Miracle-dz/UniFAR-FTUs huggingface dataset:
ESTIMATING THE PARAMETERS OF EXPONENTIALLY DAMPED OR UNDAMPED SINUSOIDAL SIGNALS IN NOISE

Abstract : We address the problem of estimating the parameters of a signal embedded in noise. The signal is composed of samples of a sum of M exponentially damped or undamped sinusoidal signals. We suggest improvements to the original approach proposed by Prony. He observed that the samples s(n) obey an M th order difference equation and that from the roots of the characteristic polynomial of the difference equation, the parameters (sk) can be determined. We present three methods to improve this approach when the signal is noise corrupted.
RXTE Studies of Long-Term X-Ray Spectral Variations in 4U 1820–30

We present the results of detailed spectral studies of the ultracompact low mass X-ray binary (LMXB) 4U 1820-30 carried out with the Rossi X-ray Timing Explorer (RXTE) during 1996-1997. 4U 1820-30 is an "atoll" source X-ray burster (XRB) located in the globular cluster NGC 6624. It is known to have an 11 minute binary period and a ~176 day modulation in its 2-12 keV flux. Observations were made with the PCA and HEXTE instruments on RXTE at roughly one-month intervals to sample this long-term period and study flux-related spectral changes. We find that the 176 day period corresponds to normal atoll source motion in the color-color diagram, indicating that the long period is due to mass accretion rate changes. There are clear correlations between our fitted spectral parameters and both the broadband (2-50 keV) flux and the position in the color-color diagram, as described by the parameter Sa introduced by Méndez et al. The hard X-ray tail becomes more prominent at low flux levels as the source moves into the island state. In addition, we find a strong correlation between the position in the color-color diagram and the frequencies of the kilohertz quasi-periodic oscillations (kHz QPOs) reported by Zhang et al. This lends further support to the notion that evidence for the last stable orbit in the accretion disk of 4U 1820-30 has been observed. For a model consisting of Comptonization of cool photons by hot electrons plus an additional blackbody component, we report an abrupt change in the spectral parameters at the same accretion rate at which the kHz QPOs disappear, suggesting a change in the accretion flow that affects both the spectrum and the timing properties. For a model consisting of a multicolor disk blackbody plus a cut-off power law, we find that the inner disk radius reaches a minimum at the same accretion rate at which the kHz QPO frequency saturates, as expected if the disk reaches the last stable orbit. Both models face theoretical and observational problems when interpreted physically for this system.
On the characterization of G-limits by means of some generalized two-scale techniques : Paper presented at the 26th Midwest-Pacific Differential Equations Conference, October 15-17, 2005, University of Alberta Edmonton, Alberta, Canada

G-convergence usually deals with the convergence of sequences of elliptic or parabolic operators. When the convergence of the sequence of operators is strong enough, it is trivial to determine the $G$-limit. Other cases need sophisticated techniques for this aim, where the most well investigated case is periodic homogenization. The main tool of today for this purpose has become the so called two-scale convergence method by Nguetseng. This approach relies on a fundamental compactness result which says that for any bounded sequence $\left\{ u_{h}\right\} $ in $L^{2}\left( \Omega \right) $ there is $u_{0}\in L^{2}\left( \Omega \times Y\right) $ such that \begin{equation*} \dint\nolimits_{\Omega }u_{h}(x)\tau _{h}v(x)dx\rightarrow \dint\nolimits_{\Omega} \dint\nolimits_{Y}u_{0}(x,y)v(x,y)dxdy\end{equation*}% for any $v\in X=L^{2}(\Omega ;C_{\sharp }(Y))$ up to a subsequence, where% \begin{equation*} \tau _{h}v(x)=v(x,\frac{x}{\varepsilon _{h}}),\varepsilon _{h}\rightarrow 0% \text{. }\end{equation*} For gradients of sequences $\left\{ u_{h}\right\} $ bounded in $H^{1}\left( \Omega \right) $ the deviation from the week limit can be made explicit in terms of a local gradient $\nabla _{y}u_{1}$, $u_{1}\in L^{2}(\Omega;H_{\sharp }^{1}(Y))$, and this is the key to the characterization of the $G$%-limit. Similar techniques can be developed for other choices of the maps $\tau _{h}$ and admissible spaces $X$ which do not necessarily depend on any periodicity assumptions. We study such examples with respect to the possible appearance of residual terms corresponding to $\nabla _{y}u_{1}$ in periodic homogenization. In particular $G$-limits for problems, where the matrices defining the operators are generated by a kind of modified Hilbert-Schmidt operators, are investigated with respect to such deviations.
Invasive Yet Inevitable? Privacy Normalization Trends in Biometric Technology

As biometric technology relies on bodily, physical information, it is among the more intrusive technologies in the contemporary consumer market. Consumer products containing biometric technology are becoming more popular and normalized, yet little is known about public perceptions concerning its privacy implications, especially from the perspective of human agency. This study examines how people perceive biometric technologies in different societal contexts and via different agents in control. Our study revealed that, in large part, people’s perceptions of biometric technology are context-dependent, based on who retrieves and who benefits from the information and the situation where the data are collected. Participants were much more comfortable with more intrusive biometric technology in airport security than in a grocery store, and if it was employed to improve their health. We conclude by considering the implications of the survey for new threats to personal privacy that arise out of emerging technologies.
Using Topic Models to Understand Rater-Mediated Writing Assessments

Abstract Integrated writing assessments are tasks that require students to construct an essay using evidence from source texts. Topic models are statistical models used to analyze text. This study analyzes two integrated writing tasks from students in grades 6 (N=1,250) and 8 (N=1,250) using topic models. Independent evaluations of the essays were also conducted to help generalize the results across the two grades and better understand students' underlying writing techniques. Four main categories were identified: (1) use of words that appeared in the prompt, (2) words that appeared in the source texts, (3) words that reflected inference, and (4) words that reflected integration. Higher-scoring students used words that reflect inference and integration of source text more often than lower-performing students.
The first 62 AGN observed with SDSS-IV MaNGA – III: stellar and gas kinematics

We investigate the effects of Active Galactic Nuclei (AGN) on the gas kinematics of their host galaxies, using MaNGA data for a sample of 62 AGN hosts and 109 control galaxies (inactive galaxies). We compare orientation of the line of nodes (kinematic Position Angle - PA) measured from the gas and stellar velocity fields for the two samples. We found that AGN hosts and control galaxies display similar kinematic PA offsets between gas and stars. However, we note that AGN have larger fractional velocity dispersion $\sigma$ differences between gas and stars [$\sigma_{frac}=(\sigma_{\rm gas}-\sigma_{stars})/\sigma_{\rm stars}$] when compared to their controls, as obtained from the velocity dispersion values of the central (nuclear) pixel (2.5" diameter). The AGN have a median value of $\sigma_{\rm frac}$ of $ _{\rm AGN}=0.04$, while the the median value for the control galaxies is $ _{\rm CTR}=-0.23$. 75% of the AGN show $\sigma_{frac}>-0.13$, while 75% of the normal galaxies show $\sigma_{\rm frac}<-0.04$, thus we suggest that the parameter $\sigma_{\rm frac}$ can be used as an indicative of AGN activity. We find a correlation between the [OIII]$\lambda$5007 luminosity and $\sigma_{frac}$ for our sample. Our main conclusion is that the AGN already observed with MaNGA are not powerful enough to produce important outflows at galactic scales, but at 1-2 kpc scales, AGN feedback signatures are always present on their host galaxies.
COMPUTATIONS OF FLOWS WITH INTERFACES USING ARBITRARY LAGRANGIAN EULERIAN METHOD

This work is devoted to the accurate simulation of incompressible two phase ows. The core of our methodology is the use of interface resolving meshes and the arbitrary Lagrangian-Eulerian (ALE) description of the uid kinematics. Our numerical scheme is based on second order nite elements, a fractional step time discretisation, and a special approximation of the curvature to incorporate surface tension ee cts. We demonstrate the potential of the proposed numerical method by the simulation of a rising bubble and the Rayleigh-Taylor instability problem.
The Power of Empathy: Experimental Evidence of the Impact of Perspective-Focused Interventions on Support for Prison Reform

As a result of COVID-19, individuals have experienced situations that may help them relate to others, including more limited ability to interact with their environment. Thus, this survey experiment (N = 2,229) tests whether perspective-focused interventions can help increase support for prison reform. Findings suggest that perspective-getting (providing the perspective of an incarcerated individual via a narrative description of dealing with confinement) increased self-reported support for prison reform initiatives, compared with information only. In addition, a perspective-taking prompt—nudging participants to put themselves in the shoes of the incarcerated individual when reading their narrative—may help boost intention to take action in support of prison reform. Future avenues for research and implications are discussed.
Degree Design Thinking: integrated design frameworks for emerging online degrees in higher education

This paper proposes a new conceptual framework for curriculum design that incorporates the principles of both educational and service design. Traditionally efforts in designing high quality online learning have relied on learning design and not on broader principles drawn from other fields of studies such as service design. This paper presents a case study of creating a quality online course on digital learning leadership to argue for the importance of an integrated approach to educational design. This new postgraduate degree in Digital Learning Leadership was aimed at the community of professionals working in the field of digital learning. The case study presents an integrated approach that combines design thinking and a Community of Inquiry framework as a way of cultivating a sense of belonging online for a network of digital learning professionals.
Pure-Strategy Equilibrium in the Generalized First-Price Auction

We revisit the classic result on the (non-)existence of pure-strategy Nash equilibria in the Generalized First-Price Auction for sponsored search advertising and show that the conclusion may be reversed when ads are ranked based on the product of stochastic quality scores and bid amounts, rather than solely on the latter. Moreover, the expected revenue in the pure strategy equilibrium of the Generalized First-Price Auction may substantially exceed that of the Generalized Second-Price Auction.
Bifidobacterium animalis ssp. lactis HY8002 (HY8002) improved intestinal integrity 2

1 Previous studies reported that and had immunomodulatory effects. Lactobacillus plantarum HY7717 (HY7717) was screened in vitro from among 3 21 other lactic acid bacteria (LAB) and demonstrated nitric oxide (NO) production. The aims of this study were to 4 investigate the individual and combined ex vivo and in vivo effects of LAB strains HY8002 and HY7717 at 5 immunostimulating mice that have been challenged with an immunosuppressant drug. The combination of HY8002 6 and HY7717 increased the secretion of cytokines such as interferon (IFN)-γ, interleukin (IL)-12, and tumor necrosis 7 factor (TNF)-α in splenocytes. In a mouse cyclophosphamide (CTX)-induced immunosuppression model, 8 administration of the foregoing LAB combination improved the splenic and hematological indices, activated natural 9 killer (NK) cells, and up-regulated plasma immunoglobulins and cytokines. Moreover, this combination treatment 10 increased Toll-like receptor 2 (TLR2) expression. The ability of the combination treatment to upregulate IFN-γ and 11 TNF-α in the splenocytes was inhibited by anti-TLR2 antibody. Hence, the immune responses stimulated by the 12 combination of HY8002 and HY7717 are associated with TLR2 activation. The preceding findings suggest that the 13 combination of the HY8002 and HY7717 LAB strains could prove to be a beneficial and efficacious immunostimulant probiotic supplement. The combination of the two probiotic strains would be applied on dairy 15 products. explored possible of efficacy between in and immunosuppressed and aimed to elucidate their molecular
CALCIUM AND LIGHT-ELEMENTS ABUNDANCE VARIATIONS FROM HIGH-RESOLUTION SPECTROSCOPY IN GLOBULAR CLUSTERS

We use abundances of Ca, O, Na, and Al from high-resolution UVES spectra of 200 red giants in 17 globular clusters (GCs) to investigate the correlation found by Lee et al. between chemical enrichment from SN II and star-to-star variations in light elements in GC stars. We find that (1) the [Ca/H] variations between first and second generation stars are tiny in most GCs (∼0.02–0.03 dex, comparable with typical observational errors). In addition, (2) using a large sample of red giants in M 4 with abundances from UVES spectra from Marino et al., we find that Ca and Fe abundances in the two populations of Na-poor and Na-rich stars are identical. These facts suggest that the separation seen in color–magnitude diagrams using the U band or hk index (as observed in NGC 1851 by Han et al.) are not due to Ca variations. Small differences in [Ca/H] as associated with hk variations might be due to a small systematic effect in abundance analysis, because most O-poor/Na-rich (He-rich) stars have slightly larger [Fe/H] (by 0.027 dex on average, due to decreased H in the ratio) than first generation stars and are then located at redder positions in the V, hk plane. While a few GCs (M 54, ω Cen, M 22, maybe even NGC 1851) do actually show various degree of metallicity spread, our findings eliminate the need of a close link between the enrichment by core-collapse supernovae with the mechanism responsible for the Na–O anticorrelation.
Accretion Disk Boundary Layers around Neutron Stars: X-Ray Production in Low-Mass X-Ray Binaries

The boundary layer where the accretion disk meets the star is expected to be the dominant source of high-energy radiation in low-mass X-ray binaries which contain weakly magnetized accreting neutron stars. We present Newtonian solutions for the structure of the boundary layer in such a system. We find that the main portion of the boundary layer gas is hot (≳108 K), has low density, and is radially and vertically extended. It will emit a large luminosity in X-rays, mainly produced by Comptonization of soft photons which pass through the hot gas. The gas is generally optically thick to scattering but optically thin to absorption. Energy is transported by viscosity from the rapidly rotating outer part of the boundary layer to the slowly rotating inner part, and this has the important effect of concentrating the energy dissipation in the dense, optically thick (to Thomson scattering) zone close to the stellar surface. Advection of energy also plays an important role in the energy balance. We explore the dependence of the boundary layer structure on the mass accretion rate and rotation rate of the star. We also examine the effects of changes in the α viscosity parameter and the viscosity prescription. Radiation pressure is the dominant source of pressure in the boundary layer. The radiation flux in the boundary layer is a substantial fraction of the Eddington limiting flux even for luminosities well below (~0.01 times) the Eddington luminosity LEdd for spherically symmetric accretion. At luminosities near LEdd, the boundary layer expands radially and has a radial extent larger than 1 stellar radius. This radial expansion increases the surface area of the boundary layer and allows it to radiate a larger total luminosity. Based on the temperatures and optical depths which characterize the boundary layer, we expect that Comptonization will produce a power-law spectrum at low source luminosities. At high luminosities the scattering optical depth is quite large, and Comptonization of low-frequency bremsstrahlung photons will produce a quasi-Planckian spectrum in the dense region where most of the energy is released. This spectrum will be altered by Comptonization as the radiation propagates through the lower density outer boundary layer.
Observations of the Ultraviolet-bright Star Y453 in the Globular Cluster M4 (NGC 6121)

We present a spectral analysis of the UV-bright star Y453 in M4. Model fits to the star’s optical spectrum yield ∼ 56,000 K. Fits to the star’s FUV spectrum, obtained with the Cosmic Origins Spectrograph on board the Hubble Space Telescope, reveal it to be considerably hotter, with ∼ 72,000 K. We adopt = 72,000 ± 2000 K and = 5.7 ± 0.2 as our best-fit parameters. Scaling the model spectrum to match the star’s optical and near-infrared magnitudes, we derive a mass and luminosity , consistent with the values expected of an evolved star in a globular cluster. Comparing the star with post-horizontal-branch evolutionary tracks, we conclude that it most likely evolved from the blue horizontal branch, departing the asymptotic giant branch before third dredge-up. It should thus exhibit the abundance pattern (O-poor and Na-rich) characteristic of the second-generation (SG) stars in M4. We derive the star’s photospheric abundances of He, C, N, O, Si, S, Ti, Cr, Fe, and Ni. CNO abundances are roughly 0.25 dex greater than those of the cluster’s SG stars, while the Si and S abundances match the cluster values. Abundances of the iron-peak elements (except for iron itself) are enhanced by 1–3 dex. Rather than revealing the star’s origin and evolution, this pattern reflects the combined effects of diffusive and mechanical processes in the stellar atmosphere.
ORBITING CIRCUMGALACTIC GAS AS A SIGNATURE OF COSMOLOGICAL ACCRETION

We use cosmological smoothed particle hydrodynamic simulations to study the kinematic signatures of cool gas accretion onto a pair of well-resolved galaxy halos. We find that cold-flow streams and gas-rich mergers produce a circumgalactic component of cool gas that generally orbits with high angular momentum about the galaxy halo before falling in to build the disk. This signature of cosmological accretion should be observable using background-object absorption-line studies as features that are offset from the galaxy's systemic velocity by ∼100 km s−1. In most cases, the accreted gas co-rotates with the central disk in the form of a warped, extended cold flow disk, such that the observed velocity offset will be in the same direction as galaxy rotation, appearing in sight lines that avoid the galactic poles. This prediction provides a means to observationally distinguish accreted gas from outflow gas: the accreted gas will show large one-sided velocity offsets in absorption-line studies while radial/bi-conical outflows will not (except possibly in special polar projections). Such a signature of rotation has already been seen in studies of intermediate-redshift galaxy–absorber pairs, and we suggest that these observations may be among the first to provide indirect observational evidence for cold accretion onto galactic halos. This cold-mode halo gas typically has ∼3–5 times more specific angular momentum than the dark matter. The associated cold-mode disk configurations are likely related to extended H i/extended UV disks that are seen around galaxies in the local universe. The fraction of galaxies with extended cold flow disks and associated offset absorption-line gas should decrease around bright galaxies at low redshift as cold-mode accretion dies out.
Explicit Examples of rational and Calabi-Yau threefolds with primitive automorphisms of positive entropy

We present the first explicit examples of a rational threefold and a Calabi-Yau threefold, admitting biregular automorphisms of positive entropy not preserving any dominant rational maps to lower positive dimensional varieties. The most crucial part is the rationality of the quotient threefold of a 3-dimensional torus of product type.
Some remarks on the automorphic spectrum of the inner forms of SL(N) (保型表現とその周辺 : RIMS研究集会報告集)

In this survey article, we start by reviewing Arthur’s conjectures for the multiplicities of -automorphic representations in the discrete spectrum. We also give a sketch of the main ideas thereof, as exemplified in Arthur’s endoscopic classification for classical groups, and then discuss its relation with the Hiraga-Saito theory for the group $SL(N)$ and its inner forms. This is based on a talk given in the RIMS workshop “Automorphic Representations and Related Topics”, Kyoto $2013$ . 1 Multiplicities in the discrete spectrum Let $F$ be a number field and $\mathbb{A}$ $:=\mathbb{A}_{F}$ its ring of ad\‘eles. Fix an algebraic closure $F$ of $F$ . We define $\Gamma_{F}$ $:=$ Gal $(\overline{F}/F)$ and denote its Weil group by $W_{F}$ . The Weil-Deligne group of $F$ is denoted by $W_{F}’. $ For a connected reductive $F$-group $G$ , one of the main concerns of the theory of -automorphic forms is to study the right regular representation of $G(\mathbb{A})$ on $L^{2}(G(F)\backslash G(\mathbb{A})^{1})=L_{disc}^{2}(G(F)\backslash G(\mathbb{A})^{1})\oplus$ (continuous spectrum) where $G(\mathbb{A})^{1}$ is the kernel of the Harish-Chandra homomorphism $H_{G}$ : $G(\mathbb{A})arrow$
Invertible integer DCT applied on progressive until lossless image compression

This paper completes the construction of FFT (fast Fourier transform) that map integers to integers by using lifting scheme and butterfly-style construction. Through building integer FFT which keeps conjugate symmetry for real signal, and expressing DCT by FFT, invertible integer DCT can be easily gotten, which makes lossless image compression possible. At last, we combine integer DCT with EZW zerotree and STQM arithmetic coding together. Experimental results show this method is quite efficient for progressive until lossless image compression.
Star Formation in the Interacting Pair NGC 7733/7734

The problem of star formation within the interacting pair NGC 7733/34 has been studied based on the UBVRI photometry of the source. The distribution of the colors of selected regions within the galaxies is used to infer an estimate for the age distribution of the star-forming regions. The results seem to indicate the presence of numerous extended young star-forming regions in the disk of one of the two galaxies, NGC 7733, with ages in the range 106–108 yr. However, there exists no evidence for any violent star formation activity in the past 108 yr in the nuclei of the two galaxies. The pair seems to be a merger-bound system with the brightest and youngest site of star-forming activity lying at the disk interface.