Miracle-dz/UniFAR-FTUs huggingface dataset:
Two physical regimes for the giant H ii regions and giant molecular clouds in the Antennae galaxies

We have combined observations of the Antennae galaxies from the radio interferometer ALMA (Atacama Large Millimeter/submillimeter Array) and from the optical interferometer GH$\alpha$FaS (Galaxy H$\alpha$ Fabry-Perot System). The two sets of observations have comparable angular and spectral resolutions, enabling us to identify 142 giant molecular clouds (GMCs) and 303 HII regions. We have measured, and compared, their basic physical properties (radius, velocity dispersion, luminosity). For the HII regions, we find two physical regimes, one for masses $>10^{5.4} \mathrm{M_{\odot}}$ of ionized gas, where the gas density increases with gas mass, the other for masses $<10^{5.4} \mathrm{M_{\odot}}$ of ionized gas, where the gas density decreases with gas mass. For the GMCs, we find, in contrast to previous studies in other galaxies over a generally lower mass range of clouds, that the gas surface density increases with the radius, hinting at two regimes for these clouds if we consider both sources of data. We also find that the GMC mass function has a break at $10^{6.7}\mathrm{M_{\odot}}$. Using the velocity dispersion measurements, we claim that the difference between the regimes is the nature of the dominant binding force. For the regions in the lower mass range, the dominant force is the external pressure, while in the higher mass range it is the internal gravity of the clouds. In the regime where gravity is dominant, the star formation rate, derived from the dust-corrected H$\alpha$ luminosity, increases super-linearly with the velocity dispersion, and the gas density increases with the gas mass.
The Incompressible Rindler fluid versus the Schwarzschild-AdS fluid

The incompressible Rindler fluid versus the Schwarzschild–AdS fluid Yoshinori Matsuo1, Makoto Natsuume1,2,∗, Masahiro Ohta1,2, and Takashi Okamura3 1KEK Theory Center, Institute of Particle and Nuclear Studies, High Energy Accelerator Research Organization, Tsukuba, Ibaraki 305-0801, Japan 2Department of Particle and Nuclear Physics, The Graduate University for Advanced Studies, Tsukuba, Ibaraki 305-0801, Japan 3Department of Physics, Kwansei Gakuin University, Sanda, Hyogo 669-1337, Japan ∗E-mail: makoto.natsuume@kek.jp
An ultraviolet flux drop preceding the X‐ray hard‐to‐soft state transition during the 2010 outburst of GX 339−4

The black hole X-ray transient GX 339-4 was observed with the Swift satellite across the hard-to-soft state transition during its 2010 outburst. The ultraviolet (UV) flux measured with the filter UVW2 of the Swift/UVOT started to decrease nearly 10 days before the drop in the hard X-ray flux when the hard-to-soft state transition started. The UV flux, F-UV, correlated with the X-ray flux, F-X, as F-UV proportional to F-X(0.50 +/- 0.04) before the drop in the UV flux. During the UV drop lasting about 16 days, the X-ray flux in 0.410 keV was increasing. The drop in the UV flux indicates that the jet started to quench 10 days before the hard-to-soft state transition seen in X-rays, which is unexpected.
Drell-Yan lepton angular distributions in perturbative QCD

We present a comprehensive comparison of the available experimental data for the Drell-Yan lepton angular coefficients $\ensuremath{\lambda}$ and $\ensuremath{\nu}$ to calculations at leading and next-to-leading order of perturbative QCD. To obtain the next-to-leading order corrections, we make use of publicly available numerical codes that allow us to compute the Drell-Yan cross section at second order in perturbation theory and from which the contributions we need can be extracted. Our comparisons reveal that perturbative QCD is able to describe the experimental data overall rather well, especially at colliders, but also in the fixed-target regime. On the basis of the angular coefficients alone, there appears to be little (if any) convincing evidence for effects that go beyond fixed-order collinear factorized perturbation theory, although the presence of such effects is not ruled out.
The formation and evolution of small star clusters

Recent observations show that small, young, stellar groupings of � 10 to 40 members tend of have a centrally-located most massive member, reminiscent of mass segregation seen in large clustered systems. Here, we analyze hydrodynamic simulations which form small clusters and analyze their properties in a manner identical to the observations. We find that the simulated clusters possess similar properties to the observed clusters, including a tendency to exhibit mass segregation. In the simulations, the central location of the most massive member is not due to dynamical evolution, since there is little interaction between the cluster members. Instead, the most massive cluster member appears to form at the center. We also find that the more massive stars in the cluster form at slightly earlier times.
Ultrathin GaN nanowires: Electronic, thermal, and thermoelectric properties

We present a comprehensive computational study of the electronic, thermal, and thermoelectric (TE) proper- ties of gallium nitride nanowires (NWs) over a wide range of thicknesses (3-9 nm), doping densities (10 18 -10 20 cm 3 ), and temperatures (300-1000 K). We calculate the low-field electron mobility based on ensemble Monte Carlo transport simulation coupled with a self-consistent solution of the Poisson and Schrodinger equations. We use the relaxation-time approximation and a Poisson-Schro¨ dinger solver to calculate the electron Seebeck coefficient and thermal conductivity. Lattice thermal cond uctivity is calculated using a phonon ensemble Monte Carlo simulation, with a real-space rough surface described by a Gaussian autocorrelation function. Through- out the temperature range, the Seebeck coefficient increase s while the lattice thermal conductivity decreases with decreasing wire cross section, both boding well for TE applications of thin GaN NWs. However, at room temperature these benefits are eventually overcome by the de trimental effect of surface roughness scattering on the electron mobility in very thin NWs. The highest room-temperature ZT of 0.2 is achieved for 4-nm-thick NWs, while further downscaling degrades it. In contrast, at 1000 K, the electron mobility varies weakly with the NW thickness owing to the dominance of polar optical phonon scattering and multiple subbands contributing to transport, so ZT increases with increasing confinement, reaching 0.8 for opt imally doped 3-nm-thick NWs. The ZT of GaN NWs increases with increasing temperature beyond 1000 K, which further emphasizes their suitability for high-temperature TE applications. PACS numbers: 72.20. Pa, 84.60. Rb. ,73.63. Nm, 65.80-g
Sejong Open Cluster Survey (SOS) – III. The young open cluster NGC 1893 in the H ii region W8

We present a UBV I and H photometric study of the young open cluster NGC 1893 in the H II region W8 (IC 410 or Sh 2-236). A total of 65 early-type members are selected from photometric diagrams. A mean reddening of the stars ishE(B V )i = 0:563 0:083 mag. The published photometric data in the near- and mid-infrared passbands are used to test the reddening law toward the cluster, and we conrm that the reddening law is normal (RV = 3:1). Zero-age main sequence tting gives a distance modulus of V0 MV = 12:7 0:2 mag, equivalent to 3:5 0:3 kpc. From H photometry 125 H emission stars and candidates are identied as pre-main sequence (PMS). The lists of young stellar objects and X-ray sources published by previous studies allow us to select a large number of PMS members down to 1M . Isochrone tting in the Hertzsprung-Russell diagram gives a turn-o age of 1.5 Myr and the median age of 1.9 Myr from the PMS members with a spread of 5 Myr. We derive the initial mass function (IMF) for stars with mass larger than 1M . The slope of the IMF ( = 1:3 0:1) is well consistent with the Salpeter/Kroupa IMF. A total mass of the cluster appears to be in excess of 1,300 M . Finally, we estimate the mass accretion rate of 82 PMS members in the mass range of 0:6M to 5M .
X-RAYS FROM SUPERNOVA SHOCKS IN DENSE MASS LOSS

Type IIn and related supernovae show evidence for an interaction with a dense circumstellar medium that produces most of the supernova luminosity. X-ray emission from shock heated gas is crucial for the energetics of the interaction and can provide diagnostics on the shock interaction. Provided that the shock is at an optical depth τw ≲ c/vs in the wind, where c is the speed of light and vs is the shock velocity, a viscous shock is expected that heats the gas to a high temperature. For τw ≳ 1, the shock wave is in the cooling regime; inverse Compton cooling dominates bremsstrahlung at higher densities and shock velocities. Although τw ≳ 1, the optical depth through the emission zone is ≲ 1 so that inverse Compton effects do not give rise to significant X-ray emission. The electrons may not reach energy equipartition with the protons at higher shock velocities. As X-rays move out through the cool wind, the higher energy photons are lost to Compton degradation. If bremsstrahlung dominates the cooling and Compton losses are small, the energetic radiation can completely photoionize the preshock gas. However, inverse Compton cooling in the hot region and Compton degradation in the wind reduce the ionizing flux, so that complete photoionization is not obtained and photoabsorption by the wind further reduces the escaping X-ray flux. We conjecture that the combination of these effects led to the low observed X-ray flux from the optically luminous SN 2006gy.
Suzaku Observation of the Intermediate Polar V1223 Sagittarii

We report on the Suzaku observation of the intermediate polar V1223 Sagittarii. Using a multi-temperature plasma emission model with its reflection from a cold matter, we obtained the shock temperature to be 37.9 +5:1 � 4:6 keV. This constrains the mass and the radius of the white dwarf (WD) in the ranges 0.82 +0:05 � 0:06 Mand (6.9˙0.4) � 10 8 cm, respectively, with the aid of a WD mass-radius relation. The solid angle of the reflector viewed from the post-shock plasma was measured to be Ω=2� = 0.91 ˙ 0.26. A fluorescent iron K˛ emission line was detected, whose central energy was discovered to be modulated with the WD rotation for the first time in magnetic-CVs. Detailed spectral analysis indicates that the line comprises a stable 6.4 keV component and a red-shifted component, the latter of which appears only around the rotational intensity-minimum phase. The equivalent width (EW )o f the former stable component, � 80 eV, together with the measured Ω indicates that the major reflector is the WD surface, and the shock height is not more than 7% of the WD radius. Comparing this limitation to the height predicted by the Aizu model (Aizu, 1973, Prog. Theor. Phys., 50, 344), we estimated the fractional area onto which the accretion occurs to be < 7 � 10 � 3 of the WD radius, which is the most severe constraint in non-eclipsing IPs. The red- shifted iron line component, on the other hand, can be interpreted as emanating from the pre-shock accretion flow
Cosmological Galaxy Evolution with Superbubble Feedback I: Realistic Galaxies with Moderate Feedback

We present the first cosmological galaxy evolved using the modern smoothed parti- cle hydrodynamics (SPH) code GASOLINE2 with superbubble feedback. We show that superbubble-driven galactic outflows powered by Type II supernovae alone can produce Lgalaxies with flat rotation curves with circular velocities � 200 km/s, low bulge-to-disc ratios, and stellar mass fractions that match observed values from high redshift to the present. These features are made possible by the high mass loadings generated by the evaporative growth of superbubbles. Outflows are driven extremely effectively at high redshift, expelling gas at early times and preventing overproduction of stars before z = 2. Centrally concentrated gas in previous simulations has often lead to unrealistically high bulge to total ratios and strongly peaked rotation curves. We show that supernova-powered superbubbles alone can produce galaxies that agree well with observed properties without the need for additional feedback mechanisms or in- creased feedback energy. We present additional results arising from properly modelled hot feedback.
Novel results for condensed matter systems with time reversal symmetry

The first half of the Thesis is dedicated to the study of the Spin Hall Effect. Contrary to Quantum Hall Effect that requires broken time inversion symmetry, the Spin Hall current may exist in “ordinary” systems due to antisymmetric behavior of spin under time inversion. Obviously such current may only exist when the system couples spatial coordinates of electrons with their spin coordinates, which naturally leads to investigation of how the spin orbit coupling may lead to existence of the Spin Hall Current. First we present a method of computing Spin Hall Current based on Streda formula. We then show an elegant derivation of the absence of Spin Hall Current in conductors with SOC of Rashba type. Next we show in detail how the spin current emerges in semiconductor systems, providing intuitive explanation for its Z2 nature by looking at the edge states. We then demonstrate by a direct numerical computation that it is possible to distinguish between the Spin Hall insulator and an ordinary insulator by comparing their response to an adiabatic pump of a magnetic flux into the system. The second half of the Thesis is dedicated to studying the effects of interactions that lead to formation of superconducting state in metallic systems that are too small to be considered superconductors. This happens when the single energy level spacing becomes comparable to the bulk superconducting gap. Even though such small systems do not carry superconducting current they exhibit peculiar correlation effects in the crossover region. Two different approaches are used to tackle exact solutions of superconducting (or pairing) Hamiltonian and to compute quantities of interest, such as superconducting gap, excitation energies and parity effects. Since the exact solution are in fact systems of equations
EARLY STRUCTURE FORMATION FROM PRIMORDIAL DENSITY FLUCTUATIONS WITH A BLUE, TILTED POWER SPECTRUM

While observations of large-scale structure and the cosmic microwave background (CMB) provide strong constraints on the amplitude of the primordial power spectrum (PPS) on scales larger than 10 Mpc, the amplitude of the power spectrum on sub-galactic length scales is much more poorly constrained. We study early structure formation in a cosmological model with a blue-tilted PPS. We assume that the standard scale-invariant PPS is modified at small length scales as P ( k ) ∼ k m s ? > with ms > 1. We run a series of cosmological hydrodynamic simulations to examine the dependence of the formation epoch and the characteristic mass of primordial stars on the tilt of the PPS. In models with ms > 1, star-forming gas clouds are formed at z > 100 when the formation of hydrogen molecules is inefficient because the intense CMB radiation destroys chemical intermediates. Without efficient coolant, the gas clouds gravitationally contract while retaining a high temperature. The protostars formed in such “hot” clouds grow very rapidly through accretion to become extremely massive stars that may leave massive black holes with a few hundred solar masses at z > 100. The shape of the PPS critically affects the properties and the formation epoch of the first generation of stars. Future experiments on CMB polarization and spectrum distortion may provide important information on the nature of the first stars and their formation epoch, and hence on the shape of the small-scale power spectrum.
Androgen Deprivation Therapy versus Apalutamide Monotherapy versus Androgen Deprivation Monotherapy in Patients with Biochemically Recurrent Prostate Cancer

Helen Diller Family Comprehensive Cancer Center, University of California San Francisco, San Francisco, CA, USA Knight Cancer Institute, Oregon Health and Science University, Portland, OR, USA Rogel Cancer Center, University of Michigan, Ann Arbor, MI, USA University of Chicago, Chicago, IL, USA University of Washington, Fred Hutchinson Cancer Research Center, Seattle, WA, USA Mayo Clinic Arizona, Scottsdale, AZ, USA Janssen Research & Development, Los Angeles, CA, USA Janssen Research & Development, Raritan, NJ, USA Janssen Research & Development, San Diego, CA, USA Merck, Rahway, NJ, USA Janssen Research & Development, Spring House, PA, USA
DMSO_A_365496 2991..3005

1Laboratory of Cardiovascular Investigation, Oswaldo Cruz Institute, FIOCRUZ, Rio de Janeiro, RJ, Brazil; 2National Center of Structural Biology and Bio-imaging, Federal University of Rio de Janeiro, Rio de Janeiro, RJ, Brazil; 3Laboratory of Physical Activity and Health Promotion, University of Rio de Janeiro, Rio de Janeiro, RJ, Brazil; 4Department of Basic Sciences, Federal Fluminense University, Nova Friburgo, RJ, Brazil
Pulsar timing analysis in the presence of correlated noise

Pulsar timing observations are usually analysed with least-squares fitting procedures under the assumption that the timing residuals are uncorrelated (statistically ‘white’). Pulsar observers are well aware that this assumption often breaks down and causes severe errors in estimating the parameters of the timing model and their uncertainties. Ad hoc methods for minimizing these errors have been developed, but we show that they are far from optimal. Compensation for temporal correlation can be done optimally if the covariance matrix of the residuals is known using a linear transformation that whitens both the residuals and the timing model. We adopt a transformation based on the Cholesky decomposition of the covariance matrix, but the transformation is not unique. We show how to estimate the covariance matrix with sufficient accuracy to optimize the pulsar timing analysis. We also show how to apply this procedure to estimate the spectrum of any time series with a steep red power-law spectrum, including those with irregular sampling and variable error bars, which are otherwise very difficult to analyse.
STELLAR AGES AND CONVECTIVE CORES IN FIELD MAIN-SEQUENCE STARS: FIRST ASTEROSEISMIC APPLICATION TO TWO KEPLER TARGETS

Using asteroseismic data and stellar evolution models we obtain the first detection of a convective core in a Kepler field main-sequence star, putting a stringent constraint on the total size of the mixed zone and showing that extra mixing beyond the formal convective boundary exists. In a slightly less massive target the presence of a convective core cannot be conclusively discarded, and thus its remaining main-sequence lifetime is uncertain. Our results reveal that best-fit models found solely by matching individual frequencies of oscillations corrected for surface effects do not always properly reproduce frequency combinations. Moreover, slightly different criteria to define what the best-fit model is can lead to solutions with similar global properties but very different interior structures. We argue that the use of frequency ratios is a more reliable way to obtain accurate stellar parameters, and show that our analysis in field main-sequence stars can yield an overall precision of 1.5%, 4%, and 10% in radius, mass, and age, respectively. We compare our results with those obtained from global oscillation properties, and discuss the possible sources of uncertainties in asteroseismic stellar modeling where further studies are still needed.
Statistical Inference for Risk-Adjusted Performance Measure

This paper examines the statistical properties of and significance tests for a popular risk-adjusted performance measure, the M-squared measure. Test statistics along with asymptotic moments and probability distributions developed by prior studies are reviewed and their applications to the M-squared measure are discussed. This paper demonstrates through an example that calculation of the analytic test statistic and the corresponding p-value can be performed easily using a spreadsheet or mathematical software. Results of significance tests using bootstrapping are similar to those based on the analytic solutions, suggesting that the analytic solution approach is a useful method for conducting statistical inference. The results appear relatively robust even in small samples.
Applied Statistics for Economists

Preface Part 1: Descriptive Statistics of an Economic Variable 1. The Role of Statistics in Economics 2. Visual Presentations of Economic Data 3. Observations and Frequency Distribution 4. Measures of Central Tendency 5. Measures of Dispersion Part 2. Temporal Descriptive Statistics: Change Over Time 6. Measuring Changes in Prices and Quantity 7. Descriptions of Stability: Short-Run Changes 8. Patterns of Long-Term Change Part 3: Statistical Inferences about a Single Variable 9. Basic Concepts in Statistical Inference 10. Statistical Estimation 11. Statistical Hypothesis Testing of a Mean Part 4: Relationships between Two Variables: Descriptions and Statistical Inference 12. Correlation Analysis 13. Simple Linear Regression, Descriptive Measures 14. Simple Regression Analysis: Statistical Inference 15. Simple Regression Analysis: Variable Scales and Functional Forms Part 5: Relationships between Multiple Variables: Description and Statistical Inferences 16. Multiple Regression Analysis: Descriptive Measures 17. Multiple Regression Analysis: Hypothesis Tests for Partial Regression Coefficients and Overall Goodness of Fit 18. Multiple Regression Analysis: Dummy Variables and Statistical Problems
Asteroid models from the Lowell photometric database

We use the lightcurve inversion method to derive new shape models and spin states of asteroids from the sparse-in-time photometry compiled in the Lowell Photometric Database. To speed up the time-consuming process of scanning the period parameter space through the use of convex shape models, we use the distributed computing project Asteroids@home, running on the Berkeley Open Infrastructure for Network Computing (BOINC) platform. This way, the period-search interval is divided into hundreds of smaller intervals. These intervals are scanned separately by different volunteers and then joined together. We also use an alternative, faster, approach when searching the best-fit period by using a model of triaxial ellipsoid. By this, we can independently confirm periods found with convex models and also find rotation periods for some of those asteroids for which the convex-model approach gives too many solutions. From the analysis of Lowell photometric data of the first 100,000 numbered asteroids, we derived 328 new models. This almost doubles the number of available models. We tested the reliability of our results by comparing models that were derived from purely Lowell data with those based on dense lightcurves, and we found that the rate of false-positive solutions is very low. We also present updated plots of the distribution of spin obliquities and pole ecliptic longitudes that confirm previous findings about a non-uniform distribution of spin axes. However, the models reconstructed from noisy sparse data are heavily biased towards more elongated bodies with high lightcurve amplitudes.