Miracle-dz/UniFAR-FTUs huggingface dataset:
Temperature-dependent absolute refractive index measurements of synthetic fused silica

Using the Cryogenic, High-Accuracy Refraction Measuring System (CHARMS) at NASA's Goddard Space Flight Center, we have measured the absolute refractive index of five specimens taken from a very large boule of Corning 7980 fused silica from temperatures ranging from 30 to 310 K at wavelengths from 0.4 to 2.6 microns with an absolute uncertainty of ±1 ×10-5. Statistical variations in derived values of the thermo-optic coefficient (dn/dT) are at the ±2 × 10-8/K level. Graphical and tabulated data for absolute refractive index, dispersion, and thermo-optic coefficient are presented for selected wavelengths and temperatures along with estimates of uncertainty in index. Coefficients for temperature-dependent Sellmeier fits of measured refractive index are also presented to allow accurate interpolation of index to other wavelengths and temperatures. We compare our results to those from an independent investigation (which used an interferometric technique for measuring index changes as a function of temperature) whose samples were prepared from the same slugs of material from which our prisms were prepared in support of the Kepler mission. We also compare our results with sparse cryogenic index data from measurements of this material from the literature.
DProvSQL: Privacy Provenance Framework for Differentially Private SQL Engine

Recent years have witnessed the adoption of differential privacy (DP) in practical database query systems. Such systems, like Pri-vateSQL and FLEX, allow data analysts to query sensitive data while providing a rigorous and provable privacy guarantee. However, existing systems may use more privacy budgets than necessary in certain cases where different data analysts with different privilege levels ask a similar or even the same query. In this work, we pro-pose DProvSQL , a fine-grained privacy provenance framework that tracks the privacy loss to each single data analyst and we build algorithms that make use of this framework to maximize the number of queries that could be answered. Preliminary empirical results show that our approach can answer 6x more queries than the baseline approach on average meanwhile the answer from our approach is 1.5x to 5.6x more accurate.
Extending the Hubble diagram by gamma ray bursts

Aims. A new method to constrain the cosmological equation of state is proposed by using combined samples of gamma-ray bursts (GRBs) and supernovae (SNeIa). Methods. The Chevallier-Polarski-Linder parameterization is adopted for the equation of state in order to find a realistic approach to achieve the deceleration/acceleration transition phase of dark energy models. Results. We find that GRBs, calibrated by SNeIa, could be good distance indicators capable of discriminating between cosmological models and ACDM model at high redshift.
The Dark Matter Programme of the Cherenkov Telescope Array

In the last decades a vaste amount of evidence for the existence of dark matter has been accumulated. At the same time, many efforts have been undertaken to try to identify what dark matter is. Indirect searches look at places in the Universe where dark matter is believed to be abundant and seek for possible annihilation or decay signatures. The Cherenkov Telescope Array (CTA) represents the next generation of imaging Cherenkov telescopes and, with one site in the Southern hemisphere and one in the Northern hemisphere, will be able to observe all the sky with unprecedented sensitivity and angular resolution above a few tens of GeV. The CTA Consortium will undertake an ambitious program of indirect dark matter searches for which we report here the brightest prospects.
Mott metal-insulator transition induced by utilizing a glasslike structural ordering in low-dimensional molecular conductors

structural orientations within the crystal structure, namely eclipsed (E) and staggered (S) with the relative orientation of the outer C{C bonds being parallel and canted, respectively. These two conformations are thermally disordered at room temperature and undergo a glass-like ordering transition at Tg 75 K. When cooling through Tg, a small fraction that depends on the cooling rate remains frozen in the S conguration, which is of slightly higher energy, corresponding to a controllable degree of structural disorder. We demonstrate that, when thermally coupled to a low-temperature heat bath, a pulsed heating current through the sample causes a very fast relaxation with cooling rates at Tg of the order of several 1000 K/min. The freezing of the structural degrees of freedom causes a decrease of the electronic bandwidth W with increasing cooling rate, and hence a Mott metal-insulator transition as the system crosses the critical ratio (W=U)c of bandwidth to on-site Coulomb repulsion U. Due to the glassy character of the transition, the eect is persistent below Tg
Domain dynamics in piezoresponse force spectroscopy: Quantitative deconvolution and hysteresis loop fine structure

Domain dynamics in the piezoresponse force spectroscopy (PFS) experiment is studied using the combination of local hysteresis loop acquisition with simultaneous domain imaging. The analytical theory for PFS signal from domain of arbitrary cross section and length is developed for the analysis of experimental data on Pb(Zr,Ti)O3 films. The results suggest formation of oblate domain at early stage of the nucleation and growth, consistent with efficient screening of depolarization field. The fine structure of the hysteresis loop is shown to be related to the observed jumps in domain geometry during domain wall propagation (nanoscale Barkhausen jumps), indicative of strong domain-defect interactions.
Atomic source selection in space-borne gravitational wave detection

Recent proposals for space-borne gravitational wave detectors based on atom interferometry rely on extremely narrow single-photon transition lines as featured by alkaline-earth metals or atomic species with similar electronic configuration. Despite their similarity, these species differ in key parameters such as abundance of isotopes, atomic flux, density and temperature regimes, achievable expansion rates, density limitations set by interactions, as well as technological and operational requirements. In this study, we compare viable candidates for gravitational wave detection with atom interferometry, contrast the most promising atomic species, identify the relevant technological milestones and investigate potential source concepts towards a future gravitational wave detector in space.
Nonlinear statistical effects in relativistic mean field theory

We investigate the relativistic mean field theory of nuclear matter at finite temperature and baryon density taking into account of nonlinear statistical effects, characterized by power-law quantum distributions. The analysis is performed by requiring the Gibbs conditions on the global conservation of baryon number and electric charge fraction. We show that such nonlinear statistical effects play a crucial role in the equation of state and in the formation of mixed phase also for small deviations from the standard Boltzmann-Gibbs statistics.
Outwards migration for planets in stellar irradiated 3D discs

For the very first time we present 3D simulations of planets embedded in stellar irradiated discs. It is well known that thermal effects could reverse the direction of planetary migration from inwards to outwards, potentially saving planets in the inner, optically thick parts of the protoplanetary disc. When considering stellar irradiation in addition to viscous friction as a source of heating, the outer disc changes from a shadowed to a flared structure. Using a suited analytical formula it has been shown that in the flared part of the disc the migration is inwards; planets can migrate outwards only in shadowed regions of the disc, because the radial gradient of entropy is stronger there. In order to confirm this result numerically, we have computed the total torque acting on planets held on fixed orbits embedded in stellar irradiated 3D discs using the hydrodynamical code FARGOCA. We find qualitatively good agreement between the total torque obtained with numerical simulations and the one predicted by the analytical formula. For large masses (>20 M-circle plus) we find quantitative agreement, and we obtain outwards migration regions for planets up to 60 M-circle plus in the early stages of accretional discs. We find nevertheless that the agreement with the analytic formula is quite fortuitous because the formula underestimates the size of the horseshoe region; this error is compensated by imperfect estimates of other terms, most likely the cooling rate and the saturation. (Less)
Morphology-based Query for Galaxy Image Databases

Galaxies of rare morphology are of paramount scientific interest, as they carry important information about the past, present, and future Universe. Once a rare galaxy is identified, studying it more effectively requires a set of galaxies of similar morphology, allowing generalization and statistical analysis that cannot be done when N = 1 . Databases generated by digital sky surveys can contain a very large number of galaxy images, and therefore once a rare galaxy of interest is identified it is possible that more instances of the same morphology are also present in the database. However, when a researcher identifies a certain galaxy of rare morphology in the database, it is virtually impossible to mine the database manually in the search for galaxies of similar morphology. Here we propose a computer method that can automatically search databases of galaxy images and identify galaxies that are morphologically similar to a certain user-defined query galaxy. That is, the researcher provides an image of a galaxy of interest, and the pattern recognition system automatically returns a list of galaxies that are visually similar to the target galaxy. The algorithm uses a comprehensive set of descriptors, allowing it to support different types of galaxies, and it is not limited to a finite set of known morphologies. While the list of returned galaxies is neither clean nor complete, it contains a far higher frequency of galaxies of the morphology of interest, providing a substantial reduction of the data. Such algorithms can be integrated into data management systems of autonomous digital sky surveys such as the Large Synoptic Survey Telescope (LSST), where the number of galaxies in the database is extremely large. The source code of the method is available at http://vfacstaff.ltu. edu/lshamir/downloads/udat.
Observation of charge accumulation and onsite Coulomb repulsion at transition metal impurities in the iron pnictides

We report a combined valence band photoemission and Auger spectroscopy study of single crystalline Ca(Fe,Co)2As2 and Ba(Fe,TM)2As2 with TM=Ni or Cu. The valence band photoemission data show directly that the TM-states move to higher binding energies with increasing atomic number, contributing less and less to the states close to the Fermi level. Furthermore, the 3d8 final state of the LVV Auger decay, which is observed for Ni and Cu, unambiguously reveals the accumulation of charge at these impurities. We also show that the onsite Coulomb interaction on the impurity strongly increases when moving from Co over Ni to Cu. Our results quantify the impurity potentials and imply that the superconducting state is robust against impurity scattering.
Supercriticality to subcriticality in dynamo transitions

Evidence from numerical simulations suggests that the nature of dynamo transition changes from supercritical to subcritical as the magnetic Prandtl number is decreased. To explore this interesting crossover, we first use direct numerical simulations to investigate the hysteresis zone of a subcritical Taylor-Green dynamo. We establish that a well defined boundary exists in this hysteresis region which separates dynamo states from the purely hydrodynamic solution. We then propose simple dynamo models which show similar crossover from supercritical to subcritical dynamo transition as a function of the magnetic Prandtl number. Our models show that the change in the nature of dynamo transition is connected to the stabilizing or de-stabilizing influence of governing non-linearities.
THE COUNTERJET OF HH 30: NEW LIGHT ON ITS BINARY DRIVING SOURCE

We present new [S ii] images of the Herbig–Haro (HH) 30 jet and counterjet observed in 2006, 2007, and 2010 that, combined with previous data, allowed us to measure with improved accuracy the positions and proper motions of the jet and counterjet knots. Our results show that the motion of the knots is essentially ballistic, with the exception of the farthest knots, which trace the large-scale “C”-shape bending of the jet. The observed bending of the jet can be produced by a relative motion of the HH 30 star with respect to its surrounding environment, caused either by a possible proper motion of the HH 30 star, or by the entrainment of environment gas by the red lobe of the nearby L1551-IRS5 outflow. Alternatively, the bending can be produced by the stellar wind from a nearby classical T Tauri star, identified in the Two Micron All Sky Survey catalog as J04314418+181047. The proper motion velocities of the knots of the counterjet show more variations than those of the jet. In particular, we identify two knots of the counterjet that have the same kinematic age but whose velocities differ by almost a factor of two. Thus, it appears from our observations that counterjet knots launched simultaneously can be ejected with very different velocities. We confirm that the observed wiggling of the jet and counterjet arises from the orbital motion of the jet source in a binary system. Precession, if present at all, is of secondary importance in shaping the jet. We derive an orbital period of τo = 114 ± 2 yr and a mass function of mμ3c = 0.014 ± 0.006 M☉. For a mass of the system of m = 0.45 ± 0.04 M☉ (the value inferred from observations of the CO kinematics of the disk), we obtain a mass of mj = 0.31 ± 0.04 M☉ for the jet source, a mass of mc = 0.14 ± 0.03 M☉ for the companion, and a binary separation of a = 18.0 ± 0.6 AU. This binary separation coincides with the value required to account for the size of the inner hole observed in the disk, which has been attributed to tidal truncation in a binary system.
THE MASS PROFILE OF THE GALAXY TO 80 kpc

The Hypervelocity Star Survey presents the currently largest sample of radial velocity measurements of halo stars out to 80 kpc. We apply spherical Jeans modeling to these data in order to derive the mass profile of the Galaxy. We restrict the analysis to distances larger than 25 kpc from the Galactic center, where the density profile of halo stars is well approximated by a single power law with logarithmic slope between −3.5 and −4.5. With this restriction, we also avoid the complication of modeling a flattened Galactic disk. In the range 25 kpc < r < 80 kpc, the radial velocity dispersion declines remarkably little; a robust measure of its logarithmic slope is between −0.05 and −0.1. The circular velocity profile also declines remarkably little with radius. The allowed range of Vc(80 kpc) lies between 175 and 231 km s−1, with the most likely value of 193 km s−1. Compared with the value at the solar location, the Galactic circular velocity declines by less than 20% over an order of magnitude in radius. Such a flat profile requires a massive and extended dark matter halo. The mass enclosed within 80 kpc is 6.9+3.0−1.2 × 1011 M☉. Our sample of radial velocities is large enough that the biggest uncertainty in the mass is not statistical but systematic, dominated by the density slope and anisotropy of the tracer population. Further progress requires modeling observed data sets within realistic simulations of galaxy formation.
Beta function and anomalous dimensions

We demonstrate that it is possible to determine the coefficients of an all-orders beta-function linear in the anomalous dimensions using as data the 2-loop coefficients together with the first one of the anomalous dimensions which are universal. The beta function allows us to determine the anomalous dimension of the fermion masses at the infrared fixed point, and the resulting values compare well with the lattice determinations.
Unification of inflation and dark energy à la quintessential inflation

This pedagogical review is devoted to quintessential inflation, which refers to unification of inflation and dark energy using a single scalar field. We present a brief but concise description of the concepts needed to join the two ends, which include discussion on scalar field dynamic, conformal coupling, instant preheating and relic gravitational waves. Models of quintessential inflation broadly fall into two classes, depending upon the early and late time behavior of the field potential. In the first type we include models in which the field potential is steep for most of the history of the universe but turn shallow at late times, whereas in the second type the potential is shallow at early times followed by a steep behavior thereafter. In models of the first category inflation can be realized by invoking high-energy brane-induced damping, which is needed to facilitate slow roll along a steep potential. In models of second type one may invoke a nonminimal coupling of the scalar field with massive neutrino matter, which might induce a minimum in the potential at late times as neutrinos turn nonrelativistic. In this category we review a class of models with noncanonical kinetic term in the Lagrangian, which can comply with recent B mode polarization measurements. The scenario under consideration is distinguished by the presence of a kinetic phase, which precedes the radiative regime, giving rise to blue spectrum of gravity waves generated during inflation. We highlight the generic features of quintessential inflation and also discuss on issues related to Lyth bound.
Doubly charged Higgsinos at the Tevatron

Several supersymmetric models with extended gauge structures, motivated by either grand unification or by neutrino mass generation, predict light doubly charged Higgsinos. In this work we study the signals of doubly charged Higgsinos at the Tevatron in both pair- and single-production modes, and show that it is possible, especially from the events containing same-sign same-flavor isolated leptons, to disentangle the effects of doubly charged Higgsinos in the Tevatron data.
Solving QED$_3$ with Conformal Bootstrap

We study the conformal bootstrap for $3D$ Quantum Electrodynamic (QED$_3$) coupled to $N_f$ flavors of two-component Dirac fermions $\Psi_i$. We bootstrap four point correlator of fermion bilinear operator, which forms an adjoint representation of the flavor symmetry $SU(N_f)$. We obtain rigorous upper bounds on the scaling dimensions of the parity even $SU(N_f)$ singlets, i.e., the fermion quadrilinear operators. We find strong evidence that the IR fixed points of standard QED$_3$ and QED$_3$-Gross-Neveu model saturate the bound with large $N_f$. The two kinks merge near $N_f=3$ and disappear for $N_f\leq2$. The $SU(N_f)$ singlets related to these kinks are irrelevant. Our results support the "merger and annihilation of fixed points" scenario. Besides, it provides a solution to the long-standing problem of the critical flavor symmetry of QED$_3$: $N_{\mathrm{crit}}=2$. Our results shed lights on several interesting problems, including high-temperature superconducting, N\'eel-Valence Bond Solid quantum phase transition and the duality web of $3D$ theories.
Predictors of Complex PTSD: The Role of Trauma Characteristics, Dissociation, and Comorbid Psychopathology

Background Complex Posttraumatic Stress Disorder (CPTSD) has previously been associated with earlier trauma onset, repeated interpersonal traumatization, more dissociation and more comorbid psychopathology. However, it is still debated if the afore-mentioned risk factors are related to CPTSD diagnosis or rather indicative of a more severe form of post-traumatic distress. The aim of this study was to compare patients with a CPTSD diagnosis to those with PTSD in trauma characteristics (onset, chronicity, interpersonal nature), dissociation, and psychiatric comorbidities, while accounting for symptom severity.
CNN and diffusion MRI’s 4th degree rotational invariants for Alzheimer’s disease identification

Recently, a general analytical formula to extract all the Rotation Invariant Features (RIFs) of the diﬀusion Magnetic Resonance Imaging (dMRI) signal was proposed. The features extracted using this formula represent a generalisation of the usual second degree RIFs such as the mean diﬀusivity. In this work, we study the usefulness of all the 12 algebraically independent RIFs extracted from 4th degree spherical harmonics that model the dMRI signal per voxel in the context of Alzheimer Disease (AD) identiﬁcation. To do so, and since we are working with imbalanced data sets, we ﬁrst introduce a non-linear metric to evaluate the performance of the models, the ( B-score ). This proposed metric allows high score only when both classes are distinguished correctly. We use the proposed metric in conjunction with a deep Convolutional Neural Network that operates on subject slices to identify if a subject has AD or not. We ﬁnd that micro-structure information communicated by RIFs is indeed useful to AD identiﬁcation and that not all RIFs are equivalently useful. We also identify the two best RIF combinations for the ADNI - SIEMENS and the ADNI - GE medical data sets respectively. The combination of these RIFs achieves a classiﬁcation B-score of 73.62% and 72.31% on the previous data sets respectively. We note the importance of combining high degree RIFs with low degree ones to improve the classiﬁcation performance.
The Dust Budget of the SMC: Are AGB Stars the Primary Dust Source at Low Metallicity?

We estimate the total dust input from the cool evolved stars in the Small Magellanic Cloud (SMC), using the 8 micron excess emission as a proxy for the dust-production rate. We find that Asymptotic Giant Branch (AGB) and red supergiant (RSG) stars produce (8.6-9.5) x 10^7 solar masses per year of dust, depending on the fraction of far-infrared sources that belong to the evolved star population (with 10%-50% uncertainty in individual dust-production rates). RSGs contribute the least (<4%), while carbon-rich AGB stars (especially the so-called "extreme" AGB stars) account for 87%-89% of the total dust input from cool evolved stars. We also estimate the dust input from hot stars and supernovae (SNe), and find that if SNe produce 10^-3 solar masses of dust each, then the total SN dust input and AGB input are roughly equivalent. We consider several scenarios of SNe dust production and destruction and find that the interstellar medium (ISM) dust can be accounted for solely by stellar sources if all SNe produce dust in the quantities seen around the dustiest examples and if most SNe explode in dense regions where much of the ISM dust is shielded from the shocks. We find that AGB stars contribute only 2.1% of the ISM dust. Without a net positive contribution from SNe to the dust budget, this suggests that dust must grow in the ISM or be formed by another unknown mechanism.