Miracle-dz/UniFAR-FTUs huggingface dataset:
Upgrading Voxel-wise Encoding Model via Integrated Integration over Features and Brain Networks

A central goal of cognitive neuroscience is to build computational models that predict and explain neural responses to sensory inputs in the cortex. Recent studies attempt to borrow the representation power of deep neural networks (DNN) to predict the brain response and suggest a correspondence between artificial and biological neural networks in their feature representations. However, each DNN instance is often specified for certain computer vision tasks which may not lead to optimal brain correspondence. On the other hand, these voxel-wise encoding models focus on predicting single voxels independently, while brain activity often demonstrates rich and dynamic structures at the population and network levels during cognitive tasks. These two important properties suggest that we can improve the prevalent voxel-wise encoding models by integrating features from DNN models and by integrating cortical network information into the models. In this work, we propose a new unified framework that addresses these two aspects through DNN feature-level ensemble learning and brain atlas-level model integration. Our proposed approach leads to superior performance over previous DNN-based encoding models in predicting whole-brain neural activity during naturalistic video perception. Furthermore, our unified framework also facilitates the investigation of the brain’s neural representation mechanism by accurately predicting the neural response corresponding to complex visual concepts.
Shigella ipaA mediates actin bundling through diffusible vinculin oligomers with activation imprint

Upon activation, vinculin reinforces cytoskeletal anchorage during cell adhesion. Activating ligands classically disrupt intramolecular interactions between the vinculin head and tail domain that binds to actin filaments. Here, we show that Shigella IpaA triggers major allosteric changes in the head domain leading to vinculin homo-oligomerization. Through the cooperative binding of its three vinculin-binding sites (VBSs), IpaA induces a striking reorientation of the D1 and D2 head subdomains associated with vinculin oligomerization. IpaA thus acts as a catalyst producing vinculin clusters that bundle actin at a distance from the activation site and trigger the formation of highly stable adhesions resisting the action of actin relaxing drugs. Unlike canonical activation, vinculin homo-oligomers induced by IpaA appear to keep a persistent imprint of the activated state in addition to their bundling activity, accounting for stable cell adhesion independent of force transduction and relevant to bacterial invasion.
Do micromagnets expose spin qubits to charge and Johnson noise

An ideal quantum dot spin qubit architecture requires a local magnetic field for one-qubit rotations. Such an inhomogeneous magnetic field, which could be implemented via a micromagnet, couples the qubit subspace with background charge fluctuations causing dephasing of spin qubits. In addition, a micromagnet generates magnetic field evanescent-wave Johnson noise. We derive an effective Hamiltonian for the combined effect of a slanting magnetic field and charge noise on a single-spin qubit and estimate the free induction decay dephasing times T2* for Si and GaAs. The effect of the micromagnet on Si qubits is comparable in size to that of spin-orbit coupling at an applied field of B=1T, whilst dephasing in GaAs is expected to be dominated by spin-orbit coupling. Tailoring the magnetic field gradient can efficiently reduce T2* in Si. In contrast, the Johnson noise generated by a micromagnet will only be important for highly coherent spin qubits.
Team i3D 3D Interaction

say that the more numerous are these factors, the stronger is the feeling of immersion and the more justiﬁed is the virtual reality expression. need: increasingly demanding users and a growing number of applications. (cid:15) a unsatisfactory situation: poor interfaces: primarily 2D, with a strong under-utilization of the human-application bandwidth. (cid:15) strong potentialities: very promising conﬁgurations and approaches to study or to conceive.
The Effect of Metallicity on the Delay-Time Distribution of Type Ia Supernova

Measuring the delay-time distribution (DTD) of type Ia supernova (SNe Ia) is an important way to constrain the progenitor nature of SNe Ia. Recently, Strolger et al. (2010, ApJ, 713, 32, hereafter SDR10) obtained a very delayed DTD, which is much different from other measurements. They suggested that metallicity could be the origin of their delayed DTD. In this paper, we show the effect of metallicity on the DTD of SNe Ia from single-degenerate models (including WD + MS and WD + RG channels). Via a binary population synthesis approach, we find that the DTD from a low-metallicity population is significantly delayed compared with that from a high-metallicity one. In addition, we also find that a substantial fraction of SNe Ia have a delay time shorter than 1 Gyr, and the fraction of SNe Ia with short delay times increases with the metallicity, i.e., about 35% for Z = 0.001, while more than 70% for Z = 0.02. These results would help to qualitatively explain the result of SDR10. Furthermore, we noticed that the contribution of the WD + RG channel from the low-metallicity population is higher than that from the high-metallicity one. However, we could not quantitatively obtain a DTD consistent with the results of SDR10 by changing the metallicity. As a consequence, metallicity may partly contribute to the DTD of SNe Ia, and should therefore be carefully checked when one derives the DTD of SNe Ia from observations.
Structural topography-mediated high temperature wetting symmetry breaking

Directed motion of liquid droplets is of considerable importance in various industrial processes. Despite extensive advances in this field of research, our understanding and the ability to control droplet dynamics at high temperature remain limited, in part due to the emergence of complex wetting states intertwined by the phase change process at the triple-phase interfaces. Here we show that two concurrent wetting states (Leidenfrost and contact boiling) can be manifested in a single droplet above its boiling point rectified by the presence of asymmetric textures. The breaking of the wetting symmetry at high temperature subsequently leads to the preferential motion towards the region with higher heat transfer coefficient. We demonstrate experimentally and analytically that the droplet vectoring is intricately dependent on the interplay between the structural topography and its imposed thermal state. Our fundamental understanding and the ability to control the droplet dynamics at high temperature represent an important advance and enable the rational design of various surfaces for multifunctional applications, especially in high temperature thermal systems where high energy efficiency, security and stability are preferred.
Beacons into the Cosmic Dark Ages: Boosted Transmission of Lyα from UV Bright Galaxies at z ≳ 7

Recent detections of Lyman alpha (Lyα) emission from z > 7.5 galaxies were somewhat unexpected given a dearth of previous non-detections in this era when the intergalactic medium (IGM) is still highly neutral. But these detections were from UV bright galaxies, which preferentially live in overdensities that reionize early, and have significantly Doppler-shifted Lyα line profiles emerging from their interstellar media (ISM), making them less affected by the global IGM state. Using a combination of reionization simulations and empirical ISM models we show, as a result of these two effects, that UV bright galaxies in overdensities have >2× higher transmission through the z ∼ 7 IGM than typical field galaxies, and that this boosted transmission is enhanced as the neutral fraction increases. The boosted transmission is not sufficient to explain the observed high Lyα fraction of Muv ≲ −22 galaxies, suggesting that Lyα emitted by these galaxies must be stronger than expected due to enhanced production and/or selection effects. Despite the bias of UV bright galaxies to reside in overdensities we show Lyα observations of such galaxies can accurately measure the global neutral hydrogen fraction, particularly when Lyα from UV faint galaxies is extinguished, making them ideal candidates for spectroscopic follow-up into the cosmic Dark Ages.
SOAR OPTICAL AND NEAR-INFRARED SPECTROSCOPIC SURVEY OF NEWLY DISCOVERED MASSIVE STARS IN THE PERIPHERY OF GALACTIC MASSIVE STAR CLUSTERS I-NGC 3603

In this work, we present the results of a spectroscopic study of very massive stars (VMSs) found outside the center of the massive stellar cluster NGC 3603. From the analysis of the associated Southern Astrophysical Research (SOAR) Telescope spectroscopic data and related optical–near-IR (NIR) photometry, we confirm the existence of several VMSs in the periphery of NGC 3603. The first group of objects (MTT58, WR42e, and RF7) is composed of three new Galactic exemplars of the OIf*/WN type, all of them with probable initial masses well above 100 and estimated ages of about 1 Myr. Based on our Goodman blue-optical spectrum of another source in our sample (MTT68), we can confirm the previous finding in the NIR of the only other Galactic exemplar (besides HD 93129A) of the O2If* type known to date. Based on its position relative to a set of theoretical isochrones in a Hertzprung–Russel (H–R) diagram, we concluded that the new O2If* star could be one of the most massive (150 ) and luminous (MV = −7.3) O-stars in the Galaxy. Also, another remarkable result is the discovery of a new O2v star (MTT31), which is the first exemplar of that class so far identified in the Milk Way. From its position in the H–R diagram it is found that this new star probably had an initial mass of 80 , as well as an absolute magnitude of MV = −6.0, corresponding to a luminosity similar to other known O2v stars in the Large Magellanic Cloud. Finally, we also communicate the discovery of a new Galactic O3.5If* star (RFS8) that is quite an intriguing case. Indeed, it is located far to the south of the NGC 3603 center, in apparent isolation at a large radial projected linear distance of ∼62 pc. Its derived luminosity is similar to that of the other O3.5If* (Sh18) found in NGC 3603's innermost region, and the fact that a such high mass star is observed so isolated in the field led us to speculate that perhaps it could have been expelled from the innermost parts of the complex by a close fly-by dynamical encounter with a very massive hard binary system.
Impact parameter smearing effects on isospin sensitive observables in heavy ion collisions

The validity of impact parameter estimation from multiplicity of charged particles at low-intermediate energies are checked within the framework of ImQMD model. The simulations show that the multiplicity of charged particles cannot distinguish the impact parameter very well, especially for central collisions at the beam energy lower than $\sim$70 MeV/u. Simulating the central collisions defined by particle multiplicity, the charge distribution is modified and the CI-R(n/p) ratios are reduced less than 10\% for neutron-rich systems relative to that obtained with fixed impact parameter at $E_{beam}$=50 MeV/u, while CI-DR(n/p) ratio is consistent with the results obtained with fixed impact parameter. The sensitivity to effective mass splitting can be amplified for $^{132}$Sn+$^{124}$Sn than that for $^{124}$Sn+$^{124}$Sn, and we propose to employ the $^{132}$Sn+$^{124}$Sn system in future experiments to distinguish the effective mass splitting.
Neutrino-4 experiment on search for sterile neutrino with multi-section model of detector

In order to carry out research in the field of possible existence of a sterile neutrino the laboratory based on SM-3 reactor (Dimitrovgrad, Russia) was created to search for oscillations of reactor antineutrino. The prototype of a multi-section neutrino detector with liquid scintillator volume of 350 l was installed in the middle of 2015. It is a moveable inside the passive shielding detector, which can be set at distance range from 6 to 11 meters from the reactor core. Measurements of antineutrino flux at such small distances from the reactor core are carried out with moveable detector for the first time. The measurements carried out with detector prototype demonstrated a possibility of measuring a reactor antineutrino flux in difficult conditions of cosmic background at Earth surface.
ESTIMATION OF DISTANCES TO STARS WITH STELLAR PARAMETERS FROM LAMOST

We present a method to estimate distances to stars with spectroscopically derived stellar parameters. The technique is a Bayesian approach with likelihood estimated via comparison of measured parameters to a grid of stellar isochrones, and returns a posterior probability density function for each star’s absolute magnitude. This technique is tailored specifically to data from the Large Sky Area Multi-object Fiber Spectroscopic Telescope (LAMOST) survey. Because LAMOST obtains roughly 3000 stellar spectra simultaneously within each ∼5° diameter “plate” that is observed, we can use the stellar parameters of the observed stars to account for the stellar luminosity function and target selection effects. This removes biasing assumptions about the underlying populations, both due to predictions of the luminosity function from stellar evolution modeling, and from Galactic models of stellar populations along each line of sight. Using calibration data of stars with known distances and stellar parameters, we show that our method recovers distances for most stars within ∼20%, but with some systematic overestimation of distances to halo giants. We apply our code to the LAMOST database, and show that the current precision of LAMOST stellar parameters permits measurements of distances with ∼40% error bars. This precision should improve as the LAMOST data pipelines continue to be refined.
HUBBLE SPACE TELESCOPE PIXEL ANALYSIS OF THE INTERACTING S0 GALAXY NGC 5195 (M51B)

We report the properties of the interacting S0 galaxy NGC 5195 (M51B), revealed in a pixel analysis using the Hubble Space Telescope/Advanced Camera for Surveys images in the F435W, F555W, and F814W (BVI) bands. We analyze the pixel color–magnitude diagram (pCMD) of NGC 5195, focusing on the properties of its red and blue pixel sequences and the difference from the pCMD of NGC 5194 (M51A; the spiral galaxy interacting with NGC 5195). The red pixel sequence of NGC 5195 is redder than that of NGC 5194, which corresponds to the difference in the dust optical depth of 2 < ΔτV < 4 at fixed age and metallicity. The blue pixel sequence of NGC 5195 is very weak and spatially corresponds to the tidal bridge between the two interacting galaxies. This implies that the blue pixel sequence is not an ordinary feature in the pCMD of an early-type galaxy, but that it is a transient feature of star formation caused by the galaxy–galaxy interaction. We also find a difference in the shapes of the red pixel sequences on the pixel color–color diagrams (pCCDs) of NGC 5194 and NGC 5195. We investigate the spatial distributions of the pCCD-based pixel stellar populations. The young population fraction in the tidal bridge area is larger than that in other areas by a factor >15. Along the tidal bridge, young populations seem to be clumped particularly at the middle point of the bridge. On the other hand, the dusty population shows a relatively wide distribution between the tidal bridge and the center of NGC 5195.
CYCLICAL CHANGES IN THE TIMING RESIDUALS FROM THE PULSAR B0919+06

We report the detection of a large glitch in the pulsar B0919+06 (J0922+0638). The glitch occurred in 2009 November 5 (MJD 55140) and was characterized by a fractional increase in the rotation frequency of Δν/ν ∼ 1.3 × 10−6. A large glitch happens in the pulsar whose rotation has an unstable character. We present the results of the analysis of the rotation behavior of this pulsar over the 30 year time span from 1979 to 2009. These results show that the pulsar's rotation frequency underwent continuous, slow oscillations that resembled glitch-like events. During the 1991–2009 interval, the pulsar experienced a continuous sequence of 12 slow glitches with a fractional increase in the rotation frequency of Δν/ν ∼ 1.5 × 10−9. All the slow glitches observed have similar signatures related to a slow increase in the rotation frequency for ∼200 days and to the subsequent relaxation back to the pre-glitch value for ∼400 days. We show that a continuous sequence of such slow glitches is characterized by practically identical amplitudes of Δν ∼ 3.5 × 10−9 Hz and identical time intervals between glitches of ∼600 days and is well described by a periodic sawtooth-like function. The detection of two different phenomena, such as a large glitch and a sequence of slow glitches, indicate the presence of two types of discontinuities in the rotation frequency of the pulsar B0919+06. These discontinuities can be classified as normal and slow glitches.
Intermediate-field two-photon absorption enhancement by shaped femtosecond pulses: Tolerance to phase deviation from perfect antisymmetry

We study in detail the coherent interference mechanism leading to the intermediate-field two-photon absorption enhancement recently found for shaped femtosecond pulses with spectral phases that are antisymmetric around one-half of the transition frequency. We particularly investigate the tolerance of the phenomenon to the phase deviation from perfect antisymmetry. We theoretically and experimentally find that this tolerance increases as the field strength increases. For the present Na excitation, the enhancement occurs even when $~$30% of the phase pattern is not antisymmetric. Our findings are of particular importance for multichannel coherent control scenarios.
GLOBAL ENERGETICS OF SOLAR FLARES. II. THERMAL ENERGIES

We present the second part of a project on the global energetics of solar flares and coronal mass ejections that includes about 400 M- and X-class flares observed with the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) during the first 3.5 yr of its mission. In this Paper II we compute the differential emission measure (DEM) distribution functions and associated multithermal energies, using a spatially-synthesized Gaussian DEM forward-fitting method. The multithermal DEM function yields a significantly higher (by an average factor of ≈14), but more comprehensive (multi-)thermal energy than an isothermal energy estimate from the same AIA data. We find a statistical energy ratio of E th / E diss ? > ≈ 2–40% between the multithermal energy Eth and the magnetically dissipated energy Ediss, which is an order of magnitude higher than the estimates of Emslie et al. . For the analyzed set of M- and X-class flares we find the following physical parameter ranges: L = 10 8.2 – 10 9.7 ? > cm for the length scale of the flare areas, T p = 10 5.7 – 10 7.4 ? > K for the DEM peak temperature, T w = 10 6.8 – 10 7.6 ? > K for the emission measure-weighted temperature, n p = 10 10.3 − 10 11.8 ? > cm−3 for the average electron density, EM p = 10 47.3 – 10 50.3 ? > cm−3 for the DEM peak emission measure, and E th = 10 26.8 – 10 32.0 ? > erg for the multithermal energies. The deduced multithermal energies are consistent with the RTV scaling law E th , RTV = 7.3 × 10 − 10 T p 3 L p 2 ? > , which predicts extremal values of E th , max ≈ 1.5 × 10 33 ? > erg for the largest flare and E th , min ≈ 1 × 10 24 ? > erg for the smallest coronal nanoflare. The size distributions of the spatial parameters exhibit powerlaw tails that are consistent with the predictions of the fractal-diffusive self-organized criticality model combined with the RTV scaling law.
Effective polymer dynamics of D-dimensional black hole interiors

We consider two different effective polymerization schemes applied to D-dimensional, spherically symmetric black hole interiors. It is shown that polymerization of the generalized area variable alone leads to a complete, regular, single-horizon spacetime in which the classical singularity is replaced by a bounce. The bounce radius is independent of rescalings of the homogeneous internal coordinate, but does depend on the arbitrary fiducial cell size. The model is therefore necessarily incomplete. It nonetheless has many interesting features: After the bounce, the interior region asymptotes to an infinitely expanding Kantowski-Sachs spacetime. If the solution is analytically continued across the horizon, the black hole exterior exhibits asymptotically vanishing quantum corrections due to the polymerization. In all spacetime dimensions except four, the falloff is too slow to guarantee invariance under Poincare transformations in the exterior asymptotic region. Hence, the four-dimensional solution stands out as the only example which satisfies the criteria for asymptotic flatness. In this case it is possible to calculate the quantum-corrected temperature and entropy. We also show that polymerization of both phase space variables, the area and the conformal mode of the metric, generically leads to a multiple horizon solution which is reminiscent of polymerized minisuperspace models of spherically symmetric blackmore » holes in loop quantum gravity. « less
High intrinsic ZT in InP3 monolayer at room temperature

Two-dimensional thermoelectric (TE) materials which have the figure of merit ZT that is greater than 1.5 at room temperature would be highly desirable in energy conversion since the efficiency is competitive to conventional energy conversion techniques. Here, we report that the indium triphosphide (InP3) monolayer shows a large ZT of 1.92 at 300 K, based on the quantum calculations within the ballistic thermal transport region. A remarkably low and isotropic phononic thermal conductivity is found due to the flat lattice vibration modes, which takes a major responsibility for the impressively high ZT at room temperature. Moreover, a large ZT of 1.67 can still be achieved even under a 1% mechanical tension on the lattice. These results suggest that the InP3 monolayer is a promising candidate for low dimensional TE applications.
Quantum Vacuum Friction in highly magnetized neutron stars

In this letter we calculate the energy loss of a highly magnetized neutron star due to Quantum Vacuum Friction (QVF). Taking into account one-loop corrections in the effective Heisenberg-Euler Lagrangian of the light-light interaction, we derive an analytic expression for QVF allowing us to take into account a magnetic field at the surface of the star as high as 1011 T. In the case of magnetars, with magnetic fields above the QED critical field, we show that the QVF is the dominating energy loss process. This has important consequences, in particular for the inferred value of the magnetic field. This also indicates the need for independent measurements of magnetic field, energy loss rate, and the braking index in order to fully characterize magnetars.
Opleiding Informatica Finding consensus knowledge in the Huntington’s Disease pathway

Huntington’s Disease (HD) is an inherited neurodegenerative disease caused by an expansion of the CAG repeat in the Huntingtin (HTT) gene. Even though it is caused by a single mutation, the underlying mechanism of HD is very complex. Many pathways have been suggested to contribute to the pathogenesis of HD, but a consensus has yet to be established. Protein-Protein Interaction Network (PPIN) tools allow for visualization and analysis of these pathways and provide a great way to consolidate existing information on the HD pathway. By using functional enrichment analysis on these networks the role of HTT can be reaffirmed, which will further the understanding of the affected cellular processes and the role of HTT in different pathways. In this research, knowledge from different databases have been compared in order to find consensus and discrepancies between them and functionally enriched terms within these parts were connected to existing scientific research to give a better image of the current knowledge surrounding the HD pathway.