pinecone/core-2020-05-10-deduplication huggingface dataset:
Driven Holographic CFTs

We study the dynamical evolution of strongly coupled field theories,
initially in thermal equilibrium, under the influence of an external driving
force. We model the field theory holographically using classical gravitational
dynamics in an asymptotically AdS spacetime. The system is driven by a source
for a (composite) scalar operator. We focus on a scenario where the external
source is periodic in time and chart out the response of several observables.
We find an interesting phase structure in the response as a function of the
amplitude of the source and driving frequency. Specifically the system
transitions from a dissipation dominated phase, via a dynamical crossover to a
highly resonant amplification phase. The diagnostics of these phases include
the response of the operator in question, entropy production, energy
fluctuations, and the temporal change of entanglement entropy for small
subsystems. We comment on evidence for a potential phase transition in the
energy fluctuations of the system.Comment: 42 pages, 39 pdf figures. v2: minor changes. published versio
Beyond adiabatic elimination: Effective Hamiltonians and singular
  perturbation

Adiabatic elimination is a standard tool in quantum optics, which produces an
effective Hamiltonian for a relevant subspace of states, incorporating effects
of its coupling to states with much higher unperturbed energy. It shares with
techniques from other fields the emphasis on the existence of widely separated
scales. Given this fact, the question arises whether it is feasible to improve
on the adiabatic approximation, similarly to some of those other approaches. A
number of authors have addressed the issue from the quantum optics/atomic
physics perspective, and have run into the issue of non-hermiticity of the
effective Hamiltonian improved beyond the adiabatic approximation, which poses
conceptual and practical problems. Here, we first briefly survey methods
present in the physics literature. Next, we rewrite the problems addressed by
the adiabatic elimination technique to make apparent the fact that they are
singular perturbation problems from the point of view of dynamical systems. We
apply the invariant manifold method for singular perturbation problems to this
case, and show that this method produces the equation named after Bloch in
nuclear physics. Given the wide separation of scales, it becomes intuitive that
the Bloch equation admits iterative/perturbative solutions. We show, using a
fixed point theorem, that indeed the iteration converges to a perturbative
solution that produces in turn an exact Hamiltonian for the relevant subspace.
We propose thus several sequences of effective Hamiltonians, starting with the
adiabatic elimination and improving on it. We show the origin of the
non-hermiticity, and that it is inessential given the isospectrality of the
effective non-hermitian operator and a corresponding effective hermitian
operator, which we build. We propose an application of the introduced
techniques to periodic Hamiltonians.Comment: 14 pages, 3 figure
The XMM-Newton serendipitous survey. VII. The third XMM-Newton
  serendipitous source catalogue

Thanks to the large collecting area (3 x ~1500 cm$^2$ at 1.5 keV) and wide
field of view (30' across in full field mode) of the X-ray cameras on board the
European Space Agency X-ray observatory XMM-Newton, each individual pointing
can result in the detection of hundreds of X-ray sources, most of which are
newly discovered. Recently, many improvements in the XMM-Newton data reduction
algorithms have been made. These include enhanced source characterisation and
reduced spurious source detections, refined astrometric precision, greater net
sensitivity and the extraction of spectra and time series for fainter sources,
with better signal-to-noise. Further, almost 50\% more observations are in the
public domain compared to 2XMMi-DR3, allowing the XMM-Newton Survey Science
Centre (XMM-SSC) to produce a much larger and better quality X-ray source
catalogue. The XMM-SSC has developed a pipeline to reduce the XMM-Newton data
automatically and using improved calibration a new catalogue version has been
produced from XMM-Newton data made public by 2013 Dec. 31 (13 years of data).
Manual screening ensures the highest data quality. This catalogue is known as
3XMM. In the latest release, 3XMM-DR5, there are 565962 X-ray detections
comprising 396910 unique X-ray sources. For the 133000 brightest sources,
spectra and lightcurves are provided. For all detections, the positions on the
sky, a measure of the quality of the detection, and an evaluation of the X-ray
variability is provided, along with the fluxes and count rates in 7 X-ray
energy bands, the total 0.2-12 keV band counts, and four hardness ratios. To
identify the detections, a cross correlation with 228 catalogues is also
provided for each X-ray detection. 3XMM-DR5 is the largest X-ray source
catalogue ever produced. Thanks to the large array of data products, it is an
excellent resource in which to find new and extreme objects.Comment: 23 pages, version accepted for publication in A&
Supersymmetric gauged Double Field Theory: Systematic derivation by
  virtue of \textit{Twist}

In a completely systematic and geometric way, we derive maximal and
half-maximal supersymmetric gauged double field theories in lower than ten
dimensions. To this end, we apply a simple twisting ansatz to the $D=10$
ungauged maximal and half-maximal supersymmetric double field theories
constructed previously within the so-called semi-covariant formalism. The
twisting ansatz may not satisfy the section condition. Nonetheless, all the
features of the semi-covariant formalism, including its complete
covariantizability, are still valid after the twist under alternative
consistency conditions. The twist allows gaugings as supersymmetry preserving
deformations of the $D=10$ untwisted theories after Scherk-Schwarz-type
dimensional reductions. The maximal supersymmetric twist requires an extra
condition to ensure both the Ramond-Ramond gauge symmetry and the $32$
supersymmetries unbroken.Comment: 1+58 pages, section 4 enhanced, refs added. To appear in JHE
A search for neutrino-antineutrino mass inequality by means of sterile
  neutrino oscillometry

The investigation of the oscillation pattern induced by the sterile neutrinos
might determine the oscillation parameters, and at the same time, allow to
probe CPT symmetry in the leptonic sector through neutrino-antineutrino mass
inequality. We propose to use a large scintillation detector like JUNO or LENA
to detect electron neutrinos and electron antineutrinos from MCi electron
capture or beta decay sources. Our calculations indicate that such an
experiment is realistic and could be performed in parallel to the current
research plans for JUNO and RENO. Requiring at least 5$\sigma$ confidence level
and assuming the values of the oscillation parameters indicated by the current
global fit, we would be able to detect neutrino-antineutrino mass inequality of
the order of 0.5% or larger, which would imply a signal of CPT anomalies.Comment: 14 pages, 10 figure
Binary Central Stars of Planetary Nebulae Discovered Through Photometric
  Variability III: The Central Star of Abell 65

A growing number of close binary stars are being discovered among central
stars of planetary nebulae. Recent and ongoing surveys are finding new systems
and contributing to our knowledge of the evolution of close binary systems. The
push to find more systems was largely based on early discoveries which
suggested that 10 to 15% of all central stars are close binaries. One goal of
this series of papers is confirmation and classification of these systems as
close binaries and determination of binary system parameters. Here we provide
time-resolved multi-wavelength photometry of the central star of Abell 65 as
well as further analysis of the nebula and discussion of possible
binary--nebula connections. Our results for Abell 65 confirm recent work
showing that it has a close, cool binary companion, though several of our model
parameters disagree with the recently published values. With our longer time
baseline of photometric observations from 1989--2009 we also provide a more
precise orbital period of 1.0037577 days.Comment: Accepted for publication in the Astronomical Journa
Your own actions influence how you perceive other people: A misattribution of action appraisals.

The attribution of personal traits to other persons depends on the actions the observer performs at the same time (Bach & Tipper, 2007). Here, we show that the effect reflects a misattribution of appraisals of the observers' own actions to the actions of others. We exploited spatial compatibility effects to manipulate how fluently-how fast and how accurately-participants identified two individuals performing sporty or academic actions. The traits attributed to each person in a subsequent rating task depended on the fluency of participants' responses in a specific manner. An individual more fluently identified while performing the academic action appeared more academic and less sporty. An individual more fluently identified while performing the sporty action appeared sportier. Thus, social perception is-at least partially-embodied. The ease of our own responses can be misattributed to the actions of others, affecting which personal traits are attributed to them
Pluto’s atmosphere from stellar occultations in 2012 and 2013

A. Dias-Oliveira is thankful for the support of the following grants: CAPES (BEX 9110/12-7) FAPERJ/PAPDRJ (E-45/2013). R. Vieira-Martins acknowledges the following grants: CNPq-306885/2013, CAPES/Cofecub-2506/2015, FAPERJ/PAPDRJ-45/2013. TRAPPIST is a project funded by the Belgian Fund for Scientific Research (F.R.S.-FNRS) under grant FRFC 2.5.594.09.F, with the participation of the Swiss National Science Foundation. J. L. Ortiz and N. Morales acknowledge funding from Proyecto de Excelencia de la Junta de Andalucía, J.A. 2012-FQM1776 and from FEDER funds. M. Gillon and E. Jehin are F.R.S.-FNRS Research Associates. C. Opitom acknowledges the support of the F.R.S.-FNRS for her PhD thesis. R. Leiva is supported by the CONICYT PCHA/Doctorado Nacional scholarship. M. Assafin thanks the CNPq (Grants 473002/2013-2 and 308721/2011-0) and FAPERJ (Grant E-26/111.488/2013). J.I.B. Camargo acknowledges CNPq for a PQ2 fellowship (process number 308489/2013-6). A.R. Gomes-Júnior thanks CAPES.We analyze two multi-chord stellar occultations by Pluto that were observed on 2012 July 18th and 2013 May 4th, and respectively monitored from five and six sites. They provide a total of fifteen light curves, 12 of which were used for a simultaneous fit that uses a unique temperature profile, assuming a clear (no haze) and pure N2 atmosphere, but allowing for a possible pressure variation between the two dates. We find a solution that satisfactorily fits (i.e., within the noise level) all of the 12 light curves, providing atmospheric constraints between ~1190 km (pressure ~11 μbar) and ~1450 km (pressure ~0.1 μbar) from Pluto's center. Our main results are: (1) the best-fitting temperature profile shows a stratosphere with a strong positive gradient between 1190 km (at 36 K, 11 μbar) and r = 1215 km (6.0 μbar), where a temperature maximum of 110 K is reached; above it is a mesosphere with a negative thermal gradient of −0.2 K km−1 up to ~1390 km (0.25 μbar), where the mesosphere connects itself to a more isothermal upper branch around 81 K; (2) the pressure shows a small (6%) but significant increase (6σ level) between the two dates; (3) without a troposphere, Pluto's radius is found to be Rp = 1190 ± 5 km. Allowing for a troposphere, RP is constrained to lie between 1168 and 1195 km; and (4) the currently measured CO abundance is too small to explain the mesospheric negative thermal gradient. Cooling by HCN is possible, but only if this species is largely saturated. Alternative explanations like zonal winds or vertical compositional variations of the atmosphere are unable to explain the observed mesospheric negative thermal gradient.Publisher PDFPeer reviewe
Three irradiated and bloated hot Jupiters: WASP-76b, WASP-82b, and WASP-90b

We report on three new transiting hot Jupiter planets, discovered from the WASP surveys, which we combine with radial velocities from OHP/SOPHIE and Euler/CORALIE and photometry from Euler and TRAPPIST. The planets WASP-76b, WASP-82b, and WASP-90b are all inflated, with radii of 1.7–1.8 RJup. All three orbit hot stars, of type F5–F7, with orbits of 1.8–3.9 d, and all three stars have evolved, post-main-sequence radii (1.7–2.2 R⊙). Thus the three planets fit a known trend of hot Jupiters that receive high levels of irradiation being highly inflated. We caution, though, about the presence of a selection effect, in that non-inflated planets around ~2 R⊙ post-MS stars can often produce transits too shallow to be detected by the ground-based surveys that have found the majority of transiting hot Jupiters.Publisher PDFPeer reviewe
Willingness to pay for unfamiliar public goods : Preserving cold-water coral in Norway

The work on this paper is carried out in the project “Habitat-Fisheries interactions: Valuation and bio-economic modeling of cold water corals” financed by the Norwegian Research Council, grant # 216485.The world's largest concentration of cold-water coral (CWC) is found off the Norwegian coast. Most CWC discoveries are recent, posing new challenges for Norwegian coastal and fishery authorities regarding the management of deep-sea resources. Scientific knowledge of CWC is limited, and many citizens have not even heard about them. This creates problems for the application of the stated preference methods to capture their economic value, and very few such studies have been conducted. To fill this gap, we designed a discrete choice experiment, which was implemented in a valuation workshop setting in order to derive estimates of participants' willingness to pay (WTP) for increasing the protection of CWC. Despite the fact that marine industries such as oil/gas and fisheries could be adversely affected by CWC protection, this did not reduce the respondents' willingness to pay for further protection. The possibility that CWCs play an important role as habitat for fish was the single most important variable to explain respondents' WTP for CWC protection. The survey revealed a high degree of preference heterogeneity, while we found an average WTP for CWC protection in the range of EUR 274–287.PostprintPeer reviewe
An exactly solvable supersymmetric spin chain of BC_N type

We construct a new exactly solvable supersymmetric spin chain related to the BC_N extended root system, which includes as a particular case the BC_N version of the Polychronakos-Frahm spin chain. We also introduce a supersymmetric spin dynamical model of Calogero type which yields the new chain in the large coupling limit. This connection is exploited to derive two different closed-form expressions for the chain's partition function by means of Polychronakos's freezing trick. We establish a boson-fermion duality relation for the new chain's spectrum, which is in fact valid for a large class of (not necessarily integrable) spin chains of BC_N type. The exact expressions for the partition function are also used to study the chain's spectrum as a whole, showing that the level density is normally distributed even for a moderately large number of particles. We also determine a simple analytic approximation to the distribution of normalized spacings between consecutive levels which fits the numerical data with remarkable accuracy. Our results provide further evidence that spin chains of Haldane-Shastry type are exceptional integrable models, in the sense that their spacings distribution is not Poissonian, as posited by the Berry-Tabor conjecture for "generic" quantum integrable systems
CARMENES input catalogue of M dwarfs I. Low-resolution spectroscopy with CAFOS

Context. CARMENES is a stabilised, high-resolution, double-channel spectrograph at the 3.5m Calar Alto telescope. It is optimally designed for radial-velocity surveys of M dwarfs with potentially habitable Earth-mass planets. Aims. We prepare a list of the brightest, single M dwarfs in each spectral subtype observable from the northern hemisphere, from which we will select the best planet-hunting targets for CARMENES. Methods. In this first paper on the preparation of our input catalogue, we compiled a large amount of public data and collected low-resolution optical spectroscopy with CAFOS at the 2.2m Calar Alto telescope for 753 stars. We derived accurate spectral types using a dense grid of standard stars, a double least-squares minimisation technique, and 31 spectral indices previously defined by other authors. Additionally, we quantified surface gravity, metallicity, and chromospheric activity for all the stars in our sample. Results. We calculated spectral types for all 753 stars, of which 305 are new and 448 are revised. We measured pseudo-equivalent widths of H α for all the stars in our sample, concluded that chromospheric activity does not affect spectral typing from our indices, and tabulated 49 stars that had been reported to be young stars in open clusters, moving groups, and stellar associations. Of the 753 stars, two are new subdwarf candidates, three are T Tauri stars, 25 are giants, 44 are K dwarfs, and 679 are M dwarfs. Many of the 261 investigated dwarfs in the range M4.0-8.0V are among the brightest stars known in their spectral subtype. Conclusions. This collection of low-resolution spectroscopic data serves as a candidate target list for the CARMENES survey and can be highly valuable for other radial-velocity surveys of M dwarfs and for studies of cool dwarfs in the solar neighbourhood
Spectral energy distribution of Markarian 501 : quiescent state vs. extreme outburst

The very high energy (VHE ; E &gt; 100 GeV) blazar Markarian 501 has a well-studied history of extreme spectral variability and is an excellent laboratory for studying the physical processes within the jets of active galactic nuclei. However, there are few detailed multiwavelength studies of Markarian 501 during its quiescent state, due to its low luminosity. A short-term multiwavelength study of Markarian 501 was coordinated in March 2009, focusing around a multi-day observation with the Suzaku X-ray satellite and including {; ; ; ; ; \gamma}; ; ; ; ; -ray data from VERITAS, MAGIC, and the Fermi Gamma-ray Space Telescope with the goal of providing a well-sampled multiwavelength baseline measurement of Markarian 501 in the quiescent state. The results of these quiescent-state observations are compared to the historically extreme outburst of April 16, 1997, with the goal of examining variability of the spectral energy distribution between the two states. The derived broadband spectral energy distribution shows the characteristic double-peaked profile. We find that the X-ray peak shifts by over two orders of magnitude in photon energy between the two flux states while the VHE peak varies little. The limited shift in the VHE peak can be explained by the transition to the Klein-Nishina regime. Synchrotron self-Compton models are matched to the data and the implied Klein-Nishina effects are explored
Production of charged pions, kaons and protons at large transverse momenta in pp and Pb–Pb collisions at √sNN = 2.76 TeV

Transverse momentum spectra of π±, K± and p(p¯) up to pT = 20 GeV/c at mid-rapidity in pp, peripheral (60–80%) and central (0–5%) Pb–Pb collisions at √sNN = 2.76 TeV have been measured using the ALICE detector at the Large Hadron Collider. The proton-to-pion and the kaon-to-pion ratios both show a distinct peak at pT ≈ 3 GeV/c in central Pb–Pb collisions. Below the peak, pT &lt; 3 GeV/c, both ratios are in good agreement with hydrodynamical calculations, suggesting that the peak itself is dominantly the result of radial flow rather than anomalous hadronization processes. For pT &gt; 10 GeV/c particle ratios in pp and Pb–Pb collisions are in agreement and the nuclear modification factors for π±, K± and p(p¯) indicate that, within the systematic and statistical uncertainties, the suppression is the same. This suggests that the chemical composition of leading particles from jets in the medium is similar to that of vacuum jets
Measurements of the ϒ(1S), ϒ(2S), and ϒ(3S) differential cross sections in pp collisions at s=7TeV

Differential cross sections as a function of transverse momentum pTpT are presented for the production of ϒ(nS)ϒ(nS) (n = 1, 2, 3) states decaying into a pair of muons. Data corresponding to an integrated luminosity of 4.9View the MathML sourcefb−1 in pp collisions at View the MathML sources=7TeV were collected with the CMS detector at the LHC. The analysis selects events with dimuon rapidity |y|&lt;1.2|y|&lt;1.2 and dimuon transverse momentum in the range View the MathML source10&lt;pT&lt;100GeV. The measurements show a transition from an exponential to a power-law behavior at View the MathML sourcepT≈20GeV for the three ϒ states. Above that transition, the ϒ(3S)ϒ(3S) spectrum is significantly harder than that of the ϒ(1S)ϒ(1S). The ratios of the ϒ(3S)ϒ(3S) and ϒ(2S)ϒ(2S) differential cross sections to the ϒ(1S)ϒ(1S) cross section show a rise as pTpT increases at low pTpT, then become flatter at higher pTpT
Perturbative QCD study of Bs decays to a pseudoscalar meson and a tensor meson

We study two-body hadronic Bs→PT decays, with P(T) being a light pseudoscalar (tensor) meson, in the perturbative QCD approach. The CP-averaged branching ratios and the direct CP asymmetries of the ΔS=0 modes are predicted, where Δ S is the difference between the strange numbers of final and initial states. We also define and calculate experimental observables for the ΔS=1 modes under the B0s–B¯0s mixing, including CP averaged branching ratios, time-integrated CP asymmetries, and the CP observables Cf , Df and Sf . Results are compared to the Bs→PV ones in the literature, and to the B→PT ones, which indicate considerable U-spin symmetry breaking. Our work provides theoretical predictions for the Bs→PT decays for the first time, some of which will be potentially measurable at future experiments
High precision predictions for exclusive V H production at the LHC

We present a resummation-improved prediction for pp → V H + 0 jets at the Large Hadron Collider. We focus on highly-boosted final states in the presence of jet veto to suppress the $ t\overline{t} $ background. In this case, conventional fixed-order calculations are plagued by the existence of large Sudakov logarithms $ \alpha_s^n{\log^m}\left( {{{{p_T^{\mathrm{veto}}}} \left/ {Q} \right.}} \right) $ for Q ~ m V + m H which lead to unreliable predictions as well as large theoretical uncertainties, and thus limit the accuracy when comparing experimental measurements to the Standard Model. In this work, we show that the resummation of Sudakov logarithms beyond the next-to-next-to-leading-log accuracy, combined with the next-to-next-to-leading order calculation, reduces the scale uncertainty and stabilizes the perturbative expansion in the region where the vector bosons carry large transverse momentum. Our result improves the precision with which Higgs properties can be determined from LHC measurements using boosted Higgs techniques
Measurement of the inclusive Z cross section via decays to tau pairs in pp collisions at \sqrt {s} = 7 TeV

The first measurement of inclusive Z → τ + τ − production in pp collisions at the LHC is presented, in the final states μ + hadrons, e + hadrons, e + μ, and μ + μ. The data sample corresponds to an integrated luminosity of 36 pb−1 collected with the CMS detector. The measured cross section is σ (pp → ZX) × B (Z → τ + τ −) = 1.00 ± 0.05(stat.) ± 0.08(syst.) ± 0.04(lumi.)nb, which is in good agreement with the next-to-next-to-leading order QCD prediction and improves on previous measurements in the Z → e+e− and μ + μ − channels. The reconstruction efficiency for hadronic τ decays is determined with a precision of 7%.Peer Reviewe