next CLIC TEST Facility (CTF3) at CERN will be built in order to demonstrate the technical feasibility of the scheme. It will also constitute a 30 GHz source with the CLIC nominal peak power and pulse length, for RF component testing. CTF3 will be installed in the area of the present LEP preinjector (LPI) and its construction and commissioning will proceed in stages over five years. In this paper we present an overview of the facility and provide a description of the different components

Injunction Against Prosecution of Divorce Actions in Other States

Aims: The formation scenario of extended counter-rotating stellar disks in galaxies is still debated. In this paper, we study the S0 galaxy IC 719 known to host two large-scale counter-rotating stellar disks in order to investigate their formation mechanism. Methods: We exploit the large field of view and wavelength coverage of the Multi Unit Spectroscopic Explorer (MUSE) spectrograph to derive two-dimensional (2D) maps of the various properties of the counter-rotating stellar disks, such as age, metallicity, kinematics, spatial distribution, the kinematical and chemical properties of the ionized gas, and the dust map. Results: Due to the large wavelength range, and in particular to the presence of the Calcium Triplet \u3bb\u3bb8498, 8542, 8662 \uc5 (CaT hereafter), the spectroscopic analysis allows us to separate the two stellar components in great detail. This permits precise measurement of both the velocity and velocity dispersion of the two components as well as their spatial distribution. We derived a 2D map of the age and metallicity of the two stellar components, as well as the star formation rate and gas-phase metallicity from the ionized gas emission maps. Conclusions: The main stellar disk of the galaxy is kinematically hotter, older, thicker and with larger scale-length than the secondary disk. There is no doubt that the latter is strongly linked to the ionized gas component: they have the same kinematics and similar vertical and radial spatial distribution. This result is in favor of a gas accretion scenario over a binary merger scenario to explain the origin of counter-rotation in IC 719. One source of gas that may have contributed to the accretion process is the cloud that surrounds IC 719

The relation between bar formation, galaxy luminosity, and environment

We derive the bar fraction in three different environments ranging from the field to Virgo and Coma clusters, covering an unprecedentedly large range of galaxy luminosities (or, equivalently, stellar masses). We confirm that the fraction of barred galaxies strongly depends on galaxy luminosity. We also show that the difference between the bar fraction distributions as a function of galaxy luminosity (and mass) in the field and Coma cluster are statistically significant, with Virgo being an intermediate case. We interpret this result as a variation of the effect of environment on bar formation depending on galaxy luminosity. We speculate that brighter disk galaxies are stable enough against interactions to keep their cold structure, thus, the interactions are able to trigger bar formation. For fainter galaxies the interactions become strong enough to heat up the disks inhibiting bar formation and even destroying the disks. Finally, we point out that the controversy regarding whether the bar fraction depends on environment could be resolved by taking into account the different luminosity ranges of the galaxy samples studied so far.Comment: 4 pages, 2 figures. To appear in the proceedings of EWASS 2012 Special Session 4, Structure of galaxy disks shaped by secular evolution and environmental processes, ed. P. Di Matteo and C. Jog, Memorie della Societ\`a Astronomica Italiana Supplement Serie

A New Ultra-dense Group of Obscured Emission-Line Galaxies

We present the discovery of an isolated compact group of galaxies that is extremely dense (median projected galaxy separation: 6.9 kpc), has a very low velocity dispersion ($\sigma_{\rm 2D}$ = 67 km s$^{-1}$), and where all observed members show emission lines and are morphologically disturbed. These properties, together with the lack of spirals and the presence of a prominent tidal tail make this group one of the most evolved compact groups.Comment: 15 pages,LaTeX, 2figures. A Postscript figure with spectra is available at ftp://astro.uibk.ac.at/pub/weinberger/ . Accepted for publication in ApJ Letter