Miracle-dz/UniFAR-FTUs huggingface dataset:
Lensing Constraints on the Mass Profile Shape and the Splashback Radius of Galaxy Clusters

The lensing signal around galaxy clusters can, in principle, be used to test detailed predictions for their average mass profile from numerical simulations. However, the intrinsic shape of the profiles can be smeared out when a sample that spans a wide range of cluster masses is averaged in physical length units. This effect especially conceals rapid changes in gradient such as the steep drop associated with the splashback radius, a sharp edge corresponding to the outermost caustic in accreting halos. We optimize the extraction of such local features by scaling individual halo profiles to a number of spherical overdensity radii, and apply this method to 16 X-ray-selected, high-mass clusters targeted in the Cluster Lensing And Supernova survey with Hubble. By forward-modeling the weak- and strong-lensing data presented by Umetsu et al., we show that, regardless of the scaling overdensity, the projected ensemble density profile is remarkably well described by a Navarro–Frenk–White (NFW) or Einasto profile out to R ∼ 2.5 h − 1 Mpc , beyond which the profiles flatten. We constrain the NFW concentration to c 200 c = 3.66 ± 0.11 at M 200 c ≃ 1.0 × 10 15 h − 1 M ⊙ , consistent with and improved from previous work that used conventionally stacked lensing profiles, and in excellent agreement with theoretical expectations. Assuming the profile form of Diemer & Kravtsov and generic priors calibrated from numerical simulations, we place a lower limit on the splashback radius of the cluster halos, if it exists, of R sp 3 D / r 200 m > 0.89 ( R sp 3 D > 1.83 h − 1 Mpc ) at 68% confidence. The corresponding density feature is most pronounced when the cluster profiles are scaled by r 200 m , and smeared out when scaled to higher overdensities.
Predicting Reappraisal Success with Innate Neural Connectivity Across the Adult Lifespan

Predicting Reappraisal Success with Innate Neural Connectivity Across the Adult Lifespan September 2022 Parker Longwell, BA. , Whittier College MS, University of Massachusetts, Amherst Directed by: Dr. Rebecca Ready Reappraisal — reinterpreting a situation to change emotional response — is an effective emotion regulation strategy that relies on cognitive control network activity, including engagement of the dorsolateral prefrontal cortex (dlPFC), to attenuate amygdala activity. Greater dlPFC-Amygdala functional connectivity predicts instructed reappraisal task success, and daily use of reappraisal for younger adults (Pico-Perez et al., 2018) but not older adults (Opitz et al., 2012), while the connectivity of the vmPFC is predictive of physiological markers of ER success for all ages (Sakaki et al., 2016 & Urry et al., 2006). However, the relationship between Resting-State Functional Connectivity (RSFC) and reappraisal task success across the lifespan has yet to be investigated. Participants in the Cambridge Center for Aging Neuroscience study (N=299) completed an 8-minute resting-state fMRI scan. In each trial of an emotion regulation task, participants either viewed or reappraised a negative film and reported post-regulation positive affect. RSFC across bilateral amygdala and the mPFC, the left and the right dlPFC were calculated with Matlab’s CONN Toolbox. The hypothesis is that the strength of the amygdala-mPFC RSFC will predict lower negative and higher positive affect scores after reappraising, however, this study data failed to find evidence to support this hypothesis. The
Semi-Minimal Pruned Hedge: A Potential Climate Change Adaptation Strategy in Viticulture

The low-input viticultural training system ‘Semi-minimal pruned hedge’ (SMPH) is progressively being more widely applied in the Central European grapegrowing regions. The present study examined the influence of (i) the training system (SMPH versus the vertical shoot position (VSP) system), (ii) the timing of shoot topping in SMPH, and (iii) the effects of mechanical thinning in SMPH on the bunch rot epidemic, grape maturity, and yield. Six-year field trials on Pinot blanc in Luxembourg demonstrated that yield levels in non-thinned SMPH treatments were 74% higher, and total soluble solids (TSS) at harvest 2.2 brix lower than in VSP. Non-thinned SMPH delayed the bunch rot epidemic and the maturity progress by 18 and 11 days compared to VSP, respectively. Different shoot-topping timings in SMPH did not affect the tested parameters. Mechanical thinning regimes reduced the yield by 28% (moderate thinning) and 53% (severe thinning) compared to non-thinned SMPH and increased TSS by 0.8 and 1.3 brix, respectively. Delayed bunch rot epidemic and maturity progress give rise to the opportunity for a longer maturity period in cooler conditions, making this system of particular interest in future, warmer climatic conditions. Providing that yield levels are managed properly, SMPH might represent an interesting climate change adaptation strategy.
Galactic habitable zone around M and FGK stars with chemical evolution models that include dust

The Galactic habitable zone is defined as the region with highly enough metallicity to form planetary systems in which Earth-like planets could be born and might be capable of sustaining life surviving to the destructive effects of nearby supernova explosion events. Galactic chemical evolution models can be useful tools for studying the galactic habitable zones in different systems. Our aim here is to find the Galactic habitable zone using chemical evolution models for the Milky Way disc, adopting the most recent prescriptions for the evolution of dust and for the probability of finding planetary systems around M and FGK stars. Moreover, for the first time, we will express those probabilities in terms of the dust-to-gas ratio of the ISM in the solar neighborhood as computed by detailed chemical evolution models. At a fixed Galactic time and Galactocentric distance we determine the number of M and FGK stars having Earths (but no gas giant planets) which survived supernova explosions, using the formalism of our Paper I. The probabilities of finding terrestrial planets but not gas giant planets around M stars deviate substantially from the ones around FGK stars for supersolar values of [Fe/H]. For both FGK and M stars the maximum number of stars hosting habitable planets is at 8 kpc from the Galactic Centre, if destructive effects by supernova explosions are taken into account. At the present time the total number of M stars with habitable planets are $\simeq$ 10 times the number of FGK stars. Moreover, we provide a sixth order polynomial fit (and a linear one but more approximated) for the relation found with chemical evolution models in the solar neighborhood between the [Fe/H] abundances and the dust-to-gas ratio.
Evaluation of Rapeseed-mustard Genotypes and Their Genetic Variabilities in Different Sowing Dates

Rapeseed-mustard is an important oilseed species with high nutritional and economic values, and it’s popularity increases due to its diverse uses. Ten genotypes of rapeseed-mustard and two sowing dates were evaluated in a split plot design with three replications. Our study demonstrated that sowing dates and genotypes greatly influenced the growth parameters, yield, and it contributing characters. BARI sarisha-16 had the highest yield (1613 kg.ha -1 ) whereas Binasarisha-9 yielded the lowest yield (840 kg.ha -1 ). All the yield contributing characters was superior in the earlier (10 November, S 1 ) sowing date than the 24 November (S 2 ), demonstrated by the highest grain yield (1120 kg.ha -1 ) which was 10 % higher than the seed sown on 24th November (S 2 ) (1025 kg.ha -1 ), and better higher vegetative growth. These results affirmed that the yield contributing traits resulted the higher seed yield. In most of the studied characters, the higher phenotypic variances were observed than that of its genotypic variances. The significant positive correlation with grain yield were found in plant height, number of primary branches/ plants, number of siliqua/plants, siliquae length, number of seed per siliquae, days of 50% flowering to maturity and 1000 seed weight. Therefore, based on the yield and the related traits, BARI sarisha-16 can be used for further utilization.
A note on Spontaneous Symmetry Breaking in flocks of birds

It is suggested that the observed scale-free correlations of speed fluctuations in flocks of birds are a consequence of the spontaneous breakdown of translational symmetry to a discrete group, and not an indication that the system is near a critical point in phase space. The observed long-range correlation length could then be attributed to the presence of a phonon mode in the flock.
Second Thoughts are Best: Learning to Re-Align With Human Values from Text Edits

We present Second Thought, a new learning paradigm that enables language models (LMs) to re-align with human values. By modeling the chain-of-edits between value-unaligned and value-aligned text, with LM fine-tuning and additional refinement through reinforcement learning, Second Thought not only achieves superior performance in three value alignment benchmark datasets but also shows strong human-value transfer learning ability in few-shot scenarios. The generated editing steps also offer better interpretability and ease for interactive error correction. Extensive human evaluations further confirm its effectiveness.
Identification of Phosphate Sorption-Desorption and Accumulation Characteristics to Reduce Environmental Consequences

ABSTRACT Phosphorus (P) enrichment of soil due to the intensification of P fertilizer usage in crop production has resulted in eutrophication and serious economic consequences. Further, rapidly decreasing P reserves have renewed interest in improving more sustainable soil P management through monitoring diverse soil P reactions in contrasting soils. Therefore, the study was conducted to (i) characterize P sorption and desorption capacities related to soil properties and (ii) determine the added P availability and distribution among the different pools of P over the period concerning P sorption capacity of the soils. Three soils, namely Ultisols, Entisols, and Inceptisols, were equilibrated with a series of P concentrations to study P sorption–desorption using Langmuir isotherms. These soils were subjected to a sequential extraction procedure to study fractions in different pools after incubating with added P for 120 days. Maximum P sorption for Ultisols, Entisols, and Inceptisols were 1,428.6, 1,666.7, and 3,333.3 mg kg−1 soil, respectively. Phosphorus desorption by Ultisol was about 1.7- and 4.2-fold higher than Entisols and Inceptisols. The maximum P sorption showed a negative and significant correlation with soil pH (r = −0.88), whereas P des % has a significant and positive correlation (r = 0.98). Exchangeable Al, Al-ox, Al-cD, and Fe-ox showed a significant positive correlation with maximum P sorption and a negative correlation with P des %. During incubation, 93.3% of added P became non-extractable in Inceptisols, and in contrast only 64.3% for Ultisols. A greater increase in labile NaHCO3-P fraction was found in Ultisols from 66.96 to 135.6 mg/kg at the end of the incubation. Accordingly, the soils with lower sorption capacity consist of more labile P pools, which indicates a higher risk of the loss of P from the soil.
Observational consequences of optical band milliarcsec-scale structure in active galactic nuclei discovered by Gaia

We interpret the recent discovery of a preferable VLBI/Gaia offset direction for radio-loud active galactic nuclei (AGNs) along the parsec-scale radio jets as a manifestation of their optical structure on scales of 1 to 100 milliarcseconds. The extended jet structure affects the Gaia position stronger than the VLBI position due to the difference in observing techniques. Gaia detects total power while VLBI measures the correlated quantity, visibility, and therefore, sensitive to compact structures. The synergy of VLBI that is sensitive to the position of the most compact source component, usually associated with the opaque radio core, and Gaia that is sensitive to the centroid of optical emission, opens a window of opportunity to study optical jets at milliarcsecond resolution, two orders of magnitude finer than the resolution of most existing optical instruments. We demonstrate that strong variability of optical jets is able to cause a jitter comparable to the VLBI/Gaia offsets at a quiet state, i.e. several milliarcseconds. We show that the VLBI/Gaia position jitter correlation with the AGN optical light curve may help to locate the region where the flare occurred, estimate its distance from the super-massive black hole and the ratio of the flux density in the flaring region to the total flux density.
Novel Pullulan/Gellan Gum Bilayer Film as a Vehicle for Silibinin-Loaded Nanocapsules in the Topical Treatment of Atopic Dermatitis

In this study a novel gellan gum/pullulan bilayer film containing silibinin-loaded nanocapsules was developed for topical treatment of atopic dermatitis (AD). The bilayer films were produced by applying a pullulan layer on a gellan gum layer incorporated with silibinin nanocapsules by two-step solvent casting method. The bilayer formation was confirmed by microscopic analysis. In vitro studies showed that pullulan imparts bioadhesitvity for the films and the presence of nanocapsules increased their occlusion factor almost 2-fold. Besides, the nano-based film presented a slow silibinin release and high affinity for cutaneous tissue. Moreover, this film presented high scavenger capacity and non-hemolytic property. In the in vivo study, interestingly, the treatments with vehicle film attenuated the scratching behavior and the ear edema in mice induced by 2,4-dinitrochlorobenzene (DNCB). However, the nano-based film containing silibinin modulated the inflammatory and oxidative parameters in a similar or more pronounced way than silibinin solution and vehicle film, as well as than hydrocortisone, a classical treatment of AD. In conclusion, these data suggest that itself gellan gum/pullulan bilayer film might attenuate the effects induced by DNCB, acting together with silibinin-loaded nanocapsules, which protected the skin from oxidative damage, improving the therapeutic effect in this AD-model.
Third Trimester Fetuses Demonstrate Priming, a Form of Implicit Memory, In Utero

Research examinations of changes in fetal heart rate (HR) to operationalize fetal memory suggests that human memory capacities emerge in utero. However, there is little evidence for a form of implicit memory or priming. The present aim was to determine if priming is evident in utero. Fetal HR, maternal HR and maternal respiratory rate (RR) were examined in 105 women during the third trimester of pregnancy. Women experienced two counterbalanced laboratory tasks, the Stroop task and the paced breathing task, and their cardiorespiratory activity functioned as a stimulus for fetuses. Repeated measures ANOVAs revealed maternal HR increased during the Stroop task but only when the Stroop task was presented first (89.64 bpm to 92.39 bpm) (p = 0.04). Maternal RR increased during the Stroop task, regardless of task order (17.72 bpm to 21.11 bpm; 18.50 bpm to 22.60 bpm) (p < 0.01). Fetal HR increased during the paced breathing task, but only when it followed maternal exposure to the Stroop task (141.13 bpm to 143.97 bpm) (p < 0.01). Fetuses registered maternal HR and RR reactivity to the Stroop task, which influenced their response during maternal engagement with a related task, suggesting priming. Further study of fetal memory may suggest another pathway by which prenatal exposures impact future development.
Lyα emitters in a cosmological volume – I. The impact of radiative transfer

Lyman-α emitters (LAEs) are a promising target to probe the large scale structure of the Universe at high redshifts, z ≳ 2. However, their detection is sensitive to radiative transfer effects that depend on local astrophysical conditions. Thus, modeling the bulk properties of this galaxy population remains challenging for theoretical models. Here we develop a physically-motivated scheme to predict LAEs in cosmological simulations. The escape of Lyα photons is computed using a Monte Carlo radiative transfer code which outputs a Lyα escape fraction. To speed-up the process of assigning escape fractions to individual galaxies, we employ fitting formulae that approximate the full Monte Carlo results within an accuracy of 10% for a broad range of column densities, gas metallicities and gas bulk velocities. We apply our methodology to the semi-analytical model GALFORM on a large N-body simulation. The Lyα photons escape through an outflowing neutral gas medium, implemented assuming different geometries. This results in different predictions for the typical column density and outflow velocities of the LAE population. To understand the impact of radiative transfer on our predictions, we contrast our models against a simple abundance matching assignment. Our full models populate LAEs in less massive haloes than what is obtained with abundance matching. Overall, radiative transfer effects result in better agreement when confronting the properties of LAEs against observational measurements. This suggest that incorporating the effects of Lyα radiative transfer in the analysis of this galaxy population, including their clustering, can be important for obtaining an unbiased interpretation of future datasets.
Minimal left-right symmetric intersecting D-brane model

We investigate left-right symmetric extensions of the standard model based on open strings ending on D-branes, with gauge bosons due to strings attached to stacks of D-branes and chiral matter due to strings stretching between intersecting D-branes. The left-handed and right-handed fermions transform as doublets under Sp(1)(L) and Sp(1)(R), and so their masses must be generated by the introduction of Higgs fields in a bifundamental (2,2) representation under the two Sp(1) gauge groups. For such D-brane configurations the left-right symmetry must be broken by Higgs fields in the doublet representation of Sp(1)(R) and therefore Majorana mass terms are suppressed by some higher physics scale. The left-handed and right-handed neutrinos pair up to form Dirac fermions which control the decay widths of the right-handed W' boson to yield comparable branching fractions into dilepton and dijet channels. Using the most recent searches at LHC13 Run II with 2016 data we constrain the (g(R), m(W)')parameter space. Our analysis indicates that independent of the coupling strength g(R), gauge bosons with masses m(W)' greater than or similar to 3.5 TeV are not ruled out. As the LHC is just beginning to probe the TeV scale, significant room for W' discovery remains.
Partially Directed Search for Prices ∗

I analyse a model of partially directed search where buyers decide which firm to visit based on correct, but incomplete, information about firms’ prices. I show that the unique symmetric pure-strategy equilibrium is in price distributions. A firm’s equilibrium price distribution assigns positive mass to prices below the marginal cost (“deals”). If some buyers are “shoppers” (i.e., better at searching than the others), then a larger fraction of shoppers can make the best deals worse. This effect can be so large that the welfare of nonshoppers is reduced. JEL codes: D43, D83, L13
ROLE OF EJECTA CLUMPING AND BACK-REACTION OF ACCELERATED COSMIC RAYS IN THE EVOLUTION OF TYPE Ia SUPERNOVA REMNANTS

We investigate the role played by initial clumping of ejecta and by efficient acceleration of cosmic rays (CRs) in determining the density structure of the post-shock region of a Type Ia supernova remnant (SNR) through detailed three-dimensional MHD modeling. Our model describes the expansion of an SNR through a magnetized interstellar medium, including the initial clumping of ejecta and the effects on shock dynamics due to back-reaction of accelerated CRs. The model predictions are compared to the observations of SN 1006. We found that the back-reaction of accelerated CRs alone cannot reproduce the observed separation between the forward shock and the contact discontinuity unless the energy losses through CR acceleration and escape are very large and independent of the obliquity angle. On the contrary, the clumping of ejecta can naturally reproduce the observed small separation and the occurrence of protrusions observed in SN 1006, even without the need of accelerated CRs. We conclude that forward shock–contact discontinuity separation is a probe of the ejecta structure at the time of explosion rather than a probe of the efficiency of CR acceleration in young SNRs.
Evolution of Spin, Orbital, and Superorbital Modulations of 4U 0114+650

We report a systematic analysis of the spin, orbital, and superorbital modulations of 4U 0114+650, a high-mass X-ray binary that consists of one of the slowest spinning neutron stars. Using the dynamic power spectrum, we found that the spin period varied dramatically and is anticorrelated with the long-term X-ray flux variation that can be observed using the Rossi X-ray Timing Explorer ASM, Swift BAT, and the Monitor of All-sky X-ray Image. The spin-up rate over the entire data set is consistent with previously reported values; however, the local spin-up rate is considerably higher. The corresponding local spin-up timescale is comparable to the local spin-up rate of OAO 1657−415, indicating that 4U 0114+650 could also have a transient disk. Moreover, the spin period evolution shows two ∼1000-day spin-down/random-walk epochs that appeared together with depressions of the superorbital modulation amplitude. This implies that the superorbital modulation was closely related to the presence of the accretion disk, which is not favored in the spin-down/random-walk epochs because the accretion is dominated by the direct wind accretion. The orbital period is stable during the entire time span; however, the orbital profile significantly changes with time. We found that the depth of the dip near the inferior conjunction of the companion is highly variable, which disfavors the eclipsing scenario. Moreover, the dip was less obvious during the spin-down/random-walk epochs, indicating its correlation with the accretion disk. Further monitoring in both X-ray and optical bands could reveal the establishment of the accretion disk in this system.
PREDICTION OF FORBIDDEN ULTRAVIOLET AND VISIBLE EMISSIONS IN COMET 67P/CHURYUMOV–GERASIMENKO

Remote observation of spectroscopic emissions is a potential tool for the identification and quantification of various species in comets. The CO Cameron band (to trace CO2) and atomic oxygen emissions (to trace H2O and/or CO2, CO) have been used to probe neutral composition in the cometary coma. Using a coupled-chemistry-emission model, various excitation processes controlling the CO Cameron band and different atomic oxygen and atomic carbon emissions have been modeled in comet 67P/Churyumov–Gerasimenko at 1.29 AU (perihelion) and at 3 AU heliocentric distances, which is being explored by ESA's Rosetta mission. The intensities of the CO Cameron band, atomic oxygen, and atomic carbon emission lines as a function of projected distance are calculated for different CO and CO2 volume mixing ratios relative to water. Contributions of different excitation processes controlling these emissions are quantified. We assess how CO2 and/or CO volume mixing ratios with respect to H2O can be derived based on the observed intensities of the CO Cameron band, atomic oxygen, and atomic carbon emission lines. The results presented in this work serve as baseline calculations to understand the behavior of low out-gassing cometary coma and compare them with the higher gas production rate cases (e.g., comet Halley). Quantitative analysis of different excitation processes governing the spectroscopic emissions is essential to study the chemistry of inner coma and to derive neutral gas composition.