238 research outputs found
Another look at anomalous J/Psi suppression in Pb+Pb collisions at P/A = 158 GeV/c
A new data presentation is proposed to consider anomalous
suppression in Pb + Pb collisions at GeV/c. If the inclusive
differential cross section with respect to a centrality variable is available,
one can plot the yield of J/Psi events per Pb-Pb collision as a function of an
estimated squared impact parameter. Both quantities are raw experimental data
and have a clear physical meaning. As compared to the usual J/Psi over
Drell-Yan ratio, there is a huge gain in statistical accuracy. This
presentation could be applied advantageously to many processes in the field of
nucleus-nucleus collisions at various energies.Comment: 6 pages, 5 figures, submitted to The European Physical Journal C;
minor revisions for final versio
Spallation Neutron Production by 0.8, 1.2 and 1.6 GeV Protons on various Targets
Spallation neutron production in proton induced reactions on Al, Fe, Zr, W,
Pb and Th targets at 1.2 GeV and on Fe and Pb at 0.8, and 1.6 GeV measured at
the SATURNE accelerator in Saclay is reported. The experimental
double-differential cross-sections are compared with calculations performed
with different intra-nuclear cascade models implemented in high energy
transport codes. The broad angular coverage also allowed the determination of
average neutron multiplicities above 2 MeV. Deficiencies in some of the models
commonly used for applications are pointed out.Comment: 20 pages, 32 figures, revised version, accepted fpr publication in
Phys. Rev.
Planets Around Low-Mass Stars (PALMS). I. A Substellar Companion to the Young M Dwarf 1RXS J235133.3+312720
We report the discovery of a brown dwarf companion to the young M dwarf 1RXS
J235133.3+312720 as part of a high contrast imaging search for planets around
nearby young low-mass stars with Keck-II/NIRC2 and Subaru/HiCIAO. The 2.4"
(~120 AU) pair is confirmed to be comoving from two epochs of high resolution
imaging. Follow-up low- and moderate-resolution near-infrared spectroscopy of
1RXS J2351+3127 B with IRTF/SpeX and Keck-II/OSIRIS reveals a spectral type of
L0. The M2 primary star 1RXS J2351+3127 A exhibits X-ray and UV
activity levels comparable to young moving group members with ages of ~10-100
Myr. UVW kinematics based the measured radial velocity of the primary and the
system's photometric distance (50 +/- 10 pc) indicate it is likely a member of
the ~50-150 Myr AB Dor moving group. The near-infrared spectrum of 1RXS
J2351+3127 B does not exhibit obvious signs of youth, but its H-band morphology
shows subtle hints of intermediate surface gravity. The spectrum is also an
excellent match to the ~200 Myr M9 brown dwarf LP 944-20. Assuming an age of
50-150 Myr, evolutionary models imply a mass of 32 +/- 6 Mjup for the
companion, making 1RXS J2351+3127 B the second lowest-mass member of the AB Dor
moving group after the L4 companion CD-35 2722 B and one of the few benchmark
brown dwarfs known at young ages.Comment: Accepted for publication in ApJ. 24 pages, 12 figures, 4 table
Precision Measurement of the Proton and Deuteron Spin Structure Functions g2 and Asymmetries A2
We have measured the spin structure functions g2p and g2d and the virtual
photon asymmetries A2p and A2d over the kinematic range 0.02 < x < 0.8 and 0.7
< Q^2 < 20 GeV^2 by scattering 29.1 and 32.3 GeV longitudinally polarized
electrons from transversely polarized NH3 and 6LiD targets. Our measured g2
approximately follows the twist-2 Wandzura-Wilczek calculation. The twist-3
reduced matrix elements d2p and d2n are less than two standard deviations from
zero. The data are inconsistent with the Burkhardt-Cottingham sum rule if there
is no pathological behavior as x->0. The Efremov-Leader-Teryaev integral is
consistent with zero within our measured kinematic range. The absolute value of
A2 is significantly smaller than the sqrt[R(1+A1)/2] limit.Comment: 12 pages, 4 figures, 2 table
Planet Populations as a Function of Stellar Properties
Exoplanets around different types of stars provide a window into the diverse
environments in which planets form. This chapter describes the observed
relations between exoplanet populations and stellar properties and how they
connect to planet formation in protoplanetary disks. Giant planets occur more
frequently around more metal-rich and more massive stars. These findings
support the core accretion theory of planet formation, in which the cores of
giant planets form more rapidly in more metal-rich and more massive
protoplanetary disks. Smaller planets, those with sizes roughly between Earth
and Neptune, exhibit different scaling relations with stellar properties. These
planets are found around stars with a wide range of metallicities and occur
more frequently around lower mass stars. This indicates that planet formation
takes place in a wide range of environments, yet it is not clear why planets
form more efficiently around low mass stars. Going forward, exoplanet surveys
targeting M dwarfs will characterize the exoplanet population around the lowest
mass stars. In combination with ongoing stellar characterization, this will
help us understand the formation of planets in a large range of environments.Comment: Accepted for Publication in the Handbook of Exoplanet
Measurement of the Proton and Deuteron Spin Structure Functions g2 and Asymmetry A2
We have measured the spin structure functions g2p and g2d and the virtual
photon asymmetries A2p and A2d over the kinematic range 0.02 < x < 0.8 and 1.0
< Q^2 < 30(GeV/c)^2 by scattering 38.8 GeV longitudinally polarized electrons
from transversely polarized NH3 and 6LiD targets.The absolute value of A2 is
significantly smaller than the sqrt{R} positivity limit over the measured
range, while g2 is consistent with the twist-2 Wandzura-Wilczek calculation. We
obtain results for the twist-3 reduced matrix elements d2p, d2d and d2n. The
Burkhardt-Cottingham sum rule integral - int(g2(x)dx) is reported for the range
0.02 < x < 0.8.Comment: 12 pages, 4 figures, 1 tabl
Measurements of the -Dependence of the Proton and Neutron Spin Structure Functions g1p and g1n
The structure functions g1p and g1n have been measured over the range 0.014 <
x < 0.9 and 1 < Q2 < 40 GeV2 using deep-inelastic scattering of 48 GeV
longitudinally polarized electrons from polarized protons and deuterons. We
find that the Q2 dependence of g1p (g1n) at fixed x is very similar to that of
the spin-averaged structure function F1p (F1n). From a NLO QCD fit to all
available data we find at
Q2=5 GeV2, in agreement with the Bjorken sum rule prediction of 0.182 \pm
0.005.Comment: 17 pages, 3 figures. Submitted to Physics Letters
Measurement of the Proton and Deuteron Spin Structure Function g_1 in the Resonance Region
We have measured the proton and deuteron spin structure functions g_1^p and
g_1^d in the region of the nucleon resonances for W^2 < 5 GeV^2 and and GeV^2 by inelastically scattering 9.7 GeV polarized
electrons off polarized and targets. We observe
significant structure in g_1^p in the resonance region. We have used the
present results, together with the deep-inelastic data at higher W^2, to
extract . This is the first
information on the low-Q^2 evolution of Gamma toward the Gerasimov-Drell-Hearn
limit at Q^2 = 0.Comment: 7 pages, 2 figure
Precision Determination of the Neutron Spin Structure Function g1n
We report on a precision measurement of the neutron spin structure function
using deep inelastic scattering of polarized electrons by polarized
^3He. For the kinematic range 0.014<x<0.7 and 1 (GeV/c)^2< Q^2< 17 (GeV/c)^2,
we obtain at an average . We find relatively large negative
values for at low . The results call into question the usual Regge
theory method for extrapolating to x=0 to find the full neutron integral
, needed for testing quark-parton model and QCD sum rules.Comment: 5 pages, 3 figures To be published in Phys. Rev. Let
Characterization of the effects of Atosiban on uterine electromyograms recorded in women with threatened preterm labor
[EN] Although research studies using electrohysterography on women without tocolytic therapy have shown
its potential for preterm birth diagnosis, tocolytics are usually administered in emergency rooms at
the first sign of threatened preterm labor (TPL). Information on the uterine response during tocolytic
treatment could prove useful for the development of tools able to predict true preterm deliveries under
normal clinical conditions. The aim of this study was thus to analyze the effects of Atosiban on Electrohysterogram (EHG) parameters and to compare its effects on women who delivered preterm (WDP) and
at term (WDT). Electrohysterograms recorded in different Atosiban therapy stages (before, during and
after drug administration) on 40 WDT and 27 WDP were analyzed by computing linear, and non-linear
EHG parameters. Results reveal that Atosiban does not greatly affect the EHG signal amplitude, but does
modify its spectral content and reduces the energy associated with the fast wave high component in both
WDP and WDT, with a faster response in the latter. EHG signal complexity remained constant in WDT,
while it increased in WDP until it reached similar values to WDT during Atosiban treatment. The spectral
and complexity parameters were able to separate (p < 0.05) WDT and WDP prior to and during tocolytic
treatment and before and after treatment, respectively. The results pave the way for developing better
and more reliable medical decision support systems based on EHG for preterm delivery prediction in TPL
women in clinical scenarios.This work received financial support from the Spanish Ministry of Economy and Competitiveness and the European Regional Development Fund (DPI2015-68397-R), VLC/Campus (UPV-FE-2018-B03) and by Conselleria de Educación, Investigación, Cultura y Deporte, Generalitat Valenciana (GV/2018/104).Mas-Cabo, J.; Prats-Boluda, G.; Ye Lin, Y.; Alberola Rubio, J.; Perales, A.; Garcia-Casado, J. (2019). Characterization of the effects of Atosiban on uterine electromyograms recorded in women with threatened preterm labor. Biomedical Signal Processing and Control. 52:198-205. https://doi.org/10.1016/j.bspc.2019.04.001S1982055
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