pinecone/core-2020-05-10-deduplication huggingface dataset:
Insights into the high-energy gamma-ray emission of Markarian 501 from extensive multifrequency observations in the Fermi era\ud

We report on the gamma-ray activity of the blazar Mrk 501 during the first 480 days of Fermi operation. We find that the average Large Area Telescope (LAT) gamma-ray spectrum of Mrk 501 can be well described by a single power-law function with a photon index of 1.78 +/- 0.03. While we observe relatively mild flux variations with the Fermi-LAT (within less than a factor of two), we detect remarkable spectral variability where the hardest observed spectral index within the LAT energy range is 1.52 +/- 0.14, and the softest one is 2.51 +/- 0.20. These unexpected spectral changes do not correlate with the measured flux variations above 0.3 GeV. In this paper, we also present the first results from the 4.5 month long multifrequency campaign (2009 March 15-August 1) on Mrk 501, which included the Very Long Baseline Array (VLBA), Swift, RXTE, MAGIC, and VERITAS, the F-GAMMA, GASP-WEBT, and other collaborations and instruments which provided excellent temporal and energy coverage of the source throughout the entire campaign. The extensive radio to TeV data set from this campaign provides us with the most detailed spectral energy distribution yet collected for this source during its relatively low activity. The average spectral energy distribution of Mrk 501 is well described by the standard one-zone synchrotron self-Compton (SSC) model. In the framework of this model, we find that the dominant emission region is characterized by a size less than or similar to 0.1 pc (comparable within a factor of few to the size of the partially resolved VLBA core at 15-43 GHz), and that the total jet power (similar or equal to 10(44) erg s(-1)) constitutes only a small fraction (similar to 10(-3)) of the Eddington luminosity. The energy distribution of the freshly accelerated radiating electrons required to fit the time-averaged data has a broken power-law form in the energy range 0.3 GeV-10 TeV, with spectral indices 2.2 and 2.7 below and above the break energy of 20 GeV. We argue that such a form is consistent with a scenario in which the bulk of the energy dissipation within the dominant emission zone of Mrk 501 is due to relativistic, proton-mediated shocks. We find that the ultrarelativistic electrons and mildly relativistic protons within the blazar zone, if comparable in number, are in approximate energy equipartition, with their energy dominating the jet magnetic field energy by about two orders of magnitude.\u
Entanglement and correlations near extremality : CFTs dual to Reissner-Nordström AdS5.\ud

We use the AdS/CFT correspondence to study models of entanglement and correlations between two d = 4 CFTs in thermofield double states at finite chemical potential. Our bulk spacetimes are planar Reissner-Nordström AdS black holes. We compute both thermo-mutual information and the two-point correlators of large-dimension scalar operators, focussing on the small-temperature behavior — an infrared limit with behavior similar to that seen at large times. The interesting feature of this model is of course that the entropy density remains finite as T → 0 while the bulk geometry develops an infinite throat. This leads to a logarithmic divergence in the scale required for non-zero mutual information between equal-sized strips in the two CFTs, though the mutual information between one entire CFT and a finite-sized strip in the other can remain non-zero even at T =0. Furthermore,despitetheinfinitethroat,therecanbeextremallychargedoperators for which the two-point correlations remain finite as T → 0. This suggests an interestingly mixed picture in which some aspects of the entanglement remain localized on scales set by the chemical potential, while others shift to larger and larger scales. We also comment on implications for the localized-quasiparticle picture of entanglement
Spectroscopic properties of cool Ursa Major group members

Until now, most members of the Ursa Major (UMa) group of stars have been
identified by means of kinematic criteria. However, in many cases kinematic
criteria alone are insufficient to ascertain, whether an individual star is
really a member of this group. Since photometric criteria are ineffective in
the case of cool dwarf members, one must use spectroscopic criteria.
Nevertheless, resulting membership criteria are inconclusive. We reanalyse
spectroscopic properties of cool UMa group dwarfs. In particular, we study the
distribution of iron abundance, the strength of the Li I absorption at 6708 A
and the Li abundance, and the infilling of the core of the H alpha line.
Twenty-five cool and northern bona-fide members are carefully selected from the
literature. Homogeneously measured stellar parameters and iron abundances are
given for all Sun-like stars selected, based on spectra of high resolution and
high signal-to-noise ratio. In addition, we measure the Li equivalent width and
abundance as well as the relative intensity of the H alpha core and the
corresponding chromospheric flux. The studied stars infer an average Ursa Major
group iron abundance of -0.03+-0.05 dex, which is higher by about 0.06 dex than
determined elsewhere. The Li abundance derived of Ursa Major group dwarf stars
is higher than in the Hyades at effective temperatures cooler than the Sun, but
lower than in the younger Pleiades, a result which is independent of the exact
value of the effective temperature adopted. The Sun-like and cooler dwarfs also
display chromospheric infilling of the H alpha core. We present spectroscopic
criteria that may be used to exclude non-members.Comment: accepted for publication in A&A, 19 pages, 10 figures, 7 table
Nonlinear Supersymmetry, Brane-bulk Interactions and Super-Higgs without
  Gravity

We derive the coupling of a hypermultiplet of N=2 global supersymmetry to the
Dirac-Born-Infeld Maxwell theory with linear N=1 and a second nonlinear
supersymmetry. At the level of global supersymmetry, this construction
corresponds to the interaction with Maxwell brane fields of bulk
hypermultiplets, such as the universal dilaton of type IIB strings compactified
on a Calabi-Yau manifold. It displays in particular the active role of a
four-form field. Constrained N=1 and N=2 superfields and the formulation of the
hypermultiplet in its single-tensor version are used to derive the nonlinear
realization, allowing a fully off-shell description. Exact results with
explicit symmetries and supersymmetries are then obtained. The
electric-magnetic dual version of the theory is also derived and the gauge
structure of the interaction is exemplified with N=2 nonlinear QED of a charged
hypermultiplet. Its Higgs phase describes a novel super-Higgs mechanism without
gravity, where the goldstino is combined with half of the hypermultiplet into
an N=1 massive vector multiplet.Comment: 42 page
The exact decomposition of gauge variables in lattice Yang-Mills theory

In this paper, we consider lattice versions of the decomposition of the Yang-
Mills field a la Cho-Faddeev-Niemi, which was extended by Kondo, Shinohara and
Murakami in the continuum formulation. For the SU(N) gauge group, we propose a
set of defining equations for specifying the decomposition of the gauge link
variable and solve them exactly without using the ansatz adopted in the
previous studies for SU(2) and SU(3). As a result, we obtain the general form
of the decomposition for SU(N) gauge link variables and confirm the previous
results obtained for SU(2) and SU(3).Comment: 16 page
Inter-layer Edge Tunneling and Transport Properties in Double-Layer
  Quantum Hall Systems

A theory of transport in the quantum Hall regime is developed for separately
contacted double-layer electron systems. Inter-layer tunneling provides a
channel for equilibration of the distribution functions in the two layers and
influences transport properties through the resulting influence on steady-state
distribution functions. Resistences for various configurations of the
electrodes are calculated as a function of the inter-layer tunneling amplitude.
The effect of misalignment of the edges of the two layers and the effect of
tilting the magnetic field away from the normal to the layers on the inter-
layer tunneling amplitude near the sample edges are investigated. The results
obtained in this work is consistent with recent experiments.Comment: 4 pages, uses sprocl.sty, one PS figures to be included by psfig.
  Paper to be published at Int. Conf. on "High Magnetic Fields in Semiconductor
  Physics", Wuerzburg, 28 July-02 August, 199
Ruling out four-neutrino oscillation interpretations of the LSND
  anomaly?

Prompted by recent solar and atmospheric data, we re-analyze the
four-neutrino description of current global neutrino oscillation data,
including the LSND evidence for oscillations. The higher degree of rejection
for non-active solar and atmospheric oscillation solutions implied by the SNO
neutral current result as well as by the latest 1489-day Super-K atmospheric
neutrino data allows us to rule out (2+2) oscillation schemes proposed to
reconcile LSND with the rest of current neutrino oscillation data. Using an
improved goodness of fit (gof) method especially sensitive to the combination
of data sets we obtain a gof of only 1.6 times 10^{-6} for (2+2) schemes.
Further, we re-evaluate the status of (3+1) oscillations using two different
analyses of the LSND data sample. We find that also (3+1) schemes are strongly
disfavoured by the data. Depending on the LSND analysis we obtain a gof of 5.6
times 10^{-3} or 7.6 times 10^{-5}. This leads to the conclusion that all
four-neutrino descriptions of the LSND anomaly, both in (2+2) as well as (3+1)
realizations, are highly disfavoured. Our analysis brings the LSND hint to a
more puzzling status.Comment: 21 pages, 7 figure
MOA-2010-BLG-328Lb: a sub-Neptune orbiting very late M dwarf ?

We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit
yields host and planetary masses of Mh = 0.11+/-0.01 M_{sun} and Mp =
9.2+/-2.2M_Earth, corresponding to a very late M dwarf and sub-Neptune-mass
planet, respectively. The system lies at DL = 0.81 +/- 0.10 kpc with projected
separation r = 0.92 +/- 0.16 AU. Because of the host's a-priori-unlikely close
distance, as well as the unusual nature of the system, we consider the
possibility that the microlens parallax signal, which determines the host mass
and distance, is actually due to xallarap (source orbital motion) that is being
misinterpreted as parallax. We show a result that favors the parallax solution,
even given its close host distance. We show that future high-resolution
astrometric measurements could decisively resolve the remaining ambiguity of
these solutions.Comment: 30 pages, 6 figures. accepted for publication in ApJ. Figure 1 and 2
  are update
Pillars and globules at the edges of H ii regions, Confronting Herschel
  observations and numerical simulations

Pillars and globules are present in many high-mass star-forming regions, such
as the Eagle nebula (M16) and the Rosette molecular cloud, and understanding
their origin will help characterize triggered star formation. The formation
mechanisms of these structures are still being debated. Recent numerical
simulations have shown how pillars can arise from the collapse of the shell in
on itself and how globules can be formed from the interplay of the turbulent
molecular cloud and the ionization from massive stars. The goal here is to test
this scenario through recent observations of two massive star-forming regions,
M16 and Rosette. The column density structure of the interface between
molecular clouds and H ii regions was characterized using column density maps
obtained from far-infrared imaging of the Herschel HOBYS key programme. Then,
the DisPerSe algorithm was used on these maps to detect the compressed layers
around the ionized gas and pillars in different evolutionary states. Finally,
their velocity structure was investigated using CO data, and all observational
signatures were tested against some distinct diagnostics established from
simulations. The column density profiles have revealed the importance of
compression at the edge of the ionized gas. The velocity properties of the
structures, i.e. pillars and globules, are very close to what we predict from
the numerical simulations. We have identified a good candidate of a nascent
pillar in the Rosette molecular cloud that presents the velocity pattern of the
shell collapsing on itself, induced by a high local curvature. Globules have a
bulk velocity dispersion that indicates the importance of the initial
turbulence in their formation, as proposed from numerical simulations.
Altogether, this study re-enforces the picture of pillar formation by shell
collapse and globule formation by the ionization of highly turbulent clouds.Comment: Accepted in A&
Coulomb branch Hilbert series and Hall-Littlewood polynomials

There has been a recent progress in understanding the chiral ring of 3d
$\mathcal{N}=4$ superconformal gauge theories by explicitly constructing an
exact generating function (Hilbert series) counting BPS operators on the
Coulomb branch. In this paper we introduce Coulomb branch Hilbert series in the
presence of background magnetic charges for flavor symmetries, which are useful
for computing the Hilbert series of more general theories through gluing
techniques. We find a simple formula of the Hilbert series with background
magnetic charges for $T_\rho(G)$ theories in terms of Hall-Littlewood
polynomials. Here $G$ is a classical group and $\rho$ is a certain partition
related to the dual group of $G$. The Hilbert series for vanishing background
magnetic charges show that Coulomb branches of $T_\rho(G)$ theories are
complete intersections. We also demonstrate that mirror symmetry maps
background magnetic charges to baryonic charges.Comment: v1: 40 pages + appendices, 3 figures; v2: minor revision, version to
  appear in JHE
D-instantons on orbifolds and gauge/gravity correspondence

D-instantons are used to probe the near-horizon geometry of D3-branes systems
on orbifold spaces. For fractional D3-branes, D-instanton calculus correctly
reproduces the gauge beta-function and U(1)_R anomaly of the corresponding N=2
non-conformal Super Yang-Mills theories. For D3-branes wrapping the orbifold
singularity, D-instantons can be identified with gauge instantons on ALE space,
providing evidence of AdS/CFT duality for gauge theories on curved spaces.Comment: minor changes, one reference adde
An Invariant Action for Noncommutative Gravity in Four-Dimensions

Two main problems face the construction of noncommutative actions for gravity
with star products: the complex metric and finding an invariant measure. The
only gauge groups that could be used with star products are the unitary groups.
I propose an invariant gravitational action in D=4 dimensions based on the
constrained gauge group U(2,2) broken to $U(1,1)\times U(1,1).$ No metric is
used, thus giving a naturally invariant measure. This action is generalized to
the noncommutative case by replacing ordinary products with star products. The
four dimensional noncommutative action is studied and the deformed action to
first order in deformation parameter is computed.Comment: 11 pages. Paper shortened. Consideration is now limited to gravity in
  four-dimension
Embedding of the bosonic string into the W$_{3}$ string

We construct new realisations of the W_3 algebra with arbitrary central charge, making use of the fact that this algebra can be linearised by the inclusion of a spin-1 current. We use the new realisations with c=102 and c=100 to build non-critical and critical W_3 BRST operators. Both of these can be converted by local canonical transformations into a BRST operator for the Virasoro string with c=28-2, together with a Kugo-Ojima topological term. Consequently, the new realisations provide embeddings of the Virasoro string into non-critical and critical W_3 strings
Rotational properties of {252, 253, 254} No: Influence of pairing correlations

Rotational bands of $^{252, 253, 254}$No and the fission barriers of $^{254}$No at spin 0$\hbar$ and 20$\hbar$ are calculated with the Hartree-Fock-Bogolyubov theory and the Lipkin-Nogami approximate particle number projection. The SLy4 Skyrme force is used in the particle-hole channel. A zero-range force with and without density-dependence is used in the particle-particle channel. The experimental ground state deformation (${\cal{Q}}_{20}$ = 32.8 b) is reproduced as well as the increase of the dynamical moment of inertia with frequency both for $^{252}$No and $^{254}$No. The rotational band of $^{253}$No is also calculated. Fission barriers of $^{254}$No at spin 0$\hbar$ and 20$\hbar$ show the robustness of shell-corrections against rotation in these heavy nuclei
Dualities in D=5, N=2 Supergravity, Black Hole Entropy, and AdS Central Charges

The issue of microstate counting for general black holes in D=5, N=2 supergravity coupled to vector multiplets is discussed from various viewpoints. The statistical entropy is computed for the near-extremal case by using the central charge appearing in the asymptotic symmetry algebra of AdS_2. Furthermore, we show that the considered supergravity theory enjoys a duality invariance which connects electrically charged black holes and magnetically charged black strings. The near-horizon geometry of the latter turns out to be AdS_3 x S^2, which allows a microscopic calculation of their entropy using the Brown-Henneaux central charges in Cardy's formula. In both approaches we find perfect agreement between statistical and thermodynamical entropy
Massive Star Evolution: Nucleosynthesis and Nuclear Reaction Rate Uncertainties

We present a nucleosynthesis calculation of a 25 solar mass star of solar composition that includes all relevant isotopes up to polonium. In particular, all stable isotopes and necessary nuclear reaction rates are covered. We follow the stellar evolution from hydrogen burning till iron core collapse and simulate the explosion using a ``piston'' approach. We discuss the influence of two key nuclear reaction rates, C12(a,g) and Ne22(a,n), on stellar evolution and nucleosynthesis. The former significantly influences the resulting core sizes (iron, silicon, oxygen) and the overall presupernova structure of the star. It thus has significant consequences for the supernova explosion itself and the compact remnant formed. The later rate considerably affects the s-process in massive stars and we demonstrate the changes that different currently suggested values for this rate cause
New spectroscopic and polarimetric observations of the A0 supergiant
  HD92207

Our recent search for the presence of a magnetic field in the bright early
A-type supergiant HD92207 using FORS2 in spectropolarimetric mode revealed the
presence of a longitudinal magnetic field of the order of a few hundred Gauss.
However, the definite confirmation of the magnetic nature of this object
remained pending due to the detection of short-term spectral variability
probably affecting the position of line profiles in left- and right-hand
polarized spectra. We present new magnetic field measurements of HD92207
obtained on three different epochs in 2013 and 2014 using FORS2 in
spectropolarimetric mode. A 3sigma detection of the mean longitudinal magnetic
field using the entire spectrum, <B_z>_all=104+-34G, was achieved in
observations obtained in 2014 January. At this epoch, the position of the
spectral lines appeared stable. Our analysis of spectral line shapes recorded
in opposite circularly polarized light, i.e. in light with opposite sense of
rotation, reveals that line profiles in the light polarized in a certain
direction appear slightly split. The mechanism causing such a behaviour in the
circularly polarized light is currently unknown. Trying to settle the issue of
short-term variability, we searched for changes in the spectral line profiles
on a time scale of 8-10min using HARPS polarimetric spectra and on a time scale
of 3-4min using time series obtained with the CORALIE spectrograph. No
significant variability was detected on these time scales during the epochs
studied.Comment: 10 pages, 11 figures, 2 tables, accepted for publication in
  Astronomische Nachrichte
Charge symmetry breaking in $\Lambda$ hypernuclei revisited

The large charge symmetry breaking (CSB) implied by the $\Lambda$ binding
energy difference $\Delta B^{4}_{\Lambda}(0^+_{\rm g.s.})\equiv
B_{\Lambda}(_{\Lambda}^4$He)$-$$B_{\Lambda}(_{\Lambda}^4$H) = 0.35$\pm$0.06 MeV
of the $A=4$ mirror hypernuclei ground states, determined from emulsion
studies, has defied theoretical attempts to reproduce it in terms of CSB in
hyperon masses and in hyperon-nucleon interactions, including one pion exchange
arising from $\Lambda-\Sigma^0$ mixing. Using a schematic strong-interaction
$\Lambda N\leftrightarrow\Sigma N$ coupling model developed by Akaishi and
collaborators for $s$-shell $\Lambda$ hypernuclei, we revisit the evaluation of
CSB in the $A=4$ $\Lambda$ hypernuclei and extend it to $p$-shell mirror
$\Lambda$ hypernuclei. The model yields values of $\Delta B^{4}_{\Lambda}
(0^+_{\rm g.s.})\sim 0.25$ MeV. Smaller size and mostly negative $p$-shell
binding energy differences are calculated for the $A=7-10$ mirror hypernuclei,
in rough agreement with the few available data. CSB is found to reduce by
almost 30 keV the 110 keV $_{~\Lambda}^{10}$B g.s. doublet splitting
anticipated from the hyperon-nucleon strong-interaction spin dependence,
thereby explaining the persistent experimental failure to observe the $2^-_{\rm
exc}\to 1^-_{\rm g.s.}$ $\gamma$-ray transition.Comment: a few clarifying statements added to v2; matches published PLB
  version plus a note added after publication on p.1
The kepler-10 planetary system revisited by harps-n : A hot rocky world and a solid neptune-mass planet

The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under Grant Agreement No. 313014 (ETAEARTH). X. Dumusque would like to thank the Swiss National Science Foundation (SNSF) for its support through an Early Postdoc Mobility fellowship. P. Figueira acknowledges support by Fundação para a Ciência e a Tecnologia (FCT) through the Investigador FCT contract of reference IF/01037/2013 and POPH/FSE (EC) by FEDER funding through the program "Programa Operacional de Factores de Competitividade - COMPETE." R. D. Haywood acknowledges support from an STFC postgraduate research studentship. This publication was made possible through the support of a grant from the John Templeton Foundation.Kepler-10b was the first rocky planet detected by the Kepler satellite and confirmed with radial velocity follow-up observations from Keck-HIRES. The mass of the planet was measured with a precision of around 30%, which was insufficient to constrain models of its internal structure and composition in detail. In addition to Kepler-10b, a second planet transiting the same star with a period of 45 days was statistically validated, but the radial velocities were only good enough to set an upper limit of 20 M⊕ for the mass of Kepler-10c. To improve the precision on the mass for planet b, the HARPS-N Collaboration decided to observe Kepler-10 intensively with the HARPS-N spectrograph on the Telescopio Nazionale Galileo on La Palma. In total, 148 high-quality radial-velocity measurements were obtained over two observing seasons. These new data allow us to improve the precision of the mass determination for Kepler-10b to 15%. With a mass of 3.33 ± 0.49 M⊕ and an updated radius of 1.47+0.03-0.02 R⊕, Kepler-10b has a density of 5.8 ± 0.8 g cm−3, very close to the value predicted by models with the same internal structure and composition as the Earth. We were also able to determine a mass for the 45-day period planet Kepler-10c, with an even better precision of 11%. With a mass of 17.2 ± 1.9 M⊕ and radius of 2.35+0.09-0.04 R⊕, Kepler-10c has a density of 7.1 ± 1.0 g cm−3. Kepler-10c appears to be the first strong evidence of a class of more massive solid planets with longer orbital periods.Publisher PDFPeer reviewe