Searcharxiv⌕ Search

arXiv subjects

M. Sullivan

Publications and source records attributed to M. Sullivan.

239 records · Page 14Linked to original sources

More on the Interaction Region of PEP-N

The PEP-N project consists of a small, very low-energy e- storage ring (VLER) located in one of the interaction-straight regions of PEP-II. The small ring is brought into collision with the low-energy (3.1 GeV) e+ beam (LER). The center-of-mass energies from this collision are between the Phi and J/Psi resonances. We achieve a head-on collision through the use of a central magnetic dipole field that generates a large horizontal bending field. This field is also the central field of the detector. The large energy range of the VLER, in order to maximize the center-of-mass energy range, complicates the collision point geometry. In order to maintain the beam orbits near the collision point two techniques are used. The first is to scale the central dipole field up and down with the energy of the VLER and the second is to use passive shielding to decrease the integral B.dl of the dipole field seen by the VLER. Changes in the orbit of the LER are corrected with local bending magnets. Further details of the interaction region geometry as well as design issues that include synchrotron radiation from the high-current positron beam are discussed.

hep-ph↗

Lattice and Compensation Schemes for the PEP-II Interaction Region

The PEP-II interaction region is designed to accommodate asymmetric beam energies, head-on collisions, small bunch spacing and provide low beta* for high luminosity. Local correction schemes are implemented to compensate non-linear chromaticity from the IP doublets as well as coupling, orbit and focusing effects from the 6 Tm asymmetric detector solenoid. The main IR optics features and local correction schemes are presented. MAD code is used for the optics calculations.

physics.acc-ph↗

Upgrade of the PEP-II Low Beta Optics

The successful commissioning and operation of the PEP-II asymmetric e+e- collider motivated further studies to increase luminosity. In this paper, we discuss a modification of the PEP-II lattice to reduce the vertical beta function at the Interaction Point (IP) from the design value of 1.5cm to 1.0cm. This could potentially reduce the colliding beam size, increase particle density at the IP and the probability of beam-beam interactions. In this paper, we outline the optics modifications, discuss tracking simulations, and overview machine implementation.

physics.acc-ph↗

Measurement of the vector analyzing power in elastic electron-proton scattering as a probe of double photon exchange amplitudes

We report the first measurement of the vector analyzing power in inclusive transversely polarized elastic electron-proton scattering at Q^2 = 0.1 (GeV/c)^2 and large scattering angles. This quantity should vanish in the single virtual photon exchange, plane wave impulse approximation for this reaction, and can therefore provide information on double photon exchange amplitudes for electromagnetic interactions with hadronic systems. We find a non-zero value of A=-15.4+/-5.4 ppm. No calculations of this observable for nuclei other than spin 0 have been carried out in these kinematics, and the calculation using the spin orbit interaction from a charged point nucleus of spin 0 cannot describe these data.

nucl-ex↗

An Ultraviolet-Selected Galaxy Redshift Survey - II: The Physical Nature of Star Formation in an Enlarged Sample

We present further spectroscopic observations for a sample of galaxies selected in the vacuum ultraviolet (UV) at 2000 Åfrom the FOCA balloon-borne imaging camera of Milliard et al. (1992). This work represents an extension of the initial study of Treyer et al. (1998). Our enlarged catalogue contains 433 sources; 273 of these are galaxies, nearly all with redshifts z=0-0.4. Nebular emission line measurements are available for 216 galaxies, allowing us to address issues of reddening and metallicity. The UV and Halpha luminosity functions strengthen our earlier assertions that the local volume-averaged star formation rate is higher than indicated from earlier surveys. Moreover, internally within our sample, we do not find a steep rise in the UV luminosity density with redshift over 0<z<0.4. Our data is more consistent with a modest evolutionary trend as suggested by recent redshift survey results. We find no evidence for a significant number of AGN in our sample. We find the UV flux indicates a consistently higher mean star formation rate than that implied by the Halpha luminosity for typical constant or declining star formation histories. Following Glazebrook et al. (1999), we interpret this discrepancy in terms of a starburst model for our UV-luminous sources. Whilst we can explain most of our observations in this way, there remains a small population with extreme UV-optical colours which cannot be understood.

astro-ph↗