pinecone/core-2020-05-10-deduplication huggingface dataset:
MAGIC Upper Limits for two Milagro-detected, Bright Fermi Sources in the
  Region of SNR G65.1+0.6

We report on the observation of the region around supernova remnant G65.1+0.6
with the stand-alone MAGIC-I telescope. This region hosts the two bright GeV
gamma-ray sources 1FGL J1954.3+2836 and 1FGL J1958.6+2845. They are identified
as GeV pulsars and both have a possible counterpart detected at about 35 TeV by
the Milagro observatory. MAGIC collected 25.5 hours of good quality data, and
found no significant emission in the range around 1 TeV. We therefore report
differential flux upper limits, assuming the emission to be point-like (<0.1
deg) or within a radius of 0.3 deg. In the point-like scenario, the flux limits
around 1 TeV are at the level of 3 % and 2 % of the Crab Nebula flux, for the
two sources respectively. This implies that the Milagro emission is either
extended over a much larger area than our point spread function, or it must be
peaked at energies beyond 1 TeV, resulting in a photon index harder than 2.2 in
the TeV band.Comment: 8 pages, 3 figures, 1 tabl
Design Concepts for the Cherenkov Telescope Array

Ground-based gamma-ray astronomy has had a major breakthrough with the
impressive results obtained using systems of imaging atmospheric Cherenkov
telescopes. Ground-based gamma-ray astronomy has a huge potential in
astrophysics, particle physics and cosmology. CTA is an international
initiative to build the next generation instrument, with a factor of 5-10
improvement in sensitivity in the 100 GeV to 10 TeV range and the extension to
energies well below 100 GeV and above 100 TeV. CTA will consist of two arrays
(one in the north, one in the south) for full sky coverage and will be operated
as open observatory. The design of CTA is based on currently available
technology. This document reports on the status and presents the major design
concepts of CTA.Comment: 115 pages, 54 figures, 5 table
The Origin of Gamma-Rays from Globular Clusters

Fermi has detected gamma-ray emission from eight globular clusters. We
suggest that the gamma-ray emission from globular clusters may result from the
inverse Compton scattering between relativistic electrons/positrons in the
pulsar wind of MSPs in the globular clusters and background soft photons
including cosmic microwave/relic photons, background star lights in the
clusters, the galactic infrared photons and the galactic star lights. We show
that the gamma-ray spectrum from 47 Tuc can be explained equally well by upward
scattering of either the relic photons, the galactic infrared photons or the
galactic star lights whereas the gamma-ray spectra from other seven globular
clusters are best fitted by the upward scattering of either the galactic
infrared photons or the galactic star lights. We also find that the observed
gamma-ray luminosity is correlated better with the combined factor of the
encounter rate and the background soft photon energy density. Therefore the
inverse Compton scattering may also contribute to the observed gamma-ray
emission from globular clusters detected by Fermi in addition to the standard
curvature radiation process. Furthermore, we find that the emission region of
high energy photons from globular cluster produced by inverse Compton
scattering is substantially larger than the core of globular cluster with a
radius >10pc. The diffuse radio and X-rays emitted from globular clusters can
also be produced by synchrotron radiation and inverse Compton scattering
respectively. We suggest that future observations including radio, X-rays, and
gamma-rays with energy higher than 10 GeV and better angular resolution can
provide better constraints for the models.Comment: Accepted by ApJ, Comments may send to Prof. K.S. Cheng:
  hrspksc@hkucc.hku.h
Optical response and spin relaxation in semiconductor systems under
  excitation with arbitrary polarization

The equations-of-motion for the density matrix are derived in a multiband
model to describe the response of semiconductors (bulk or quantum well
structures) under optical excitation with arbitrary polarization. The multiband
model used, comprising the twofold conduction band and the fourfold topmost
valence band (or heavy- and light-hole states), incorporates spin-splitting of
the single-particle states. The interaction terms include besides the direct
Coulomb coupling between carriers also the electron-hole exchange interaction,
which together with the spin-splitting terms is responsible for spin
relaxation. Applying the Hartree-Fock truncation scheme leads to a set of
coherent semiconductor Bloch equations for the multiband case. This concept
provides the theoretical frame for describing phenomena connected with optical
response under excitation with arbitrary light polarization and spin
relaxation: polarized optical response, polarization dynamics of VCSELs, spin
relaxation, and the circular photovoltaic effect.Comment: 11 pages, no figure
Towards the lattice study of M-theory (II)

We present new results of the quenched simulations of the reduced D=4
supersymmetric Yang - Mills quantum mechanics for larger gauge groups SU(N),
2<N<9. The model, studied at finite temperature, reveals existence of the two
distinct regions which may be precursors of a black hole and the elementary D0
branes phases of M-theory conjectured in the literature. Present results for
higher groups confirm the picture found already for N=2. Similar behaviour is
observed in the preliminary simulations for the D=6 and D=10 models.Comment: Talk presented at XIX International Symposium on Lattice Field Theory
  lattice2001(surfaces
Interpreting the time-dependent CP asymmetry in $B^0 \to \pi^0 K_S$

Flavor SU(3) is used for studying the time-dependent CP asymmetry in $B^0 \to
\pi^0 K_S$ by relating this process to $B^0\to \pi^0\pi^0$ and $B^0 \to
K^+K^-$. We calculate correlated bounds on $S_{\pi K} - \sin 2\beta$ and
$C_{\pi K}$, with maximal magnitudes of 0.2 and 0.3, where $S_{\pi K}$ and
$C_{\pi K}$ are coefficients of $\sin\Delta mt$ and $\cos\Delta mt$ in the
asymmetry. Stronger upper limits on $B^0 \to K^+K^-$ are expected to reduce
these bounds and to imply nonzero lower limits on these observables. The
asymmetry is studied as a function of a strong phase and the weak phase
$\gamma$.Comment: 11 pages, 2 figures, to be published in Phys. Lett. B. Some equations
  corrected leading to small changes in figure
Diversity of GRB energetics vs. SN homogeneity: supernova 2013cq
  associated with the gamma-ray burst 130427A

Long-duration gamma-ray bursts (GRBs) have been found to be associated with
broad-lined type-Ic supernovae (SNe), but only a handful of cases have been
studied in detail. Prompted by the discovery of the exceptionally bright,
nearby GRB130427A (redshift z=0.3399), we aim at characterising the properties
of its associated SN2013cq. This is the first opportunity to test directly the
progenitors of high-luminosity GRBs. We monitored the field of the Swift long
duration GRB130427A using the 3.6-m TNG and the 8.2-m VLT during the time
interval between 3.6 and 51.6 days after the burst. Photometric and
spectroscopic observations revealed the presence of the type Ic SN2013cq.
Spectroscopic analysis suggests that SN2013cq resembles two previous GRB-SNe,
SN1998bw and SN2010bh associated with GRB980425 and XRF100316D, respectively.
The bolometric light curve of SN2013cq, which is significantly affected by the
host galaxy contribution, is systematically more luminous than that of SN2010bh
($\sim$ 2 mag at peak), but is consistent with SN1998bw. The comparison with
the light curve model of another GRB-connected SN2003dh, indicates that
SN2013cq is consistent with the model when brightened by 20%. This suggests a
synthesised radioactive $^{56}$Ni mass of $\sim 0.4 M_\odot$.
GRB130427A/SN2013cq is the first case of low-z GRB-SN connection where the GRB
energetics are extreme ($E_{\rm \gamma, iso} \sim 10^{54}$ erg). We show that
the maximum luminosities attained by SNe associated with GRBs span a very
narrow range, but those associated with XRFs are significantly less luminous.
On the other hand the isotropic energies of the accompanying GRBs span 6 orders
of magnitude (10$^{48}$ erg $< E_{\rm \gamma, iso} <$ 10$^{54}$ erg), although
this range is reduced when corrected for jet collimation. The GRB total
radiated energy is in fact a small fraction of the SN energy budget.Comment: To appear in Astronomy and Astrophysics: 10 pages, 5 figure
Jet Vetoes Interfering with H->WW

Far off-shell Higgs production in $H \rightarrow WW,ZZ$, is a particularly
powerful probe of Higgs properties, allowing one to disentangle Higgs width and
coupling information unavailable in on-shell rate measurements. These
measurements require an understanding of the cross section in the far off-shell
region in the presence of realistic experimental cuts. We analytically study
the effect of a $p_T$ jet veto on far off-shell cross sections, including
signal-background interference, by utilizing hard functions in the soft
collinear effective theory that are differential in the decay products of the
$W/Z$. Summing large logarithms of $\sqrt{\hat s}/p_T^{veto}$, we find that the
jet veto induces a strong dependence on the partonic centre of mass energy,
$\sqrt{\hat s}$, and modifies distributions in $\sqrt{\hat s}$ or $M_T$. The
example of $gg\rightarrow H \rightarrow WW$ is used to demonstrate these
effects at next to leading log order. We also discuss the importance of jet
vetoes and jet binning for the recent program to extract Higgs couplings and
widths from far off-shell cross sections.Comment: 31 pages, 8 figures. v2: Journal Versio
MUSE integral-field spectroscopy towards the Frontier Fields Cluster
  Abell S1063: I. Data products and redshift identifications

We present the first observations of the Frontier Fields Cluster Abell S1063
taken with the newly commissioned Multi Unit Spectroscopic Explorer (MUSE)
integral field spectrograph. Because of the relatively large field of view (1
arcmin^2), MUSE is ideal to simultaneously target multiple galaxies in blank
and cluster fields over the full optical spectrum. We analysed the four hours
of data obtained in the Science Verification phase on this cluster and measured
redshifts for 53 galaxies. We confirm the redshift of five cluster galaxies,
and determine the redshift of 29 other cluster members. Behind the cluster, we
find 17 galaxies at higher redshift, including three previously unknown
Lyman-alpha emitters at z>3, and five multiply-lensed galaxies. We report the
detection of a new z=4.113 multiply lensed galaxy, with images that are
consistent with lensing model predictions derived for the Frontier Fields. We
detect C III], C IV, and He II emission in a multiply lensed galaxy at z=3.116,
suggesting the likely presence of an active galactic nucleus. We also created
narrow-band images from the MUSE datacube to automatically search for
additional line emitters corresponding to high-redshift candidates, but we
could not identify any significant detections other than those found by visual
inspection. With the new redshifts, it will become possible to obtain an
accurate mass reconstruction in the core of Abell S1063 through refined strong
lensing modelling. Overall, our results illustrate the breadth of scientific
topics that can be addressed with a single MUSE pointing. We conclude that MUSE
is a very efficient instrument to observe galaxy clusters, enabling their mass
modelling, and to perform a blind search for high-redshift galaxies.Comment: 11 pages, 10 figures, accepted for publication in A&
A "general boundary" formulation for quantum mechanics and quantum
  gravity

I propose to formalize quantum theories as topological quantum field theories
in a generalized sense, associating state spaces with boundaries of arbitrary
(and possibly finite) regions of space-time. I further propose to obtain such
``general boundary'' quantum theories through a generalized path integral
quantization. I show how both, non-relativistic quantum mechanics and quantum
field theory can be given a ``general boundary'' formulation. Surprisingly,
even in the non-relativistic case, features normally associated with quantum
field theory emerge from consistency conditions. This includes states with
arbitrary particle number and pair creation. I also note how three dimensional
quantum gravity is an example for a realization of both proposals and suggest
to apply them to four dimensional quantum gravity.Comment: 5 pages, 2 figures, LaTeX + revtex4 + eps; abstract shortened, other
  minor corrections, references update
Phenomenology of Large $N_{c}$ QCD

These lectures are designed to introduce the methods and results of large N_c QCD in a presentation intended for nuclear and particle physicists alike. Beginning with definitions and motivations of the approach, we demonstrate that all quark and gluon Feynman diagrams are organized into classes based on powers of 1/N_c. We then show that this result can be translated into definite statements about mesons and baryons containing arbitrary numbers of constituents. In the mesons, numerous well-known phenomenological properties follow as immediate consequences of simply counting powers of N_c, while for the baryons, quantitative large N_c analyses of masses and other properties are seen to agree with experiment, even when ``large'' N_c is set equal to its observed value of 3. Large N_c reasoning is also used to explain some simple features of nuclear interactions
The accretion of planets and brown dwarfs by giant stars; 2, solar mass stars on the red giant branch

This paper extends our previous study of planet/brown dwarf accretion by giant stars to solar mass stars located on the red giant branch. The model assumes that the planet is dissipated at the bottom of the convective envelope of the giant star. The giant's evolution is then followed in detail. We analyze the effects of different accretion rates and different initial conditions. The computations indicate that the accretion process is accompanied by a substantial expansion of the star, and in the case of high accretion rates, hot bottom burning can be activated. The possible observational signatures that accompany the engulfing of a planet are also extensively investigated. They include : the ejection of a shell and a subsequent phase of IR emission, an increase in the 7Li surface abundance and a potential stellar metallicity enrichment, spin-up of the star due to the deposition of orbital angular momentum, the possible generation of magnetic fields and a related X-ray activity due to the development of shear at the base of the convective envelope, and the effects on the morphology of the horizontal branch in globular clusters. We propose that the IR excess and high Li abundance observed in 4-8% of the G and K giants originate from the accretion of a giant planet, a brown dwarf or a very low-mass star
Noncritical M-theory and the Gross-Neveu model in 2+1 dimensions

We point out a non-trivial connection between the model proposed by Horava
and Keeler as a candidate for noncritical M-theory and the Gross-Neveu model
with fermionic fields obeying periodic boundary conditions in 2+1 dimensions.
Specifically, the vacuum energy of the former is identified with the large-N
free-energy of the latter up to an overall constant. This identification
involves an appropriate analytic continuation of the subtraction point in
noncritical M-theory, which is related to the volume of the Liouville
dimension. We show how the world-sheet cosmological constant may be obtained
from the Gross-Neveu model. At its critical point, which is given in terms of
the golden mean, the values of the vacuum energy and of the cosmological
constant are 4/5 and 2/5 of the corresponding values at infinite string
coupling constant.Comment: 10 pages, improved discussion to appear in Phys. Lett.
Measurement of the W-Pair Production Cross Section and W-Decay Branching Fractions in $e^{+}e^{-}$ Interactions at $\sqrt{s}$= 189 GeV

The data collected by the L3 experiment at LEP at a centre-of-mass energy of $188.6~\rm{Ge\kern -0.1em V}$ are used to measure the W-pair production cross section and the W-boson decay branching fractions. These data correspond to an integrated luminosity of 176.8~pb$^{-1}$. The total cross section for W-pair production, combining all final states, is measured to be $\sigma_{\rm{WW}}= 16.24 \pm 0.37~(stat.) \pm 0.22~(syst.)$~pb. Including our data collected at lower centre-of-mass energies, the hadronic branching fraction of the W-boson is determined to be $ B(\rm{W} \rightarrow \rm{qq})= \left[ 68.20 \pm 0.68~(stat.) \pm 0.33~(syst.)\right]~\%$. The results agree with the Standard Model predictions.The data collected by the L3 experiment at LEP at a centre-of-mass energy of 188.6 GeV are used to measure the W-pair production cross section and the W-boson decay branching fractions. These data correspond to an integrated luminosity of 176.8pb^-1. The total cross section for W-pair production, combining all final states, is measured to be sigma_WW = 16.24 +/- 0.37(stat.) +/- 0.22(syst.) pb. Including our data collected at lower centre-of-mass energies, the hadronic branching fraction of the W-boson is determined to be B(W ->qq) = [68.20 +/- 0.68 (stat.) +/- 0.33 (syst.) ] %. The results agree with the Standard Model predictions.The data collected by the L3 experiment at LEP at a centre-of-mass energy of 188.6 GeV are used to measure the W-pair production cross section and the W-boson decay branching fractions. These data correspond to an integrated luminosity of 176.8 pb −1 . The total cross section for W-pair production, combining all final states, is measured to be σ WW =16.24±0.37 (stat.)±0.22 (syst.) pb. Including our data collected at lower centre-of-mass energies, the hadronic branching fraction of the W-boson is determined to be B (W→qq)=[68.20±0.68 (stat.)±0.33 (syst.)]%. The results agree with the Standard Model predictions
Planck Scale Physics of the Single Particle Schrodinger Equation with Gravitational Self-Interaction

We consider the modification of a single particle Schr\"{o}dinger equation by the inclusion of an additional gravitational self-potential term which follows from the prescription that the' mass-density'that enters this term is given by $m |\psi (\vec {r},t)|^2$, where $\psi (\vec {r}, t)$ is the wavefunction and $m$ is the mass of the particle. This leads to a nonlinear equation, the ' Newton Schrodinger' equation, which has been found to possess stationary self-bound solutions, whose energy can be determined exactly using an asymptotic method. We find that such a particle strongly violates superposition and becomes a black hole as its mass approaches the Planck mass
Heavy quark colorimetry of QCD matter

We consider propagation of heavy quarks in QCD matter. Because of large quark mass, the radiative quark energy loss appears to be qualitatively different from that of light quarks at all energies of practical importance. Finite quark mass effects lead to an in-medium enhancement of the heavy-to-light D/\pi ratio at moderately large (5--10 GeV) transverse momenta. For hot QCD matter a large enhancement is expected, whose magnitude and shape are exponentially sensitive to the density of colour charges in the medium
The $q_{T}$ spectrum of the Higgs boson at the LHC in QCD perturbation theory

We consider the transverse-momentum (q_T) distribution of Higgs bosons produced at hadron colliders. We use a formalism that uniformly treats both the small-q_T and large-q_T regions in QCD perturbation theory. At small q_T (q_T << M_H, M_H being the mass of the Higgs boson), we implement an all-order resummation of logarithmically-enhanced contributions up to next-to-next-to-leading logarithmic accuracy. At large q_T (q_T \gtap M_H), we use fixed-order perturbation theory up to next-to-leading order. The resummed and fixed-order approaches are consistently matched by avoiding double-counting in the intermediate-q_T region. In this region, the introduction of unjustified higher-order terms is avoided by imposing unitarity constraints, so that the integral of the q_T spectrum exactly reproduces the perturbative result for the total cross section up to next-to-next-to-leading order. Numerical results at the LHC are presented. These show that the main features of the q_T distribution are quite stable with respect to perturbative QCD uncertainties
On energy functionals, Kahler-Einstein metrics, and the
  Moser-Trudinger-Onofri neighborhood

We prove that the existence of a Kahler-Einstein metric on a Fano manifold is
equivalent to the properness of the energy functionals defined by Bando, Chen,
Ding, Mabuchi and Tian on the set of Kahler metrics with positive Ricci
curvature. We also prove that these energy functionals are bounded from below
on this set if and only if one of them is. This answers two questions raised by
X.-X. Chen. As an application, we obtain a new proof of the classical
Moser-Trudinger-Onofri inequality on the two-sphere, as well as describe a
canonical enlargement of the space of Kahler potentials on which this
inequality holds on higher-dimensional Fano Kahler-Einstein manifolds.Comment: v2: 1. style and exposition changes made, 2. added Remark 4.5, 3.
  added several references. v3: added footnote on p. 8. v4: minor changes. To
  appear in Journal of Functional Analysi
Homotopy types of complements of 2-arrangements in R^4

We study the homotopy types of complements of arrangements of n transverse
planes in R^4, obtaining a complete classification for n <= 6, and lower bounds
for the number of homotopy types in general. Furthermore, we show that the
homotopy type of a 2-arrangement in R^4 is not determined by the cohomology
ring, thereby answering a question of Ziegler. The invariants that we use are
derived from the characteristic varieties of the complement. The nature of
these varieties illustrates the difference between real and complex
arrangements.Comment: LaTeX2e, 25 pages with 5 figures. Revised version, to appear in
  Topolog
Independent Measurement of the Total Active 8B Solar Neutrino Flux Using an Array of 3He Proportional Counters at the Sudbury Neutrino Observatory

The Sudbury Neutrino Observatory (SNO) used an array of He3 proportional counters to measure the rate of neutral-current interactions in heavy water and precisely determined the total active (x) B8 solar neutrino flux. This technique is independent of previous methods employed by SNO. The total flux is found to be 5.54-0.31+0.33(stat)-0.34+0.36(syst)106cm-2s-1, in agreement with previous measurements and standard solar models. A global analysis of solar and reactor neutrino results yields m2=7.59-0.21+0.1910-5eV2 and =34.4-1.2+1.3 degrees. The uncertainty on the mixing angle has been reduced from SNO's previous results