Miracle-dz/UniFAR-FTUs huggingface dataset:
Hamiltonian structure of Hořava gravity

The Hamiltonian formulation of Horava gravity is derived. In a closed universe the Hamiltonian is a sum of generators of gauge symmetries, the foliation-preserving diffeomorphisms, and vanishes on shell. The scalar constraint is second class, except for a global, first-class part that generates time reparametrizations. A reduced phase space formulation is given in which the local part of the scalar constraint is solved formally for the lapse as a function of the 3 metric and its conjugate momentum. In the infrared limit the scalar constraint is linear in the square root of the lapse. For asymptotically flat boundary conditions the Hamiltonian is a sum of bulk constraints plus a boundary term that gives the total energy. This energy expression is identical to the one for Einstein-aether theory which, for static spherically symmetric solutions, is the usual Arnowitt-Deser-Misner energy of general relativity with a rescaled Newton constant.
End-to-End Design of Bespoke, Dexterous Snake-Like Surgical Robots: A Case Study With the RAVEN II

Keyhole surgery requires highly dexterous snake-like robotic arms capable of bending around anatomical obstacles to access clinical targets that diverge from the direct port-of-access. Design optimization for these robots under patient-specific anatomical constraints is still lacking, particularly concerning the critical metric of dexterity. In this article, we propose an end-to-end design and production workflow for patient-specific surgical manipulators, assessing dexterity using orientability constrained by task space obstacles. In our work, parametric evolutionary optimization maximizes dexterity in patient-specific task spaces for challenging knee arthroscopy operations. We implement our framework in the design of SnakeRaven—a 3-D printed tool to be attached to the RAVEN II surgical robot in a phantom study for knee arthroscopy. The solution achieved more than three times the dexterity of a state-of-the-art rigid instrument and more than twice the dexterity of a volume-based approach for the same task. We further assemble and validate this design by teleoperating the robot to reach the desired clinical targets in a phantom. We also investigate the changes in the design morphology to changes in the task objectives and found an advantage in task specialization. We also observe guidelines for achieving a dexterous design produced by our algorithms.
Donors of Persistent Neutron-Star Low-Mass X-Ray Binaries

Properties of X-ray luminosities in low-mass X-ray binaries (LMXBs) mainly depend on donors. We have carried out a detailed study of donors in persistent neutron-star LMXBs (PLMXBs) by means of a population synthesis code. PLMXBs with different donors have different formation channels. Our numerical simulations show that more than 90% of PLMXBs have main-sequence (MS) donors, and PLMXBs with red giant (RG) donors via stellar wind (wind) are negligible. In our model, most of the neutron stars (NSs) in PLMXBs with hydrogen-rich donors form via core-collapse supernovae, while more than 90% of the NSs in PLMXBs with naked helium star (He) donors or white dwarf (WD) donors form via an evolution-induced collapse via helium star (1.4 ≤ MHe/M⊙ ≤ 2.5) or an accretion-induced collapse for an accreting ONeMg WD. PLMXBs with different donors have different properties. In PLMXBs with MS donors, the orbital periods are between ∼ 1 hr and 100 hr, and the mass transfer is driven by donor evolution or magnetic braking. Our population synthesis code shows that their X-ray luminosities are mainly around ∼ 10 36 ergs s - 1 . Similarly, in PLMXBs with RG donors via Roche lobe overflow (Roche), the mass transfer is driven by donor evolution, but orbital periods are between ∼ 10 hr and 1000 hr. Their X-ray luminosities are ∼ 10 37 ergs s - 1 . The two known LMXBs (Cyg X-2 and GX 13 + 1) can belong to PLMXBs with RG (Roche) donors. PLMXBs with RG (wind) donors have the longest orbital periods and low X-ray luminosities ( ∼ 10 33 ergs s - 1 ). Their contributions to X-ray luminosities can be negligible. In PLMXBs with He donors, the orbital periods are shorter than 80 minutes, and the mass transfer is mainly driven by magnetic braking. Results of our numerical simulations predict that PLMXBs with X-ray luminosities of ∼ 10 38 ergs s - 1 mainly come from binaries with He donors. In PLMXBs with WD donors, the orbital periods are shorter than 1 hr, and the mass transfer is mainly driven by gravitational radiation. According to results of our population synthesis code, their X-ray luminosities are between ∼6 × 1035 and 10 39 ergs s - 1 , and most of the LMXBs with WD donors are transient.
Quantification of ESD Pulses Caused by Collision of Objects

Well-insulated portable devices are exposed to field coupled impulsive ESDs if they are carried e.g., in a backpack. These pulses are created by tribo-charging of metallic objects as a result of movement and subsequent discharges. Due to the size of the metallic objects and low charge voltages, the frequency spectrum exceeds 5 GHz. The pulses can damage or upset devices. The paper quantifies the charge voltages and transient field strength by reproducing typical scenario and capturing transient fields with a bandwidth of more than 10 GHz. The charge voltages are estimated by comparing measurements to numerical modeling of the discharges.
Spectrophotometric Libraries, Revised Photonic Passbands, and Zero Points for UBVRI, Hipparcos, and Tycho Photometry

We have calculated improved photonic passbands for the UBVRI, Hipparcos Hp, and Tycho BT and VT standard systems using the extensive spectrophotometric libraries of NGSL and MILES. Using the Hp passband, we adjusted the absolute flux levels of stars in the spectrophotometric libraries so that their synthetic Hp magnitudes matched the precise Hipparcos Catalogue value. Synthetic photometry based on the renormalized fluxes was compared with the standard UBVRI, BT and VT magnitudes, and revised synthetic zero points were determined. The Hipparcos and Tycho photometry system zero points were also compared with the V-magnitude zero points of the SAAO UBVRI system, the homogenized UBV system, and the Walraven VB system. The confusion in the literature concerning broadband magnitudes, fluxes, passbands, and the choice of appropriate mean wavelengths is detailed and discussed in the Appendix.
PRECIPITATION-REGULATED STAR FORMATION IN GALAXIES

Galaxy growth depends critically on the interplay between radiative cooling of cosmic gas and the resulting energetic feedback that cooling triggers. This interplay has proven exceedingly difficult to model, even with large supercomputer simulations, because of its complexity. Nevertheless, real galaxies are observed to obey simple scaling relations among their primary observable characteristics. Here we show that a generic emergent property of the interplay between cooling and feedback can explain the observed scaling relationships between a galaxyʼs stellar mass, its total mass, and its chemical enrichment level, as well as the relationship between the average orbital velocity of its stars and the mass of its central black hole. These relationships naturally result from any feedback mechanism that strongly heats a galaxyʼs circumgalactic gas in response to precipitation of colder clouds out of that gas, because feedback then suspends the gas in a marginally precipitating state.
Cache Size Effects and Content Request in Spatially Dispersed Caching Strategy

The design of Information-Centric Networking (ICN) technology aims to create a reliable network that can meet the present and future needs. Nowadays, almost every aspect of data exchanges uses the internet, which the ICN is an important technology for the internet. One of the strategic models for ICN have been created is Spatially Dispersed Caching (SDC). Thus, this strategy, groups content based on unique names to dispersed spatially. And, the more popular content will be cached in many routers. Finally, in this study will further deepen the SDC strategy and analyze the cache hit values by changing the value of several parameters, namely the number of users, cache size, and content requests. In addition, have been found that the parameter more effect on the cache hit is the cache size, where the increase in cache size correlates by 45% against the increase in a cache hit. While the increase in the number of users and content requests only have a proportion of the increase in cache hits by 22% and 32%. Meanwhile, the effect of the number of users, cache size, and content requests on cache hits is fixed even though it has been experimented by changing the topology, but for the results of path stretch, topology changes have an effect where the second topology with average value 1.76 will always be better than the first topology with average value 2.7 because the second topology has two nodes that are directly connected to the user so that it will make content delivery more effective.
Impact Estimation of Emergency Events Using Social Media Streams

In recent years, Social Media platforms have attracted millions of users, becoming a primary communication channel. They offer the possibility to massively ingest and instantly share big volumes of user-generated content before, during, and after emergency events. Being able to accurately quantity the impact of such hazardous events could greatly help all organizations involved in the emergency management cycle to adequately plan the required recovery operations. In this work, we propose a novel Natural Language Processing approach built on rule-based algorithms able to estimate, from tweets posted during natural hazards, the impact of emergency events in terms of affected population and infrastructures. We implement our approach in an operational environment and present its validation on a publicly released dataset of more than 1.4K manually annotated tweets, showing an overall weighted F1 score of 0.77.
Numerical Investigation to Improve the Performance of Induction Heating Oven for Tyre Mould Preheating

This paper presents a numerical analysis of an industrial-scale induction heating oven to improve heat transfer performance for applications in the tyre manufacturing industry. Tyre mould preheating is a vital step in the tyre manufacturing process, for which the local industry is currently using conventional heating techniques. Research has shown that induction heating has the potential to significantly reduce the heating time and the energy use of the tyre mould preheating. However, some limitations in obtaining the required temperature profiles have prevented the local industry in moving toward induction heating. Hence, this research focused on using finite element analysis to study the induction heating process to propose an improved oven unit for tyre mould preheating. The simulation was conducted on a simplified and scaled-down model of a tyre mould to study the effects of key parameters. The simulation results showed that. The pancake type coils are recommended for the application and the maximum Ohmic losses could be obtained when the coil air gap is 7-8 mm.
Observed trend in the star formation history and the dark matter fraction of galaxies at redshift z ≈ 0.8

We study the star formation history for a sample of 154 galaxies with stellar mass $10^{10}\lesssim M_{\ast}\lesssim 10^{12} M_{\odot}$ in the redshift range $0.7 < z < 0.9$. We do this using stellar population models combined with full-spectrum fitting of good quality spectra and high resolution photometry. For a subset of 68 galaxies ($M_{\ast}\gtrsim 10^{11} M_{\odot}$) we additionally construct dynamical models. These use an axisymmetric solution to the Jeans equations, which allows for velocity anisotropy, and adopts results from abundance matching techniques to account for the dark matter content. We find that: (i) The trends in star formation history observed in the local universe are already in place by $z\sim1$: the most massive galaxies are already passive, while lower mass ones have a more extended star formation histories, and the lowest mass galaxies are actively forming stars; (ii) we place an upper limit of a factor 1.5 to the size growth of the massive galaxy population; (iii) we present strong evidence for low dark matter fractions within $1R_{\rm e}$ (median of 9 per cent and 90th percentile of 21 per cent) for galaxies with $M_{\ast} \gtrsim 10^{11} M_{\odot}$ at these redshifts; and (iv) we confirm that these galaxies have, on average, a Salpeter normalisation of the stellar initial mass function.
Lattice methods for quantum chromodynamics

Continuum QCD and Its Phenomenology Path Integration Renormalization and the Renormalization Group Yang-Mills Theory on the Lattice Fermions on the Lattice Numerical Methods for Bosons Numerical Methods for Fermions Data Analysis for Lattice Simulations Designing Lattice Actions Spectroscopy Lattice Perturbation Theory Operators with Anomalous Dimension Chiral Symmetry and Lattice Simulations Finite Volume Effects Testing the Standard Model with Lattice Calculations QCD at High Finite Temperature and Density.
MINOR MERGERS OR PROGENITOR BIAS? THE STELLAR AGES OF SMALL AND LARGE QUENCHED GALAXIES

We investigate the origin of the evolution of the population-averaged size of quenched galaxies (QGs) through a spectroscopic analysis of their stellar ages. This evolution has been claimed to arise from either the size growth of individual galaxies through a sequence of dry minor mergers, or the addition of larger, newly quenched galaxies to the pre-existing population (i.e., a progenitor bias effect). We use the 20k zCOSMOS-bright spectroscopic survey to select bona fide QGs at 0.2 < z < 0.8. We stack their spectra in bins of redshift, stellar mass, and size to compute stellar population parameters through fits to the rest-frame optical spectra and Lick indices. The size–age relation differs below and above ∼1011 M⊙: at , at all redshifts the stellar populations of the largest galaxies are younger than those of the smaller counterparts, indicating progenitor bias as the main driver of the average size evolution. In contrast, at higher masses, there is no clear size–age trend, supporting a substantial role of dry mergers in increasing with cosmic time the sizes of these most massive QGs. The [α/Fe] abundance ratios of QGs are (i) above-solar over the entire redshift range of our analysis, hinting at universally short timescales for the buildup of the stellar populations of QGs, and (ii) similar at all masses and sizes, suggesting similar (short) timescales for the whole QG population—and strengthening the role of mergers in the buildup of the most massive QGs in the universe.
Detecting extrasolar planets from stellar radial velocities using Bayesian evidence

Stellar radial velocity (RV) measurements have proven to be a very successful method for detecting extrasolar planets. Analysing RV data to determine the parameters of the extrasolar planets is a significant statistical challenge owing to the presence of multiple planets and various degeneracies between orbital parameters. Determining the number of planets favoured by the observed data is an even more difficult task. Bayesian model selection provides a mathematically rigorous solution to this problem by calculating marginal posterior probabilities of models with different number of planets, but the use of this method in extrasolar planetary searches has been hampered by the computational cost of the evaluating Bayesian evidence. None the less, Bayesian model selection has the potential to improve the interpretation of existing observational data and possibly detect yet undiscovered planets. We present a new and efficient Bayesian method for determining the number of extrasolar planets, as well as for inferring their orbital parameters, without having to calculate directly the Bayesian evidence for models containing a large number of planets. Instead, we work iteratively and at each iteration obtain a conservative lower limit on the odds ratio for the inclusion of an additional planet into the model. We apply this method to simulated data sets containing one and two planets and successfully recover the correct number of planets and reliable constraints on the orbital parameters. We also apply our method to RV measurements of HD 37124, 47 Ursae Majoris and HD 10180. For HD 37124, we confirm that the current data strongly favour a three-planet system. We find strong evidence for the presence of a fourth planet in 47 Ursae Majoris, but its orbital period is suspiciously close to 1 yr, casting doubt on its validity. For HD 10180 we find strong evidence for a six-planet system.
The expansion of massive young star clusters – observation meets theory

Most stars form as part of a star cluster. The most massive clusters in the Milky Way exist in two groups - loose and compact clusters - with significantly different sizes at the end of the star formation process. After their formation both types of clusters expand up to a factor 10-20 within the first 20 Myr. Gas expulsion at the end of the star formation process is usually regarded as only possible process that can lead to such an expansion.We investigate the effect of gas expulsion by a direct comparison between numerical models and observed clusters concentrating on clusters with masses >10^3 M(sun). For these clusters the initial conditions before gas expulsion, the characteristic cluster development, its dependence on cluster mass, and the star formation efficiency (SFE) are investigated. We perform N-body simulations of the cluster expansion process after gas expulsion and compare the results with observations. We find that the expansion processes of the observed loose and compact massive clusters are driven by completely different physical processes. As expected the expansion of loose massive clusters is largely driven by the gas loss due to the low SFE of ~30%. One new revelation is that all the observed massive clusters of this group seem to have a very similar size of 1-3 pc at the onset of expansion. It is demonstrated that compact clusters have a much higher effective SFE of 60-70% and are as a result much less affected by gas expulsion. Their expansion is mainly driven by stellar ejections caused by interactions between the cluster members. The reason why ejections are so efficient in driving cluster expansion is that they occur dominantly from the cluster centre and over an extended period of time. Thus during the first 10 Myr the internal dynamics of loose and compact clusters differ fundamentally.
THE EVOLUTION OF THE DUSTY TORUS COVERING FACTOR IN QUASARS

We have assembled a large sample of 5996 quasars at 2.0 ⩽ z ⩽ 2.4 (high-z) or 0.7 ⩽ z ⩽ 1.1 (low-z) from the Sloan Digital Sky Survey (SDSS) ninth and seventh data release and quasar catalogs. The spectral energy distributions of quasars were constructed by collecting WISE, UKIDSS, and GALEX photometric data in addition to SDSS data, from which the IR luminosity at 1–7 μm and bolometric luminosity at 1100 Å–1 μm were calculated. A red tail is clearly seen in the distribution of the spectral index over 1100 Å–1 μm for both the high-z and low-z sources; this tail is likely due to red or reddened quasars. The covering factor (CF) of the dusty torus is estimated as the ratio of the IR luminosity to the bolometric luminosity. We find significant anti-correlations between the CF and the bolometric luminosity, in both the high-z and low-z quasars; however, these two groups follow different tracks. At overlapping bolometric luminosities, the CF of high-z quasars is systematically larger than those of low-z quasars, implying an evolution of the CF with redshift.
Application of organic and inorganic fertilizer against results onion plants with chillies

Intercropping is a crop cultivation system where more than one plant is planted in one planting area, this is used to maximize land function and increase farmers' income. The aim of the study was to obtain the response of growth and yield of intercropping to reducing doses of inorganic fertilizers with organic fertilizers, in order to obtain the optimal dosage mix. The research was conducted in rice fields in Subak Rapuan, Banjar Tarukan, Mas Village, Ubud, Gianyar. This experiment is a factorial experiment with a Randomized Block Design (RAK) which consists of two factors, namely organic fertilizer kerambitan agro (K) consisting of 4 levels: K0 = 0 ton.ha-1; K1 = 10 ton.ha-1 ; K2 = 20 ton.ha-1; K3 = 30 ton.ha-1and the dose of NPK Mutiara fertilizer consisted of 3 levels, namely N1= 100 kg.ha-1 ; N2= 200 kg.ha-1 N3= 300 kg.ha-1 . The results showed that the interaction of organic fertilizers with inorganic fertilizers had no significant effect (P≥0.05) on all observed variables.
A Statistical Overview of Convection During the First CPEA Campaign( CPEA-Coupling Processes in the Equatorial Atmosphere)

Data from the Equatorial Atmosphere Radar (EAR) were analysed during the Coupling Processes in the Equatorial Atmosphere (CPEA) campaign of April-May 2004. Statistical averages of the daily perturbations of wind velocity, temperature and humidity were examined. In the lower stratosphere, horizontal wind variances of up to 1.5 m 2 s -2 were visible above the afternoon tropospheric convection. Vertical wind variances of up to 0.03 m 2 s -2 occurred at the same time. The average variances of temperature and humidity in the lower troposphere also increased in the afternoon. Estimates of average momentum flux were made. In the lower stratosphere (18.0-20.0 km), the average magnitudes were 0.7-0.9 m 2 s -2 for both |u'w'| and |u'w'|. These fluxes were observed above the convective cells and indicate the average momentum emitted by them. Residuals of the momentum flux components showed a small westward preference and very small northward directional preference for wave propagation during CPEA. Four individual convective events and three Super Cloud Clusters (SCCs) were examined in detail. Tropospheric horizontal and vertical wind variances increased by 5 to 10 times during intense convection. Directly above this convection, in the lower stratosphere, increases in variance were also recorded. Vertical wind velocity fluctuation amplitudes in the lower stratosphere increased from 0.05-0.1 ms -1 away from convection, to be 0.1-0.4 ms -1 during convection. The amplitudes decreased to their background levels as soon as the convection had passed the EAR site. In the lower troposphere, the virtual temperature perturbations increased to 1.0-2.0°C during convection, an increase from a background value of about 0.5°C. During two of the four individual events, the amplitude of the temperature perturbations stayed enhanced for several hours after the end of convection. This contrasts with the vertical velocities in the lower troposphere, which quickly decreased following the passage of the storms. Specific humidity profiles in most cases showed large increases in the amount of water vapour below 4 km during times of convection. At certain heights and times during intense convection, the specific humidity increased by up to 50% from its background level.
VARIABLE STARS IN METAL-RICH GLOBULAR CLUSTERS. IV. LONG-PERIOD VARIABLES IN NGC 6496

We present VI-band photometry for stars in the metal-rich globular cluster NGC 6496. Our time-series data were cadenced to search for long-period variables (LPVs) over a span of nearly two years, and our variability search yielded the discovery of 13 new variable stars, of which 6 are LPVs, 2 are suspected LPVs, and 5 are short-period eclipsing binaries. An additional star was found in the ASAS database, and we clarify its type and period. We argue that all of the eclipsing binaries are field stars, while five to six of the LPVs are members of NGC 6496. We compare the period–luminosity distribution of these LPVs with those of LPVs in the Large Magellanic Cloud and 47 Tucanae, and with theoretical pulsation models. We also present a VI color–magnitude diagram, display the evolutionary states of the variables, and match isochrones to determine a reddening of E ( B − V ) = 0.21 ± 0.02 mag ? > and apparent distance modulus of 15.60 ± 0.15 ? > mag.