319 research outputs found
Precision luminosity measurement at ILC
In these proceedings a novel approach to deal with the beam-induced effects
in luminosity measurement is presented. Based on the relativistic kinematics of
the collision frame of the Bhabha process, the beam-beam related uncertainties
can be reduced to the permille level independently of a precision with which
the beam parameters are known. Specific event selection combined with the
corrective methods we introduce, leads to the systematic uncertainty from the
beam-induced effects to be at a few permille level in the peak region above the
80% of the nominal centre-of-mass energies at ILC.Comment: Talk presented on behalf of the FCAL Collaboration at the
International Workshop on Future Linear Colliders (LCWS13) Tokyo, Japan,
11-15 November 201
Luminosity measurement at ILC
In this paper we describe a method of luminosity measurement at the future
linear collider ILC that estimates and corrects for the impact of the dominant
sources of systematic uncertainty originating from the beam-induced effects and
the background from physics processes. Based on the relativistic kinematics of
the collision frame of the Bhabha process, the beam-beam related uncertainty is
reduced to a permille independently of the precision with which the beam
parameters are known. With the specific event selection, different from the
isolation cuts based on topology of the signal used at LEP, combined with the
corrective methods we introduce, the overall systematic uncertainty in the peak
region above 80% of the nominal center-of-mass energy meets the physics
requirements to be at the few permille level at all ILC energies.Comment: Accepted for publication in JINST (submission JINST_016P_0413
Measurement of shower development and its Moli\`ere radius with a four-plane LumiCal test set-up
A prototype of a luminometer, designed for a future e+e- collider detector,
and consisting at present of a four-plane module, was tested in the CERN PS
accelerator T9 beam. The objective of this beam test was to demonstrate a
multi-plane tungsten/silicon operation, to study the development of the
electromagnetic shower and to compare it with MC simulations. The Moli\`ere
radius has been determined to be 24.0 +/- 0.6 (stat.) +/- 1.5 (syst.) mm using
a parametrization of the shower shape. Very good agreement was found between
data and a detailed Geant4 simulation.Comment: Paper published in Eur. Phys. J., includes 25 figures and 3 Table
The Gaia-ESO Survey: Detailed Abundances in the Metal-poor Globular Cluster NGC 4372
We present the abundance analysis for a sample of 7 red giant branch stars in
the metal-poor globular cluster NGC 4372 based on UVES spectra acquired as part
of the Gaia-ESO Survey. This is the first extensive study of this cluster from
high resolution spectroscopy. We derive abundances of O, Na, Mg, Al, Si, Ca,
Sc, Ti, Fe, Cr, Ni, Y, Ba, and La. We find a metallicity of [Fe/H] = -2.19
0.03 and find no evidence for a metallicity spread. This metallicity
makes NGC 4372 one of the most metal-poor galactic globular clusters. We also
find an {\alpha}-enhancement typical of halo globular clusters at this
metallicity. Significant spreads are observed in the abundances of light
elements. In particular we find a Na-O anti-correlation. Abundances of O are
relatively high compared with other globular clusters. This could indicate that
NGC 4372 was formed in an environment with high O for its metallicity. A Mg-Al
spread is also present which spans a range of more than 0.5 dex in Al
abundances. Na is correlated with Al and Mg abundances at a lower significance
level. This pattern suggests that the Mg-Al burning cycle is active. This
behavior can also be seen in giant stars of other massive, metal-poor clusters.
A relation between light and heavy s-process elements has been identified.Comment: 14 pages, 14 figures, accepted for publication in A&
Nitrogen Enrichment in Atmospheres of A- and F- Type Supergiants
Using new accurate fundamental parameters of 30 Galactic A and F supergiants,
namely their effective temperatures Teff and surface gravities log g, we
implemented a non-LTE analysis of the nitrogen abundance in their atmospheres.
It is shown that the non-LTE corrections to the N abundances increase with
Teff. The nitrogen overabundance as a general feature of this type of stars is
confirmed. A majority of the stars has a nitrogen excess [N/Fe] between 0.2 and
0.9 dex with the maximum position of the star's distribution on [N/Fe] between
0.4 and 0.7 dex. The N excesses are discussed in light of predictions for
B-type main sequence (MS) stars with rotationally induced mixing and for their
next evolutionary phase, i.e. A- and F-type supergiants that have experienced
the first dredge-up. Rotationally induced mixing in the MS progenitors of the
supergiants may be a significant cause of the nitrogen excesses. When comparing
our results with predictions of the theory developed for stars with the mixing,
we find that the bulk of the supergiants (28 of 30) show the N enrichment that
can be expected (i) either after the MS phase for stars with the initial
rotational velocities v0 = 200-400 km s-1, (ii) or after the first dredge-up
for stars with v0 = 50-400 km s-1. The latter possibility is preferred on
account of the longer lifetime for stars on red-blue loops following the first
dredge-up. Two supergiants without a discernible N enrichment, namely HR 825
and HR 7876, may be post-MS objects with the relatively low initial rotational
velocity of about 100 km s-1. The suggested range for v0 is approximately
consistent with inferences from the observed projected rotational velocities of
B-type MS stars, progenitors of A and F supergiants.Comment: 14 pages, 13 figure
Chemically tagging the Hyades Supercluster: A homogeneous sample of F6-K4 kinematically selected northern stars
Stellar kinematic groups are kinematical coherent groups of stars that might
have a common origin. These groups are dispersed throughout the Galaxy over
time by the tidal effects of both Galactic rotation and disc heating, although
their chemical content remains unchanged. The aim of chemical tagging is to
establish that the abundances of every element in the analysis are homogeneus
among the members. We study the case of the Hyades Supercluster to compile a
reliable list of members (FGK stars) based on our chemical tagging analysis.
For a total of 61 stars from the Hyades Supercluster, stellar atmospheric
parameters (Teff, logg, xi, and [Fe/H]) are determined using our code called
StePar, which is based on the sensitivity to the stellar atmospheric parameters
of the iron EWs measured in the spectra. We derive the chemical abundances of
20 elements and find that their [X/Fe] ratios are consistent with Galactic
abundance trends reported in previous studies. The chemical tagging method is
applied with a carefully developed differential abundance analysis of each
candidate member of the Hyades Supercluster, using a well-known member of the
Hyades cluster as a reference (vB 153). We find that only 28 stars (26 dwarfs
and 2 giants) are members, i.e. that 46% of our candidates are members based on
the differential abundance analysis. This result confirms that the Hyades
Supercluster cannot originate solely from the Hyades cluster.Comment: A&A, in pres
ECFA Detector R&D Panel, Review Report
Two special calorimeters are foreseen for the instrumentation of the very
forward region of an ILC or CLIC detector; a luminometer (LumiCal) designed to
measure the rate of low angle Bhabha scattering events with a precision better
than 10 at the ILC and 10 at CLIC, and a low polar-angle
calorimeter (BeamCal). The latter will be hit by a large amount of
beamstrahlung remnants. The intensity and the spatial shape of these
depositions will provide a fast luminosity estimate, as well as determination
of beam parameters. The sensors of this calorimeter must be radiation-hard.
Both devices will improve the e.m. hermeticity of the detector in the search
for new particles. Finely segmented and very compact electromagnetic
calorimeters will match these requirements. Due to the high occupancy, fast
front-end electronics will be needed. Monte Carlo studies were performed to
investigate the impact of beam-beam interactions and physics background
processes on the luminosity measurement, and of beamstrahlung on the
performance of BeamCal, as well as to optimise the design of both calorimeters.
Dedicated sensors, front-end and ADC ASICs have been designed for the ILC and
prototypes are available. Prototypes of sensor planes fully assembled with
readout electronics have been studied in electron beams.Comment: 61 pages, 51 figure
The Gaia-ESO Survey: metallicity of the Chamaeleon I star forming region
Context. Recent metallicity determinations in young open clusters and
star-forming regions suggest that the latter may be characterized by a slightly
lower metallicity than the Sun and older clusters in the solar vicinity.
However, these results are based on small statistics and inhomogeneous
analyses. The Gaia-ESO Survey is observing and homogeneously analyzing large
samples of stars in several young clusters and star-forming regions, hence
allowing us to further investigate this issue.
Aims. We present a new metallicity determination of the Chamaeleon I
star-forming region, based on the products distributed in the first internal
release of the Gaia-ESO Survey.
Methods. 48 candidate members of Chamaeleon I have been observed with the
high-resolution spectrograph UVES. We use the surface gravity, lithium line
equivalent width and position in the Hertzsprung-Russell diagram to confirm the
cluster members and we use the iron abundance to derive the mean metallicity of
the region.
Results. Out of the 48 targets, we confirm 15 high probability members.
Considering the metallicity measurements for 9 of them, we find that the iron
abundance of Chamaeleon I is slightly subsolar with a mean value
[Fe/H]=-0.08+/-0.04 dex. This result is in agreement with the metallicity
determination of other nearby star-forming regions and suggests that the
chemical pattern of the youngest stars in the solar neighborhood is indeed more
metal-poor than the Sun. We argue that this evidence may be related to the
chemical distribution of the Gould Belt that contains most of the nearby
star-forming regions and young clusters.Comment: 13 pages, 11 figures, 3 tables, Accepted for publication in Astronomy
& Astrophysic
Performance of fully instrumented detector planes of the forward calorimeter of a Linear Collider detector
Detector-plane prototypes of the very forward calorimetry of a future
detector at an e+e- collider have been built and their performance was measured
in an electron beam. The detector plane comprises silicon or GaAs pad sensors,
dedicated front-end and ADC ASICs, and an FPGA for data concentration.
Measurements of the signal-to-noise ratio and the response as a function of the
position of the sensor are presented. A deconvolution method is successfully
applied, and a comparison of the measured shower shape as a function of the
absorber depth with a Monte-Carlo simulation is given.Comment: 25 pages, 32 figures, revised version following comments from
referee
The Gaia-ESO Survey: the most metal-poor stars in the Galactic bulge
We present the first results of the EMBLA survey (Extremely Metal-poor BuLge
stars with AAOmega), aimed at finding metal-poor stars in the Milky Way bulge,
where the oldest stars should now preferentially reside. EMBLA utilises
SkyMapper photometry to pre-select metal-poor candidates, which are
subsequently confirmed using AAOmega spectroscopy. We describe the discovery
and analysis of four bulge giants with -2.72<=[Fe/H]<=-2.48, the lowest
metallicity bulge stars studied with high-resolution spectroscopy to date.
Using FLAMES/UVES spectra through the Gaia-ESO Survey we have derived
abundances of twelve elements. Given the uncertainties, we find a chemical
similarity between these bulge stars and halo stars of the same metallicity,
although the abundance scatter may be larger, with some of the stars showing
unusual [{\alpha}/Fe] ratios.Comment: 7 pages, 5 figures. Accepted for publication by MNRA
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