Miracle-dz/UniFAR-FTUs huggingface dataset:
Applying Deep Learning on a Few EEG Electrodes during Resting State Reveals Depressive States: A Data Driven Study

The growing number of depressive people and the overload in primary care services make it necessary to identify depressive states with easily accessible biomarkers such as mobile electroencephalography (EEG). Some studies have addressed this issue by collecting and analyzing EEG resting state in a search of appropriate features and classification methods. Traditionally, EEG resting state classification methods for depression were mainly based on linear or a combination of linear and non-linear features. We hypothesize that participants with ongoing depressive states differ from controls in complex patterns of brain dynamics that can be captured in EEG resting state data, using only nonlinear measures on a few electrodes, making it possible to develop cheap and wearable devices that could be even monitored through smartphones. To validate such a perspective, a resting-state EEG study was conducted with 50 participants, half with depressive state (DEP) and half controls (CTL). A data-driven approach was applied to select the most appropriate time window and electrodes for the EEG analyses, as suggested by Giacometti, as well as the most efficient nonlinear features and classifiers, to distinguish between CTL and DEP participants. Nonlinear features showing temporo-spatial and spectral complexity were selected. The results confirmed that computing nonlinear features from a few selected electrodes in a 15 s time window are sufficient to classify DEP and CTL participants accurately. Finally, after training and testing internally the classifier, the trained machine was applied to EEG resting state data (CTL and DEP) from a publicly available database, validating the capacity of generalization of the classifier with data from different equipment, population, and environment obtaining an accuracy near 100%.
Limits to the planet candidate GJ 436c

We report on H-band, ground-based observations of a transit of the hot Neptune GJ 436b. Once combined to achieve sampling equivalent to archived observations taken with Spitzer, our measurements reach comparable precision levels. We analyze both sets of observations in a consistent way, and measure the rate of orbital inclination change to be of 0.02+/-0.04 degrees in the time span between the two observations (253.8 d, corresponding to 0.03+/-0.05 degrees/yr if extrapolated). This rate allows us to put limits on the relative inclination between the two planets by performing simulations of planetary systems, including a second planet, GJ 436c, whose presence has been recently suggested (Ribas et al. 2008). The allowed inclinations for a 5 M_E super-Earth GJ 436c in a 5.2 d orbit are within ~7 degrees of the one of GJ 436b; for larger differences the observed inclination change can be reproduced only during short sections (<50%) of the orbital evolution of the system. The measured times of three transit centers of the system do not show any departure from linear ephemeris, a result that is only reproduced in <1% of the simulated orbits. Put together, these results argue against the proposed planet candidate GJ 436c.
DPAL activities in Japan: update

Activities on diode pumped alkali laser (DPAL) in Japan are updated. Since the last presentation in Chengdu, we have continued our DPAL research mainly targeting the development of tools for future scaling-up and high-efficiency operation. In particular, the focus is on a numerical simulation that combines computational fluid dynamics (CFD) and wave optics. To confirm the agreement between the experimental and simulation results, we designed and built several experimental apparatuses. Our latest gas-flow type DPAL produced 15.5 W output power with 80% slope efficiency based on the absorbed pump light. The agreement with theoretical prediction was excellent not only for output power but also for transverse mode shape and beam quality. Additionally, to accurately predict the performance of Cs DPAL, we measured the main reaction cross sections, namely, mixing and quenching reaction cross sections of the two P states of Cs with various hydrocarbon buffer gases. The main result of the repetitive pulsed operation by the cavity dumping technique and relevant numerical simulation is also discussed.
Generic quantum spin ice

We consider possible exotic ground states of quantum spin ice as realized in rare earth pyrochlores. Prior work [Savary and Balents, Phys. Rev. Lett. 108, 037202 (2012). ] introduced a gauge mean-field theory (gMFT) to treat spin or pseudospin Hamiltonians for such systems, reformulated as a problem of bosonic spinons coupled to a $U(1)$ gauge field. We extend gMFT to treat the most general nearest-neighbor exchange Hamiltonian, which contains a further exchange interaction. This term leads to interactions between spinons and requires a significant extension of gMFT, which we provide. As an application, we focus especially on the non-Kramers materials Pr${}_{2}T{M}_{2}$O${}_{7}$ ($TM=$ Sn, Zr, Hf, and Ir), for which the additional term is especially important, but for which an Ising-planar exchange coupling discussed previously is forbidden by time-reversal symmetry. In this case, when the planar $\mathit{XY}$ exchange is unfrustrated, we perform a full analysis and find three quantum ground states: a $U(1)$ quantum spin liquid (QSL), an antiferroquadrupolar ordered state and a noncoplanar ferroquadrupolar ordered one. We also consider the case of frustrated $\mathit{XY}$ exchange, and find that it favors a $\ensuremath{\pi}$-flux QSL, with an emergent line degeneracy of low-energy spinon excitations. This feature greatly enhances the stability of the QSL with respect to classical ordering.
THE LUMINOSITY FUNCTION OF STAR CLUSTERS IN 20 STAR-FORMING GALAXIES BASED ON HUBBLE LEGACY ARCHIVE PHOTOMETRY

Luminosity functions (LFs) have been determined for star cluster populations in 20 nearby (4–30 Mpc), star-forming galaxies based on Advanced Camera for Surveys source lists generated by the Hubble Legacy Archive (HLA). These cluster catalogs provide one of the largest sets of uniform, automatically generated cluster candidates available in the literature at present. Comparisons are made with other recently generated cluster catalogs demonstrating that the HLA-generated catalogs are of similar quality, but in general do not go as deep. A typical cluster LF can be approximated by a power law, dN/dL∝Lα, with an average value for α of −2.37 and rms scatter = 0.18 when using the F814W (“I”) band. A comparison of fitting results based on methods that use binned and unbinned data shows good agreement, although there may be a systematic tendency for the unbinned (maximum likelihood) method to give slightly more negative values of α for galaxies with steeper LFs. We find that galaxies with high rates of star formation (or equivalently, with the brightest or largest numbers of clusters) have a slight tendency to have shallower values of α. In particular, the Antennae galaxy (NGC 4038/39), a merging system with a relatively high star formation rate (SFR), has the second flattest LF in the sample. A tentative correlation may also be present between Hubble type and values of α, in the sense that later type galaxies (i.e., Sd and Sm) appear to have flatter LFs. Hence, while there do appear to be some weak correlations, the relative similarity in the values of α for a large number of star-forming galaxies suggests that, to first order, the LFs are fairly universal. We examine the bright end of the LFs and find evidence for a downturn, although it only pertains to about 1% of the clusters. Our uniform database results in a small scatter (≈0.4 to 0.5 mag) in the correlation between the magnitude of the brightest cluster (Mbrightest) and log of the number of clusters brighter than MI = −9 (log N). We also examine the magnitude of the brightest cluster versus log SFR for a sample including both dwarf galaxies and ULIRGs. This shows that the correlation extends over roughly six orders of magnitude but with scatter that is larger than for our spiral sample, probably because of the high levels of extinction in many of the LIRGs.
Enhancement of the Solubility and Dissolution Rate of Telmisartan by Surface Solid Dispersions Employing Superdisintegrants, Hydrophilic Polymers and Combined Carriers

Telmisartan (Tel) is a potent antihypertensive drug with a very poor aqueous solubility, especially in pH ranging from 3 to 9 (i.e., biological fluids) that results in poor bioavailability. Our aim was to improve Tel solubility and dissolution rates without the need for expensive multistep procedures, and without inclusion of alkalinizers. This study adopted the use of surface solid dispersions (SSDs) employing superdisintegrants, hydrophilic polymers and combined carriers including a superdisintegrant with a hydrophilic polymer. Tel-SSDs were formulated using thesolvent evaporation method. Compatibility between Tel and different carriers was examined via FT-IR. Tel-SSDs were evaluated optically and thermally to reveal a complete loss of the crystalline nature of the drug. Both drug content and percentage yield were calculated to judge the efficiency of the preparation technique used. Saturation, aqueous solubility, and dissolutions rates were determined. Dissolution profiles were studied using model dependent and independent approaches and were subjected to the pair-wise procedure using the DDsolver software program. Effect of aging was studied by comparing the drug content and dissolution profiles of freshly prepared SSDs with aged samples. All Tel-SSDs showed acceptable physical properties. Tel-SSDs showed pertinent enhancement related to the carrier used. Combined surface solid dispersions employing superdisintegrant croscarmellose sodium with either hydrophilic polymer PEG 4000 or Poloxamer 407 gave remarkable enhancement in solubility and dissolution rates of Tel where more than 90% of the drug was released within 20 min. The effect of aging results proved a non-significant difference in the drug content and dissolution profiles between fresh and aged samples. Formulation of Tel SSDs using combined carriers proved to be effective in enhancing the aqueous solubility and dissolution rates of Tel, as well as showing good stability upon aging.
Nitrogen line spectroscopy in O-stars - III. The earliest O-stars

This is the third paper in a series aiming at the analysis of nitrogen abundances in O-type stars, to enable further constraints on the early evolution of massive stars. We provide first theoretical predictions for the NIV4058/NIII4640 emission line ratio in dependence of various parameters, and confront them with results from the analysis of a sample of early LMC/SMC O-stars. Stellar and wind parameters are determined by line profile fitting of H/He/N lines, exploiting the helium and nitrogen ionization balance. Corresponding synthetic spectra are calculated using the NLTE atmospheric code FASTWIND. Though there is a monotonic relationship between the emission line ratio and Teff, all other parameters being equal, theoretical predictions indicate additional dependencies, most notably, on the nitrogen abundance. These basic predictions are confirmed by results from atmospheric code CMFGEN. The effective temperatures for the earliest O-stars, inferred from the nitrogen ionization balance, are partly considerably hotter than indicated by previous studies. Consistent with earlier results, effective temperatures increase from supergiants to dwarfs for all spectral types in the LMC. The relation between observed NIV4058/NIII4640 emission line ratio and Teff, for a given luminosity class, turned out to be quite monotonic for our sample stars, and fairly consistent with our model predictions. The scatter within a spectral sub-type is mainly produced by abundance effects. Our findings suggest that the Walborn et al. (2002) classification scheme is able to provide a meaningful relation between spectral type and Teff, provided that it is possible to discriminate for the luminosity class. This might be difficult to achieve in low-Z environments such as the SMC, owing to rather low wind-strengths. According to our predictions, the major bias of the classification scheme is due to nitrogen content.
PULSE-PHASE-DEPENDENT VARIATIONS OF THE CYCLOTRON ABSORPTION FEATURES OF THE ACCRETING PULSARS A0535+26, XTE J1946+274, AND 4U 1907+09 WITH SUZAKU

We have performed a detailed pulse-phase-resolved spectral analysis of cyclotron resonant scattering features (CRSFs) of the two Be/X-ray pulsars A0535+26 and XTE J1946+274 and the wind accreting HMXB pulsar 4U 1907+09 using Suzaku observations. The CRSF parameters vary strongly over the pulse phase and can be used to map the magnetic field, and a possible deviation forms the dipole geometry in these sources. It also reflects the conditions at the accretion column and the local environment over the changing viewing angles. The pattern of variation with pulse phase is obtained with more than one continuum spectral model for each source, all of which give consistent results. Care is also taken in performing the analysis over a stretch of data having constant spectral characteristics and luminosity in order to ensure that the results reflect the variations due to the changing viewing angle alone. For A0535+26 and XTE J1946+274, which show energy-dependent dips in their pulse profiles, a partial covering absorber is added in the continuum spectral models to take into account an additional absorption at those phases by the accretion stream/column blocking our line of sight.
Geometric Bell-like inequalities for steering

Many of the standard Bell inequalities (e.g., CHSH) are not effective for detection of quantum correlations which allow for steering, because for a wide range of such correlations they are not violated. We present Bell-like inequalities which have lower bounds for non-steering correlations than for local causal models. The inequalities involve all possible measurement settings at each side. We arrive at interesting and elegant conditions for steerability of arbitrary two-qubit states.
A large sample of Kohonen selected E+A (post-starburst) galaxies from the Sloan Digital Sky Survey

We aim to create a large sample of local post-starburst (PSB) galaxies to study their characteristic properties, particularly morphological features indicative of gravitational distortions and indications for active galactic nuclei (AGNs). The selection is based on a huge Kohonen self-organising map (SOM) of about one million SDSS spectra. The SOM is made fully available for the astronomical community, in combination with an interactive user interface. We compiled a catalogue of 2665 PSB galaxies with redshifts z < 0.4. In the colour-mass diagram, the PSB sample is found to be clearly concentrated towards the region between the red and the blue cloud, in agreement with the idea that PSB galaxies represent the transitioning phase between actively and passively evolving galaxies. The relative frequency of morphologically distorted PSB galaxies is at least 57%, significantly higher than in a comparison sample. The search for AGNs based on conventional selection criteria in the radio and MIR results in a low AGN fraction of 2 - 3%. We confirm an MIR excess in the mean SED of the PSB galaxy sample that may indicate hidden AGNs, though other sources are also possible. (Abstract modified to match the arXiv format.)
Differential Emission Measures from the Regularized Inversion of Hinode and SDO data

Aims. To demonstrate the capabilities of regularized inversion to recover differential emission measures (DEMs) from multiwavelength observations provided by telescopes such as Hinode and SDO. Methods. We develop and apply an enhanced regularization algorithm, used in RHESSI X-ray spectral analysis, to constrain the ill-posed inverse problem that is determining the DEM from solar observations. We demonstrate this computationally fast technique applied to a range of DEM models simulating broadband imaging data from SDO/AIA and high resolution line spectra from Hinode/EIS, as well as actual active region observations with Hinode/EIS and XRT. As this regularization method naturally provides both vertical and horizontal (temperature resolution) error bars we are able to test the role of uncertainties in the data and response functions. Results. The regularization method is able to successfully recover the DEM from simulated data of a variety of model DEMs (single Gaussian, multiple Gaussians and CHIANTI DEM models). It is able to do this, at best, to over four orders of magnitude in DEM space but typically over two orders of magnitude from peak emission. The combination of horizontal and vertical error bars and the regularized solution matrix allows us to easily determine the accuracy and robustness of the regularized DEM. We find that the typical range for the horizontal errors is ΔlogT ≈ 0.1−0.5 and this is dependent on the observed signal to noise, uncertainty in the response functions as well as the source model and temperature. With Hinode/EIS an uncertainty of 20% greatly broadens the regularized DEMs for both Gaussian and CHIANTI models although information about the underlying DEMs is still recoverable. When applied to real active region observations with Hinode/EIS and XRT the regularization method is able to recover a DEM similar to that found via a MCMC method but in considerably less computational time. Conclusions. Regularized inversion quickly determines the DEM from solar observations and provides reliable error estimates (both horizontal and vertical) which allows the temperature spread of coronal plasma to be robustly quantified.
The rise and fall of star formation in z ~ 0.2 merging galaxy clusters

CIZA J2242.8+5301 ('Sausage') and 1RXS J0603.3+4213 ('Toothbrush') are two lowredshift (z ~ 0.2), massive (~2 × 10 15 M · ), post-core passage merging clusters, which host-shock waves traced by diffuse radio emission. To study their star formation properties, we uniformly survey the 'Sausage' and 'Toothbrush' clusters in broad- and narrow-band filters and select a sample of 201 and 463 line emitters, down to a rest-frame equivalent width (13 A). We robustly separate between Hα and higher redshift emitters using a combination of optical multiband (B, g, V, r, i, z) and spectroscopic data. We build Hα luminosity functions for the entire cluster region, near the shock fronts, and away from the shock fronts and find striking differences between the two clusters. In the dynamically younger, 1 Gyr old 'Sausage' cluster we find numerous (59) Hα emitters above a star formation rate (SFR) of 0.17 M · yr -1 surprisingly located in close proximity to the shock fronts, embedded in very hot intracluster medium plasma. The SFR density for the cluster population is at least at the level of typical galaxies at z ~2. Down to the same SFR, the possibly dynamically more evolved 'Toothbrush' cluster has only nine Hα galaxies. The cluster Hα galaxies fall on the SFR-stellarmass relation z ~ 0.2 for the field. However, the 'Sausage' cluster has an Hαa emitter density >20 times that of blank fields. If the shock passes through gas-rich cluster galaxies, the compressed gas could collapse into dense clouds and excite star formation for a few 100 Myr. This process ultimately leads to a rapid consumption of the molecular gas, accelerating the transformation of gas-rich field spirals into cluster S0s or ellipticals.
The Effect of Customer Engagement in the Relationship between Brand Commitment and Customer Retention

The goal of this research is to determine the role of social media involvement as a moderating variable in the link between brand commitment and customer retention for smartphone businesses. The study is a conclusive descriptive research and employs a deductive technique. The study utilizes the regulatory engagement theory to investigate the proposed research model in the egyptian smartphone industry context. The study targeted a sample of 317 undergraduate students from the faculty of business at Ain Shams University. Structural equation model (SEM) was used to test the conceptual framework in this research. The study focused on the affective and continuance brand commitments as two key positive paths to customer retention. The results indicate that customer engagement positively influences the relationship between brand commitment and customer retention. In addition, affective commitment exceeds continuance commitment in term of customer retention.
OGLE-2008-BLG-355Lb: A MASSIVE PLANET AROUND A LATE-TYPE STAR

We report the discovery of a massive planet, OGLE-2008-BLG-355Lb. The light curve analysis indicates a planet:host mass ratio of q = 0.0118 ± 0.0006 at a separation of 0.877 ± 0.010 Einstein radii. We do not measure a significant microlensing parallax signal and do not have high angular resolution images that could detect the planetary host star. Therefore, we do not have a direct measurement of the host star mass. A Bayesian analysis, assuming that all host stars have equal probability to host a planet with the measured mass ratio, implies a host star mass of and a companion of mass , at a projected separation of AU. The implied distance to the planetary system is DL = 6.8 ± 1.1 kpc. A planetary system with the properties preferred by the Bayesian analysis may be a challenge to the core accretion model of planet formation, as the core accretion model predicts that massive planets are far more likely to form around more massive host stars. This core accretion model prediction is not consistent with our Bayesian prior of an equal probability of host stars of all masses to host a planet with the measured mass ratio. Thus, if the core accretion model prediction is right, we should expect that follow-up high angular resolution observations will detect a host star with a mass in the upper part of the range allowed by the Bayesian analysis. That is, the host would probably be a K or G dwarf.
Seed power dependence of mode instabilities in high-power fiber amplifiers

A semi-analytical model of stimulated thermal Rayleigh scattering, which assumes that there is a frequency offset between the fundamental mode and the high-order mode at the input of the amplifier, has been employed to study the effects of seed power on thermal-induced mode instability. Both the effects of gain saturation and photodarkening have been taken into consideration. The dependence of the threshold power and the maximal coupling frequency on various seed powers has been investigated when different parameters of fiber amplifier systems, such as the core/pump cladding diameter, and the level of photodarkening, are changed. The nonlinear dependence of the threshold at lower seed powers is mainly ascribed to the influence of gain saturation, while the reduction behavior of the threshold at higher seed powers is put down to the effects of photodarkening. The maximal coupling frequency is shown to vary with different parameters of fiber amplifier systems, such as seed powers, the level of the photodarkening, and core/pump cladding diameters. Comparing the results with the recently published experimental results, reveals that the experimental observation can be explained within this framework.
Tang poetry and tourism: Cultural effects after 1000 years

It is impossible to overstate the importance of culture and literature in tourism. Most studies have relied on qualitative evidence to the exclusion of precise secondary data to show a direct link between literature and tourism. Using a novel and unique index of Tang poems ranks as a proxy for cultural status and heritage accumulation to quantify the effects of Tang poetry on the expansion of domestic and international tourism, this research adds significantly to the body of knowledge on literary tourism. Based on ordinary least squares and bias-corrected propensity score matching regression analysis, the top 100 Tang poetry rankings are favorably associated with domestic tourist growth but not with international tourism expansion. These findings are crucial for the development of literary tourism.