120364457
Results from the E835 scintillating fiber detector
A cylindrical scintillating-fiber tracker for the measurement of the polar coordinate θ has been built for experiment E835 at Fermilab. This detector combines the high granularity, flexibility and fast response of the scintillating fibers with the high quantum efficiency of the Visible-Light Photon Counters (VLPC). Complete results about the tracker performance are given: tracking and timing resolution, photoelectron yield per mip, detection efficiency, single–double-track discrimination.
125331327
The Fermilab anti-p accumulator ring for the charmonium experiment
108986863
Performance measurements of histe-V VLPC photon detectors for E835 at FNAL
A set of 144 VLPC chips has been used by experiment E835 at FNAL for the readout of its scintillating fiber detector. During the data taking, the fibers have been exposed to rates up to 2.5×104 mips/sec, corresponding to 3.5×106 photons/sec on each VLPC pixel surface. This paper reports about a study on rate dependence of gain and quantum efficiency throughout the run, as well as VLPC failure statistics during operation. No significant aging effects are observed. A review about the overall system performance is given.
123064237
The charged trigger of the experiment E835 at Fermilab
Abstract Fermilab experiment E835 studies the charmonium states primarily through their electromagnetic decays. A kinematical charged trigger has been designed to select the electromagnetic final states e + e − and e + e − X and the hadronic decay c c → φφ →4 K ± . A detailed description of the charged trigger is presented here. The design, its implementation and the performances are given.
119627299
HIGH-RESOLUTION SILICON DETECTORS FOR COLLIDING BEAM PHYSICS
Abstract Resolution and linearity of the position measurement of Pisa multi-electrode silicon detectors are presented. The detectors are operated in slightly underdepleted mode and take advantage of their intrinsic resistivity for resistive charge partition between adjacent strips. 22 μm resolution is achieved with readout lines spaced 300 μm. Possible applications in colliding beam experiments for the detection of secondary vertices are discussed.
119936495
Hadronic Physics with Antiprotons at FAIR
The physics program of the future FAIR facility covers a wide range of topics that address central issues of strong interactions and QCD. The antiproton beam of unprecedented quality in the momentum range from 1 GeV/c to 15 GeV/c will allow to make high precision, high statistics measurements, from charmonium spectroscopy to the search for exotic hadrons and the study of nucleon structure, from the study of in-medium modifications of hadron masses to the physics of hypernuclei. These topics form the scientific program of the PANDA experiment. In addition to that the possibility to polarize antiprotons will provide the possibility to perform new, unique measurements of single- and double-spin observables, which are part of the experimental program of PAX.
119290984
ON THE CONNECTION BETWEEN SHAPE AND STELLAR POPULATION IN EARLY-TYPE GALAXIES
We report on the discovery of a relation between the stellar mass M* of early-type galaxies (hereafter ETGs), their shape, as parameterized by the Sersic index n, and their stellar mass-to-light ratio M*/L. In a three-dimensional log space defined by these variables, the ETGs populate a plane surface with small scatter. This relation tells us that galaxy shape and stellar population are not independent physical variables, a result that must be accounted for by theories of galaxy formation and evolution.
117368372
The visible environment of gas-accreting galaxies
We studied the environment of a sample of galaxies in which the presence of polar rings or the presence of gas- and stars- counterrotation is observed. These galaxies are believed to have accreted this material, now in peculiar motion, from their environment. 
The variable considered here are the number of possible companions in the field, down to an apparent magnitude 22, their size, their concentration around the accreting galaxy, and a set of related parameters. A control sample of 'normal' galaxies has also been studied. From Kolgomorov-Smirnov tests of the considered variables, no significant differences have been found between the population of objects around the our accreting galaxies and the control sample. 
These results seems to give support to the models suggesting a long formation time for the acquisition process, starting from a diffuse gas instead of fagocitation of small satellite.
119251924
A multiwavelength study of the IRAS Deep Survey galaxy sample - III. Spectral classification and dynamical properties
The infrared deep sample (IDS), in the north ecliptical polar region (NEPR), is the first complete, far--IR selected sample, on which numerous studies of galaxy evolution are based. Here we present and analyze the spectral classification of several galaxies in the IDS sample together with rotation curves which allow estimating the lower mass limits of a subsample of objects. We measured fluxes and intensity ratios of the emission lines in the visible region of the spectrum (lambda 4000-9000 A) for 75 galaxy members. Moreover, for some of them (55%), the spectra obtained with the Keck II telescope have sufficient wavelength and spatial resolution to derive their rotation curve. These galaxies turn out to be disk like systems, with a high fraction (~50%) of interacting systems. The spectroscopic classification of 42 galaxies, using the emission-line ratio diagnostic diagrams, shows that the NEPR sample is predominantly composed of starburst galaxies (71%), while the fraction of AGNs (7%) and LINERs (21%) is small. The dynamical analysis allows us to estimate the lower mass limits of 39 galaxies. The rest-frame FIR luminosity distribution of these galaxies spans the same range as that of the FIR selected complete sample, i.e. three orders of magnitude, with the same mean value, log(L_FIR)=10.2. This emphasizes that such galaxies represent FIR properties of the whole sample well. Moreover, their optical properties are typical of the sample itself since 62% of these belong to the 60mu selected complete sample.
23729217
The evolution of early-type galaxies in clusters from z ~ 0.8 to z ~ 0: the ellipticity distribution and the morphological mix
We present the ellipticity distribution and its evolution for early-type galaxies in clusters from z~ 0.8 to the current epoch, based on the WIde-field Nearby Galaxy-cluster Survey (0.04 ≤ z ≤ 0.07) and the ESO Distant Cluster Survey (0.4 ≤ z ≤ 0.8). We first investigate a mass-limited sample and we find that above a fixed mass limit (M_(*) ≥ 10^(10.2) M_⊙), the ellipticity (e) distribution of early-type galaxies notably evolves with redshift. In the local Universe, there are proportionally more galaxies with higher ellipticity, hence flatter, than in distant clusters. This evolution is due partly to the change in 
the mass distribution and mainly to the change in the morphological mix with z among the early types, the fraction of ellipticals goes from ~70 per cent at high z to ~40 per cent at low z). Analysing separately the ellipticity distribution of the different morphological types, we find no evolution both for ellipticals and for S0s. However, for ellipticals a change with redshift in the median value of the distributions is detected. This is due to a larger population of very round (e M_(B)+ 1.208z > −21. Analysing this sample, we do not recover exactly the same results as the mass-limited sample. This indicates that the selection criteria are crucial to characterize the galactic properties: the choice of the magnitude-‘delimited’ sample implies the loss of many less-massive galaxies and so it biases the final conclusions. Moreover, although we are adopting the same selection criteria, our results in the magnitude-‘delimited’ sample are also not in agreement with those of Holden et al. This is due to the fact that our and their low-zsamples have a different magnitude distribution because the Holden et al. sample suffers from incompleteness at faint magnitudes.
17610175
Are truncated stellar disks linked to the molecular gas density
We know that the slope of the radial, stellar light distribution in galaxies is well described by an exponential decline and this distribution is often truncated at a break radius ($R_{br}$). We don't have a clear understanding for the origin of these outer truncations and several hypotheses have been proposed to explain them. We want to test the various theories with direct observations of the cold molecular gas for a few truncated galaxies in comparison with the non-truncated ones. The answer to the existence of a possible link between truncated stellar disks and the molecular gas density cannot be obtained from CO maps in the literature, because so far there are no galaxies with a clear truncation observed in CO at high resolution.