Miracle-dz/UniFAR-FTUs huggingface dataset:
The feeble giant. Discovery of a large and diffuse Milky Way dwarf galaxy in the constellation of Crater

We announce the discovery of the Crater 2 dwarf galaxy, identified in imaging data of the VST ATLAS survey. Given its half-light radius of ~1100 pc, Crater 2 is the fourth largest dwarf in the Milky Way, surpassed only by the LMC, SMC and the Sgr dwarf. With a total luminosity of $M_V\approx-8$, this satellite galaxy is also one of the lowest surface brightness dwarfs. Falling under the nominal detection boundary of 30 mag arcsec$^{-2}$, it compares in nebulosity to the recently discovered Tuc 2 and Tuc IV and UMa II. Crater 2 is located ~120 kpc from the Sun and appears to be aligned in 3-D with the enigmatic globular cluster Crater, the pair of ultra-faint dwarfs Leo IV and Leo V and the classical dwarf Leo II. We argue that such arrangement is probably not accidental and, in fact, can be viewed as the evidence for the accretion of the Crater-Leo group.
FORMATION OF MAGNETIC FLUX ROPES DURING CONFINED FLARING WELL BEFORE THE ONSET OF A PAIR OF MAJOR CORONAL MASS EJECTIONS

NOAA active region (AR) 11429 was the source of twin super-fast coronal mass ejections (CMEs). The CMEs took place within an hour from each other, with the onset of the first taking place in the beginning of 2012 March 7. This AR fulfills all the requirements for a “super active region”; namely, Hale's law incompatibility and a δ-spot magnetic configuration. One of the biggest storms of Solar Cycle 24 to date ( D st = − 143 ? > nT) was associated with one of these events. Magnetic flux ropes (MFRs) are twisted magnetic structures in the corona, best seen in ∼10 MK hot plasma emission and are often considered the core of erupting structures. However, their “dormant” existence in the solar atmosphere (i.e., prior to eruptions), is an open question. Aided by multi-wavelength observations by the Solar Dynamics Observatory (SDO) and by the Solar Terrestrial Relations Observatory (STEREO) and a nonlinear force-free model for the coronal magnetic field, our work uncovers two separate, weakly twisted magnetic flux systems which suggest the existence of pre-eruption MFRs that eventually became the seeds of the two CMEs. The MFRs could have been formed during confined (i.e., not leading to major CMEs) flaring and sub-flaring events which took place the day before the two CMEs in the host AR 11429.
Longitudinal deep truck: Deep longitudinal model with application to sim2real deep reinforcement learning for heavy‐duty truck control in the field

To develop cooperative adaptive cruise control (CACC), the choice of control approach often influences and can limit the choice of model structure, and vice versa. For heavy‐duty trucks, practical application of CACC in the field is heavily influenced by the accuracy of the used model. Deep learning and deep reinforcement learning (deep‐RL) have recently been used to demonstrate improved modeling and control performance for vehicles such as cars and quadrotors compared to state‐of‐the‐art. The literature on the application of deep learning and deep‐RL for heavy‐duty trucks in the field, which are significantly more complex than cars, is still sparse, however. In this article, we develop a two‐layer gray‐box deep learning model to capture longitudinal dynamics of heavy‐duty trucks while abstracting their complexity and present an approach to properly break the nested feedback loops in the model for training. We compare this model with three other alternative models and show that it achieves ~ 10 x $\unicode{x0007E}10x$ better general performance compared to a standard artificial neural network and results in ~ 4 x $\unicode{x0007E}4x$ and ~ 40 x $\unicode{x0007E}40x$ slower steady‐state acceleration and speed error growth rates, respectively. We then present an architecture to utilize these deep learning models within the deep‐RL framework and use it to develop baseline CACC controllers that can be zero‐shot transferred to the field. To carry out the work, we present a setup of differently configured trucks along with their interface architecture and stochastic driving cycle generators for data collection. Numerical validation of the approach demonstrated stationary and bounded modeling error, and demonstrated transfer of CACC controllers with consistent overshoot bounds and a stable approximately‐zero steady‐state error. Validation from field experiments demonstrated similarly consistent results. Compared to a state‐of‐the‐art benchmark, the deep‐RL controller achieved lower speed and time‐gap error variance but higher time‐gap error offset.
Equation of state in the pion condensation phase in asymmetric nuclear matter using a holographic QCD model

We study the asymmetric nuclear matter using a holographic QCD model by introducing a baryonic charge in the infrared boundary. We first show that, in the normal hadron phase, the predicted values of the symmetry energy and it's slope parameter are comparable with the empirical values. We find that the phase transition from the normal phase to the pion condensation phase is delayed compared with the pure mesonic matter: The critical chemical potential is larger than the pion mass which is obtained for the pure mesonic matter. We also show that, in the pion condensation phase, the pion contribution to the isospin number density increases with the chemical potential, while the baryonic contribution is almost constant. Furthermore, the value of chiral condensation implies that the enhancement of the chiral symmetry breaking occurs in the asymmetric nuclear matter as in the pure mesonic matter. We also give a discussion on how to understand the delay in terms of the 4-dimensional chiral Lagrangian including the rho and omega mesons based on the hidden local symmetry.
A data-analysis driven comparison of analytic and numerical coalescing binary waveforms: nonspinning case

We compare waveforms obtained by numerically evolving nonspinning binary black holes to postNewtonian (PN) template families currently used in the search for gravitational waves by groundbased detectors. We find that the time-domain 3.5PN template family, which includes the inspiral phase, has fitting factors (FFs) ≥ 0.96 for binary systems with total mass M = 10–20M⊙. The timedomain 3.5PN effective-one-body template family, which includes the inspiral, merger and ring-down phases, gives satisfactory signal-matching performance with FFs ≥ 0.96 for binary systems with total mass M = 10–120M⊙. If we introduce a cutoff frequency properly adjusted to the final black-hole ring-down frequency, we find that the frequency-domain stationary-phase-approximated template family at 3.5PN order has FFs ≥ 0.96 for binary systems with total mass M = 10–20M⊙. However, to obtain high matching performances for larger binary masses, we need to either extend this family to unphysical regions of the parameter space or introduce a 4PN order coefficient in the frequencydomain GW phase. Finally, we find that the phenomenological Buonanno-Chen-Vallisneri family has FFs ≥ 0.97 with total mass M = 10–120M⊙. The main analyses use the noise spectral-density of LIGO, but several tests are extended to VIRGO and advanced LIGO noise-spectral densities.
Relationship of Emotional Intelligence with Social Anxiety and Social Competence of Adolescents

This study was an effort to find out the relationship of emotional intelligence with social anxiety and social competence of adolescents. The study was carried out at Ibne Sina College and SICAS. A sample of 130 adolescents between the ages of 14-16 years was randomly selected. Emotional quotient inventory youth version (EQi- YV) by Baron, Kutcher Social Anxiety Disorder Scale for Adolescents (K-GSADS-A) and Measures of Adolescence Social Performance (MASP) were used to find out the emotional intelligence, social anxiety and social competence respectively. Data was analyzed using descriptive statistics as well as independent samples t-test, ANOVA and Pearson correlation coefficient. Results showed that girls experience more social anxiety as compared to boys. Further analysis revealed a negative correlation between emotional intelligence and social anxiety, a positive relation between emotional intelligence and social competence and a negative relation between social anxiety and social competence of both boys and girls.
Distributed Layer-Partitioned Training for Privacy-Preserved Deep Learning

Deep Learning techniques have achieved remarkable results in many domains. Often, training deep learning models requires large datasets, which may require sensitive information to be uploaded to the cloud to accelerate training. To adequately protect sensitive information, we propose distributed layer-partitioned training with step-wise activation functions for privacy-preserving deep learning. Experimental results attest our method to be simple and effective.
Very fast photometric and X-ray observations of the intermediate polar V2069 Cygni (RX J2123.7+4217)

We present fast timing photometric observations of the intermediate polar V2069 Cygni (RX J2123.7+4217) using the Optical Timing Analyzer (OPTIMA) at the 1.3-m telescope of Skinakas Observatory. The optical (450–950 nm) light curve of V2069 Cygni was measured with sub-second resolution for the first time during 2009 July and revealed a double-peaked pulsation with a period of 743.38 ± 0.25 s. A similar double-peaked modulation was found in the simultaneous Swift satellite observations. We suggest that this period represents the spin of the white dwarf accretor. Moreover, we present results from a detailed analysis of the XMM–Newton observation, which also shows a double-peaked modulation, however shifted in phase, with a period of 742.35 ± 0.23 s. The X-ray spectra obtained from the XMM– Newton European Photon Imaging Camera (EPIC) instruments were modelled by a plasma emission and a soft blackbody component with a partial covering photoelectric absorption model with a covering fraction of 0.65. An additional Gaussian emission line at 6.385 keV with an equivalent width of 243 eV is required to account for fluorescent emission from neutral iron. The iron fluorescence (∼6.4 keV) and Fe XXVI lines (∼6.95 keV) are clearly resolved in the EPIC spectra. In the Porb–Pspin diagram of intermediate polars, V2069 Cyg shows a low spin-to-orbit ratio of ∼0.0276 in comparison with ∼0.1 for other intermediate polars.
Filaments in VIPERS: galaxy quenching in the infalling regions of groups

We study the quenching of galaxies in different environments and its evolution in the redshift range $0.43 \leq z \leq 0.89$. For this purpose, we identify galaxies inhabiting filaments, the isotropic infall region of groups, the field, and groups in the VIMOS Public Extragalactic Redshift Survey (VIPERS). We classify galaxies as quenched (passive), through their $NUV-r$ versus $r-K$ colours. We study the fraction of quenched galaxies ($F_{r}$) as a function of stellar mass and environment at two redshift intervals. Our results confirm that stellar mass is the dominant factor determining galaxy quenching over the full redshift range explored. We find compelling evidence of evolution in the quenching of intermediate mass galaxies $(9.3 \leq \log(M_{*}/M_{\odot}) \leq 10.5)$ for all environments. For this mass range, $F_{r}$ is largest for galaxies in groups and smallest for galaxies in the field, while galaxies in filaments and in the isotropic infall regions appear to have intermediate values with the exception of the high redshift bin, where the latter show similar fraction of quenched galaxies as in the field. Galaxies in filaments are systematically more quenched than their counterparts infalling from other directions, in agreement to similar results found at low redshift. The least massive galaxies in our samples do not show evidence of internal or environmental quenching.
Discovery of Gas Bulk Motion in the Galaxy Cluster Abell 2256 with Suzaku

The results from Suzaku observations of the galaxy cluster Abell2256 are presented. This cluster is a prototypical and well-studied merging system, exhibiting substructures both in the X-ray surface brightness and in the radial velocity distribution of member galaxies. There are main and sub components separating by 3'. 5 in the sky and by about 2000 km s$^{-1}$ in radial velocity peaks of member galaxies. In order to measure Doppler shifts of iron K-shell lines from the two gas components by the Suzaku XIS, the energy scale of the instrument was evaluated carefully and found to be calibrated well. A significant shift of the radial velocity of the sub component gas with respect to that of the main cluster was detected. All three XIS sensors show the shift independently and consistently among the three. The difference is found to be 1500 $\pm 300$ (statistical) $\pm 300$ (systematic) km s$^{-1}$. The X-ray determined absolute redshifts of and hence the difference between the main and sub components are consistent with those of member galaxies in optical. The observation indicates robustly that the X-ray emitting gas is moving together with galaxies as a substructure within the cluster. These results along with other X-ray observations of gas bulk motions in merging clusters are discussed.
Generation mode-locked square-wave pulse based on reverse saturable absorption effect in graded index multimode fiber

We firstly report mode-locked square-wave pulse in Yb-doped fiber laser based on graded index multimode fiber of reverse suturable absorption. By adjusting the pump power, the width of the square-wave can be tuned range from 350 ps to 52.6 ns with 3dB bandwidth spectrum of 0.73 nm. The supermode suppression ratio exceeds ~ 65 dB, which indicates excellent mode-locked operation state, and we also study the characteristic of pulse by the chirp measurement system. The mode-locked square-wave pulse fiber laser can sever as high power light source for industrial applications.
Strongly regular n-e.c. graphs

A result of Erd\"os and R\'enyi shows that for a fixed integer n almost all graphs satisfy the n-e.c. adjacency property. However, there are few explicit constructions of n e.c. graphs for n > 2, and almost all known families of n-e.c. graphs are strongly regular graphs. In this paper we derive parameter bounds on strongly regular n-e.c. graphs constructed from the point sets of partial geometries. This work generalizes bounds on n-e.c. block intersection graphs of balanced incomplete block designs given by McKay and Pike. It also relates to work by Griggs, Grannel, and Forbes' determining 3-e.c. graphs that are block intersection graphs of Steiner triple systems. In addition to these bounds, we give examples of strongly regular graphs that contain every possible subgraph of small order but are not n-e.c. for n > 2.
Heavily reddened quasars at z ∼ 2 in the UKIDSS Large Area Survey: a transitional phase in AGN evolution

We present a new sample of purely near-infrared-selected KVega 2.5] quasar candidates at z ∼ 2 from ≃900 deg2 of data in the UKIDSS Large Area Survey (LAS). Five of these are spectroscopically confirmed to be heavily reddened type 1 active galactic nuclei (AGN) with broad emission lines bringing our total sample of reddened quasars from the UKIDSS-LAS to 12 at z = 1.4–2.7. At these redshifts, Hα (6563 A) is in the K band. However, the mean Hα equivalent width of the reddened quasars is only 10 per cent larger than that of the optically selected population and cannot explain the extreme colours. Instead, dust extinction of AV ∼ 2–6 mag is required to reproduce the continuum colours of our sources. This is comparable to the dust extinctions seen in submillimetre galaxies at similar redshifts. We argue that the AGN are likely being observed in a relatively short-lived breakout phase when they are expelling gas and dust following a massive starburst, subsequently turning into UV-luminous quasars. Some of our quasars show direct evidence for strong outflows (v ∼ 800–1000 km s−1) affecting the Hα line consistent with this scenario. We predict that a larger fraction of reddened quasar hosts are likely to be submillimetre bright compared to the UV-luminous quasar population. We use our sample to place new constraints on the fraction of obscured type 1 AGN likely to be missed in optical surveys. Taken at face value our findings suggest that the obscured fraction depends on quasar luminosity. The space density of obscured quasars is approximately five times that inferred for UV-bright quasars from the Sloan Digital Sky Survey (SDSS) luminosity function at Mi < −30 but seems to drop at lower luminosities even accounting for various sources of incompleteness in our sample. We find that at Mi ∼ −28 for example, this fraction is unlikely to be larger than ∼20 per cent although these fractions are highly uncertain at present due to the small size of our sample. A deeper K-band survey for highly obscured quasars is clearly needed to test this hypothesis fully and is now becoming possible with new sensitive all-sky infrared surveys such as the VISTA Hemisphere Survey and the Wide Infrared Survey Explorer (WISE) All Sky Survey.
Convection roll-driven generation of supra-wavelength periodic surface structures on dielectrics upon irradiation with femtosecond pulsed lasers

The significance of the magnitude of the Prandtl number of a fluid in the propagation direction of induced convection rolls is elucidated. Specifically, we report on the physical mechanism to account for the formation and orientation of previously unexplored supra-wavelength periodic surface structures in dielectrics, following melting and subsequent capillary effects induced upon irradiation with ultrashort laser pulses. Counterintuitively, it is found that such structures exhibit periodicities, which are markedly, even multiple times, higher than the laser excitation wavelength. It turns out that the extent to which the hydrothermal waves relax depends upon the laser beam energy, produced electron densities upon excitation with femtosecond pulsed lasers, the magnitude of the induced initial local roll disturbances, and the magnitude of the Prandtl number with direct consequences on the orientation and size of the induced structures. It is envisaged that this elucidation may be useful for the interpretation of similar, albeit large-scale periodic or quasiperiodic structures formed in other natural systems due to thermal gradients, while it can also be of great importance for potential applications in biomimetics.
Strategies of Global Corporate Philanthropy: The Case of Spanish Firms in Latin America

La responsabilidad social corporativa (RSC) ha pasado a ser una prioridad en las agendas de los directivos de numerosas empresas. El impacto social de las actividades de las empresas no sólo afecta a las condiciones de vida de una sociedad sino que pueden llegar a afectar a la riqueza y bienestar de los propios accionistas de la empresa. Dentro de las actividades de RSC de una empresa, son especialmente relevantes los programas de acción social o de filantropía, por el impacto que tienen sobre la reputación de la empresa. Asimismo, las empresas con presencia en distintos países no sólo emprenden acciones de filantropía en sus países de origen sino también en los países destinos de sus inversiones. En este sentido, mientras que existe un amplio abanico de estudios sobre la This paper contributes to the literature of CSR and International Business by studying the internationalization of corporate philanthropy in multinationals. Based on a sample of Spanish firms in Latin America, the results show that this phenomenon is linked to the learning dynamics embedded in the internationalization process of the firms, since firms with a larger international exposure are more likely to start international philanthropic programmes. Moreover, the research reveals that global firms with a strong global corporate reputation are more likely to follow a single common philanthropy strategy, while multidomestic firms will establish different local philanthropic strategies. Estrategias de Filantropía Corporativa Global: El Caso de las empresas españolas en Latinoamérica
Are all challenge stressors beneficial for learning? A meta-analytical assessment of differential effects of workload and cognitive demands

ABSTRACT Previous meta-analyses showed that challenge stressors are, though stressful, also motivating. However, their hypothesised gains related to learning are less well understood. In addition to the lack of meta-analytical assessments, there are conflicting theoretical perspectives on the learning effects of challenge stressors. In contrast to the challenge–hindrance stressor framework, action regulation theory posits that cognitive demands, but not workload, are conducive to learning. Furthermore, job control, the level of a stressor, and the type of occupation may moderate the effects of these two challenge stressors. Based on 417 independent samples collectively including 319,306 individuals, this meta-analysis tested the associations of workload and cognitive demands with learning, motivation, and strain and examined potential moderation effects. Results showed that workload was negatively related to learning and motivation and positively related to strain. Cognitive demands were positively related to learning and motivation and negatively related to strain. The detrimental effects of workload were more pronounced for care and social worker and for measures of overload. No moderations were found for country-level job control. Taken together, the results cast doubts on whether stressors can actually be simultaneously detrimental and beneficial, as neither workload nor cognitive demands were found to have such a pattern.
Discrete averaging relations for micro to macro transition

The well-known Hill's averaging theorems for stresses and strains as well as the so-called Hill-Mandel principle of macrohomogeneity are essential ingredients for the coupling and the consistency between the micro and macro scales in multiscale finite element procedures (FE$^2$). We show in this paper that these averaging relations hold exactly under standard finite element discretizations, even if the stress field is discontinuous across elements and the standard proofs based on the divergence theorem are no longer suitable. The discrete averaging results are derived for the three classical types of boundary conditions (affine displacement, periodic and uniform traction boundary conditions) using the properties of the shape functions and the weak form of the microscopic equilibrium equations. The analytical proofs are further verified numerically through a simple finite element simulation of an irregular representative volume element undergoing large deformations. Furthermore, the proofs are extended to include the effects of body forces and inertia, and the results are consistent with those in the smooth continuum setting. This work provides a solid foundation to apply Hill's averaging relations in multiscale finite element methods without introducing an additional error in the scale transition due to the discretization.