Miracle-dz/UniFAR-FTUs huggingface dataset:
OfﬁceLearn: An OpenAI Gym Environment for Reinforcement Learning on Occupant-Level Building’s Energy Demand Response

Energy Demand Response (DR) will play a crucial role in balancing renewable energy generation with demand as grids decarbonize. There is growing interest in developing Reinforcement Learning (RL) techniques to optimize DR pricing, as pricing set by electric utilities often cannot take behavioral irrationality into account. However, so far, attempts to standardize RL efforts in this area do not exist. In this paper, we present a ﬁrst of the kind OpenAI gym environment for testing DR with occupant level building dynamics. We demonstrate the ﬂexibility with which a researcher can customize our simulated ofﬁce environment through the explicit input parameters we have provided. We hope that this work enables future work in DR in buildings.
Factors Involving In Dental Implant Failure -A Review

Dental implants are generally considered as a long-term successful treatment modality in a dental clinic. Though many cases have been reported in relation to the failure of implants. Successful implants are those which stay healthy in the oral cavity and also doesn’t cause damage to its surrounding tissues. Recognizing any diseases or abnormalities in the oral cavity prior to the placement of the implant increases the chances of successful implant placement. Other factors such as age, sex, smoking, dietary habits, alcohol consumption and location of the abutment placement also play a major role in the success of implant placement. The follow up procedure after the implant placement is very important considering the longevity and stability of the implant. prosthetic component for plaque and calculus, stability of the implant abutment, peri implant tissue margin, implant body, and radiographs should be done after every 12–18 months in maintenance. oral lichen planus, parafunctional habits are some of the other clinical and conventional flap , flapless surgery, status of dentition, piezoelectric surgical technique and causes deleterious effects of smoking habit .
Integration Of The Exponential Function Of A Complex Quadratic Form

The system and method for normalizing the amplitude of servo code derived signals in a disc drive, includes an improved embedded servo code format of separate magnetic dibit fields, recorded in half track steps. One magnetic dibit field is an automatic gain control field in which the magnetic head sees the same amount of magnetic dibit regardless of its position with respect to the track. A fast settling AGC loop responding to signals from the AGC field, produces a gain adjust signal while the magnetic head is still in the AGC field, which is used to normalize the amplitude of all following servo code and data code signals in that sector. The cycle of automatic gain control is repeated for each track in each sector. A sector mark following the AGC field has a magnetic dibit pattern which is fault tolerant. It is transduced in three parts to minimize error in its detection and identification and provides a timing reference for servo signals which follow. A defect dibit is recorded if the following servo gap is found to be defective during manufacture so that the next servo gap may be ignored. A track position servo code field provides signals for track following.
Promoting health equity in the health-care system: How can we identify potentially vulnerable patients?

Background: There is documented social inequality in cancer. The health-care system may contribute to health equity by targeting interventions to potentially vulnerable patients who may be at risk of not receiving optimal treatment and care. Aim: This study aimed to develop and pilot test a tool to identify patients who may need additional support. Method: The study took place in a department of palliative medicine and in a team for head and neck cancer within an oncology department. The tool to identify potentially vulnerable patients was developed based on literature reviews and interviews with patients and health-care personnel. It was pilot tested in a six-month period, with subsequent interviews with health-care personnel. Results: In total, 212 consecutive patients referred to the departments were systematically screened with the tool by health-care personnel. Of these, 74 (35%) patients were considered potentially vulnerable. The most frequently reported sign of vulnerability was ‘few supportive relations’ (47% of the vulnerable patients). Most health-care personnel found it relevant to focus systematically on these patients. However, some were concerned that using the tool could prove to be stigmatising and were critical of attributing the vulnerability to the individual. Conclusions: Most patients were considered in need of additional support because they lacked a social network or had difficulties communicating with health-care personnel. Applying a tool to identify potentially vulnerable patients was feasible and increased attention to this group of patients. However, the screening procedure was also questioned.
Online time-modal monitoring of non stationnary systems

A new algorithm for the online monitoring of varying modal parameters in vibrating structures subjected to unknown excitations is presented by using a vector autoregressive model. The method consists in applying a Short Time Sliding Window (STSW) on the signal. The solution, inside each sliding window, is found by applying a recursive multivariable least squares method via the computation of the QR factorization on the vector autoregressive model. In this method, only the R sub-matrices of the QR factorization need to be manipulated. An efficient model order is real time defined and updated. The minimum description length criterion is utilized to select an efficient model order which may be updated by increasing or decreasing order with respect to time from previous computational window. Various numerical and experimental data are presented to validate the proposed method; by investigating either abrupt or gradual changes in the system under white noise and various kinds of excitations such an impulsion, a sinusoidal or a random force. The results show that the modal parameters variation can be accurately identified and monitored but the monitoring of damping variation is more difficult if the system is continuously subjected to gradual changes or is excited by random excitations with high variances.
Maximal unbalanced families

A family of subsets of the set {1,2,. ,n} is said to be unbalanced if the convex hull of its characteristic vectors misses the diagonal in the n-cube.The purpose of this article is to develop the combinatorics of maximal unbalanced families. Specifically, we will prove lower and upper bounds on the number of maximal unbalanced families of subsets of an n-element set -- both bounds are of the form 2^{C n^2} for some C > 0. These families correspond to the chambers of a hyperplane arrangement, the restricted all-subset arrangement, that has arisen in various forms in physics, economics and psychometrics. In particular, our bounds answer a question posed in thermal field theory concerning the order of the number of chambers of this arrangement.
Orbits and masses in the young triple system TWA 5

Aims. We aim to improve the orbital elements and determine the individual masses of the components in the triple system TWA 5. Methods. Five new relative astrometric positions in the H band were recorded with the adaptive optics system at the Very Large Telescope (VLT). We combine them with data from the literature and a measurement in the Ks band. We derive an improved fit for the orbit of TWA 5Aa-b around each other. Furthermore, we use the third component, TWA 5B, as an astrometric reference to determine the motion of Aa and Ab around their center of mass and compute their mass ratio. Results. We fi nd an orbital period of 6.03 ± 0.01 years and a semi-major axis of 63.7 ± 0. 2m as (3.2 ± 0.1 AU). With the trigonometric distance of 50.1 ± 1.8 pc, this yields a system mass of 0.9 ± 0.1 M� , where the error is dominated by the error of the distance. The dynamical mass agrees with the system mass predicted by a number of theoretical models if we assume that TWA5 is at the young end of the age range of the TW Hydrae association. We find a mass ratio of MAb/MAa = 1.3 +0.6 −0.4 , where the less luminous component Ab is more massive. This result is likely to be a consequence of the large uncertainties due to the limited orbital coverage of the observations.
Quantum Nature of Relaxation of Paramagnetic and Optical Systems by Strong Dipole-Photon and Dipole-Phonon Coupling

Matrix-operator difference-differential equations for dynamics of spectroscopic transitions in 1D multiqubit exchange coupled (para)magnetic and optical systems by strong dipole-photon and dipole-phonon coupling are derived within the framework of quantum electrodynamics and quantum phonon field theory. It has been established, that in the model considered the relaxation processes are of pure quantum character, which is determined by the formation of the coherent system of the resonance phonons and by the appearence along with absorption process of EM-field energy the coherent emission process, acompanying by phonon Rabi quantum oscillation, which can be time-shared. For the case of radiospectroscopy it corresponds to the possibility of the simultaneous observation along with (para)magntic spin resonance the acoustic spin resonance. Theoretical conclusions are confirmed experimentally in radiospectroscopy. It has been found in particular, that the lifetime of coherent state of collective subsystem of resonance phonons in disordered carbon samples - anthracites of medium-scale metamorphism - is very long and even by room temperature it is evaluated in $\sim 10$ ms. The phenomenon of the formation of the coherent system of the resonance phonons can be used in a number of practical applications, in particular by elaboration of logic quantum systems including quantum computers and quantum communication systems.
Event based simulation of an EPR-B experiment by local hidden variables: epr-simple and epr-clocked

In this note, I analyse the data generated by M. Fodje's simulation programs "epr-simple" and "epr-clocked" using appropriate modified Bell-CHSH type inequalities: the Larsson detection loophole adjusted CHSH, and the Larsson-Gill coincidence loophole adjusted CHSH. The experimental efficiencies turn out to be approximately eta = 81% and gamma = 55% respectively, and the observed value of CHSH is (of course) well within the adjusted bounds.
Modeling Particle Acceleration at Interplanetary Shocks

A brief review of particle acceleration at inner heliospheric interplanetary and coronal mass ejection (CME)‐driven shocks is presented. The discussion is presented in terms of a specific event that was modeled using the Particle Acceleration and Transport in the Heliosphere model (hereafter PATH) code.
A universal bound on excitations of heavy fields during inflation

We discuss a universal bound on any excitation of heavy fields during inflation: the ratio of the heavy field's energy density to the one driving inflation must be less than the maximally allowed relative amplitude of oscillations in the power-spectrum ρh/ρI ≲ 0.01 according to PLANCK). This bound can be traced back to the sudden change of the equation of state parameter across the excitation event. We employ a sudden transition approximation at the perturbed level, which has been used before in different settings; we check its validity by comparison to the full multi-field result in a concrete case study involving a sudden mass change of an inflaton.
Predicted UV properties of very metal-poor starburst galaxies

Aims. We study the expected properties of starburst galaxies in order to provide the point of reference for interpretation of high-z galaxy surveys and of very metal-poor galaxies. We concentrate mainly on the UV characteristics such as the ionizing spectra, the UV continuum, the Lyα and He ii λ1640 line and two-photon continuum emission. Methods. We use evolutionary synthesis models covering metallicities from Pop III to solar and a wide range of IMFs. We also combine the synthetic SEDs with the CLOUDY photoionization code for more accurate predictions of nebular emission, and to study possible departures from case B assumed in the synthesis models. Results. The ionizing fluxes, UV continuum properties, and predicted Lyα and He ii λ1640 line strengths are presented for synthesis models covering a wider range of parameter space than our earlier calculations. Strong departures from case B predictions are obtained for Lyα and 2γ continuum at low metallicities. At low nebular densities both are shown to be enhanced proportionally to the mean energy carried by the Lyman continuum photons emitted by the ionizing source. Larger Lyα equivalent widths are therefore predicted at low metallicity. The He ii λ1640 line can be weaker than case B predicts (in terms of flux as well as the equivalent width) due to its ionization parameter dependence and to the enhanced underlying 2γ continuum. Conclusions. Our results have implications for the interpretation of star-forming metal-poor and/or high redshift galaxies, for galaxies among the Lyα emitters (LAE) and Lyman Break galaxy (LBG) populations, and for searches of Population III stars in the distant Universe.
SGR A* AND ITS ENVIRONMENT: LOW-MASS STAR FORMATION, THE ORIGIN OF X-RAY GAS AND COLLIMATED OUTFLOW

We present high-resolution multiwavelength radio continuum images of the region within 150″ of Sgr A*, revealing a number of new extended features and stellar sources in this region. First, we detect a continuous 2″ east–west ridge of radio emission, linking Sgr A* and a cluster of stars associated with IRS 13 N and IRS 13E. The ridge suggests that an outflow of east–west blob-like structures is emerging from Sgr A*. In particular, we find arc-like radio structures within the ridge with morphologies suggestive of photoevaporative protoplanetary disks. We use infrared Ks and L′ fluxes to show that the emission has similar characteristics to those of a protoplanetary disk irradiated by the intense radiation field at the Galactic center. This suggests that star formation has taken place within the S-cluster 2″ from Sgr A*. We suggest that the diffuse X-ray emission associated with Sgr A* is due to an expanding hot wind produced by the mass loss from B-type main sequence stars, and/or the disks of photoevaporation of low mass young stellar objects (YSOs) at a rate of ∼10−6 M ⊙ ? > yr−1. The proposed model naturally reduces the inferred accretion rate and is an alternative to the inflow–outflow style models to explain the underluminous nature of Sgr A*. Second, on a scale of 5″ from Sgr A*, we detect new cometary radio and infrared sources at a position angle PA ∼ 50° which is similar to that of two other cometary sources X3 and X7, all of which face Sgr A*. In addition, we detect a striking tower of radio emission at a PA ∼ 50°–60° along the major axis of the Sgr A East supernova remnant shell on a scale of 150″ from Sgr A*. We suggest that the cometary sources and the tower feature are tracing interaction sites of a mildly relativistic jet from Sgr A* with the atmosphere of stars and the nonthermal Sgr A East shell at a PA ∼ 50°–60° with M ˙ ∼ 1 × 10 − 7 M ⊙ yr - 1 ? > , and opening angle 10°. Lastly, we suggest that the east–west ridge of radio emission traces an outflow that is potentially associated with past flaring activity from Sgr A*. The position angle of the outflow driven by flaring activity is close to −90°.
Symmetry and Self-Organization in Complex Systems

We show that, in contrast to classical random graph models, many real-world complex systems -- including a variety of biological regulatory networks and technological networks such as the internet -- spontaneously self-organize to a richly symmetric state. We consider the organizational origins of symmetry and find that growth with preferential attachment confers symmetry in highly branched networks. We deconstruct the automorphism group of some real-world networks and find that some, but not all, real-world symmetry can be accounted for by branching. We also uncover an intriguing correspondence between the size of the automorphism group of growing random trees and the random Fibonacci sequences.
The Gravity of Situation

In this thesis we examine several ways in which we can explore the early universe through gravitational-waves and the fundamental nature of gravity through cosmology and observations of dynamics within the solar system. Both of these topics have taken center stage, as we are living at a unique time which promises to bring fundamental insights into the nature of gravity with the discovery of new binary pulsar systems, the building of increasingly precise solar system and tabletop experiments and the birth of gravitational-wave observatories-- to name a few recent and upcoming advances. We first discuss whether we may be able to directly detect gravitational waves from inflation using future space-based interferometers. We then describe how the direct detection of inflationary gravitational waves will allow us to probe the fundamental physics that operated at the earliest moments of the universe. Next, a new constraint to a general cosmological gravitational wave background is presented using the observations of the cosmic microwave background. Moving away from general relativity, we consider alternative theories of gravity. One reason to consider alternative theories of gravity is the observation that the expansion of the universe is currently accelerating. It is possible that this accelerated expansion is due to a modification of gravity. However, any theory that modifies gravity in order to produce accelerated expansion must also conform to the dynamics that we observe within the Solar System. We discuss how the observation of the deflection of light around the Sun places severe limitations on a particular modified gravity theory, known as f(R) gravity. Our discussion of f(R) gravity leads us to ask whether the parameterized post Newtonian parameter, γPPN, takes on a universal value. We identify measurements made of strong lensing around early type galaxies in the Sloan Lens ACS (SLACS) survey as a first step in performing this new test of gravity. Finally, we explore some consequences of Chern-Simons gravity. One of the unique aspects of Chern-Simons gravity is that it introduces parity violation into the gravitational sector. As a consequence, it predicts a different gravitomagnetic field around the rotating Earth than is predicted in general relativity. We show how recent measurements of this gravitomagnetic field made by observing the two LAser GEOdynamics Satellites (LAGEOS) and Gravity Probe B satellites constrain Chern-Simons gravity. Finally, we discuss how future observations of binary pulsar systems may allow for a more general exploration of the gravitomagnetic structure around rotating objects.
Correcting cosmological parameter biases for all redshift surveys induced by estimating and reweighting redshift distributions

Photometric redshift uncertainties are a major source of systematic error for ongoing and future photometric surveys. We study different sources of redshift error caused by choosing a suboptimal redshift histogram bin width and propose methods to resolve them. The selection of a too large bin width is shown to oversmooth small- scale structure of the radial distribution of galaxies. This systematic error can significantly shift cosmological parameter constraints by up to 6 sigma for the dark energy equation-of-state parameter w. Careful selection of bin width can reduce this systematic by a factor of up to 6 as compared with commonly used current binning approaches. We further discuss a generalized resampling method that can correct systematic and statistical errors in cosmological parameter constraints caused by uncertainties in the redshift distribution. This can be achieved without any prior assumptions about the shape of the distribution or the form of the redshift error. Our methodology allows photometric surveys to obtain unbiased cosmological parameter constraints using a minimum number of spectroscopic calibration data. For a DES-like galaxy clustering forecast, we obtain unbiased results with respect to errors caused by suboptimal histogram bin width selection, using only 5k representative spectroscopic calibration objects per tomographic redshift bin.
Gapless pairing and the Fermi arc in the cuprates

We argue that the Fermi arc observed in angle-resolved photoemission measurements in underdoped cuprates can be understood as a consequence of inelastic scattering in a phase-disordered d-wave superconductor. We analyze this phenomenon in the context of strong-coupling Eliashberg theory, deriving a 'single-lifetime' model for describing the temperature evolution of the spectral gap as measured by single-particle probes such as photoemission and tunneling.
Using R for Numerical Analysis in Science and Engineering

Introduction Obtaining and Installing R Learning R Learning Numerical Methods Finding Help Augmenting R with Packages Learning More about R Calculating Basic Operators and Functions Complex Numbers Numerical Display, Round-Off Error, and Rounding Assigning Variables Relational Operators Vectors Matrices Time and Date Calculations Graphing Scatter Plots Function Plots Other Common Plots Customizing Plots Error Bars Superimposing Vectors in a Plot Modifying Axes Adding Text and Math Expressions Placing Several Plots in a Figure Two- and Three-Dimensional Plots The Plotrix Package Animation Additional Plotting Packages Programming and Functions Conditional Execution: If and If Else Loops User-Defined Functions Debugging Built-in Mathematical Functions Special Functions of Mathematical Physics Polynomial Functions in Packages Case Studies Solving Systems Of Algebraic Equations Finding the Zeroes of a Polynomial Finding the Zeroes of a Function Systems of Linear Equations: Matrix Solve Matrix Inverse Singular Matrix Overdetermined Systems and Generalized Inverse Sparse Matrices Matrix Decomposition Systems of Nonlinear Equations Case Studies Numerical Differentiation and Integration Numerical Differentiation Numerical Integration Symbolic Manipulations in R Case Studies Optimization One-Dimensional Optimization Multi-Dimensional Optimization with Optim() Other Optimization Packages Optimization with Constraints Global Optimization with Many Local Minima Linear and Quadratic Programming Mixed-Integer Linear Programming Case Study Ordinary Differential Equations Euler Method Improved Euler Method deSolve Package Matrix Exponential Solution for Sets of Linear ODEs Events and Roots Difference Equations Delay Differential Equations Differential Algebraic Equations rootSolve for Steady State Solutions of Systems of ODEs bvpSolve Package for Boundary Value ODE Problems Stochastic Differential Equations: Gillespiessa Package Case Studies Partial Differential Equations Diffusion Equation Wave Equation Laplace's Equation Solving PDEs with the Reactran Package Examples with the Reactran Package Case Studies Analyzing Data Getting Data into R Data Frames Summary Statistics for a Single Data Set Statistical Comparison of Two Samples Chi-Squared Test for Goodness of Fit Correlation Principal Component Analysis Cluster Analysis Case Studies Fitting Models To Data Fitting Data with Linear Models Fitting Data with Nonlinear Models Inverse Modeling of ODEs with the FME Package Improving the Convergence of Series: Pade and Shanks Interpolation Time Series, Spectrum Analysis, and Signal Processing Case Studies