Miracle-dz/UniFAR-FTUs huggingface dataset:
Observational constraints on new exact inflationary scalar-field solutions

An algorithm is used to generate new solutions of the scalar-field equations in homogeneous and isotropic universes. Solutions can be found for pure scalar fields with various potentials in the absence and presence of spatial curvature and other perfect fluids. A series of generalizations of the Chaplygin gas and bulk viscous cosmological solutions for inflationary universes are found. Furthermore other closed-form solutions which provide inflationary universes are presented. We also show how the Hubble slow-roll parameters can be calculated using the solution algorithm and we compare these inflationary solutions with the observational data provided by the Planck 2015 collaboration in order to constrain and rule out some of these models.
Modeling and Estimation of High-dimensional Vector Autoregressions.

Modeling and Estimation of High-dimensional Vector Autoregressions by Sumanta Basu Chair: George Michailidis Vector Autoregression (VAR) represents a popular class of time series models in applied macroeconomics and finance, widely used for structural analysis and simultaneous forecasting of a number of temporally observed variables. Over the years it has gained popularity in the fields of control theory, statistics, economics, finance, genetics and neuroscience. In addition to the “curse of dimensionality” introduced by a quadratically growing dimension of the parameter space, VAR estimation poses considerable challenges due to the temporal and cross-sectional dependence in the data. In the first part of this thesis, we discuss modeling and estimation of highdimensional VAR from short panels of time series, with applications to reconstruction of gene regulatory network from time course gene expression data. We investigate adaptively thresholded lasso regularized estimation of VAR models and propose a thesholded group lasso regularization framework to incorporate a priori available pathway information in the model. The properties of the proposed methods are assessed both theoretically and via numerical experiments. The study is illustrated on
Ultra-lightweight hybrid woven fabric containing stainless steel/polyester composite yarn for total EMI shielding in frequency range 8–18 GHz

This article describes the preparation of composite conductive yarn from stainless steel and polyester staple fibre with different fibre composition adopting worsted spinning system. The conducting yarn was successfully woven into variety of hybrid woven structures in the Picanol Gammax Rapier Loom. The aim of this research was to develop conducting yarn of different conductivity level (linear resistance 6–9 kΩ/m to 150–200 Ω/m) and subsequent conversion of yarn into ultra-lightweight woven fabric (~100 gsm) for providing electro-magnetic interference/radio frequency interference shielding effectiveness to the electronic equipment/devices. The electromagnetic shielding effectiveness of these woven fabrics was evaluated in free space microwave measurement system in microwave frequency (8–18 GHz) for vertical and horizontal polarization of electromagnetic wave. EMSE of ~31 dB in single layer of fabric is achieved. The effect of various fabric parameters, i.e. yarn spacing, yarn density and weave structure, on behaviour of electromagnetic wave has also been studied.
Variability of GeV gamma-ray emission in QSO B0218+357 due to microlensing on intermediate size structures

Strong gravitational lensing leads to an occurrence of multiple images, with different magnifications, of a lensed source. Those magnifications can in turn be modified by microlensing on smaller mass scales within the lens. Recently, measurements of the changes in the magnification ratio of the individual images have been proposed as a powerful tool for estimation of the size and velocity of the emission region in the lensed source. The changes of the magnification ratios in blazars PKS1830-211 and QSO B0218+357, if interpreted as caused by a microlensing on individual stars, put strong constraints on those two variables. These constraints are difficult to accommodate with the current models of gamma-ray emission in blazars. In this paper we study if similar changes in the magnification ratio can be caused by microlensing on intermediate size structures in the lensing galaxy. We investigate in details three classes of possible lenses: globular clusters (GC), open clusters (OC) and giant molecular clouds (GMC). We apply this scenario to the case of QSO B0218+357. Our numerical simulations show that changes in magnifi- cations with similar time scales can be obtained for relativistically moving emission regions with sizes up to 0.01 pc in the case of microlensing on the cores of GCs or clumps in GMCs. From the density of such structures in spiral galaxies we estimate however that lensing in giant molecular clouds would be more common.
List of Abbreviations and Symbols

ABA Abscisic acid ACC 1-aminocyclopropane-I-carboxylate ANOVA Analysis of variance Al Aluminum BNF Biological nitrogen fixation BSA Bovine serum albumin BLAST Basic local alignment search tool C Carbon °C Degree centigrade Ca Calcium CAS Chrome azurol S Chi Chlorophyll cfu Colony forming unit cm Centimeter Cd Cadmium Cu Copper Cr Chromium Cr(VI) Hexavalent chromium Cr(111) Trivalent chromium DAS Days after sowing DAE Days after emergence DI-IBA 2, 3-Dihydroxy benzoic acid df Degree of freedom DNA Deoxyribo nucleic acid EPS Exopolysaccharides EDX Energy dispersive X-ray EMBL European molecular biology laboratory FTIR Fourier transform infrared spectroscopy Fig. Figure Fe Iron g Gram GR Glutathione reductase
Stabilities of Parallel Flow and Horizontal Convection

In the first part, the stability of two-dimensional parallel flow is discussed. A more restrictively general stability criterion for inviscid parallel flow is obtained analytically. In the second part, we report the numerical simulations of the partial-penetrating flow in horizontal convection within a squire cavity tank at high Rayleigh numbers $10^7<Ra<10^{10}$. The fast estab but slowly steadied flow is simulated, where a shallow and closed circulation cell is obtained numerically as partial-penetrating flow for the first time, which is consistent with the experiment.
A probabilistic representation for the vorticity of a 3D viscous fluid and for general systems of parabolic equations

A probabilistic representation formula for general systems of linear parabolic equations, coupled only through the zero-order term, is given. On this basis, an implicit probabilistic representation for the vorticity in a 3D viscous fluid (described by the Navier-Stokes equations) is carefully analysed, and a theorem of local existence and uniqueness is proved.
Detecting metrologically useful asymmetry and entanglement by a few local measurements

Important properties of a quantum system are not directly measurable, but they can be disclosed by how fast the system changes under controlled perturbations. In particular, asymmetry and entanglement can be verified by reconstructing the state of a quantum system. Yet, this usually requires experimental and computational resources which increase exponentially with the system size. Here we show how to detect metrologically useful asymmetry and entanglement by a limited number of measurements. This is achieved by studying how they affect the speed of evolution of a system under a unitary transformation. We show that the speed of multiqubit systems can be evaluated by measuring a set of local observables, providing exponential advantage with respect to state tomography. Indeed, the presented method requires neither the knowledge of the state and the parameter-encoding Hamiltonian nor global measurements performed on all the constituent subsystems. We implement the detection scheme in an all-optical experiment.
Enhancement of nonvolatile polarization and pyroelectric sensitivity in lithium tantalate (LT)/poly(vinylidene fluoride) (PVDF) nanocomposite

We report the ferroelectric and pyroelectric properties of the composite films of lithium tantalate (LT) nanoparticle in poly(vinylidene fluoride) PVDF matrix at different volume fractions of LT (fLT = 0.047, 0.09 and 0.17). For an applied electric field of 150 kV cm−1 the nonvolatile polarization of the composite was observed to increase from 0.014 µC cm−2 at fLT = 0 to 2.06 µC cm−2 at fLT = 0.17. For fLT = 0.17, the composite films exhibit a saturated ferroelectric hysteresis loop with a remanent polarization (2Pr = 4.13 µC cm−2). Compared with pure poled PVDF the composite films also showed a factor of about five enhancement in the pyroelectric coefficient at fLT = 0.17. When used in energy detection mode the pyroelectric voltage sensitivity of the composite films was found to increase from 3.93 to 18.5 V J−1 with an increase in fLT from 0.0 to 0.17.
GraphDiffs: Graph Modeling with Differential Sequence for Document-Grounded Conversation

Knowledge grounded dialogue systems need to 001 incorporate natural transitions between knowl-002 edge for dialogue to flow smoothly. Current 003 systems not only lack good structured rep-004 resentations for knowledge that span multi-005 ple documents, but also effective algorithms 006 that utilize such resources. We design a 007 Co-Referential Multi-Document Graph(CoRM-008 DoG) that seamlessly captures inter-document 009 correlations and intra-document co-referential 010 knowledge relations. To best linearise this 011 static graph into sequential dialogues, we con-012 tribute a Graph Modeling with Differential Se-013 quence (GraphDiffs) method for knowledge 014 transitions in dialogue. GraphDiffs performs 015 knowledge selection by natively accounting for 016 contextual graph structure and introducing dif-017 ferential sequence learning to effectively learn 018 multi-turn knowledge transitions. Our analysis 019 shows that GraphDiffs based on CoRM-DoG 020 significantly outperforms the current state-of-021 the-art by 9 . 5 % and 7 . 4 % on two public bench-022 marks, WoW and Holle-E, where the modeling 023 of co-reference and differential sequence are 024 critical factors for its success. 025
THE SLOAN DIGITAL SKY SURVEY QUASAR CATALOG. V. SEVENTH DATA RELEASE

We present the fifth edition of the Sloan Digital Sky Survey (SDSS) Quasar Catalog, which is based upon the SDSS Seventh Data Release. The catalog, which contains 105,783 spectroscopically confirmed quasars, represents the conclusion of the SDSS-I and SDSS-II quasar survey. The catalog consists of the SDSS objects that have luminosities larger than Mi = −22.0 (in a cosmology with H0 = 70 km s−1 Mpc−1, ΩM = 0.3, and ΩΛ = 0.7), have at least one emission line with FWHM larger than 1000 km s−1 or have interesting/complex absorption features, are fainter than i ≈ 15.0, and have highly reliable redshifts. The catalog covers an area of ≈9380 deg2. The quasar redshifts range from 0.065 to 5.46, with a median value of 1.49; the catalog includes 1248 quasars at redshifts greater than 4, of which 56 are at redshifts greater than 5. The catalog contains 9210 quasars with i < 18; slightly over half of the entries have i < 19. For each object the catalog presents positions accurate to better than 0. ″1 rms per coordinate, five-band (ugriz) CCD-based photometry with typical accuracy of 0.03 mag, and information on the morphology and selection method. The catalog also contains radio, near-infrared, and X-ray emission properties of the quasars, when available, from other large-area surveys. The calibrated digital spectra cover the wavelength region 3800–9200 Å at a spectral resolution of ≃ 2000; the spectra can be retrieved from the SDSS public database using the information provided in the catalog. Over 96% of the objects in the catalog were discovered by the SDSS. We also include a supplemental list of an additional 207 quasars with SDSS spectra whose archive photometric information is incomplete.
Software Product Reliability Based on Basic Block Metrics Recomposition

In the context of functional verification, the focus has always been on hardware and its ability to be both resilient to errors and to recover from them autonomously. In order to evaluate these characteristics, an extensive use of Fault Injection tools is made to achieve clear and granular results. These testing campaigns are carried out on the entire DUT and require a consistent amount of time and computational resources. The possibility of reducing these costs applying modern techniques as the study of the Dysfunctional State Machine or the proof of concept regarding the composability of single block fault injection campaigns to obtain a library of component of which the reliability metrics are well known, as already been extensively discussed and proven on hardware. In this work instead the application of this methodologies to software is presented for the first time. In order to do so, the software has been divided into basic block, atomic chunks of code having precise carachteristics that will ensure the possibility to study them singularly and then recompose them into a software product which reliability metrics are known, without the need for complete Fault injection campaign.
The CoNFIG Catalogue - II. Comparison of Space Densities in the FR Dichotomy

This paper focuses on a comparison of the space densities of FRI and FRII sources at different epochs, with a particular focus on FRI sources. First, we present the concluding steps in constructing the Combined NVSS-FIRST Galaxy catalogue (CoNFIG), including new VLA observations, optical identifications and redshift estimates. The final catalogue consists of 859 sources over 4 samples (CoNFIG-1, 2, 3 and 4 with flux density limits of S1.4GHz =1.3, 0.8, 0.2 and 0.05 Jy respectively). It is 95.7% complete in radio morphology classification and 74.3% of the sources have redshift data. Combining CoNFIG with complementary samples, the distribution and evolution of FRI and FRII sources are investigated. We find that FRI sources undergo mild evolution and that, at the same radio luminosity, FRI and FRII sources show similar space density enhancements in various redshift ranges, possibly implying a common evolution.
Robustness of Majorana fermions in proximity-induced superconductors

In two-dimensional chiral $p$-wave superconductors, the zero-energy Majorana fermion excitations trapped at vortex cores are protected from the thermal effects by the minigap, ${\ensuremath{\Delta}}^{2}/{ϵ}_{F}$ ($\ensuremath{\Delta}$: bulk gap, ${ϵ}_{F}$: Fermi energy), which is the excitation gap to the higher energy bound states in the vortex cores. Robustness to thermal effects is guaranteed only when $T⪡{\ensuremath{\Delta}}^{2}/{ϵ}_{F}\ensuremath{\sim}0.1\text{ }\text{mK}$, which is a very severe experimental constraint. Here we show that when $s$-wave superconductivity is proximity-induced on the surface of a topological insulator or a spin-orbit-coupled semiconductor, as has been recently suggested, the minigaps of the resultant non-Abelian states can be orders of magnitude larger than in a chiral $p$-wave superconductor. Specifically, for interfaces with sufficient barrier transparencies, the minigap can be as high as $\ensuremath{\sim}\ensuremath{\Delta}⪢{\ensuremath{\Delta}}^{2}/{ϵ}_{F}$, where $\ensuremath{\Delta}$ is the bulk gap of the $s$-wave superconductor.
A KECK HIRES DOPPLER SEARCH FOR PLANETS ORBITING METAL-POOR DWARFS. II. ON THE FREQUENCY OF GIANT PLANETS IN THE METAL-POOR REGIME

We present an analysis of three years of precision radial velocity (RV) measurements of 160 metal-poor stars observed with HIRES on the Keck 1 telescope. We report on variability and long-term velocity trends for each star in our sample. We identify several long-term, low-amplitude RV variables worthy of followup with direct imaging techniques. We place lower limits on the detectable companion mass as a function of orbital period. Our survey would have detected, with a 99.5% confidence level, over 95% of all companions on low-eccentricity orbits with velocity semiamplitude K ≳ 100 m s−1, or Mpsin i ≳ 3.0 MJ(P/yr)(1/3), for orbital periods P ≲ 3 yr. None of the stars in our sample exhibits RV variations compatible with the presence of Jovian planets with periods shorter than the survey duration. The resulting average frequency of gas giants orbiting metal-poor dwarfs with −2.0≲[Fe/H]≲−0.6 is fp < 0.67% (at the 1σ confidence level). We examine the implications of this null result in the context of the observed correlation between the rate of occurrence of giant planets and the metallicity of their main-sequence solar-type stellar hosts. By combining our data set with the Fischer & Valenti (2005) uniform sample, we confirm that the likelihood of a star to harbor a planet more massive than Jupiter within 2 AU is a steeply rising function of the host's metallicity. However, the data for stars with −1.0≲[Fe/H]≲0.0 are compatible, in a statistical sense, with a constant occurrence rate fp ≃ 1%. Our results can usefully inform theoretical studies of the process of giant-planet formation across two orders of magnitude in metallicity.
Period doubling bifurcation and high-order resonances in RR Lyrae hydrodynamical models

We investigated period doubling, a well-known phenomenon in dynamical systems, for the first time in RR Lyrae models. These studies provide theoretical background for the recent discovery of period doubling in some Blazhko RR Lyrae stars with the Kepler space telescope. Since period doubling has been observed only in Blazhko-modulated stars so far, the phenomenon can help in understanding the modulation as well. Utilizing the Florida–Budapest turbulent convective hydrodynamical code, we have identified the phenomenon in both radiative and convective models. A period-doubling cascade was also followed up to an eight-period solution, confirming that destabilization of the limit cycle is indeed the underlying phenomenon. Floquet stability roots were calculated to investigate the possible causes and occurrences of the phenomenon. A two-dimensional diagnostic diagram was constructed to illustrate the various resonances between the fundamental mode and the different overtones. Combining the two tools, we confirmed that the period-doubling instability is caused by a 9:2 resonance between the ninth overtone and the fundamental mode. Destabilization of the limit cycle by a resonance of a high-order mode is possible because the overtone is a strange mode. The resonance is found to be strong enough to shift the period of overtone by up to 10 per cent. Our investigations suggest that a more complex interplay of radial (and presumably non-radial) modes could happen in RR Lyrae stars that might have connections with the Blazhko effect as well.
Magnetic fields of accreting pulsars

Accreting pulsars are rotating, highly magnetized neutron stars in binary systems which emit pulsed X-rays. This emission is powered by the gra vitational energy of the plasma accreted from a non degenerate companion funne led onto the polar caps of the neutron star by the magnetic field, and thermalize d to X-rays either in the impact with the surface of the neutron star, or in the so-c alled accretion column. Although discovered more than forty years ago many aspects o f the emission form accreting pulsars remain puzzling. One of the key open issue s i the magnetic field of the neutron stars in these systems and how we can measure it . The X-ray spectrum of these systems is characterized by a cut -off power-law, interpreted as the result of the comptonization of the brems trahlung and cyclotron emission produced in the highly magnetized accreted plasma in the vicinity of the polar caps by the hot in-falling plasma. The theoretical des cription of the spectra is, however, far from complete. The presence of a strong magneti c fi ld (B∼ 1012 G) constrains and quantizes the motion of the electrons perpen dicularly to the field in the Landau levels, thus modifying the cross-section for Com pt n scatterings. The scattering cross-section strongly depends on the photon mo mentum and the magnetic field which manifests as the so-called cyclotron reson ance scattering features (CRSFs), observed as line-like absorption features in the s pectra of some pulsars. The centroid energy of these features is directly related to the magnetic field in the line-forming region viaEcyc[keV] ≃ 11.57×10−12BG, providing a way to directly measure the magnetic field of a neutron star. The timing properties of a neutron star, and more specificall y the changes of the pulse spin frequency, can be also used to estimate its magnet ic field. Neutron stars are very compact objects with a low intrinsic moment of inert ia and therefore their spin is completely governed by the external torques. These t orques depend on the interaction between the magnetosphere, determined by the s trength of the field, and the accreted matter. Therefore the study of these torques an d the spin history can provide an estimate of the magnetic field. In this thesis the role of these torques in the spin history of a sample of slow-
Wireless Method for Measuring the Rotational Speed of Roller Bearing in a High-Temperature Environment

Roller bearings are important rotating components of engines and have been widely used in the commercial, aerospace, railway transportation, and military fields. The inner race of a bearing that operates at high speeds can attain a temperature of almost 200 °C. Therefore, accurately measuring the speed of bearing inner race under a high-temperature thermal load is vital to ensure that engine is working properly. Herein, we propose a wireless method for measuring the bearing speed. The proposed method has a higher temperature application range and better accuracy than previous used methods. It measures the bearing’s inner race speed based on the eddy current effect and impedance matching. Adding a silver/copper layer to the surface of the bearing substrate changes its conductivity, magnetic permeability, and the equivalent impedance of the antenna. After passing through the coupler and detection circuit, the signal is output to the oscilloscope as a periodic voltage. The rotational speed of the bearing’s inner ring is measured by calculating the periodicity of the waveform. A bearing speed test platform is built and used for multiple groups of bearing speed measurements at 20 °C, 100 °C, and 200 °C on the platform. The results indicate that the method provides excellent stability and accuracy in the range of 0–1000 rpm, with a stable relative error of less than 1.64% and a maximum hysteresis of 1.72%. The maximum repeatability is 1.63658% (1000 rpm, 200 °C), and the maximum uncertainty is 0.66782 (1000 rpm, 200 °C).
IMAGING OF THREE POSSIBLE LOW-REDSHIFT ANALOGS TO HIGH-REDSHIFT COMPACT RED GALAXIES

As part of a larger program to identify and characterize possible low-redshift analogs to massive compact red galaxies found at high redshift, we have examined the morphologies of three low-redshift compact galaxies drawn from the sample of Trujillo et al. Using deeper and higher resolution images, we have found faint and relatively extensive outer structures in addition to the compact cores identified in the earlier measurements. One object appears to have a small companion that may be involved in an ongoing minor merger of the sort that could be responsible for building up the outer parts of these galaxies. The ages of the dominant stellar populations in these objects are found to be around 2–4 Gyr, in good agreement with the previous estimates. The presence of diffuse outer structures in these galaxies indicates that truly compact and massive red galaxies are exceedingly rare at low redshift. The relatively young stellar populations suggest that the accretion of the extensive outer material must occur essentially universally on relatively short timescales of a few billion years or less. These results confirm and extend previous suggestions that the driving mechanism behind the size evolution of high-redshift compact galaxies cannot be highly stochastic processes such as major mergers, which would inevitably leave a non-negligible fraction of survivors at low redshift.