Miracle-dz/UniFAR-FTUs huggingface dataset:
Whole-Brain fMRI Functional Connectivity Signatures Predict Sustained Emotional Experience in Naturalistic Contexts

Determining and decoding emotional brain processes under ecologically valid conditions remains a key challenge in affective neuroscience. The current functional magnetic resonance imaging (fMRI) based emotion decoding studies are mainly based on brief and isolated episodes of emotion induction, while sustained emotional experience in naturalistic environments that mirror daily life experiences are scarce. Here we use 10-minute movie clips as ecologically valid emotion-evoking procedures in n=52 individuals to explore emotion-specific fMRI functional connectivity (FC) profiles on the whole-brain level at high spatial resolution (400 atlas based parcels). Employing machine-learning based decoding and cross validation procedures allowed to develop predictive FC profiles that can accurately distinguish sustained happiness and sadness and that generalize across movies and subjects. Both functional brain network-based and subnetwork-based emotion prediction results suggest that emotion manifests as distributed representation of multiple networks, rather than a single functional network or subnetwork. Further, the results show that the Visual Network (VN) and Default Mode Network (DMN) associated functional networks, especially VN-DMN, exhibit a strong contribution to emotion prediction. To further estimate the cumulative effect of naturalistic long-term movie-based video-evoking emotions, we divide the 10-min episode into three stages: early stimulation (1 ~ 200 s), middle stimulation (201 ~ 400 s), and late stimulation (401 ~ 600 s) and examine the emotion prediction performance at different stimulation stages. We found that the late stimulation has a stronger predictive ability (accuracy=85.32%, F1-score=85.62%) compared to early and middle stimulation stages, implying that continuous exposure to emotional stimulation can lead to more intense emotions and further enhance emotion-specific distinguishable representations. The present work demonstrates that sustained sadness and happiness under naturalistic conditions are presented in emotion-specific network profiles and these expressions may play different roles in the generation and modulation of emotions. These findings elucidate the importance of network level adaptations for sustained emotional experiences during naturalistic contexts and open new venues for imaging network level contributions under naturalistic conditions.
Segregation of pathways leading to pexophagy

Pexophagy occurs via distinct NIX- and USP30/NBR1-dependent pathways. Peroxisomes are organelles with key roles in metabolism including long-chain fatty acid production. Their metabolic functions overlap and interconnect with those of mitochondria, with which they share an overlapping but distinct proteome. Both organelles are degraded by selective autophagy processes termed pexophagy and mitophagy. Although mitophagy has received intense attention, the pathways linked to pexophagy and associated tools are less well developed. We have identified the neddylation inhibitor MLN4924 as a potent activator of pexophagy and show that this is mediated by the HIF1α-dependent up-regulation of BNIP3L/NIX, a known adaptor for mitophagy. We show that this pathway is distinct from pexophagy induced by the USP30 deubiquitylase inhibitor CMPD-39, for which we identify the adaptor NBR1 as a central player. Our work suggests a level of complexity to the regulation of peroxisome turnover that includes the capacity to coordinate with mitophagy, via NIX, which acts as a rheostat for both processes.
Experiments on a videotape atom chip: fragmentation and transport studies

This paper reports on experiments with ultracold rubidium atoms confined in microscopic magnetic traps created using a piece of periodically magnetized videotape mounted on an atom chip. The roughness of the confining potential is studied with atomic clouds at temperatures of a few μK and at distances between 30 and 80 μm from the videotape-chip surface. The inhomogeneities in the magnetic field created by the magnetized videotape close to the central region of the chip are characterized in this way. In addition, we demonstrate a novel transport mechanism whereby we convey cold atoms confined in arrays of videotape magnetic micro-traps over distances as large as ∼1 cm parallel to the chip surface. This conveying mechanism enables us to survey the surface of the chip and observe potential-roughness effects across different regions.
MASS AND ENVIRONMENT AS DRIVERS OF GALAXY EVOLUTION. III. THE CONSTANCY OF THE FAINT-END SLOPE AND THE MERGING OF GALAXIES

Using our continuity approach, we explore the underlying connections between the evolution of the faint-end slope αs of the stellar mass function of star-forming galaxies, the logarithmic slope β of the specific star formation rate (sSFR)–mass relation, and the merging of galaxies. We derive analytically the consequences of the observed constancy of αs since redshifts of at least z ∼ 2. If the logarithmic slope β of the sSFR–mass relation is negative, then the faint-end slope αs should quickly diverge due to the differential mass increase of galaxies on the star-forming main sequence, and this will also quickly destroy the Schechter form of the mass function. This problem can be solved by removing low-mass galaxies by merging them into more massive galaxies. We quantify this process by introducing the specific merger mass rate (sMMR) as the specific rate of mass added to a given galaxy through mergers. For a modest negative value of β ∼ −0.1, an average sMMR ∼ 0.1 sSFR across the population is required to keep αs constant with epoch, as observed. This in turn implies a merger rate of ∼0.2 sSFR for major mergers, which is consistent with the available observational estimates. More negative values of β require higher sMMR and higher merger rates, and the steepening of the mass function becomes impossible to control for β < −(αs + 2). The close link that is required between the in situ sSFR and the sMMR probably arises because both are closely linked to the buildup of dark matter halos. These new findings further develop the formalism for the evolving galaxy population that we introduced earlier and show how striking symmetries in the galaxy population can emerge as the result of deep links between the physical processes involved.
CONSTRAINING CHANGES IN THE PROTON–ELECTRON MASS RATIO WITH INVERSION AND ROTATIONAL LINES

We report deep Green Bank Telescope spectroscopy in the redshifted NH3 (1,1), CS 1–0, and H2CO 000–101 lines from the z ∼ 0.685 absorber toward B0218+357. The inversion (NH3) and rotational (CS, H2CO) line frequencies have different dependences on the proton–electron mass ratio μ, implying that a comparison between the line redshifts is sensitive to changes in μ. A joint three-component fit to the NH3, CS, and H2CO lines yields [Δμ/μ] = (−3.5 ± 1.2) × 10−7, from z ∼ 0.685 to today, where the error includes systematic effects from comparing lines from different species and possible frequency-dependent source morphology. Two additional sources of systematic error remain, due to time variability in the source morphology and velocity offsets between nitrogen-bearing and carbon-bearing species. We find no statistically significant (⩾3σ) evidence for changes in μ and obtain the stringent 3σ constraint, [Δμ/μ] < 3.6 × 10−7, over 6.2 Gyr; this is the best present limit on temporal changes in μ from any technique, and for any look-back time, by a factor ≳5.
The Hard X-Ray Spectrum as a Probe for Black Hole Growth in Radio-Quiet Active Galactic Nuclei

We study the hard X-ray spectral properties of 10 highly luminous radio-quiet (RQ) active galactic nuclei (AGNs) at z = 1.3–3.2, including new XMM-Newton observations of four of these sources. We find a significant correlation between the normalized accretion rate (L/LEdd) and the hard X-ray photon index (Γ) for 35 moderate- to high-luminosity RQ AGNs, including our 10 highly luminous sources. Within the limits of our sample, we show that a measurement of Γ and LX can provide an estimate of L/LEdd and black hole mass (MBH) with a mean uncertainty of a factor of ≲3 on the predicted values of these properties. This may provide a useful probe for tracing the history of BH growth in the universe, utilizing samples of X-ray-selected AGNs for which L/LEdd and MBH have not yet been determined systematically. It may prove to be a useful way to probe BH growth in distant Compton-thin type 2 AGNs. We also find that the optical-X-ray spectral slope (αox) depends primarily on optical-UV luminosity rather than on L/LEdd in a sample of RQ AGNs spanning 5 orders of magnitude in luminosity and over 2 orders of magnitude in L/LEdd. We detect a significant Compton-reflection continuum in two of our highly luminous sources, and in the stacked X-ray spectrum of seven other sources with similar luminosities, we obtain a mean relative Compton reflection of R = 0.9+ 0.6−0.5 and an upper limit on the rest-frame equivalent width of a neutral Fe Kα line of 105 eV. We do not detect a significant steepening of the X-ray power-law spectrum below rest-frame 2 keV in any of our highly luminous sources, suggesting that a soft-excess feature, commonly observed in local AGNs, either does not depend strongly on L/LEdd, or is not accessible at high redshifts using current X-ray detectors.
Spinning bodies in curved spacetime

We study the motion of neutral and charged spinning bodies in curved space-time in the test-particle limit. We construct equations of motion using a closed covariant Poisson-Dirac bracket formulation which allows for dierent choices of the hamiltonian. We derive conditions for the existence of constants of motion and apply the formalism to the case of spherically symmetric space-times. We show that the periastron of a spinning body in a stable orbit in a Schwarzschild or Reissner-Nordstrm background not only precesses, but also varies radially. By analysing the stability conditions for circular motion we nd the innermost
A simplified view of blazars: contribution to the X-ray and γ-ray extragalactic backgrounds

The "blazar simplified view" is a new paradigm that explains well the diverse statistical properties of blazars observed over the entire electromagnetic spectrum on the basis of minimal assumptions on blazars' physical and geometrical properties. In this paper, the fourth in a series, we extend the predictions of this paradigm below the sensitivity of existing surveys and estimate the contribution of blazars to the X-ray and gamma-ray extragalactic backgrounds. We find that the integrated light from blazars can explain up to 100% of the cosmic background at energies larger than ~10 GeV, and contribute ~40 to 70% of the gamma-ray diffuse radiation between 100 MeV and 10 GeV. The contribution of blazars to the X-ray background, between 1 and 50 keV, is approximately constant and of the order of 4-5%. On the basis of an interpolation between the estimated flux at X-ray and gamma-ray energies we can expect that the contribution of blazars raises to ~10% at 100 keV, and continues to increase with energy until it becomes the dominant component at a few MeV. Finally, we show that a strong dependence of the synchrotron peak frequency on luminosity, as postulated by the "blazar sequence", is ruled out by the observational data as it predicts a gamma-ray background above a few GeV that is far in excess of the observed value.
A critical assessment of turbulence models for 1D core-collapse supernova simulations

It has recently been proposed that global or local turbulence models can be used to simulate core-collapse supernova explosions in spherical symmetry (1D) more consistently than with traditional approaches for parametrized 1D models. However, a closer analysis of the proposed schemes reveals important consistency problems. Most notably, they systematically violate energy conservation as they do not balance buoyant energy generation with terms that reduce potential energy, thus failing to account for the physical source of energy that buoyant convection feeds on. We also point out other non-trivial consistency requirements for viable turbulence models. The Kuhfuss model from the 1980s proves more consistent than the newly proposed approaches for supernovae, but still cannot account naturally for all the relevant physics for predicting explosion properties. We perform numerical simulations for a $20 \, \mathrm{M}_\odot$ progenitor to further illustrate problems of 1D turbulence models. If the buoyant driving term is formulated in a conservative manner, the explosion energy of ${\sim }2\times 10^{51}\, \mathrm{erg}$ for the corresponding non-conservative turbulence model is reduced to $\lt 10^{48} \, \mathrm{erg}$ even though the shock expands continuously. This demonstrates that the conservation problem cannot be ignored. Although plausible energies can be reached using an energy-conserving model when turbulent viscosity is included, it is doubtful whether the energy budget of the explosion is regulated by the same mechanism as in multidimensional models. We conclude that 1D turbulence models based on a spherical Reynolds decomposition cannot provide a more consistent approach to supernova explosion and remnant properties than other phenomenological approaches before some fundamental problems are addressed.
Quantum critical scaling behavior of deconfined spinons

We perform a renormalization group analysis of some important effective field theoretic models for deconfined spinons. We show that deconfined spinons are critical for an isotropic $\mathrm{SU}(N)$ Heisenberg antiferromagnet, if $N$ is large enough. We argue that nonperturbatively this result should persist down to $N=2$ and provide further evidence for the so-called deconfined quantum criticality scenario. Deconfined spinons are also shown to be critical for the case describing a transition between quantum spin nematic and dimerized phases. On the other hand, the deconfined quantum criticality scenario is shown to fail for a class of easy-plane models. For the cases where deconfined quantum criticality occurs, we calculate the critical exponent $\ensuremath{\eta}$ for the decay of the two-spin correlation function to first-order in $ϵ=4\ensuremath{-}d$. We also note the scaling relation $\ensuremath{\eta}=d+2(1\ensuremath{-}\ensuremath{\varphi}∕\ensuremath{\nu})$ connecting the exponent $\ensuremath{\eta}$ for the decay to the correlation length exponent $\ensuremath{\nu}$ and the crossover exponent $\ensuremath{\varphi}$.
Black Hole Mass Estimation: How Good is the Virial Estimate?

Abstract Black hole mass is a key factor in determining how a black hole interacts with its environment. However, the determination of black hole masses at high redshifts depends on secondary mass estimators, which are based on empirical relationships and broad approximations. A dynamical disk wind broad line region model (BLR) of active galactic nuclei is built in order to test the impact of different BLR geometries and inclination angles on the black hole mass estimation. Monte Carlo simulations of two disk wind models are constructed to recover the virial scale factor, f, at various inclination angles. The resulting f values strongly correlate with inclination angle, with large f values associated with small inclination angles (close to face-on) and small f values with large inclination angles (close to edge-on). The recovered f factors are consistent with previously determined f values, found from empirical relationships. Setting f as a constant may introduce a bias into virial black hole mass estimates for a large sample of active galactic nuclei. However, the extent of the bias depends on the line width characterisation (e.g. full width at half maximum or line dispersion). Masses estimated using $f_{\text{FWHM}}$ tend to be biased towards larger masses, but this can generally be corrected by calibrating for the width or shape of the emission line.
More on the structure of tidal tails

We investigate the epicyclic motion of stars escaping from star clusters. Using streaklines, we visualise the path of escaping stars and show how epicyclic motion leads to over- and underdensities in tidal tails of star clusters moving on circular and eccentric orbits about a galaxy. Additionally, we investigate the effect of the cluster mass on the tidal tails, by showing that their structure is better matched when the perturbing effect of the cluster mass is included. By adjusting streaklines to results of N-body computations we can accurately and quickly reproduce all observed substructure, especially the streaky features often found in simulations which may be interpreted in observations as multiple tidal tails. Hence, we can rule out tidal shocks as the origin of such substructures. Finally, from the adjusted streakline parameters we can verify that for the star clusters we studied escape mainly happens from the tidal radius of the cluster, given by xL = (GM/( 2 ∂ 2 �/∂R 2 )) 1/3 . We find, however, that there is another limiting radius, the “edge” radius, which gives the smallest radius from which a star can escape during one cluster orbit about the galaxy. For eccentric cluster orbits the edge radius shrinks with increasing orbital eccentricity (for fixed apocentric distance) but is always significantly larger than the respective perigalactic tidal radius. In fact, the edge radii of the clusters we investigated, which are extended and tidally filling, agree well with their (fitted) King radii, which may indicate a fundamental connection between these two quantities.
The role of OH in the chemical evolution of protoplanetary disks. I. The comet-forming region

Context. Time-dependent gas-grain chemistry can help us understand the layered structure of species deposited onto the surface of grains during the lifetime of a protoplanetary disk. The history of trapping large quantities of carbon-and oxygen-bearing molecules onto the grains is especially significant for the formation of more complex (organic) molecules on the surface of grains. Aims. Among other processes, cosmic ray-induced UV photoprocesses can lead to the efficient formation of OH. Using a more accurate treatment of cosmic ray-gas interactions for disks, we obtain an increased cosmic ray-induced UV photon flux of 3.8 x 10(5) photons cm(-2) s(-1) for a cosmic-ray ionization rate of H-2 value of 5 x 10(-17) s(-1) (compared to previous estimates of 10(4) photons cm(-2) s(-1) based on ISM dust properties). We explore the role of the enhanced OH abundance on the gas-grain chemistry in the midplane of the disk at 10 AU, which is a plausible location of comet formation. We focus on studying the formation/destruction pathways and timescales of the dominant chemical species. Methods. We solved the chemical rate equations based on a gas-grain chemical network and correcting for the enhanced cosmic ray-induced UV field. This field was estimated from an appropriate treatment of dust properties in a protoplanetary disk, as opposed to previous estimates that assume an ISM-like grain size distribution. We also explored the chemical effects of photodesorption of water ice into OH+H. Results. Near the end of the disk's lifetime our chemical model yields H2O, CO, CO2, and CH4 ice abundances at 10 AU (consistent with a midplane density of 10(10) cm(-3) and a temperature of 20 K) that are compatible with measurements of the chemical composition of cometary bodies for a [C/O] ratio of 0.16. This comparison puts constraints on the physical conditions in which comets were formed.
The growth of black holes from Population III remnants in the Renaissance simulations

The formation of stellar mass black holes from the remnants of Population III stars provides a source of initial black hole seeds with the potential to grow into intermediate or, in rare cases, possibly supermassive black holes. We use the Renaissance simulation suite to follow the growth of over 15,000 black holes born into mini-haloes in the early Universe. The black holes populate haloes from 10^6 Msun up to 10^9 Msun. We find that all of the black holes display very inefficient growth. On average the black holes increase their initial mass by a factor 10^-5, with the most active black holes increasing their mass by approximately 10%. Only a single black hole experiences any period of super-Eddington accretion, but the duration is very short and not repeated. Furthermore, we find no correlation of black hole accretion with halo mass in the mass range sampled. Within most haloes, we identify clumps of cool, dense gas for which accretion rates would be high, but instances of black holes encountering these clumps are rare and short-lived. Star formation competes with black hole growth by consuming available gas and driving down accretion rates through feedback. We conclude that the black holes born from Population III remnants do not form a significant population of intermediate mass black holes in the early Universe and will need to wait until later times to undergo significant accretion, if at all.
Bulk-edge correspondence for topological photonic continua

Here, building on our previous work [Phys. Rev. B 92, 125153 (2015)], it is shown that the propagation of unidirectional gapless edge states at an interface of two topologically distinct electromagnetic continua with a well-behaved asymptotic electromagnetic response is rigorously predicted by the bulk-edge correspondence principle. We work out detailed examples demonstrating that when the spatial cutoff of the nonreciprocal part of the material response is considered self-consistently in the solution of the relevant electromagnetic problem, the number of unidirectional gapless edge modes is identical to the difference of the Chern numbers of the bulk materials. Furthermore, it is shown how the role of the spatial cutoff can be imitated in realistic systems using a tiny air gap with a specific thickness. This theory provides a practical roadmap for the application of topological concepts to photonic platforms formed by nonreciprocal electromagnetic continua.
Isolation, screening and molecular identification of biosurfactant producing bacteria from automobile workshops and optimization of parameters for biosurfactant production Biotechnology

Biosurfactants are amphiphilic compounds produced usually within the cell surfaces of microbes or excreted extracellularly. It contains hydrophobic and hydrophilic parts that reduce surface tension and interfacial tension between individual molecules at the surface and interface respectively. The primary aim of the study was to isolate biosurfactant producing organisms from oil contaminated soil. Through primary and secondary screening methods, it was found that the five isolated organisms were capable of producing biosurfactants. Among these, the organism B, which showed the highest biosurfactant production was selected on the basis of emulsification index and oil displacement activity. The biochemical and molecular characterization of the organism B confirmed that the organism is Aeromonas caviae . The 16S rRNA was sequenced using Sanger dideoxy sequencing method inorder o characterize the biosurfuctant producing strain. The new Aeromonas caviae strain, KVMBS1 isolated from oil contaminated site was deposited in National center for Biotechnology Information (NCBI), Gene Bank, USA and accession number is MT322926.1. From the optimization of production parameters, its optimum temperature was found to be 37 o C and the optimum pH was found to be 7. The best carbon and nitrogen source was found to be kerosene and sodium nitrate respectively. The final production using the optimized parameters was done and the biosurfactant was extracted. The dry weight of the biosurfactant was found to be 0.051g. and it was concluded that the biosurfactant produced by Aeromonas caviae is a glycolipid. From the study, the isolated organism, Aeromonas caviae was found to be producing a glycolipid biosurfactant. It can be a promising candidate to be used in several industries.