pinecone/core-2020-05-10-deduplication huggingface dataset:
Constraints on the Nucleon Strange Form Factors at Q^2 ~ 0.1 GeV^2

We report the most precise measurement to date of a parity-violating
asymmetry in elastic electron-proton scattering. The measurement was carried
out with a beam energy of 3.03 GeV and a scattering angle <theta_lab>=6
degrees, with the result A_PV = -1.14 +/- 0.24 (stat) +/- 0.06 (syst) parts per
million. From this we extract, at Q^2 = 0.099 GeV^2, the strange form factor
combination G_E^s + 0.080 G_M^s = 0.030 +/- 0.025 (stat) +/- 0.006 (syst) +/-
0.012 (FF) where the first two errors are experimental and the last error is
due to the uncertainty in the neutron electromagnetic form factor. This result
significantly improves current knowledge of G_E^s and G_M^s at Q^2 ~0.1 GeV^2.
A consistent picture emerges when several measurements at about the same Q^2
value are combined: G_E^s is consistent with zero while G_M^s prefers positive
values though G_E^s=G_M^s=0 is compatible with the data at 95% C.L.Comment: minor wording changes for clarity, updated references, dropped one
  figure to improve focu
Accurate Nucleon-Nucleon Potential Based upon Chiral Perturbation Theory

We present an accurate nucleon-nucleon ($NN$) potential based upon chiral
effective Lagrangians. The model includes one- and two-pion exchange
contributions up to chiral order three. We show that a quantitative fit of the
$NN$ $D$-wave phase shifts requires contact terms (which represent the short
range force) of order four. Within this framework, the $NN$ phase shifts below
300 MeV lab. energy and the properties of the deuteron are reproduced with
high-precision. This chiral $NN$ potential represents a reliable starting point
for testing the chiral effective field theory approach in exact few-nucleon and
microscopic nuclear many-body calculations. An important implication of the
present work is that the chiral $2\pi$ exchange at order four is of crucial
interest for future chiral $NN$ potential development.Comment: 7 pages RevTex, 3 figures, 1 tabl
Dynamic receptor team formation can explain the high signal transduction
  gain in E. coli

Evolution has provided many organisms with sophisticated sensory systems that
enable them to respond to signals in their environment. The response frequently
involves alteration in the pattern of movement, such as the chemokinesis of the
bacterium Escherichia coli, which swims by rotating its flagella. When rotated
counterclockwise (CCW) the flagella coalesce into a propulsive bundle,
producing a relatively straight ``run'', and when rotated clockwise (CW) they
fly apart, resulting in a ``tumble'' which reorients the cell with little
translocation. A stochastic process generates the runs and tumbles, and in a
chemoeffector gradient runs that carry the cell in a favorable direction are
extended. The overall structure of the signal transduction pathways is
well-characterized in E. coli, but important details are still not understood.
Only recently has a source of gain in the signal transduction network been
identified experimentally, and here we present a mathematical model based on
dynamic assembly of receptor teams that can explain this observation.Comment: Accepted for publication in the Biophysical Journa
Renormalization group improved pQCD prediction for $\Upsilon(1S)$
  leptonic decay

The complete next-to-next-to-next-to-leading order short-distance and
bound-state QCD corrections to $\Upsilon(1S)$ leptonic decay rate
$\Gamma(\Upsilon(1S)\to \ell^+\ell^-)$ has been finished by Beneke {\it et al.}
\cite{Beneke:2014qea}. Based on those improvements, we present a
renormalization group (RG) improved pQCD prediction for $\Gamma(\Upsilon(1S)\to
\ell^+\ell^-)$ by applying the principle of maximum conformality (PMC). The PMC
is based on RG-invariance and is designed to solve the pQCD renormalization
scheme and scale ambiguities. After applying the PMC, all known-type of
$\beta$-terms at all orders, which are controlled by the RG-equation, are
resummed to determine optimal renormalization scale for its strong running
coupling at each order. We then achieve a more convergent pQCD series, a
scheme- independent and more accurate pQCD prediction for $\Upsilon(1S)$
leptonic decay, i.e. $\Gamma_{\Upsilon(1S) \to e^+ e^-}|_{\rm PMC} =
1.270^{+0.137}_{-0.187}$ keV, where the uncertainty is the squared average of
the mentioned pQCD errors. This RG-improved pQCD prediction agrees with the
experimental measurement within errors.Comment: 11 pages, 4 figures. Numerical results and discussions improved,
  references updated, to be published in JHE
Gamma-rays from Type Ia supernova SN2014J

The whole set of INTEGRAL observations of type Ia supernova SN2014J, covering
the period 19-162 days after the explosion has being analyzed. For spectral
fitting the data are split into "early" and "late" periods covering days 19-35
and 50-162, respectively, optimized for $^{56}$Ni and $^{56}$Co lines. As
expected for the early period much of the gamma-ray signal is confined to
energies below $\sim$200 keV, while for the late period it is most strong above
400 keV. In particular, in the late period $^{56}$Co lines at 847 and 1248 keV
are detected at 4.7 and 4.3 $\sigma$ respectively. The lightcurves in several
representative energy bands are calculated for the entire period. The resulting
spectra and lightcurves are compared with a subset of models. We confirm our
previous finding that the gamma-ray data are broadly consistent with the
expectations for canonical 1D models, such as delayed detonation or
deflagration models for a near-Chandrasekhar mass WD. Late optical spectra (day
136 after the explosion) show rather symmetric Co and Fe lines profiles,
suggesting that unless the viewing angle is special, the distribution of
radioactive elements is symmetric in the ejecta.Comment: 21 pages, 16 figures, accepted by Ap
Quasinormal modes of (Anti-)de Sitter black holes in the 1/D expansion

We use the inverse-dimensional expansion to compute analytically the
frequencies of a set of quasinormal modes of static black holes of
Einstein-(Anti-)de Sitter gravity, including the cases of spherical, planar or
hyperbolic horizons. The modes we study are decoupled modes localized in the
near-horizon region, which are the ones that capture physics peculiar to each
black hole (such as their instabilities), and which in large black holes
contain hydrodynamic behavior. Our results also give the unstable
Gregory-Laflamme frequencies of Ricci-flat black branes to two orders higher in
1/D than previous calculations. We discuss the limits on the accuracy of these
results due to the asymptotic but not convergent character of the 1/D
expansion, which is due to the violation of the decoupling condition at finite
D. Finally, we compare the frequencies for AdS black branes to calculations in
the hydrodynamic expansion in powers of the momentum k. Our results extend up
to k^9 for the sound mode and to k^8 for the shear mode.Comment: 20 pages, 3 figure
Synthetic foundations of cevian geometry, I: Fixed points of affine maps
  in triangle geometry

We give synthetic proofs of many new results in triangle geometry, focusing
especially on fixed points of certain affine maps which are defined in terms of
the cevian triangle $DEF$ of a point $P$ with respect to a given triangle
$ABC$, as well as the cevian triangle of the isotomic conjugate $P'$ of $P$
with respect to $ABC$. We prove a formula for the cyclocevian map in terms of
the isotomic and isogonal maps using an entirely synthetic argument, and show
that the complement $Q$ of the isotomic conjugate $P'$ has many interesting
properties. If $T_P$ is the affine map taking $ABC$ to $DEF$, we show
synthetically that $Q$ is the unique ordinary fixed point of $T_P$ when $P$ is
any point not lying on the sides of triangle $ABC$, its anti-complementary
triangle, or the Steiner circumellipse of $ABC$. We also show that $T_P(Q')=P$
if $Q'$ is the complement of $P$, and that the affine map $T_P T_{P'}$ is
either a homothety or a translation which always has the $P$-ceva conjugate of
$Q$ as a fixed point. Finally, we show that $P$ lies on the Steiner
circumellipse if and only if $T_PT_{P'}=K^{-1}$, where $K$ is the complement
map for $ABC$. This paper forms the foundation for several more papers to
follow, in which the conic on the 5 points $A,B,C,P,Q$ is studied and its
center is characterized as a fixed point of the map $\lambda=T_{P'} T_P^{-1}$.Comment: 25 pages, 6 figure
Towards a first estimate of the gluon Sivers function from $A_N$ data in
  $pp$ collisions at RHIC

Within a generalized parton model approach, with inclusion of spin and
intrinsic transverse momentum effects, we show how the latest, highly precise,
midrapidity data on the transverse single spin asymmetry measured in
$pp\to\pi^0\, X$ by the PHENIX Collaboration at RHIC [1], can be used to get a
first estimate on the still poorly known gluon Sivers distribution. To this end
we also adopt the present information on the quark Sivers functions, as
extracted from semi-inclusive deeply inelastic scattering data. This analysis
updates a previous study by some of us where a first bound on this distribution
was obtained [2].Comment: RevTex4, 10 pages, 7 eps figures. V2: discussion on the process
  dependence of the quark Sivers function, with two new plots (Fig. 4), added
  in Section II. One reference added. Results unchanged. Matches the published
  versio
Nuclear shadowing in photoproduction of $\rho$ mesons in ultraperipheral
  nucleus collisions at RHIC and the LHC

We argue that with an increase of the collision energy, elastic
photoproduction of $\rho$ mesons on nuclei becomes affected by the significant
cross section of photon inelastic diffraction into large masses, which results
in the sizable inelastic nuclear shadowing correction to $\sigma_{\gamma A \to
\rho A}$ and the reduced effective $\rho$-nucleon cross section. We take these
effects into account by combining the vector meson dominance model, which we
upgrade to include the contribution of high-mass fluctuations of the photon
according to QCD constraints, and the Gribov-Glauber approximation for nuclear
shadowing, where the inelastic nuclear shadowing is included by means of cross
section fluctuations. The resulting approach allows us to successfully describe
the data on elastic $\rho$ photoproduction on nuclei in heavy ion UPCs in the
$7 \ {\rm GeV} < W_{\gamma p} < 46$ GeV energy range and to predict the value
of the cross section of coherent $\rho$ photoproduction in Pb-Pb UPCs at
$\sqrt{s_{NN}}=5.02$ TeV in Run 2 at the LHC, $d\sigma_{Pb Pb \to \rho Pb Pb}
(y=0)/dy= 560 \pm 25$ mb.Comment: 19 pages, 6 figure
From starburst to quiescence : testing AGN feedback in rapidly Quenching post-starburst galaxies

We acknowledge financial support from the NSF grant AST-0808133. C.C.H. is grateful to the Klaus Tschira Foundation for financial support.Post-starbursts are galaxies in transition from the blue cloud to the red sequence. Although they are rare today, integrated over time they may be an important pathway to the red sequence. This work uses SDSS, GALEX, and WISE observations to identify the evolutionary sequence from starbursts to fully quenched post-starbursts in the narrow mass range log M(Msun) = 10.3-10.7, and identifies "transiting" post-starbursts which are intermediate between these two populations. In this mass range, ∼0.3% of galaxies are starbursts, ∼0.1% are quenched post-starbursts, and ∼0.5% are the transiting types in between. The transiting post-starbursts have stellar properties that are predicted for fast-quenching starbursts and morphological characteristics that are already typical of early-type galaxies. The AGN fraction, as estimated from optical line ratios, of these post-starbursts is about 3 times higher (∼>36 ± 8%) than that of normal star-forming galaxies of the same mass, but there is a significant delay between the starburst phase and the peak of nuclear optical AGN activity (median age difference of ∼> 200 ± 100$ Myr), in agreement with previous studies. The time delay is inferred by comparing the broad-band near NUV-to-optical photometry with stellar population synthesis models. We also find that starbursts and post-starbursts are significantly more dust-obscured than normal star-forming galaxies in the same mass range. About 20% of the starbursts and 15% of the transiting post-starbursts can be classified as the "Dust-Obscured Galaxies" (DOGs), while only 0.8% of normal galaxies are DOGs.The time delay between the starburst phase and AGN activity suggests that AGN do not play a primary role in the original quenching of starbursts but may be responsible for quenching later low-level star formation during the post-starburst phase.PostprintPeer reviewe
Ultraviolet and extreme-ultraviolet emissions at the flare footpoints observed by atmosphere imaging assembly

A solar flare is composed of impulsive energy release events by magnetic reconnection, which forms and heats flare loops. Recent studies have revealed a two-phase evolution pattern of UV 1600 Å emission at the feet of these loops: a rapid pulse lasting for a few seconds to a few minutes, followed by a gradual decay on timescales of a few tens of minutes. Multiple band EUV observations by the Atmosphere Imaging Assembly further reveal very similar signatures. These two phases represent different but related signatures of an impulsive energy release in the corona. The rapid pulse is an immediate response of the lower atmosphere to an intense thermal conduction flux resulting from the sudden heating of the corona to high temperatures (we rule out energetic particles due to a lack of significant hard X-ray emission). The gradual phase is associated with the cooling of hot plasma that has been evaporated into the corona. The observed footpoint emission is again powered by thermal conduction (and enthalpy), but now during a period when approximate steady-state conditions are established in the loop. UV and EUV light curves of individual pixels may therefore be separated into contributions from two distinct physical mechanisms to shed light on the nature of energy transport in a flare. We demonstrate this technique using coordinated, spatially resolved observations of UV and EUV emissions from the footpoints of a C3.2 thermal flare.Publisher PDFPeer reviewe
Gaia-ESO Survey: Analysis of pre-main sequence stellar spectra

Context. The Gaia-ESO Public Spectroscopic Survey is obtaining high-quality spectroscopy of some 100 000 Milky Way stars using the FLAMES spectrograph at the VLT, down to V = 19 mag, systematically covering all the main components of the Milky Way and providing the first homogeneous overview of the distributions of kinematics and chemical element abundances in the Galaxy. Observations of young open clusters, in particular, are giving new insights into their initial structure, kinematics, and their subsequent evolution. Aims. This paper describes the analysis of UVES and GIRAFFE spectra acquired in the fields of young clusters whose population includes pre-main sequence (PMS) stars. The analysis is applied to all stars in such fields, regardless of any prior information on membership, and provides fundamental stellar atmospheric parameters, elemental abundances, and PMS-specific parameters such as veiling, accretion, and chromospheric activity. Methods. When feasible, different methods were used to derive raw parameters (e.g. line equivalent widths) fundamental atmospheric parameters and derived parameters (e.g. abundances). To derive some of these parameters, we used methods that have been extensively used in the past and new ones developed in the context of the Gaia-ESO survey enterprise. The internal precision of these quantities was estimated by inter-comparing the results obtained by these different methods, while the accuracy was estimated by comparison with independent external data, such as effective temperature and surface gravity derived from angular diameter measurements, on a sample of benchmarks stars. A validation procedure based on these comparisons was applied to discard spurious or doubtful results and produce recommended parameters. Specific strategies were implemented to resolve problems of fast rotation, accretion signatures, chromospheric activity, and veiling. Results. The analysis carried out on spectra acquired in young cluster fields during the first 18 months of observations, up to June 2013, is presented in preparation of the first release of advanced data products. These include targets in the fields of the ρ Oph, Cha I, NGC 2264, γ Vel, and NGC 2547 clusters. Stellar parameters obtained with the higher resolution and larger wavelength coverage from UVES are reproduced with comparable accuracy and precision using the smaller wavelength range and lower resolution of the GIRAFFE setup adopted for young stars, which allows us to provide stellar parameters with confidence for the much larger GIRAFFE sample. Precisions are estimated to be ≈120 K rms in Teff, ≈0.3 dex rms in log g, and ≈0.15 dex rms in [Fe/H] for the UVES and GIRAFFE setups
Measurement of the distributions of event-by-event flow harmonics in lead-lead collisions at = 2.76 TeV with the ATLAS detector at the LHC

The distributions of event-by-event harmonic flow coefficients v_n for n=2-4 are measured in sqrt(s_NN)=2.76 TeV Pb+Pb collisions using the ATLAS detector at the LHC. The measurements are performed using charged particles with transverse momentum pT> 0.5 GeV and in the pseudorapidity range |eta|<2.5 in a dataset of approximately 7 ub^-1 recorded in 2010. The shapes of the v_n distributions are described by a two-dimensional Gaussian function for the underlying flow vector in central collisions for v_2 and over most of the measured centrality range for v_3 and v_4. Significant deviations from this function are observed for v_2 in mid-central and peripheral collisions, and a small deviation is observed for v_3 in mid-central collisions. It is shown that the commonly used multi-particle cumulants are insensitive to the deviations for v_2. The v_n distributions are also measured independently for charged particles with 0.5<pT<1 GeV and pT>1 GeV. When these distributions are rescaled to the same mean values, the adjusted shapes are found to be nearly the same for these two pT ranges. The v_n distributions are compared with the eccentricity distributions from two models for the initial collision geometry: a Glauber model and a model that includes corrections to the initial geometry due to gluon saturation effects. Both models fail to describe the experimental data consistently over most of the measured centrality range
S table Eχ tensions with(out) gravity

We investigate the vacuum stability as well as the gravitational corrections in extensions of the Standard Model featuring a new complex scalar, and two Dirac fermions for different choices of the hypercharge of the scalar and one of the two fermions. The neutral fermion acquires loop-induced magnetic interactions with the Standard Model and could be identified with a dark matter candidate. To the lowest order in perturbation theory we show that these extensions can save the electroweak vacuum from being metastable. We then add the gravitational corrections to the different beta functions and discover that the models can be compatible with the asymptotically safe gravity scenario at the price of a heavier Higgs and lighter top mass
A convenient implementation of the overlap between arbitrary Hartree–Fock–Bogoliubov vacua for projection

Overlap between Hartree–Fock–Bogoliubov (HFB) vacua is very important in the beyond mean-field calculations. However, in the HFB transformation, the <math altimg="si1.gif" xmlns="http://www.w3.org/1998/Math/MathML"><mi>U</mi><mo>,</mo><mi>V</mi></math> matrices are sometimes singular due to the exact emptiness ( <math altimg="si2.gif" xmlns="http://www.w3.org/1998/Math/MathML"><msub><mrow><mi>v</mi></mrow><mrow><mi>i</mi></mrow></msub><mo>=</mo><mn>0</mn></math> ) or full occupation ( <math altimg="si3.gif" xmlns="http://www.w3.org/1998/Math/MathML"><msub><mrow><mi>u</mi></mrow><mrow><mi>i</mi></mrow></msub><mo>=</mo><mn>0</mn></math> ) of some single-particle orbits. This singularity may cause some problem in evaluating the overlap between HFB vacua through Pfaffian. We found that this problem can be well avoided by setting those zero occupation numbers <math altimg="si4.gif" xmlns="http://www.w3.org/1998/Math/MathML"><msub><mrow><mi>u</mi></mrow><mrow><mi>i</mi></mrow></msub></math> , <math altimg="si5.gif" xmlns="http://www.w3.org/1998/Math/MathML"><msub><mrow><mi>v</mi></mrow><mrow><mi>i</mi></mrow></msub></math> to some tiny values denoted by <math altimg="si6.gif" xmlns="http://www.w3.org/1998/Math/MathML"><mi>ε</mi><mspace width="0.2em"/><mo stretchy="false">(</mo><mo>&gt;</mo><mn>0</mn><mo stretchy="false">)</mo></math> , which numerically satisfies <math altimg="si7.gif" xmlns="http://www.w3.org/1998/Math/MathML"><mn>1</mn><mo>+</mo><msup><mrow><mi>ε</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>=</mo><mn>1</mn></math> (e.g., <math altimg="si8.gif" xmlns="http://www.w3.org/1998/Math/MathML"><mi>ε</mi><mo>=</mo><msup><mrow><mn>10</mn></mrow><mrow><mo>−</mo><mn>8</mn></mrow></msup></math> when using the double precision data type). This treatment does not change the HFB vacuum state because <math altimg="si9.gif" xmlns="http://www.w3.org/1998/Math/MathML"><msubsup><mrow><mi>u</mi></mrow><mrow><mi>i</mi></mrow><mrow><mn>2</mn></mrow></msubsup><mo>,</mo><msubsup><mrow><mi>v</mi></mrow><mrow><mi>i</mi></mrow><mrow><mn>2</mn></mrow></msubsup><mo>=</mo><msup><mrow><mi>ε</mi></mrow><mrow><mn>2</mn></mrow></msup></math> are numerically zero relative to 1. Therefore, for arbitrary HFB transformation, we say that the U , V matrices can always be nonsingular. From this standpoint, we present a new convenient Pfaffian formula for the overlap between arbitrary HFB vacua, which is especially suitable for symmetry restoration. Testing calculations have been performed for this new formula. It turns out that our method is reliable and accurate in evaluating the overlap between arbitrary HFB vacua
Muon-induced background to proton decay in the p→K+ν decay channel with large underground liquid argon TPC detectors

Large liquid argon TPC detector programs such as LBNE and LAGUNA-LBNO will be able to make measurements of the proton lifetime which will outperform Cherenkov detectors in the proton decay channel p→K+ν . At the large depths which are proposed for such experiments, a non-negligible source of isolated charged kaons may be produced in the showers of cosmogenic muons. We present an estimate of the cosmogenic muon background to proton decay in the p→K+ν channel. The simulation of muon transport to a depth of 4 km w.e. is performed in the MUSIC framework and the subsequent propagation of muons and secondary particles in the vicinity of a cylindrical 20 kt LAr target is performed using Geant 4. An exposure time of 100 years is considered, with a rate of <0.0012 events/kt/year at 90% CL predicted from our simulations