Miracle-dz/UniFAR-FTUs huggingface dataset:
“THE NEW OASIS”: IMPLEMENTASI PERMENDIKBUD TENTANG PENCEGAHAN DAN PENANGANAN KEKERASAN SEKSUAL DI PERGURUAN TINGGI

Sexual violence in the world of higher education needs a special attention. The protection of every citizen from sexual violence is part of the obligation of state in protecting human rights. The Decree of the Minister of Education and Culture Number 30/2021 on the Prevention and Handling of Sexual Violence in Higher Education (Permendikbud 30/2021) which has been released is providing a new hope for the citizens to gain appropriate protection. This study aims to examine to what extent has Permendikbud 30/2021 been implemented so far. The study is expected to provide recommendations on necessary things to be done by Indonesian universities to implement the decree. It employed a desk study scrutinizing relevant academic literature and any data or information from official sources in several universities. We found that the government has taken some efforts to guarantee the protection of the citizens against sexual violence in the world of higher education by releasing the decree. However, not all higher educational institutions have implemented. Therefore, the government is required to push this direction and all universities are required to increase their awareness as to put the regulation at work. Keywords: Sexual Violence, Higher Education, The Decree Of The Ministry Of Education And Culture No. 30/2021, The Protection Of Human Rights AbstrakKekerasan seksual di perguruan tinggi perlu mendapat perhatian khusus. Perlindungan setiap warga negara terhadap kasus kekerasan seksual merupakan kewajiban negara dalam pemenuhan aspek hak asasi manusia. Permendikbud Nomor 30 Tahun 2021 mengenai Pencegahan dan Penanganan Kekerasan Seksual di lingkungan Perguruan Tinggi yang telah disahkan seolah memberi harapan baru bagi anak bangsa untuk mendapat perlindungan yang selayaknya. Penelitian ini bertujuan untuk mengkaji sejauh mana implementasi Permendikbud Nomor 30 Tahun 2021 di perguruan tinggi di Indonesia. Penelitian ini akan memberi saran atau rekomendasi mengenai hal apa saja yang perlu dilakukan oleh setiap perguruan tinggi di Indonesia untuk mengimplementasikan Permendikbud Nomor 30 Tahun 2021. Metode yang digunakan yaitu desk study dengan menelaah literatur akademik yang relevan dan berbagai data atau informasi dari sumber resmi di beberapa perguruan tinggi. Hasil penelitian ini menunjukkan bahwa pemerintah telah berusaha menjamin perlindungan hak warga negara terhadap kasus kekerasan seksual di perguruan tinggi dengan mengesahkan peraturan tersebut, namun belum semua perguruan tinggi mengimplementasikannya sehingga diperlukan dorongan dari pemerintah dan kesadaran setiap perguruan tinggi yang ada di Indonesia untuk segera mewujudnyatakannya. Kata Kunci: Kekerasan Seksual, Perguruan Tinggi, Permendikbud No. 30/2021, Perlindungan HAM
Cosmological constraint on Brans-Dicke Model

We combine new Cosmic Microwave Background (CMB) data from Planck with Baryon Acoustic Oscillation (BAO) data to constrain the Brans-Dicke (BD) theory, in which the gravitational constant G evolves with time. Observations of type Ia supernovae (SNeIa) provide another important set of cosmological data, as they may be regarded as standard candles after some empirical corrections. However, in theories that include modified gravity like the BD theory, there is some risk and complication when using the SNIa data because their luminosity may depend on G. In this paper, we assume a power law relation between the SNIa luminosity and G, but treat the power index as a free parameter. We then test whether the difference in distances measured with SNIa data and BAO data can be reduced in such a model. We also constrain the BD theory and cosmological parameters by making a global fit with the CMB, BAO and SNIa data set. For the CMB+BAO+SNIa data set, we find 0.08 × 10−2 < ζ < 0.33 × 10−2 at the 68% confidence level (CL) and −0.01 × 10−2 < ζ < 0.43 × 10−2 at the 95% CL, where ζ is related to the BD parameter ω by ζ = ln(1 + 1/ω).
Identiﬁcation of Potential Biomarkers for Cancer Cachexia and Anti-Fn14 Therapy

Simple Summary: Cancer cachexia is an underestimated condition with huge impact on survival and quality of life for many cancer patients. Currently, there is no reliable diagnosis for this condition, particularly for cancer cachexia at an early stage. The aim of our study is to develop potential biomarkers that can be used not only for diagnosing cancer cachexia but also evaluating potential anti-cachexia therapy such as anti-Fn14 mAb treatment. We identiﬁed several circulating biomarkers for cancer cachexia and conﬁrmed that LCN2 is a promising biomarker for cancer cachexia in humans. These biomarkers could accelerate both diagnosis and clinical trials for cancer cachexia. Abstract: Background: Developing therapies for cancer cachexia has not been successful to date, in part due to the challenges of achieving robust quantitative measures as a readout of patient treatment. Hence, identifying biomarkers to assess the outcomes of treatments for cancer cachexia is of great interest and important for accelerating future clinical trials. Methods: We established a novel xenograft model for cancer cachexia with a cachectic human PC3* cell line, which was responsive to anti-Fn14 mAb treatment. Using RNA-seq and secretomic analysis, genes differentially expressed in cachectic and non-cachectic tumors were identiﬁed and validated by digital droplet PCR (ddPCR). Correlation analysis was performed to investigate their impact on survival in cancer patients. Results: A total of 46 genes were highly expressed in cachectic PC3* tumors, which were downregulated by anti-Fn14 mAb treatment. High expression of the top 10 candidates was correlated with low survival and high cachexia risk in different cancer types. Elevated levels of LCN2 were observed in serum samples from cachectic patients compared with non-cachectic cancer patients. Conclusion: The top 10 candidates identiﬁed in this study are candidates as potential biomarkers for cancer cachexia. The diagnostic value of LCN2 in detecting cancer cachexia is conﬁrmed in patient samples.
Multiscale image dehazing network based on spatially weighted sparse representation

Abstract. Due to the influence of hazy weather, the images captured often suffer from severe degradation, which will reduce the effectiveness of the devices for computer-related applications. To eliminate the degradation of hazy images, a multiscale image dehazing network based on spatially weighted sparse representation is proposed. The model is mainly divided into two modules: multiscale module (MSM) and detail enhancement module (DEM). The MSM can effectively obtain more feature information in more hazy images. Specifically, the degradation of hazy image is considered in terms of haze distribution and image details. A spatially weighted nonlocal sparse attention module was developed to focus on channel-level features adaptively and to pay more attention to the recovery of dense haze areas in response to the problem of uneven distribution of haze in images. In addition, an independent feature fusion module is proposed to capture better the contextual information, which can also effectively address the traditional fusion, leading to redundant feature extraction and hindering the reconstructive performance of the network. Finally, a DEM is employed by a combination of pyramid pooling and resblock group, which guides the adaptive fusion of latent features, where different details and plausible appearances are integrated. Experimental results on public datasets show that this method is effective and superior in the metrics of structure similarity (SSIM), peak-signal-to-noise ratio, multiscale-SSIM, and root-mean-square error.
Estimating competition in metacommunities: accounting for biases caused by dispersal

Estimating the strength of interactions among species in natural communities has always been a challenge for empirical ecologists. Sessile organisms, like plants or corals, often occur in metacommunities where they compete only with their immediate neighbours but disperse propagules over a wider area. To estimate the strength of competitive interactions, ecologists often count abundances in cells on a spatial grid for at least two time‐points. This data is then analysed using regression, by modelling the change in population size as a function of local densities, using cells as independent data‐points: a technique known as space‐for‐time substitution. These analyses generate estimates of competition coefficients; however, the method ignores dispersal among cells. To determine the impact of ignoring dispersal, we derived the bias that would arise when we apply regression methods to a metacommunity in which a fraction of seeds disperse beyond their natal cells but this dispersal is ignored in the model fitting process. We present results from a range of population models that make different assumptions about the nature of competition and assess the performance of our bias formulae by analysing data from simulated metacommunities. We reveal that: estimates of competition coefficients are biased when dispersal is not properly accounted for; and the resulting bias is often correlated with abundance, with rare species suffering the greatest overestimation. We also provide a standardized metric of competition that allows the bias to be calculated for a broad range of other population models. Our study suggests that regression methods that ignore dispersal produce biased estimates of competition coefficients when using space‐for‐time substitution. Our analytical bias formula allows empirical ecologists to potentially correct for biases, but it requires either tailored experiments in controlled conditions or an estimate of the average dispersal rate in a natural community, so may be challenging to apply to real datasets.
Casimir-Polder repulsion: Polarizable atoms, cylinders, spheres, and ellipsoids

Recently, the topic of Casimir repulsion has received a great deal of attention, largely because of the possibility of technological application. The general subject has a long history, going back to the self-repulsion of a conducting spherical shell and the repulsion between a perfect electric conductor and a perfect magnetic conductor. Recently it has been observed that repulsion can be achieved between ordinary conducting bodies, provided sufficient anisotropy is present. For example, an anisotropic polarizable atom can be repelled near an aperture in a conducting plate. Here we provide new examples of this effect, including the repulsion on such an atom moving on a trajectory nonintersecting a conducting cylinder; in contrast, such repulsion does not occur outside a sphere. Classically, repulsion does occur between a conducting ellipsoid placed in a uniform electric field and an electric dipole. The Casimir-Polder force between an anisotropic atom and an anisotropic dielectric semispace does not exhibit repulsion. The general systematics of repulsion are becoming clear.
Dynamic Response in a Finite Size Composite Multiferroic Thin Film

Composite multiferroics, heterostructures of ferromagnetic (FM) and ferroelectric (FE) materials, are characterized by a remarkable magnetoelectric effect at the interface. Previous work has supported the ferromagnetic structure with magnetic spins and the ferroelectric with pseudospins which act as electric dipoles in a microscopic model, coupled with a magnetoelectric interaction [J. Appl. Phys. 118, 124109 (2015)]. In this work, by solving the stochastic Landau-Lifshitz-Gilbert equation, the electric-field-induced magnetization switching in a twisted boundary condition has been studied, and a behavior of domain wall in the ferromagnetic structure is discussed.
Globular cluster scale sizes in giant galaxies: orbital anisotropy and tidally underfilling clusters in M87, NGC 1399 and NGC 5128

We investigate the shallow increase in globular cluster half-light radii with projected galactocentric distance $R_{gc}$ observed in the giant galaxies M87, NGC 1399, and NGC 5128. To model the trend in each galaxy, we explore the effects of orbital anisotropy and tidally under-filling clusters. While a strong degeneracy exists between the two parameters, we use kinematic studies to help constrain the distance $R_\beta$ beyond which cluster orbits become anisotropic, as well as the distance $R_{f\alpha}$ beyond which clusters are tidally under-filling. For M87 we find $R_\beta > 27$ kpc and $20 13$ kpc and $10 5$ kpc and $R_{f\alpha} > 30$ kpc. While we cannot rule out a dependence on $R_{gc}$, NGC 5128 is well fitted by a tidally filling cluster population with an isotropic distribution of orbits, suggesting it may have formed via an initial fast accretion phase. Perturbations from the surrounding environment may also affect a galaxy's orbital anisotropy profile, as outer clusters in M87 and NGC 1399 have primarily radial orbits while outer NGC 5128 clusters remain isotropic.
MULTIPLE-PLANET SCATTERING AND THE ORIGIN OF HOT JUPITERS

Doppler and transit observations of exoplanets show a pile-up of Jupiter-size planets in orbits with a 3 day period. A fraction of these hot Jupiters have retrograde orbits with respect to the parent star's rotation, as evidenced by the measurements of the Rossiter–McLaughlin effect. To explain these observations we performed a series of numerical integrations of planet scattering followed by the tidal circularization and migration of planets that evolved into highly eccentric orbits. We considered planetary systems having three and four planets initially placed in successive mean-motion resonances, although the angles were taken randomly to ensure orbital instability in short timescales. The simulations included the tidal and relativistic effects, and precession due to stellar oblateness. Our results show the formation of two distinct populations of hot Jupiters. The inner population (Population I) is characterized by semimajor axis a < 0.03 AU and mainly formed in the systems where no planetary ejections occurred. Our follow-up integrations showed that this population was transient, with most planets falling inside the Roche radius of the star in <1 Gyr. The outer population of hot Jupiters (Population II) formed in systems where at least one planet was ejected into interstellar space. This population survives the effects of tides over >1 Gyr and fits nicely the observed 3 day pile-up. A comparison between our three-planet and four-planet runs shows that the formation of hot Jupiters is more likely in systems with more initial planets. Due to the large-scale chaoticity that dominates the evolution, high eccentricities and/or high inclinations are generated mainly by close encounters between the planets and not by secular perturbations (Kozai or otherwise). The relative proportion of retrograde planets seems of be dependent on the stellar age. Both the distribution of almost aligned systems and the simulated 3 day pile-up also fit observations better in our four-planet simulations. This may suggest that the planetary systems with observed hot Jupiters were originally rich in the number of planets, some of which were ejected. In a broad perspective, our work therefore hints on an unexpected link between the hot Jupiters and recently discovered free floating planets.
Breakdown of separability due to confinement, submitted to Report on mathematical physics

A simple system of two particles in a bidimensional configurational space $S$ is studied. The possibility of breaking in $S$ the time independent Schr\"{o}dinger equation of the system into two separated one-dimensional one-body Schr\"{o}dinger equations is assumed. In this paper, we focus on how the latter property is countered by imposing such boundary conditions as confinement in a limited region of $S$ and/or restrictions on the joint coordinate probability density stemming from the sign-invariance condition of the relative coordinate (an impenetrability condition). Our investigation demonstrates the reducibility of the problem under scrutiny into that of a single particle living in a limited domain of its bidimensional configurational space. These general ideas are illustrated introducing the coordinates $X_c$ and $x$ of the center of mass of two particles and of the associated relative motion, respectively. The effects of the confinement and the impenetrability are then analyzed by studying with the help of an appropriate Green's function and the time evolution of the covariance of $X_c$ and $x$. Moreover, to calculate the state of the single particle constrained within a square, a rhombus, a triangle and a rectangle the Green's function expression in terms of Jacobi $\theta_3$-function is applied. All the results are illustrated by examples.
A NEW MAXIMUM-LIKELIHOOD TECHNIQUE FOR RECONSTRUCTING COSMIC-RAY ANISOTROPY AT ALL ANGULAR SCALES

The arrival directions of TeV–PeV cosmic rays show weak but significant anisotropies with relative intensities at the level of one per mille. Due to the smallness of the anisotropies, quantitative studies require careful disentanglement of detector effects from the observation. We discuss an iterative maximum-likelihood reconstruction that simultaneously fits cosmic-ray anisotropies and detector acceptance. The method does not rely on detector simulations and provides an optimal anisotropy reconstruction for ground-based cosmic-ray observatories located in the middle latitudes. It is particularly well suited to the recovery of the dipole anisotropy, which is a crucial observable for the study of cosmic-ray diffusion in our Galaxy. We also provide general analysis methods for recovering large- and small-scale anisotropies that take into account systematic effects of the observation by ground-based detectors.
Timing and Spectral Study of IGR J19294+1816 with the RXTE: The Discovery of Cyclotron Features

The Rossi X-Ray Timing Explorer/Proportional Counter Array (PCA) observations of IGR J19294+1816 covering two outburst episodes are reported. The first outburst happened during MJD 54921-54925 (2009 C.E.), and the second one happened during MJD 55499–55507 (2010 C.E.). In both cases, the PCA observations were made during the decay phase of the outburst, with the source exhibiting a temporal and spectral evolution with the change in flux. At the bright flux level, an absorption feature at 35.5 keV is detected in the spectra, which may be attributed to the Cyclotron Resonance Scattering Feature corresponding to a magnetic field of Gauss. This is also detected at a lower significance in two other observations. In addition, an Fe line emission at 6.4 keV is prominently detected during the highest flux. X-ray pulsations are detected in 9 out of 10 observations; no pulsations were found in the observation with the lowest flux level. During this observation with the lowest flux, the pulsation phenomenon becomes detectable only at the soft X-ray bands.
Limits of the quantum SO(3) representations for the one-holed torus

For $N \geq 2$, we study a certain sequence $(\rho_p^{(c_p)})$ of N-dimensional representations of the mapping class group of the one-holed torus arising from SO(3)-TQFT, and show that the conjecture of Andersen, Masbaum, and Ueno \cite{1} holds for these representations. This is done by proving that, in a certain basis and up to a rescaling, the matrices of these representations converge as $p$ tends to infinity. Moreover, the limits describe the action of $SL_{2}(\mathbb{Z})$ on the space of homogeneous polynomials of two variables of total degree $N-1$.
The fermion propagator in cosmological spaces with constant deceleration

We calculate the fermion propagator in Friedmann–Lemaître–Robertson–Walker (FLRW) spacetimes with constant deceleration for excited states. For fermions whose mass is generated by a scalar field through a Yukawa coupling m = gYϕ, we assume ϕ ∝ H. We first solve the mode functions by splitting the spinor into a direct product of helicity and chirality spinors. We also allow for non-vacuum states. We normalize the spinors using a consistent canonical quantization and by requiring orthogonality of particle and anti-particle spinors. We apply our propagator to calculate the one-loop effective action and renormalize using dimensional regularization. Since the Hubble parameter is now treated dynamically, this paves the way to study the dynamical backreaction of fermions on the background spacetime.
Physical and chemical conditions in methanol maser selected hot cores and UCH ii regions

We present the results of a targeted 3-mm spectral line survey towards the eighty-three 6.67GHz methanol maser selected star-forming clumps observed by Purcell. In addition to the previously reported measurements of HCO+(1-0), H13CO+(1-0) and CH3CN(5-4) and (6-5), we used the Mopra antenna to detect emission lines of N2H+(1-0), HCN(1-0) and HNC(1-0) towards 82/83 clumps (99 per cent), and CH3OH(2-1) towards 78/83 clumps (94 per cent). The molecular line data have been used to derive virial and local thermodynamic equilibrium masses, rotational temperatures and chemical abundances in the clumps, and these properties have been compared between subsamples associated with different indicators of evolution. The greatest differences are found between clumps associated with 8.6GHz radio emission, indicating the presence of an Ultra-Compact HII (UCHII) region, and `isolated' masers (without associated radio emission), and between clumps exhibiting CH3CN emission and those without. In particular, thermal CH3OH is found to be brighter and more abundant in UCHII regions and in sources with detected CH3CN, and may constitute a crude molecular clock in single dish observations. Clumps associated with 8.6GHz radio emission tend to be more massive and more luminous than clumps without radio emission. This is likely because the most massive clumps evolve so rapidly that a Hyper-Compact HII or UCHII region is the first visible tracer of star formation. The gas mass to submm/infrared luminosity relation for the combined sample was found to be L ~ M0.68, considerably shallower than expected for massive main-sequence stars. This implies that the mass of the clumps is comparable to, or greater than, the mass of the stellar content. We also find that the mass of the hot core is correlated with the mass of the clump in which it is embedded.
Young star clusters in circumnuclear starburst rings

We analyse the cluster luminosity functions (CLFs) of the youngest star clusters in three galaxies exhibiting prominent circumnuclear starburst rings. We focus specifically on NGC 1512 and NGC 6951, for which we have access to H$\alpha$ data that allow us to unambiguously identify the youngest sample clusters. To place our results on a firm statistical footing, we first explore in detail a number of important technical issues affecting the process from converting the observational data into the spectral-energy distributions of the objects in our final catalogues. The CLFs of the young clusters in both galaxies exhibit approximate power-law behaviour down to the 90 per cent observational completeness limits, thus showing that star cluster formation in the violent environments of starburst rings appears to proceed similarly as that elsewhere in the local Universe. We discuss this result in the context of the density of the interstellar medium in our starburst-ring galaxies.