Miracle-dz/UniFAR-FTUs huggingface dataset:
Harmonically trapped two-atom systems: Interplay of short-range s-wave interaction and spin-orbit coupling

The coupling between the spin degrees of freedom and the orbital angular momentum has a profound effect on the properties of nuclei, atoms and condensed matter systems. Recently, synthetic gauge fields have been realized experimentally in neutral cold atom systems, giving rise to a spin-orbit coupling term with "strength" $k_{\text{so}}$. This paper investigates the interplay between the single-particle spin-orbit coupling term of Rashba type and the short-range two-body $s$-wave interaction for cold atoms under external confinement. Specifically, we consider two different harmonically trapped two-atom systems. The first system consists of an atom with spin-orbit coupling that interacts with a structureless particle through a short-range two-body potential. The second system consists of two atoms that both feel the spin-orbit coupling term and that interact through a short-range two-body potential. Treating the spin-orbit term perturbatively, we determine the correction to the ground state energy for various generic parameter combinations. Selected excited states are also treated. An important aspect of our study is that the perturbative treatment is not limited to small $s$-wave scattering lengths but provides insights into the system behavior over a wide range of scattering lengths, including the strongly-interacting unitary regime. Our perturbative results are confirmed by numerical calculations that expand the eigenfunctions of the two-particle Hamiltonian in terms of basis functions that contain explicitly correlated Gaussians.
INTEGRAL results on Supergiant Fast X-ray Transients

We performed a systematic analysis of all INTEGRAL observations from 2003 to 2009 of 14 supergiant fast X-ray transients (SFXTs), implying a net exposure time of about 30 Ms. For each source we obtained light curves and spectra (3–100 keV), discovering several new outbursts. We discuss the X-ray behaviour of SFXTs emerging from our analysis in the framework of the clumpy wind accretion mechanism we proposed. We discuss the effect of X-ray photoionization on accretion in close binary systems such as IGR J16479−4514 and IGR J17544−2619. We show that, because of X-ray photoionization, there is a high probability of an accretion disc forming from the capture of angular momentum in IGR J16479−4514, and we suggest that the formation of transient accretion discs could be partly responsible for the flaring activity in SFXTs with narrow orbits. We also propose an alternative way to explain the origin of flares with peculiar shapes observed in our analysis applying the model of Lamb et al., which is based on accretion via the Rayleigh–Taylor instability and was originally proposed to explain Type II bursts.
Building a better understanding of the massive high-redshift BOSS CMASS galaxies as tools for cosmology

GF is supported by the Ministerio de Educacion y Ciencia of the Spanish Government through FPI grant AYA2010-2131-C02-01 and wishes to thank the Smithsonian Center for Astrophysics and the Harvard University, Astronomy Department, for the hospitality during the creation of this work. GF acknowledges support from the Spanish Government through EEBB-I-13-07167 and EEBB-I-12-05220 grants. GF, FP, and CC acknowledge support from the Spanish MICINNs Consolider-Ingenio 2010 Programme under grant MultiDark CSD2009-00064, MINECO Centro de Excelencia Severo Ochoa Programme under grant SEV-2012-0249, and MINECO grant AYA2014-60641-C2-1-P. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the U.S. Department of Energy.
Generalized likelihood uncertainty estimation (GLUE) and approximate Bayesian computation: What's the connection?

There has been a recent debate in the hydrological community about the relative merits of the informal generalized likelihood uncertainty estimation (GLUE) approach to uncertainty assessment in hydrological modeling versus formal probabilistic approaches. Some recent literature has suggested that the methods can give similar results in practice when properly applied. In this note, we show that the connection between formal Bayes and GLUE is not merely operational but goes deeper, with GLUE corresponding to a certain approximate Bayesian procedure even when the “generalized likelihood” is not a true likelihood. The connection we describe relates to recent approximate Bayesian computation (ABC) methods originating in genetics. ABC algorithms involve the use of a kernel function, and the generalized likelihood in GLUE can be thought of as relating to this kernel function rather than to the model likelihood. Two interpretations of GLUE emerge, one as a computational approximation to a Bayes procedure for a certain “error‐free” model and the second as an exact Bayes procedure for a perturbation of that model in which the truncation of the generalized likelihood in GLUE plays a role. The intent of this study is to encourage cross‐fertilization of ideas regarding GLUE and ABC in hydrologic applications. The connection we outline suggests the possibility of combining a formal likelihood with a kernel based on a generalized likelihood within the ABC framework and also allows advanced ABC computational methods to be used in GLUE applications. The model‐based interpretation of GLUE may also be helpful in partially illuminating the implicit assumptions in different choices of generalized likelihood.
USING M DWARF SPECTRA TO MAP EXTINCTION IN THE LOCAL GALAXY

We use spectra of more than 56,000 M dwarfs from the Sloan Digital Sky Survey (SDSS) to create a high-latitude extinction map of the local Galaxy. Our technique compares spectra from the stars in the SDSS Data Release 7 M dwarf sample in low-extinction lines of sight, as determined by Schlegel et al., to other SDSS M dwarf spectra in order to derive improved distance estimates and accurate line-of-sight extinctions. Unlike most previous studies, which have used a two-color method to determine extinction, we fit extinction curves to fluxes across the spectral range from 5700 to 9200 Å for every star in our sample. Our result is an AV map that extends from a few tens of pc to approximately 2 kpc away from the Sun. We also use a similar technique to create a map of RV values within approximately 1 kpc of the Sun and find that they are consistent with the widely accepted diffuse interstellar medium value of 3.1. Using our extinction data, we derive a dust scale height for the local Galaxy of 119 ± 15 pc and find evidence for a local dust cavity.
A Lyman Break Galaxy Candidate at z ~ 9

We report the discovery of a z ∼ 9 Lyman break galaxy candidate, selected from the NICMOS Parallel Imaging Survey as a J-dropout with J110 − H160 = 1.7. Spitzer/IRAC photometry reveals that the galaxy has a blue H160 − 3.6 μm color and a spectral break between 3.6 and 4.5 μm. We interpret this break as the Balmer break and derive a best-fit photometric redshift of z ∼ 9. We use Monte Carlo simulations to test the significance of this photometric redshift, and we show that there is a 96% probability of z ⩾ 7. We estimate that the lower limit to the comoving number density of such galaxies at z ∼ 9 is ϕ > 3.8 × 10−6 Mpc−3. If the high redshift of this galaxy is confirmed, this will indicate that the luminous end of the rest-frame UV luminosity function has not evolved substantially from z ∼ 9 to z ∼ 3. Still, some small degeneracy remains between this z ∼ 9 model and models at z ∼ 2–3; deep optical imaging (reaching IAB ∼ 29) can rule out the lower z models.
Technology Acceptance of Digital Bag Tag for Airline Passengers

The purpose of this paper is to identify the relationship of user’s attitudes, technology adoption, external factors and intention to use the digital bag tag by using an extended technology acceptance model (TAM). This study used an online survey to assess the proposed determinants of digital bag tag adoption. Data from 400 global respondents collected online and at Suvarnabhumi Airport were used to examine the research model using multiple regression analysis, independent-sample t-test and one-way analysis of variance (ANOVA). The positive relationships were found between original TAM constructs and external factors; relative advantage, system quality, availability/mobility, self-efficacy, security/privacy and social influences but negative relationship on cost. Attitudes played a significant role in predicting the intention. However, perceived ease of use had stronger support than perceived usefulness towards the attitudes. The difference of geographic and travel frequency was also found having relationship towards the overall technology acceptance. The digital bag tag is one of the latest innovations in the aviation industry, empirical study on user perceptions of and attitudes toward it remain preliminary.
A sample of relatively unstudied star clusters in the Large Magellanic Cloud: fundamental parameters determined from Washington photometry

Aims. To enlarge our growing sample of well-studied star clusters in the Large Magellanic Cloud (LMC), we present CCD Washington CT1 photometry to T1∼ 23 in the fields of twenty-three mostly unstudied clusters lo cated in the inner disc and outer regions of the LMC. Methods. We estimated cluster radii from star counts. Using the cluster Washington (T1, C− T1) colour-magnitude diagrams, statistically cleaned from field star contamination, we derived cl uster ages and metallicities from a comparison with theoretical isochrones of the Padova group. Whenever possible, we also derived ages usingδT1 - the magnitude difference between the red giant clump and the main sequence turn off - and estimated metallicities from the standard giant branch procedure. We enlarged our sample by adding clusters with published ages and metallicities determined on a similar scale by applying the same methods. We examined relationships between their positions in the LMC, ages and metallicities. Results. We find that the two methods for age and metallicity determina tion agree well with each other. Fourteen clusters are found to be intermediate-age clusters (1-2 Gyr), with [Fe/H] values ranging from -0.4 to -0.7. The remaining nine clusters turn out to be younger than 1 Gyr, with metallicities between 0.0 and -0.4. Conclusions. Our 23 clusters represent an increase of∼ 30% in the current total amount number of well-studied LMC clusters using Washington photometry. In agreement with previous studies, we find no evidence for a metallicity gradient. We also find th at the younger clusters were formed closer to the LMC centre than the older ones.
ULTRAVIOLET AND X-RAY VARIABILITY OF THE SEYFERT 1.5 GALAXY MARKARIAN 817

We present an investigation of the ultraviolet and X-ray spectra of the Seyfert 1.5 galaxy Markarian 817. The ultraviolet analysis includes two recent observations taken with the Cosmic Origins Spectrograph (COS) in 2009 August and December, as well as archival spectra from the International Ultraviolet Explorer and the Hubble Space Telescope. Twelve Lyα absorption features are detected in the 1997 Goddard High Resolution Spectrograph (GHRS) and 2009 COS spectra—of these, four are associated with high-velocity clouds in the interstellar medium, four are at low significance, and the remaining four are intrinsic features, which vary between the GHRS and COS observations. The strongest intrinsic absorber in the 1997 spectrum has a systemic velocity of ∼−4250 km s−1. The corresponding feature in the COS data is five times weaker than the GHRS absorber. The three additional weak (equivalent width from 13 to 54 mÅ) intrinsic Lyα absorbers are at systemic velocities of −4100 km s−1, −3550 km s−1, and −2600 km s−1. However, intrinsic absorption troughs from highly ionized C iv and N v are not detected in the COS observations. No ionized absorption signatures are detected in the ∼14 ks XMM-Newton EPIC spectra. The factor of five change in the intrinsic Lyα absorber is most likely due to bulk motions in the absorber, since there is no drastic change in the UV luminosity of the source from the GHRS to the COS observations. In a study of the variability of Mrk 817, we find that the X-ray luminosity varies by a factor of ∼40 over 20 years, while the UV continuum/emission lines vary by at most a factor of ∼2.3 over 30 years. The variability of the X-ray luminosity is strongly correlated with the X-ray power-law index, but no correlation is found with the simultaneous optical/UV photometry.
Measuring cosmic magnetic fields by rotation measure-galaxy cross-correlations in cosmological simulations

Using cosmological magnetohydrodynamical (MHD) simulations of the magnetic field in galaxy clusters and filaments, we evaluate the possibility to infer the magnetic field strength in filaments by measuring cross-correlation functions between Faraday rotation measures (RM) and the galaxy density field. We also test the reliability of recent estimates considering the problem of data quality and Galactic foreground (GF) removal in current data sets. Besides the two self-consistent simulations of cosmological magnetic fields based on primordial seed fields and galactic outflows analysed here, we also explore a larger range of models scaling up the resulting magnetic fields of one of the simulations. We find that, if an unnormalized estimator for the cross-correlation functions and a GF removal procedure is used, the detectability of the cosmological signal is only possible for future instruments (e.g. SKA and ASKAP). However, mapping of the observed RM signal to the underlying magnetization of the Universe (both in space and time) is an extremely challenging task which is limited by the ambiguities of our model parameters, as well as to the weak response of the RM signal in low-density environments. Therefore, we conclude that current data cannot constrain the amplitude and distribution of magnetic fields within the large-scale structure and a detailed theoretical understanding of the build-up and distribution of magnetic fields within the Universe will be needed for the interpretation of future observations.
The ultra-high energy cosmic rays image of Virgo A

Arrival directions of ultra-high energy cosmic rays from the direction of ten brightest radio sources lying within 50 Mpc from our Galaxy were studied by using recent models of the largescale Galactic magnetic field. A detailed study, where also small-scale turbulent magnetic field component was implemented, is presented for the radiogalaxy Virgo A. This radiogalaxy is located far from the Galactic plane which leads to a unique image of this UHECR source candidate, if the flux is composed from a mixture of intermediate mass nuclei. We present a method suitable for identifying cosmic rays arriving from this close-by radiogalaxy.
Entanglement spectrum of a topological phase in one dimension

We show that the Haldane phase of S=1 chains is characterized by a double degeneracy of the entanglement spectrum. The degeneracy is protected by a set of symmetries (either the dihedral group of $\pi$-rotations about two orthogonal axes, time-reversal symmetry, or bond centered inversion symmetry), and cannot be lifted unless either a phase boundary to another, "topologically trivial", phase is crossed, or the symmetry is broken. More generally, these results offer a scheme to classify gapped phases of one dimensional systems. Physically, the degeneracy of the entanglement spectrum can be observed by adiabatically weakening a bond to zero, which leaves the two disconnected halves of the system in a finitely entangled state.
Potentials for soft-wall AdS/QCD

Soft-wall models in AdS/QCD generally have dilaton and scalar fields that vary with the fifth-dimension coordinate. These fields can be parametrized to yield hadron mass spectra with linear radial trajectories and to incorporate spontaneous breaking of chiral symmetry. We show how to construct scalar potentials which lead to such solutions.
An Indirect Model Predictive Control Method for Grid-Connected Three-Level Neutral Point Clamped Converters With <inline-formula><tex-math notation="LaTeX">$LCL$</tex-math></inline-formula> Filters

This article presents a model predictive control (MPC) algorithm for a three-level neutral point clamped converter connected to the grid via an LCL filter. The proposed long-horizon MPC method, formulated as a multicriterion quadratic program (QP), simultaneously controls the grid and converter current as well as the filter capacitor voltage, while meeting the relevant grid standards. To achieve the latter, a carrier-based pulsewidth modulation stage is employed. Finally, soft constraints are included to ensure operation of the system within its safe operating limits, particularly with regards to a potential overcurrent or overvoltage trip during transient operation. The presented simulation results based on a medium-voltage system as well as experimental studies based on a scaled-down prototype verify the effectiveness of the proposed method.
Phase transitions in three-dimensional loop models and the $CP^{n-1}$ sigma model

We consider the statistical mechanics of a class of models involving close-packed loops with fugacity $n$ on three-dimensional lattices. The models exhibit phases of two types as a coupling constant is varied: in one, all loops are finite, and in the other, some loops are infinitely extended. We show that the loop models are discretizations of $C{P}^{n\ensuremath{-}1}$ $\ensuremath{\sigma}$ models. The finite and infinite loop phases represent, respectively, disordered and ordered phases of the $\ensuremath{\sigma}$ model, and we discuss the relationship between loop properties and $\ensuremath{\sigma}$ model correlators. On large scales, loops are Brownian in an ordered phase and have a nontrivial fractal dimension at a critical point. We simulate the models, finding continuous transitions between the two phases for $n=1,2,3$ and first order transitions for $n\ensuremath{\ge}4$. We also give a renormalization-group treatment of the $C{P}^{n\ensuremath{-}1}$ model that shows how a continuous transition can survive for values of $n$ larger than (but close to) 2, despite the presence of a cubic invariant in the Landau-Ginzburg description. The results we obtain are of broader relevance to a variety of problems, including $\mathrm{SU}(n)$ quantum magnets in (2+1) dimensions, Anderson localization in symmetry class $C$, and the statistics of random curves in three dimensions.
Nonlinear perturbation theory with halo bias and redshift-space distortions via the Lagrangian picture

The nonlinear perturbation theory of gravitational instability is extended to include effects of both biasing and redshift-space distortions, which are inevitable in predicting observable quantities in galaxy surveys. Weakly nonlinear effects in galaxy clustering on large scales recently attracted great interest, since the precise determination of scales of baryon acoustic oscillations is crucial to investigate the nature of dark energy by galaxy surveys. We find that a local Lagrangian bias and redshift-space distortions are naturally incorporated in our formalism of perturbation theory with a resummation technique via the Lagrangian picture. Our formalism is applicable to any biasing scheme which is local in Lagrangian space, including the halo bias as a special case. Weakly nonlinear effects on halo clustering in redshift space are analytically given. We assume only a fundamental idea of the halo model: haloes form according to the extended Press-Schechter theory, and the spatial distributions are locally biased in Lagrangian space. There is no need for assuming the spherical collapse model to follow the dynamical evolution, which is additionally assumed in standard halo prescriptions. One-loop corrections to the power spectrum and correlation function of haloes in redshift space are explicitly derived and presented. Instead of relying on expensive numerical simulations, our approach provides an analytic way of investigating the weakly nonlinear effects, simultaneously including the nonlinear biasing and nonlinear redshift-space distortions. Nonlinearity introduces a weak scale dependence in the halo bias. The scale dependence is a smooth function in Fourier space, and the bias does not critically change the feature of baryon acoustic oscillations in the power spectrum. The same feature in the correlation function is less affected by nonlinear effects of biasing.
Probing light bino and higgsinos at the LHC

Motivated by the naturalness, we study a simplified MSSM scenario where only the bino-like LSP and higgsino-like NLSP are light. We first scan the parameter space of this scenario, considering the constraints from the Higgs mass, flavor physics, electroweak precision measurements and dark matter experiments. Then in the allowed parameter space, we perform a Monte Carlo simulation for the $\tilde{\chi}^\pm_1 \tilde{\chi}^0_{2,3}$ production followed by $\tilde{\chi}^\pm_1 \to W^\pm \tilde{\chi}^0_1$ and $\tilde{\chi}^0_{2,3} \to Z\tilde{\chi}^0_1$. By examining the presently available trilepton bounds on the wino-like chargino/neutralino, we find that only a narrow region $40\,\rm{GeV} \lesssim m_{\tilde{\chi}^0_1} \lesssim 50\,\rm{GeV}$ and $160\,\rm{GeV} \lesssim m_{\tilde{\chi}^0_{2,3}} \lesssim 170\,\rm {GeV}$ on the plane of $m_{\tilde{\chi}^0_1}-m_{\tilde{\chi}^0_{2,3}}$ can be excluded. Finally, we explore the potential of trilepton signature in probing such a scenario at 14 TeV LHC and find that the region with $40\,\rm{GeV} \lesssim m_{\tilde{\chi}^0_1} \lesssim 60\,\rm {GeV}$ and $160 \rm {GeV}\,\lesssim m_{\tilde{\chi}^0_{2,3}} \lesssim 300\,\rm{GeV}$ can be covered at $3\sigma$ level with luminosity ${\cal L}=300$ fb$^{-1}$.
On the relation between Seyfert 2 accretion rate and environment at z > 0.1

We analyse different properties of the small scale environment of Seyfert 2 for two samples selected according to the accretion rate parameter , R, from the DR7-SDSS survey. We compare the results with two control samples of non-active galaxies that cover the same redshift range, luminosity, colours, morphology, age and stellar mass content. Our study shows that both high and low accretion rate subsamples reside in bluer and lower density environments than the control samples. However, we find that this difference is at least two times stronger for the low accretion rate Seyferts. In the vicinity of Seyfert 2, red galaxies have systematically lower values of stellarmass as compared with corresponding control samples. The lower values of stellar mass for red neighbours is more significant at higher density environments and it is more evident for low accretion rate Seyfert. We also find that this effect is independent of the host’s stellar mass. Our results are consistent with a scenario where AGN occurrence is higher in lower/medium density environments with a higher merger rate and a lack of a dense intergalactic medium (that can strip gas from these systems) that provide suitable conditions for the central black hole feeding. We find this particularly evident for the low accretion rate Seyferts that could compensate through the intergalactic medium the lack of gas of their hosts.