Miracle-dz/UniFAR-FTUs huggingface dataset:
CHANDRA DEEP OBSERVATION OF XDCP J0044.0-2033, A MASSIVE GALAXY CLUSTER AT z > 1.5

We report the analysis of the Chandra observation of XDCP J0044.0-2033, a massive, distant (z = 1.579) galaxy cluster discovered in the XDCP survey. The total exposure time of 380 ks with Chandra ACIS-S provides the deepest X-ray observation currently achieved on a massive, high-redshift cluster. Extended emission from the intra cluster medium (ICM) is detected at a very high significance level (S/N ∼ 20) on a circular region with a 44″ radius, corresponding to Rext = 375 kpc at the cluster redshift. We perform an X-ray spectral fit of the ICM emission modeling the spectrum with a single-temperature thermal mekal model. Our analysis provides a global temperature keV, and a iron abundance (error bars correspond to 1σ). We fit the background-subtracted surface brightness profile with a single β-model out to 44″, finding a rather flat profile with no hints of a cool core. We derive the deprojected electron density profile and compute the ICM mass within the extraction radius Rext = 375 kpc to be MICM(r < Rext) = (1.48 ± 0.20) × 1013 M☉. Under the assumption of hydrostatic equilibrium and assuming isothermality within Rext, the total mass is for kpc. Extrapolating the profile at radii larger than the extraction radius Rext we find for kpc. This analysis establishes the existence of virialized, massive galaxy clusters at redshift z ∼ 1.6, paving the way to the investigation of the progenitors of the most massive clusters today. Given its mass and the XDCP survey volume, XDCP J0044.0-2033 does not create significant tension with the WMAP-7 ΛCDM cosmology.
Thermal Fluctuations and Bouncing Cosmologies

We study the conditions under which thermal fluctuations generated in the contracting phase of a non-singular bouncing cosmology can lead to a scale-invariant spectrum of cosmological fluctuations at late times in the expanding phase. We consider point particle gases, holographic gases and string gases. In the models thus identified, we also study the thermal non-Gaussianities of the resulting distribution of inhomogeneities. For regular point particle radiation, we find that the background must have an equation of state w = 7/3 in order to obtain a scale-invariant spectrum, and that the non-Gaussianities are suppressed on scales larger than the thermal wavelength. For Gibbons-Hawking radiation, we find that a matter-dominated background yields scale-invariance, and that the non-Gaussianities are large. String gases are also briefly considered.
Neuromuscular organization and haptoral armament of Polyclithrum ponticum (Monogenea: Gyrodactylidae)

Abstract Most gyrodactylids have a haptor armed with a pair of hamuli, two connecting bars and 16 marginal hooks. In some gyrodactylids, however, the haptor is disc-shaped and reinforced by additional sclerites. The genus Polyclithrum has arguably the most elaborate haptor in this group. This study aimed to gain better understanding of the anatomy of Polyclithrum by examining neuromusculature and haptoral armament of Polyclithrum ponticum, a species parasitizing Mugil cephalus in the Black Sea, with emphasis on haptoral sclerites and musculature in connection with host-attachment mechanisms. Musculature was stained by phalloidin, the nervous system by anti-serotonin and anti-FMRFamide antibodies, and haptoral sclerites were visualized in reflected light. The study provided new information on sclerites: in addition to previously described supplementary sclerites (A1–6), ear-shaped sclerites (ESSs) and two paired groups of ribs, reflected light revealed a rod-shaped process on the ESSs and a pair of small posterior sclerites. The sclerites were shown to be operated by 16 muscles, the most prominent of which were two transverse muscles connecting the hamular roots, three muscles attached to sclerite A2, the muscle fibres of anterior ribs and a set of extrinsic muscles. The nervous system consists of a pair of cerebral ganglia connected by a commissure and three pairs of nerve cords that unite in the haptor to form a loop between the opposite cords. The arrangement of sclerites and muscles suggests that Polyclithrum initiates the attachment by clamping a host's surface with longitudinally folded haptor and then secures its position with marginal hooks.
Coherent state, local excitation in 2D conformal field theory

In this paper we discuss the topics concerning the local excitation and coherent state in 2D CFT. It is shown that the local excitation of primary operator can be taken as a coherent state of the global conformal group. We also discuss the entanglement property of such state. For rational CFT the entanglement entropy between the holomorphic and anti-holomorphic sector of the local excitation of some primary operator is related to the quantum dimension of the operator, consistent with previous approach, but by a differentmethod. We comment on the possible application of so-defined group coherent state in the holographic view. We also study the coherent state in the free massless boson field, their time evolution and entanglement property. We introduce the deformed local excitation and the entangled state constructed by them. It is shown the violation of Bell inequality for such entangled state.
The Halo Occupation Distribution of Black Holes: Dependence on Mass

We investigate the halo occupation distribution (HOD) of black holes within a hydrodynamic cosmological simulation that directly follows black hole growth. Similar to the HOD of galaxies/subhalos, we find that the black hole occupation number can be described by the form N_BH proportional to 1+ (M_Host)^alpha where alpha evolves mildly with redshift indicating that a given mass halo (M_Host) at low redshift tends to host fewer BHs than at high redshift (as expected as a result of galaxy and BH mergers). We further divide the occupation number into contributions from black holes residing in central and satellite galaxies within a halo. The distribution of M_BH within halos tends to consist of a single massive BH (distributed about a peak mass strongly correlated with M_Host), and a collection of relatively low-mass secondary BHs, with weaker correlation with M_Host. We also examine the spatial distribution of BHs within their host halos, and find they typically follow a power-law radial distribution (i.e. much more centrally concentrated than the subhalo distribution). Finally, we characterize the host mass for which BH growth is feedback dominated (e.g. star formation quenched). We show that halos with M_Host > 3 * 10^12 M_sun have primary BHs that are feedback dominated by z~3 with lower mass halos becoming increasingly more affected at lower redshift.
Off the beaten path: a new approach to realistically model the orbital decay of supermassive black holes in galaxy formation simulations

We introduce a force correction term to better model the dynamical friction (DF) experienced by a supermassive black hole (SMBH) as it orbits within its host galaxy. This new approach accurately follows the orbital decay of a SMBH and drastically improves over commonly used advection methods. The force correction introduced here naturally scales with the force resolution of the simulation and converges as resolution is increased. In controlled experiments we show how the orbital decay of the SMBH closely follows analytical predictions when particle masses are significantly smaller than that of the SMBH. In a cosmological simulation of the assembly of a small galaxy, we show how our method allows for realistic black hole orbits. This approach overcomes the limitations of the advection scheme, where black holes are rapidly and artificially pushed toward the halo center and then forced to merge, regardless of their orbits. We find that SMBHs from merging dwarf galaxies can spend significant time away from the center of the remnant galaxy. Improving the modeling of SMBH orbital decay will help in making robust predictions of the growth, detectability, and merger rates of SMBHs, especially at low galaxy masses or at high redshift.
Why Are Inﬂation and Real Interest Rates So Low? A Mechanism of Low and Floating Real Interest and Inﬂation Rates

Real interest and inflation rates have been very low in many industrialized countries since the Great Recession. In this paper, a mechanism of low and floating real interest and inflation rates is examined based on the concept a “Nash equilibrium of a Pareto inefficient path” and the law of motion for trend inflation. I show that, because the link between the marginal product of capital and the real interest rate is severed on this path, the real interest rate loses its anchor and therefore floats. In addition, the inflation rate floats together with the real interest rate. There are, however, upper and lower bounds of the floating rates. It is also likely that the real interest rate floats below the marginal product of capital on this path and the inflation rate floats below the target rate of inflation.
Optical and Magnetic Properties of Dust Grains

The optical and magnetic properties of dust grains are reviewed, as they relate to the problem of interstellar grain alignment. Grain geometry plays an important role in determining the optical properties, and scattering and absorption of starlight will produce radiative torques which may drive grains to suprathermal rates of rotation in interstellar clouds; these radiative torques appear likely to play an active role in the alignment process. The likely magnetic properties of grains are discussed, with particular attention to the imaginary part of the magnetic susceptibility.
EVOLUTION OF COLD STREAMS AND THE EMERGENCE OF THE HUBBLE SEQUENCE

A new physical framework for the emergence of the Hubble sequence is outlined, based on novel analyses performed to quantify the evolution of cold streams of a large sample of galaxies from a state-of-the-art ultra-high resolution, large-scale adaptive mesh-refinement hydrodynamic simulation in a fully cosmological setting. It is found that the following three key physical variables of galactic cold inflows crossing the virial sphere substantially decrease with decreasing redshift: the number of streams N90 that make up 90% of concurrent inflow mass flux, average inflow rate per stream and mean (mass flux weighted) gas density in the streams ngas. Another key variable, the stream dimensionless angular momentum parameter λ, is found to instead increase with decreasing redshift. Assimilating these trends and others naturally leads to a physically coherent scenario for the emergence of the Hubble sequence, including the following expectations: (1) the predominance of a mixture of disproportionately small irregular and complex disk galaxies at z ⩾ 2 when most galaxies have multiple concurrent streams, (2) the beginning of the appearance of flocculent spirals at z ∼ 1–2 when the number of concurrent streams are about 2–3, (3) the grand-design spiral galaxies appear at z ⩽ 1 when galaxies with only one major cold stream significantly emerge. These expected general trends are in good accord with observations. Early-type galaxies are those that have entered a perennial state of zero cold gas stream, with their abundance increasing with decreasing redshift.
Area efficient GF(p) architectures for GF(p/sup m/) multipliers

This contribution describes new GF(p) multipliers, for p>2, specially suited for GF(p/sup m/) multiplication. We construct truth tables whose inputs are the bits of the multiplicand and multiplier and whose output are the bits that represent the modular product. However, contrary to previous approaches, we do not represent the elements of GF(p) in the normal binary positional system. Rather, we choose a representation which minimizes the resulting Boolean function. We obtain improvements of up to 35% in area when compared to previous approaches for small odd prime fields. We report transistor counts for all multipliers with p<2/sup 5/ which we obtained through the SIS sequential circuit synthesis program.
CONSTRAINTS ON THE INTERGALACTIC MAGNETIC FIELD WITH GAMMA-RAY OBSERVATIONS OF BLAZARS

Distant BL Lacertae objects emit γ-rays that interact with the extragalactic background light (EBL), creating electron–positron pairs, and reducing the flux measured by ground-based imaging atmospheric Cherenkov telescopes (IACTs) at very-high energies (VHE). These pairs can Compton-scatter the cosmic microwave background, creating a γ-ray signature at slightly lower energies that is observable by the Fermi Large Area Telescope (LAT). This signal is strongly dependent on the intergalactic magnetic field (IGMF) strength (B) and its coherence length (LB). We use IACT spectra taken from the literature for 5 VHE-detected BL Lac objects and combine them with LAT spectra for these sources to constrain these IGMF parameters. Low B values can be ruled out by the constraint that the cascade flux cannot exceed that observed by the LAT. High values of B can be ruled out from the constraint that the EBL-deabsorbed IACT spectrum cannot be greater than the LAT spectrum extrapolated into the VHE band, unless the cascade spectrum contributes a sizable fraction of the LAT flux. We rule out low B values (B ≲ 10−19 G for LB ≥ 1 Mpc) at >5σ in all trials with different EBL models and data selection, except when using >1 GeV spectra and the lowest EBL models. We were not able to constrain high values of B.
Efficient Augmented Inverse Probability Weighted Estimation in Missing Data Problems

When analyzing data with missing data, a commonly used method is the inverse probability weighting (IPW) method, which reweights estimating equations with propensity scores. The popularity of the IPW method is due to its simplicity. However, it is often being criticized for being inefficient because most of the information from the incomplete observations is not used. Alternatively, the regression method is known to be efficient but is nonrobust to the misspecification of the regression function. In this article, we propose a novel way of optimally combining the propensity score function and the regression model. The resulting estimating equation enjoys the properties of robustness against misspecification of either the propensity score or the regression function, as well as being locally semiparametric efficient. We demonstrate analytically situations where our method leads to a more efficient estimator than some of its competitors. In a simulation study, we show the new method compares favorably with its competitors in finite samples. Supplementary materials for this article are available online.
Voluntary HIV Counselling and Testing Services: Knowledge, Attitudes, and Correlates of Utilisation among Young People in the Tema Metropolis, Ghana

Voluntary HIV counselling and testing (VHCT) is a successful intervention for fostering early HIV detection, which is essential for the management of the disease. This study sought to determine the prevalence and factors that influence the utilization of VHCT services among young people. In this study, young people in the Tema Metropolis were cross-sectionally surveyed. The simple random sampling method was used to select the participants. The majority (60%) of the participants were unaware of VHCT, and 83% did not know of any VHCT centre. The majority (72%) of the participants indicated that VHCT was important, and 81% were willing to test for HIV if VHCT services were available in schools. Young people who knew that parental consent was not a requirement during VHCT were about two times more likely to have been tested for HIV (COR = 1.96; 95% CI: 1.05–3.63) compared to their counterparts. Additionally, young people who were willing to test in youth-friendly clinics (AOR = 2.87; 95% CI: 1.09–7.51) had higher odds of testing for HIV compared to their counterparts. The utilisation of VHCT services among young people in Tema was found to be very low. Additionally, young people’s knowledge of VHCT services was below expectations.
THE PROPERTIES OF DYNAMICALLY EJECTED RUNAWAY AND HYPER-RUNAWAY STARS

Runaway stars are stars observed to have large peculiar velocities. Two mechanisms are thought to contribute to the ejection of runaway stars, both of which involve binarity (or higher multiplicity). In the binary supernova scenario, a runaway star receives its velocity when its binary massive companion explodes as a supernova (SN). In the alternative dynamical ejection scenario, runaway stars are formed through gravitational interactions between stars and binaries in dense, compact clusters or cluster cores. Here we study the ejection scenario. We make use of extensive N-body simulations of massive clusters, as well as analytic arguments, in order to characterize the expected ejection velocity distribution of runaway stars. We find that the ejection velocity distribution of the fastest runaways (v ≳ 80 km s−1) depends on the binary distribution in the cluster, consistent with our analytic toy model, whereas the distribution of lower velocity runaways appears independent of the binaries' properties. For a realistic log constant distribution of binary separations, we find the velocity distribution to follow a simple power law: Γ(v)∝v−8/3 for the high-velocity runaways and v−3/2 for the low-velocity ones. We calculate the total expected ejection rates of runaway stars from our simulated massive clusters and explore their mass function and their binarity. The mass function of runaway stars is biased toward high masses and strongly depends on their velocity. The binarity of runaways is a decreasing function of their ejection velocity, with no binaries expected to be ejected with v > 150 km s−1. We also find that hyper-runaways with velocities of hundreds of km s−1 can be dynamically ejected from stellar clusters, but only at very low rates, which cannot account for a significant fraction of the observed population of hyper-velocity stars in the Galactic halo.
On localization sequences in the algebraic K-theory of ring spectra

We identify the $K$-theoretic fiber of a localization of ring spectra in terms of the $K$-theory of the endomorphism algebra spectrum of a Koszul-type complex. Using this identification, we provide a negative answer to a question of Rognes for $n>1$ by comparing the traces of the fiber of the map $K(BP(n))\rightarrow K(E(n))$ and of $K(BP(n-1))$ in rational topological Hochschild homology.
Full-sky weak-lensing simulation with 70 billion particles

We have performed a 70 billion dark-matter particles N-body simulation in a 2 h −1 Gpc periodic box, using the concordance, cosmological model as favored by the latest WMAP3 results. We have computed a full-sky convergence map with a resolution of Δθ � 0.74 arcmin 2 , spanning 4 orders of magnitude in angular dynamical range. Using various high-order statistics on a realistic cut sky, we have characterized the transition from the linear to the nonlinear regime at � � 1000 and shown that realistic galactic masking affects high-order moments only below �< 200. Each domain (Gaussian and non-Gaussian) spans 2 decades in angular scale. This map is therefore an ideal tool for testing map-making algorithms on the sphere. As a first step in addressing the full map reconstruction problem, we have benchmarked in this paper two denoising methods: 1) Wiener filtering applied to the Spherical Harmonics decomposition of the map and 2) a new method, called MRLens, based on the modification of the Maximum Entropy Method on a Wavelet decomposition. While the latter is optimal on large spatial scales, where the signal is Gaussian, MRLens outperforms the Wiener method on small spatial scales, where the signal is highly non-Gaussian. The simulated full-sky convergence map is freely available to the community to help the development of new map-making algorithms dedicated to the next generation of weak-lensing surveys.
Revisiting the Kitaev material candidacy of 
Ir4+
 double perovskite iridates

Kitaev materials, based on bond-directional Ising interactions, offer an intriguing platform for hosting exotic magnetic ground states and excitations. Significant Kitaev interactions are most commonly realized in heavy transition metal magnets with so-called ${J}_{\mathrm{eff}}$ = \textonehalf{} electronic ground states for the transition metal and local geometries consisting of metal-ligand edge-sharing octahedra. Here, the authors show that Kitaev materials can also be realized in ${J}_{\mathrm{eff}}$ = \textonehalf{} magnets via extended superexchange pathways mediated by more than one anion.
Systematic Review of Fitbit Charge 2 Validation Studies for Exercise Tracking

ABSTRACT Context There are research-grade devices that have been validated to measure either heart rate (HR) by electrocardiography with a Polar chest strap or step count with ActiGraph accelerometer. However, wearable activity trackers that measure HR and steps concurrently have been tested against research-grade accelerometers and HR monitors with conflicting results. This review examines validation studies of the Fitbit Charge 2 (FBC2) for accuracy in measuring HR and step count and evaluates the device’s reliability for use by researchers and clinicians. Design This registered review was conducted using the Preferred Reporting Items for Systematic Reviews and Meta-Analyses guidelines. The risk-of-bias visualization (robvis) tool was used to assess the strength of each considered article. Eligibility Criteria Eligible articles published between 2018 and 2019 were identified using PubMed, the Cumulative Index to Nursing and Allied Health Literature, Embase, Cochran, and World of Science databases and hand searches. All articles were HR and/or step count validation studies for the FBC2 in adult ambulatory populations. Study Selection Eight articles were examined in accordance with the eligibility criteria alignment and agreement among the authors and research librarian. Main Outcome Measures Concordance correlation coefficients (CCC) were used to measure agreement between the tracker and criterion devices. Mean absolute percent error (MAPE) was used to average the individual absolute percent errors. Results Studies that measured CCC found that agreement between the FBC2 and criterion devices ranged between 26% and 92% for HR monitoring, decreasing in accuracy as exercise intensity increased. Inversely, CCC increased from 38% to 99% for step count when exercise intensity increased. HR error between MAPE was 9.21% to 68% and showed more error as exercise intensity increased. Step measurement error MAPE was 12% for healthy persons aged 24–72 yr but was reported at 46% in an older population with heart failure. Conclusions Relative agreement with criterion and low-to-moderate MAPE were consistent in most studies reviewed and support validation of the FBC2 to accurately measure HR at low or moderate exercise intensities. However, more investigation controlling testing and measurement congruency is needed to validate step capabilities. The literature supports the validity of the FBC2 to accurately monitor HR, but for step count, it is inconclusive, so the device may not be suitable for recommended use in all populations.