Miracle-dz/UniFAR-FTUs huggingface dataset:
Different Methods of Canine Retraction- Part 1

Background: This review aimed at explaining different methods of canine retraction along the archwire. Methods: Searching for different methods of canine retraction using fixed orthodontic appliances was carried out using different databases, including PubMed Central, Science Direct, Wiley Online Library, the Cochrane Library, Textbooks, Google Scholar, Research Gate, and hand searching from 1930 till February 2022. Results: After excluding the duplicate articles, papers describing the methods of canine retraction along the archwires were included. The most commonly used methods are NiTi closed coil spring and elastic chain. Conclusions: Various methods of canine retraction along the archwires were explained in detail regarding their advantages, disadvantages, and comparisons among different methods supported by clinical trials, systematic review, and meta-analysis. The preferred method is canine retraction with NiTi closed coil spring with 150 and 200 gm. Elastic chain is considered an alternative, low-cost option.
GALACTIC AND CIRCUMGALACTIC O vi AND ITS IMPACT ON THE COSMOLOGICAL METAL AND BARYON BUDGETS AT 2 < z ≲ 3.5

We present the first results from our NASA Keck Observatory Database of Ionized Absorbers toward Quasars (KODIAQ) survey which aims to characterize the properties of the highly ionized gas of galaxies and their circumgalactic medium (CGM) at 2 < z < 4. We select absorbers optically thick at the Lyman limit (τLL > 1, ) as probes of these galaxies and their CGM where both transitions of the O vi doublet have little contamination from the Lyα, β forests. We found 20 absorbers that satisfy these rules: 7 Lyman limit systems (LLSs), 8 super-LLSs (SLLSs) and 5 damped Lyα (DLAs). The O vi detection rate is 100% for the DLAs, 71% for the LLSs, and 63% for the SLLSs. When O vi is detected, , an average O vi column density substantially larger and with a smaller dispersion than found in blind O vi surveys at similar redshifts. Strong O vi absorption is therefore nearly ubiquitous in the CGM of z ∼ 2–3 galaxies. The total velocity widths of the O vi profiles are also large ( km s−1). These properties are quite similar to those seen for O vi in low-z star-forming galaxies, and therefore we hypothesize that these strong CGM O vi absorbers (with τLL > 1) at 2 < z ≲ 3.5 also probe outflows of star-forming galaxies. The LLSs and SLLSs with no O vi absorption have properties consistent with those seen in cosmological simulations tracing cold streams feeding galaxies. When the highly ionized (Si iv and O vi) gas is taken into account, we determine that the τLL > 1 absorbers could contain as much as 3%–14% of the cosmic baryon budget at z ∼ 2–3, only second to the Lyα forest. We conservatively show that 5%–20% of the metals ever produced at z ∼ 2–3 are in form of highly ionized metals ejected in the CGM of galaxies.
Studying the evolution of galaxies in compact groups over the past 3 Gyr – I. Nuclear activity

We present the first -- of a series -- study of the evolution of galaxies in compact groups over the past 3 Gyr. This paper focuses on the evolution of the nuclear activity and how it has been affected by the dense environment of the groups. Our analysis is based on the largest multiwavelength compact group sample to-date, containing complete ultraviolet-to-infrared (UV-to-IR) photometry for 1,770 isolated groups (7,417 galaxies). We classified the nuclear activity of the galaxies based on optical emission line and mid-infrared diagnostic methods, as well as using spectral energy distribution fitting. We observe a 15% increase on the number of the AGN-hosting late-type galaxies found in dynamically old groups, over the past 3 Gyr, accompanied by the corresponding decrease of their circumnuclear star formation. Comparing our compact group results with those of local isolated field and interacting pair galaxies, we find no differences in the AGN at the same redshift range. Based on both optical and mid-IR colour classifications, we report the absence of Seyfert 1 nuclei and we attribute this to the low accretion rates, caused by the depletion of gas. We propose that the observed increase of LINER and Seyfert 2 nuclei (at low-z's), in the early-type galaxies of the dynamically young groups, is due to the morphological transformation of lenticular into elliptical galaxies. Finally, we show that at any given stellar mass, galaxies found in dynamically old groups are more likely to host an AGN. Our findings suggest that the depletion of gas, due to past star formation and tidal stripping, is the major mechanism driving the evolution of the nuclear activity in compact groups of galaxies.
An autonomous and reversible Maxwell's demon

Building on a model introduced by Mandal and Jarzynski (Proc. Natl. Acad. Sci. U.S.A., 109 (2012) 11641), we present a simple version of an autonomous reversible Maxwell's demon. By changing the entropy of a tape consisting of a sequence of bits passing through the demon, the demon can lift a mass using the coupling to a heat bath. Our model becomes reversible by allowing the tape to move in both directions. In this thermodynamically consistent model, total entropy production consists of three terms one of which recovers the irreversible limit studied by MJ. Our demon allows an interpretation in terms of an enzyme transporting and transforming molecules between compartments. Moreover, both genuine equilibrium and a linear response regime with corresponding Onsager coefficients are well defined. Efficiency and efficiency at maximum power are calculated. In linear response, the latter is shown to be bounded by 1/2, if the demon operates as a machine and by 1/3, if it is operated as an eraser.
The Effect of Self-Administration of Medication During Hospitalization on Patient’s Self-Efficacy and Medication Adherence After Discharge

Purpose The effect of self-administration of medication (SAM), in which capable hospitalized patients administer medication themselves on medication self-efficacy is inconclusive. The aim of this study was to evaluate the effect of SAM on medication self-efficacy, adherence and patient satisfaction. Patients and Methods A prospective pre-post intervention study on the orthopedic ward of the Sint Maartenskliniek (Nijmegen) was conducted from January 2020 to July 2021. All adults admitted to this ward were eligible for participation. The primary outcome was the level of medication self-efficacy measured by the Self-Efficacy for Appropriate Medication Use Scale (SEAMS) one week after discharge. Secondary outcomes were SEAMS-score three months after hospitalization, medication adherence measured by the Medication Adherence Rating Scale (MARS) one week and three months after hospitalization and patient satisfaction expressed on a five-point Likert scale in patients who experienced SAM. The differences in median SEAMS-scores and non-adherence pre- versus post-implementation of SAM were statistically analyzed. Patients’ agreement regarding satisfaction with SAM was calculated as proportion per Likert scale answer. Results Of the 197 patients participating in the study, 96 were included pre- and 101 post-implementation of SAM. Median SEAMS-scores one week after discharge were 35 [IQR 31–38] and 34 [IQR 30–36] pre- and post-intervention respectively (p = 0.08). There was no difference in the proportion of non-adherent patients at one week and three months after discharge pre- and post-intervention, 52.4%, 53.2%, 57.9% and 64.4% respectively. Of the patients that experienced SAM 32% agreed and 49% strongly agreed that they would like to self-manage medication again during a future hospitalization. Conclusion In this orthopedic population with high medication self-efficacy scores at discharge, SAM did not affect patients’ medication self-efficacy nor medication adherence after hospitalization. Most patients preferred SAM. Additional studies should focus on the effect of SAM in other patient populations.
Collisionally induced atomic clock shifts and correlations

We develop a formalism to incorporate exchange symmetry considerations into the calculation of collisional frequency shifts for atomic clocks using a density-matrix formalism. The formalism is developed for both fermionic and bosonic atomic clocks. Numerical results for a finite-temperature {sup 87}Sr {sup 1}S{sub 0} (F=9/2) atomic clock in a magic wavelength optical lattice are presented.
The Multi-dimensional Character of Core-collapse Supernovae

Core-collapse supernovae, the culmination of massive stellar evolution, are spectacular astronomical events and the principle actors in the story of our elemental origins. Our understanding of these events, while still incomplete, centers around a neutrino-driven central engine that is highly hydrodynamically unstable. Increasingly sophisticated simulations reveal a shock that stalls for hundreds of milliseconds before reviving. Though brought back to life by neutrino heating, the development of the supernova explosion is inextricably linked to multi-dimensional fluid flows. In this paper, the outcomes of three-dimensional simulations that include sophisticated nuclear physics and spectral neutrino transport are juxtaposed to learn about the nature of the three dimensional fluid flow that shapes the explosion. Comparison is also made between the results of simulations in spherical symmetry from several groups, to give ourselves confidence in the understanding derived from this juxtaposition.
THE SCHMIDT–KENNICUTT LAW OF MATCHED-AGE STAR-FORMING REGIONS; Paα OBSERVATIONS OF THE EARLY-PHASE INTERACTING GALAXY TAFFY I

In order to test a recent hypothesis that the dispersion in the Schmidt–Kennicutt law arises from variations in the evolutionary stage of star-forming molecular clouds, we compared molecular gas and recent star formation in an early-phase merger galaxy pair, Taffy I (UGC 12915/UGC 12914, VV 254) which went through a direct collision 20 Myr ago and whose star-forming regions are expected to have similar ages. Narrowband Paα image is obtained using the ANIR near-infrared camera on the mini-TAO 1 m telescope. The image enables us to derive accurate star formation rates within the galaxy directly. The total star formation rate, 22.2 M☉ yr−1, was found to be much higher than previous estimates. Ages of individual star-forming blobs estimated from equivalent widths indicate that most star-forming regions are ∼7 Myr old, except for a giant H ii region at the bridge which is much younger. Comparison between star formation rates and molecular gas masses for the regions with the same age exhibits a surprisingly tight correlation, a slope of unity, and star formation efficiencies comparable to those of starburst galaxies. These results suggest that Taffy I has just evolved into a starburst system after the collision, and the star-forming sites are at a similar stage in their evolution from natal molecular clouds except for the bridge region. The tight Schmidt–Kennicutt law supports the scenario that dispersion in the star formation law is in large part due to differences in evolutionary stage of star-forming regions.
Determining Cross‐Linguistic Phonological Similarity Between Segments

Although the general notion of "phonological similarity" has figured prominently in linguistic scholarship, the manner in which talkers determine similarity between phonological units is not well understood. Recent research has shown that perceptual similarity does not account for input-output mappings between languages as well as it does within a language. I argue that this disparity arises due to the fact that, unlike phonological similarity within a language, phonological similarity between languages is highly influenced by an abstract, between-system level of analysis that is only relevant cross-linguistically. I review an array of findings in cross-linguistic research to demonstrate, first, a dissociation between acoustic distance and phonemic correspondence and, second, a consistent preference for relating segments and natural classes cross-linguistically on the basis of phonemic correspondence. This type of abstract comparison helps to explain why effects of perceptual similarity are often masked in cross-linguistic circumstances, and I point to possible bases of these comparisons: (1) inventory niches based on contrastive feature oppositions and/or relative phonetics, and (2) distributional parallelisms.
Advocacy and Creativity in Community: A Social Justice Project for Counseling Students

The proven effective teaching of social justice advocacy competencies while recognized as important by the counseling profession and counselor education programs, remains somewhat nascent in its implementation. Evidence suggests that experiential and constructivist approaches to the teaching of multicultural and social justice counseling competencies represent a worthwhile pedagogical foundation and set of tools in furthering multicultural and social justice counseling competencies in counseling students. The author relates, in detail, the implementation of an experiential, client/community-based, social justice and mental health advocacy project, the Advocacy and Creativity in Community (ACC) Project as a final class assignment in the last term prior to graduation within a CACREP-accredited clinical mental health counseling program in the Northwest region of the United States. Descriptions of student projects, the multitude of benefits for clients/participants and students as elicited from student reflections, and the author’s reflection after three years of implementing this project are presented. This project exemplifies the benefits within the literature of taking an experiential and constructivist approach to social justice advocacy training in counselor education programs.
A simple method to calculate first-passage time densities of non-smooth processes

Numerous applications all the way from biology and physics to economics depend on the density of first crossings over a boundary. Motivated by the lack of analytical tools for computing first-passage time densities (FPTDs) for complex problems, we propose a new simple method based on the Independent Interval Approximation (IIA). We generalise previous formulations of the IIA to handle non-smooth processes, and derive a closed form expression for the FPTD in Laplace and $z$-transform space for arbitrary boundary and starting points in one dimension. We focus on Markov processes for which the IIA is exact. To apply our equations, we calculate the FPTD in two cases: the Ornstein-Uhlenbeck process and the discrete time Brownian walk. Our results are in good agreement with Langevin dynamics simulations.
Entanglement entropy across a deformed sphere

I study the entanglement entropy (EE) across a deformed sphere in conformal field theories (CFTs). I show that the sphere (locally) minimizes the universal term in EE among all shapes. In arXiv:1407.7249 it was derived that the sphere is a local extremum, by showing that the contribution linear in the deformation parameter is absent. In this paper I demonstrate that the quadratic contribution is positive and is controlled by the coefficient of the stress tensor two point function, $C_T$. Such a minimization result contextualizes the fruitful relation between the EE of a sphere and the number of degrees of freedom in field theory. I work with CFTs with gravitational duals, where all higher curvature couplings are turned on. These couplings parametrize conformal structures in stress tensor $n$-point functions, hence I show the result for infinitely many CFT examples.
PROPERTIES OF MICROLENSING EVENTS BY WIDE-SEPARATION PLANETS WITH A MOON

We investigate the properties of microlensing events caused by planetary systems where planets with a moon are widely separated from their host stars. From this investigation, we find that the moon feature generally appears as a very short-duration perturbation on the smooth asymmetric light curve of the lensing event induced by the wide-separation planet; thus it can be easily discriminated from the planet feature responsible for the overall asymmetric light curve. For typical Galactic lensing events with an Einstein radius of ∼2 au, the asymmetry of the light curves due to bound planets can be noticed up to ∼20 au. We also find that the perturbations of wide planetary systems become dominated by the moon as the projected star–planet separation increases, and eventually the light curves of events produced by such systems appear as the single lensing light curve of the planet itself with a very short-duration perturbation induced by the moon, which is a representative light curve of the event induced by a star and a planet, except on the Einstein timescale of the planet. We also study the effect of a finite source star on the moon feature in wide planetary lensing events. From this study, we find that when the lunar caustic is sufficiently separated from the planetary caustic, the lower limit on the ratio of the size of the lunar caustic to the source radius causing a ≥5% lunar deviation depends mostly on the projected planet–moon separation regardless of the moon/star mass ratio, and it decreases as the planet–moon separation becomes smaller or larger than the planetary Einstein radius.
The mechanism of antibody formation in mouse bone marrow

textabstractThe bone marrow (BM) is the major production site of B lymphocytes. The newly formed small B lymphocytes migrate, after a maturation period of one or more days, to the peripheral lymphoid organs (spleen, lymph nodes, tonsils, etc.), where they can be activated by antigen (after which they can differentiate into antibody-forming cells) or die. According to this view, most of the immunoglobul in(lg)- and antibodyproducing eel ls are considered to be confined to the peripheral lymphoid organs. However, publications have appeared during the last ninety years presenting evidence that antibody formation can also take place in the BM (Chapter 3). This thesis further investigates this phenomenon with mice as experimental animals. After primary immunization of mice with thymus-dependent (TO) antigens, antibody formation almost exclusively takes place in the peripheral lymphoid organs. However, after secondary immunization with the same antigen, substantial numbers of antibody-producing plaqueforming eel ls (PFC) are found not only in the peripheral lymphoid organs, but also in the BM. The first phase of the secondary response, about 1 week of duration, is characterized by much higher numbers of PFC in the spleen and/or lymph nodes than in the BM. But after this first phase, the PFC response in the BM is much higher than in al 1 other lymphoid organs together
Common Factors in Nonstationary Panel Data with a Deterministic Trend – Estimation and Distribution Theory

The paper studies large-dimention factor models with nonstationary factors and allows for deterministic trends and factors integrated of order higher then one.We follow the model speci.cation of Bai (2004) and derive the convergence rates and the limiting distributions of estimated factors, factors loadings and common components. We discuss in detail a model with a linear time trend. We ilustrate the theory with an empirical exmple that studies the fluctuations of the real activity of U.S.economy. We show that these . uctuationas can be explained by two nonstationary factors and a small number of stationary factors. We test the economic interpretation of nonstationary factors.
A Stata Package for the Estimation of the Dose-response Function through Adjustment for the Generalized Propensity Score

In this article, we briefly review the role of the propensity score in estimating dose–response functions as described in Hirano and Imbens (2004, Applied Bayesian Modeling and Causal Inference from Incomplete-Data Perspectives, 73–84). Then we present a set of Stata programs that estimate the propensity score in a setting with a continuous treatment, test the balancing property of the generalized propensity score, and estimate the dose–response function. We illustrate these programs by using a dataset collected by Imbens, Rubin, and Sacerdote.
Dark energy and doubly coupled bigravity

We analyse the late time cosmology and the gravitational properties of doubly coupled bigravity in the constrained vielbein formalism (equivalent to the metric formalism) when the mass of the massive graviton is of the order of the present Hubble rate. We focus on one of the two branches of background cosmology where the ratio between the scale factors of the two metrics is algebraically determined. We find that the late time physics depends on the mass of the graviton, which dictates the future asymptotic cosmological constant. The Universe evolves from a matter dominated epoch to a dark energy dominated era where the equation of state of dark energy can always be made close to −1 now by appropriately tuning the graviton mass. We also analyse the perturbative spectrum of the theory in the quasi-static approximation, well below the strong coupling scale where no instability is present, and we show that there are five scalar degrees of freedom, two vectors and two gravitons. In Minkowski space, where the four Newtonian potentials vanish, the theory manifestly reduces to one massive and one massless graviton. In a cosmological FRW background for both metrics, four of the five scalars are Newtonian potentials which lead to a modification of gravity on large scales. The fifth one gives rise to a ghost which decouples from pressure-less matter in the quasi-static approximation. In this scalar sector, gravity is modified with effects on both the growth of structure and the lensing potential. In particular, we find that the Σ parameter governing the Poisson equation of the weak lensing potential can differ from one in the recent past of the Universe. Overall, the nature of the modification of gravity at low energy, which reveals itself in the growth of structure and the lensing potential, is intrinsically dependent on the couplings to matter and the potential term of the vielbeins. We also find that the time variation of Newton’s constant in the Jordan frame can easily satisfy the bound from solar system tests of gravity. Finally we show that the two gravitons present in the spectrum have a non-trivial mass matrix whose origin follows from the potential term of bigravity. This mixing leads to gravitational birefringence.