Miracle-dz/UniFAR-FTUs huggingface dataset:
Compressed simulation of evolutions of the X Y model

We extend the notion of compressed quantum simulation to the XY-model. We derive a quantum circuit processing log(n) qubits which simulates the 1D XY-model describing n qubits. In particular, we demonstrate how the adiabatic evolution can be realized on this exponentially smaller system and how the magnetization, which witnesses a quantum phase transition can be observed. Furthermore, we analyze several dynamical processes, like quantum quenching and finite time evolution and derive the corresponding compressed quantum circuit.
CARBON AND OXYGEN ABUNDANCES IN COOL METAL-RICH EXOPLANET HOSTS: A CASE STUDY OF THE C/O RATIO OF 55 CANCRI

The super-Earth exoplanet 55 Cnc e, the smallest member of a five-planet system, has recently been observed to transit its host star. The radius estimates from transit observations, coupled with spectroscopic determinations of mass, provide constraints on its interior composition. The composition of exoplanetary interiors and atmospheres are particularly sensitive to elemental C/O ratio, which to first order can be estimated from the host stars. Results from a recent spectroscopic study analyzing the 6300 Å [O i] line and two C i lines suggest that 55 Cnc has a carbon-rich composition (C/O = 1.12 ± 0.09). However, oxygen abundances derived using the 6300 Å [O i] line are highly sensitive to a Ni i blend, particularly in metal-rich stars such as 55 Cnc ([Fe/H] =0.34 ± 0.18). Here, we further investigate 55 Cnc's composition by deriving the carbon and oxygen abundances from these and additional C and O absorption features. We find that the measured C/O ratio depends on the oxygen lines used. The C/O ratio that we derive based on the 6300 Å [O i] line alone is consistent with the previous value. Yet, our investigation of additional abundance indicators results in a mean C/O ratio of 0.78 ± 0.08. The lower C/O ratio of 55 Cnc determined here may place this system at the sensitive boundary between protoplanetary disk compositions giving rise to planets with high (>0.8) versus low (<0.8) C/O ratios. This study illustrates the caution that must applied when determining planet host star C/O ratios, particularly in cool, metal-rich stars.
Model-independent determination on $H_0$ using the latest $H(z)$ data

We perform the improved constraints on the Hubble constant $H_0$ by using the model-independent method, Gaussian Processes. Utilizing the latest 36 $H(z)$ measurements, we obtain $H_0=69.21\pm3.72$ km s$^{-1}$ Mpc$^{-1}$, which is consistent with the Planck 2015 and Riess et al. 2016 analysis at $1\sigma$ confidence level, and reduces the uncertainty from $6.5\%$ (Busti et al. 2014) to $5.4\%$. Different from the results of Busti et al. 2014 by only using 19 $H(z)$ measurements, our reconstruction results of $H(z)$ and the derived values of $H_0$ are independent of the choice of covariance functions.
STAR FORMATION IN INTERMEDIATE REDSHIFT 0.2 < z < 0.7 BRIGHTEST CLUSTER GALAXIES

We present a multi-wavelength photometric and spectroscopic study of 42 Brightest Cluster Galaxies (BCGs) in two samples of galaxy clusters chosen for a gravitational lensing study. The study’s initial sample combines 25 BCGs from the Cluster Lensing and Supernova Survey with Hubble sample and 37 BCGs from the Sloan Giant Arcs Survey with a total redshift range of Using archival GALEX, Hubble Space Telescope, Wide-Field Infrared Survey Explorer, Herschel, and Very Large Array data we determine the BCGs’ stellar mass, radio power, and star formation rates. The radio power is higher than expected if due to star formation, consistent with the BCGs being active galactic nucleus (AGN)-powered radio sources. This suggests that the AGN and star formation are both fueled by cold gas in the host galaxy. The specific star formation rate (sSFR) is low and constant with redshift. The mean sSFR is 9.42 × 10−12 yr−1, which corresponds to a mass doubling time of 105 billion years. These findings are consistent with models for hierarchical formation of BCGs, which suggest that star formation is no longer a significant channel for galaxy growth for z 1. Instead, stellar growth (of the order of a factor of at least two) during this period is expected to occur mainly via minor dry mergers.
Effectual accuracy of OCT image retinal segmentation with the aid of speckle noise reduction and boundary edge detection strategy

Optical coherence tomography (OCT) has shown to be a valuable imaging tool in the field of ophthalmology, and it is becoming increasingly relevant in the field of neurology. Several OCT image segmentation methods have been developed previously to segment retinal images, however sophisticated speckle noises with low‐intensity restrictions, complex retinal tissues, and inaccurate retinal layer structure remain a challenge to perform effective retinal segmentation. Hence, in this research, complicated speckle noises are removed by using a novel far‐flung ratio algorithm in which preprocessing has been done to treat the speckle noise thereby highly decreasing the speckle noise through new similarity and statistical measures. Additionally, a novel haphazard walk and inter‐frame flattening algorithms have been presented to tackle the weak object boundaries in OCT images. These algorithms are effective at detecting edges and estimating minimal weighted paths to better diverge, which reduces the time complexity. In addition, the segmentation of OCT images is made simpler by using a novel N‐ret layer segmentation approach that executes simultaneous segmentation of various surfaces, ensures unambiguous segmentation across neighbouring layers, and improves segmentation accuracy by using two grey scale values to construct data. Consequently, the novel work outperformed the OCT image segmentation with 98.5% of accuracy.
Combining QCD and electroweak corrections to dilepton production in the framework of the FEWZ simulation code

We combine the next-to-next-to-leading order (NNLO) QCD corrections to lepton-pair production through the Drell-Yan mechanism with the next-to-leading order (NLO) electroweak corrections within the framework of the FEWZ simulation code. Control over both sources of higher-order contributions is necessary for measurements where percent-level theoretical predictions are crucial, and in phase-space regions where the NLO electroweak corrections grow large. The inclusion of both corrections in a single simulation code eliminates the need to separately incorporate such effects as final-state radiation and electroweak Sudakov logarithms when comparing many experimental results to theory. We recalculate the NLO electroweak corrections in the complex-mass scheme for both massless and massive final-state leptons, and modify the QCD corrections in the original FEWZ code to maintain consistency with the complex-mass scheme to the lowest order. We present phenomenological results for LHC studies that include both NNLO QCD and NLO electroweak corrections. In addition, we study several interesting kinematics features induced by experimental cuts in the distribution of photon radiation at the LHC.
The investigations of anisotropy in orientations of galaxies

In 1994 Parnovsky, Karachentsev and Karachentseva suggested a modified method for investigation of the orientations of galaxies. Using this method they analyzed galaxies from the UGC and ESO catalogues, as well as from their's own catalogue inclusive of flat, edge-on galaxies. They found statistically significant anisotropy in the galaxies orientations'. In 1995 Flin suggested that this anisotropy has to be specific to LOcal Supercluster (LSC) In the present paper, using the method proposed by Parnovsky, Karachentsev and Karachentseva in 1994, we analyzed orientation of galaxies in the sample of galaxies belonging to LSC founding only a weak anisotropy. The relation of this method to Hawley and Peebles (1975) method of the investigation of the orientation of galaxies was discussed as well.
Role of the fsr Quorum-Sensing System in Enterococcus faecalis Bloodstream Infection

First, we conducted an advanced study on the genomic differences between colonizing and infecting E. faecalis, which provides support and evidence for early and accurate diagnoses. Second, we discovered that fsr was significantly associated with blood infections, which also provides additional information for studies exploring the invasiveness of E. faecalis. Most importantly, we found that fsr played an important role in both biofilm formation and serum resistance ability in E. faecalis. ABSTRACT Enterococcus faecalis is an important intestinal colonizing bacteria and can cause various tissue infections, including invasive blood infection (BI). The annual incidence of E. faecalis BI has been estimated to be ~4.5 per 100,000, with a fatality rate that can reach 20%. However, whether bacterial colonization or invasive infections are tissue based has not been thoroughly studied. In this study, we analyzed 537 clinical isolates from 7 different tissues to identify the key genomic elements that facilitate the colonization and invasive infection of E. faecalis. Comparative genomic analysis revealed that the BI E. faecalis isolates had the largest genome size but the lowest GC content, fsr quorum-sensing system genes were enriched in the BI E. faecalis, and the fsr gene cluster could enhance biofilm formation and serum resistance ability. Our findings also provide deep insight into the genomic differences between different tissue isolates, and the fsr quorum-sensing systems could be a key factor promoting E. faecalis invasion into the blood. IMPORTANCE First, we conducted an advanced study on the genomic differences between colonizing and infecting E. faecalis, which provides support and evidence for early and accurate diagnoses. Second, we discovered that fsr was significantly associated with blood infections, which also provides additional information for studies exploring the invasiveness of E. faecalis. Most importantly, we found that fsr played an important role in both biofilm formation and serum resistance ability in E. faecalis.
Matter and twin matter in bimetric MOND

Bimetric MOND (BIMOND) theories, propounded recently, predict peculiar gravitational interactions between matter and twin matter (TM). TM is the hypothetical matter that might couple directly only to the second metric of the theory, as standard matter couples only to the first. Considerations of cosmology in the BIMOND framework suggest that such TM might exist and copy matter in its attributes. Here, I investigate the indirect interactions that BIMOND theories predict between local, non-relativistic mass concentrations of matter and TM. The most salient result is that in the deep-MOND regime of the matter–TM symmetric theories, TM behaves as if it has a negative gravitational mass relative to matter (active and passive, with the inertial mass still positive). To wit, interaction within each sector is attractive MOND gravity, but between matter and TM it is repulsive MOND gravity. Using the space-conformal invariance of the theory in the deep-MOND regime, I derive various exact results; e.g. the repulsive force between a matter and TM point masses (space-conformal theories are a natural framework for masses of opposite signs). In the high-acceleration regime, the interaction depends on a parameter, (the strength of the Einstein–Hilbert action for matter). For the favoured value , matter and TM do not interact in this regime, for they attract and for they repel each other. Such interactions may have substantial ramifications for all aspects of structure formation, such as matter distribution, peculiar velocities and effects on the cosmic microwave background. The repulsive interactions probably lead to segregation of matter and TM structures, leading, in turn, to intermeshing of the respective cosmic webs, with high-density nodes of one sector residing in the voids of the other (possibly conducing to efficient evacuation of the voids). Weak gravitational lensing by TM seems the best way to detect it or constrain its attributes. In the MOND regime, a TM body acts on matter photons as a diverging lens. Strong lensing occurs in the high-acceleration regime and thus depends on . For , a TM mass does not bend (matter) light in the high-acceleration regime: no strong lensing effects of TM are expected in this case. I also discuss briefly asymmetric theories.
Quantum quenches in extended systems

We study in general the time evolution of correlation functions in a extended quantum system after the quench of a parameter in the Hamiltonian. We show that correlation functions in d dimensions can be extracted using methods of boundary critical phenomena in d+1 dimensions. For d = 1 this allows us to use the powerful tools of conformal field theory in the case of critical evolution. Several results are obtained in generic dimension in the Gaussian (mean field) approximation. These predictions are checked against the real time evolution of some solvable models that allow us also to understand which features are valid beyond the critical evolution. All our findings may be explained in terms of a picture generally valid, whereby quasiparticles, entangled over regions of the order of the correlation length in the initial state, then propagate with a finite speed through the system. Furthermore we show that the long time results can be interpreted in terms of a generalized Gibbs ensemble. We discuss some open questions and possible future developments.
Connecting the new H.E.S.S. diffuse emission at the Galactic Center with the Fermi GeV excess: A combination of millisecond pulsars and heavy dark matter?

The H.E. S.S. Collaboration has reported a high-energy spherically symmetric diffuse γ-ray emission in the inner 50 pc of the Milky Way, up to ∼50 TeV. Here, we propose a leptonic model which provides an alternative to the hadronic scenario presented by the H.E. S.S. Collaboration, and connects the newly reported TeV emission to the Fermi-LAT Galactic Center GeV excess. Our model relies on a combination of inverse Compton emission from a population of millisecond pulsars—which can account for the GeV excess—and a supermassive black hole-induced spike of heavy (∼60 TeV) dark matter particles annihilating into electrons with a subthermal cross section. With an up-to-date interstellar radiation field, as well as a standard magnetic field and diffusion setup, our model accounts for the spectral morphology of the detected emission. Moreover, we show that the dark matter-induced emission reproduces the spatial morphology of the H.E. S.S. signal above ∼10 TeV, while we obtain a slightly more extended component from pulsars at lower energies, which could be used as a prediction for future H.E. S.S. observations.
Elliptically polarized terahertz radiation from a chiral oxide

Polarization control of terahertz wave is a challenging subject in terahertz science and technology. Here, we report a simple method to control polarization state of the terahertz wave in terahertz generation process. At room temperature, terahertz radiation from a noncentrosymmetric and chiral oxide, sillenite Bi$_{12}$GeO$_{20}$, is observed by the irradiation of linearly polarized femtosecond laser pulses at 800 nm. The polarization state of the emitted terahertz wave is found to be elliptic with an ellipticity of $\sim$0.37$\pm$0.10. Furthermore, the ellipticity was altered to a nearly zero ($\sim$0.01$\pm$0.01) by changing the polarization of the incident linearly polarized femtosecond laser pulses. Such a terahertz radiation characteristic is attributable to variation of the polarization state of the emitted terahertz waves, which is induced by retardation due to the velocity mismatch between the incident femtosecond laser pulse and generated terahertz wave and by the polarization tilting due to the optical activity at 800 nm.
Natural fueling of a tokamak fusion reactor

A natural fueling mechanism that helps to maintain the main core deuterium and tritium (DT) density profiles in a tokamak fusion reactor is presented. In H-mode plasmas dominated by ion-temperature gradient (ITG) driven turbulence, cold DT ions near the edge will naturally pinch radially inward toward the core. This mechanism is due to the quasineutral heat flux dominated nature of ITG turbulence and still applies when trapped and passing kinetic electron effects are included. Fueling using shallow pellet injection is augmented by an inward pinch of cold DT fuel. The natural fueling mechanism is investigated using the gyrokinetic turbulence code GEM [Y. Chen and S. E. Parker, J. Comput. Phys. 220, 839 (2007)] and is analyzed using quasilinear theory. Profiles similar to those used for conservative International Thermonuclear Experimental Reactor [R. Aymar et al., Nucl. Fusion 41, 1301 (2001)] transport modeling that have a completely flat density profile are examined and it is found that natural fueling a.
The OGLE Collection of Variable Stars. Anomalous Cepheids in the Magellanic Clouds

We present a collection of 250 anomalous Cepheids (ACs) discovered in the OGLE-IV fields toward the Large (LMC) and Small Magellanic Cloud (SMC). The LMC sample is an extension of the OGLE-III Catalog of ACs published in 2008, while the SMC sample contains the first known bona fide ACs in this galaxy. The total sample is composed of 141 ACs in the LMC and 109 ACs in the SMC. All these stars pulsate in single modes: fundamental (174 objects) or first overtone (76 objects). Additionally, we report the discovery of four ACs located in the foreground of the Magellanic Clouds. These are the first fundamental-mode ACs known in the Galactic field. We demonstrate that the coefficients phi_21 and phi_31 determined by the Fourier light curve decomposition are useful discriminators between classical Cepheids and ACs, at least in the LMC and in the field of the Milky Way. In the SMC, the light curve shapes and mean magnitudes of short-period classical Cepheids make them similar to ACs, which is a source of difficulties in the discrimination of both classes of pulsators. The presence of unidentified ACs in the catalogs of classical Cepheids may be partly responsible for the observed non-linearity of the period-luminosity relation observed for short-period Cepheids in the SMC. We compare spatial distributions of ACs, classical Cepheids and RR Lyr stars. We show that the distribution of ACs resembles that of old stars (RR Lyr variables), although in the LMC there are visible structures typical for young population (classical Cepheids): the bar and spiral arms. This may suggest that ACs are a mixture of relatively young stars and mergers of very old stars.
Complete Genome Sequences of Four Pseudomonas aeruginosa Bacteriophages: Kara-mokiny 8, Kara-mokiny 13, Kara-mokiny 16, and Boorn-mokiny 1

Pseudomonas aeruginosa is an opportunistic pathogen. Here, we report the isolation of four bacteriophages from wastewater. All four bacteriophages belong to the Myoviridae family. Kara-mokiny 8, 13, and 16 are of the Pbunavirus genus and have genomes between 65,527 and 66,420-bp. Boorn-mokiny 1 is of the Phikzvirus genus and has a 278,796-bp genome. ABSTRACT Pseudomonas aeruginosa is an opportunistic pathogen. Here, we report the isolation of four bacteriophages from wastewater. All four bacteriophages belong to the Myoviridae family. Kara-mokiny 8, 13, and 16 are of the Pbunavirus genus and have genomes between 65,527 and 66,420-bp. Boorn-mokiny 1 is of the Phikzvirus genus and has a 278,796-bp genome.
The baryonic Tully–Fisher relation and galactic outflows

Most of the baryons in the Universe are not in the form of stars and cold gas in galaxies. Galactic outflows driven by supernovae/stellar winds are the leading mechanisms for explaining this fact. The scaling relation between galaxy mass and outer rotation velocity (also known as the baryonic Tully–Fisher relation, BTF) has recently been used as evidence against this viewpoint. We use a Λ cold dark matter (ΛCDM)-based semi-analytic disc galaxy formation model to investigate these claims. In our model, galaxies with less efficient star formation and higher gas fractions are more efficient at ejecting gas from galaxies. This somewhat counter intuitive result is due to the (observational) fact that galaxies with less efficient star formation and higher gas fractions tend to live in dark matter haloes with lower circular velocities, from which less energy is required to escape the potential well. In our model the intrinsic scatter in the BTF is ≃0.15 dex, and mostly reflects scatter in dark halo concentration. The scatter is largely independent of galaxy structure because of the large radius within which galaxy rotation velocities are measured. The observed scatter, equal to ≃0.24 dex, is dominated by measurement errors. The best estimate for the intrinsic scatter is that it is less than 0.15 dex, and thus our ΛCDM-based model (which does not include all possible sources of scatter) is only just consistent with this. Future observations of the BTF scatter could be made with a more stringent measurement of the intrinsic scatter, and thus provide a strong constraint to galaxy formation models. In our model, gas-rich galaxies, at fixed virial velocity (Vvir), with lower stellar masses have lower baryonic masses. This is consistent with the expectation that galaxies with lower stellar masses have had less energy available to drive an outflow. However, when the outer rotation velocity (Vflat) is used the correlation has the opposite sign, with a slope in agreement with observations. This is due to the fact there is scatter in the relation between Vflat and Vvir. In summary, contrary to some previous claims, we show that basic features of the BTF are consistent with a ΛCDM-based model in which the low efficiency of galaxy formation is determined by galactic outflows.
Model of spatial competition on discrete markets

We propose a dynamical model of price formation on a spatial market where sellers and buyers are placed on the nodes of a graph, and the distribution of the buyers depends on the positions and prices of the sellers. We ﬁnd that, depending on the positions of the sellers and on the level of information available, the price dynamics of our model can either converge to ﬁxed prices, or produce cycles of diﬀerent amplitudes and periods. We show how to measure the strength of competition in a spatial network by extracting the exponent of the scaling of the prices with the size of the system. As an application, we characterize the diﬀerent level of competition in street networks of real cities across the globe. Finally, using the model dynamics we can deﬁne a novel measure of node centrality, which quantiﬁes the relevance of a node in a competitive market.
Long time behavior of run-and-tumble particles in two dimensions

We study the long-time asymptotic behavior of the position distribution of a run-and-tumble particle (RTP) in two dimensions in the presence of translational diffusion and show that the distribution at a time t can be expressed as a perturbative series in (γt)−1 , where γ −1 is the persistence time of the RTP. We show that the higher order corrections to the leading order Gaussian distribution generically satisfy an inhomogeneous diffusion equation where the source term depends on the previous order solutions. The explicit solution of the inhomogeneous equation requires the position moments, and we develop a recursive formalism to compute the same. We find that the subleading corrections undergo shape transitions as the translational diffusion is increased.