Miracle-dz/UniFAR-FTUs huggingface dataset:
Are Outflows Biasing Single-Epoch CIV Black Hole Mass Estimates?

We use a combination of reverberation mapping data and single-epoch spectra of the C iv emission line in a sample of both low and high-redshift active galactic nuclei (AGNs) to investigate sources of the discrepancies between C ivand Hβ-based single-epoch black hole mass estimates. We find that for all reverberation mapped sources, there is a component of the line profile that does not reverberate, and the velocity characteristics of this component vary from object-to-object. The differing strength and properties of this non-variable component are responsible for much of the scatter in C iv-based black hole masses compared to Hβ masses. The C iv mass bias introduced by this non-variable component is correlated with the shape of the C iv line, allowing us to make an empirical correction to the black hole mass estimates. Using this correction and accounting for other sources of scatter such as poor data quality and data inhomogeneity reduces the scatter between the C iv and Hβ masses in our sample by a factor of ∼2, to only ∼0.2 dex. We discuss the possibility that this non-variable C iv component originates in an orientation-dependent outflow from either the proposed broad line region (BLR) disk-wind or the intermediate line region (ILR), a high-velocity inner extension of the narrow line region (NLR). Subject headings: galaxies: active — galaxies: nuclei — line: profiles — quasars: emission lines
TOWARD A COMPLETE ACCOUNTING OF ENERGY AND MOMENTUM FROM STELLAR FEEDBACK IN GALAXY FORMATION SIMULATIONS

We investigate the momentum and energy budget of stellar feedback during different stages of stellar evolution, and study its impact on the interstellar medium (ISM) using simulations of local star-forming regions and galactic disks at the resolution affordable in modern cosmological zoom-in simulations. In particular, we present a novel subgrid model for the momentum injection due to radiation pressure and stellar winds from massive stars during early, pre-supernova (pre-SN) evolutionary stages of young star clusters. Early injection of momentum acts to clear out dense gas in star-forming regions, hence limiting star formation. The reduced gas density mitigates radiative losses of thermal feedback energy from subsequent SN explosions. The detailed impact of stellar feedback depends sensitively on the implementation and choice of parameters. Somewhat encouragingly, we find that implementations in which feedback is efficient lead to approximate self-regulation of the global star formation efficiency. We compare simulation results using our feedback implementation to other phenomenological feedback methods, where thermal feedback energy is allowed to dissipate over timescales longer than the formal gas cooling time. We find that simulations with maximal momentum injection suppress star formation to a similar degree as is found in simulations adopting adiabatic thermal feedback. However, different feedback schemes are found to produce significant differences in the density and thermodynamic structure of the ISM, and are hence expected to have a qualitatively different impact on galaxy evolution.
Resolution numerique de l'equation de navier-stokes avec reconnection d'interfaces. Methode de suivi de volume et application a l'atomisation

Cette these est consacree a l'etude numerique de l'ecoulement incompressible de deux fluides non miscibles. La methode numerique comporte trois volets: ? representation et suivi de l'interface. modelisation de la force capillaire. resolution des equations de navier-stokes. La methode de volume de fluide est utilisee pour suivre l'interface: l'interface est reconstruite par un segment en 2d (un polygone en 3d) et l'interface ainsi reconstruite est advectee par une methode lagrangienne. Les resultats pour de simples tests, la translation et la rotation de l'interface, sont satisfaisant en 2d et en 3d. Les equations de la quantite de mouvement sont discretisees par une methode de projection: nous avons utilise d'une part, une methode mac pour le maillage cartesien, d'autre part, nous avons developpe en 2d une methode colocatif pour le maillage curviligne. L'equation de poisson pour la pression est obtenue a partir de l'equation de la continuite et resolue par une methode de multigrille robuste et efficace. La modelisation de la force capillaire est realisee a l'aide du modele de tenseur capillaire continu. Notre methode numerique est validee en comparant avec une theorie lineaire de l'instabilite de kelvin-helmholtz et appliquee a l'atomisation
Geomagnetic Disturbances That Cause GICs: Investigating Their Interhemispheric Conjugacy and Control by IMF Orientation

Nearly all studies of impulsive geomagnetic disturbances (GMDs, also known as magnetic perturbation events MPEs) that can produce dangerous geomagnetically induced currents (GICs) have used data from the northern hemisphere. In this study, we investigated GMD occurrences during the first 6 months of 2016 at four magnetically conjugate high latitude station pairs using data from the Greenland West Coast magnetometer chain and from Antarctic stations in the conjugate AAL‐PIP magnetometer chain. Events for statistical analysis and four case studies were selected from Greenland/AAL‐PIP data by detecting the presence of >6 nT/s derivatives of any component of the magnetic field at any of the station pairs. For case studies, these chains were supplemented by data from the BAS‐LPM chain in Antarctica as well as Pangnirtung and South Pole in order to extend longitudinal coverage to the west. Amplitude comparisons between hemispheres showed (a) a seasonal dependence (larger in the winter hemisphere), and (b) a dependence on the sign of the By component of the interplanetary magnetic field (IMF): GMDs were larger in the north (south) when IMF By was >0 (<0). A majority of events occurred nearly simultaneously (to within ±3 min) independent of the sign of By as long as |By| ≤ 2 |Bz|. As has been found in earlier studies, IMF Bz was <0 prior to most events. When IMF data from Geotail, Themis B, and/or Themis C in the near‐Earth solar wind were used to supplement the time‐shifted OMNI IMF data, the consistency of these IMF orientations was improved.
STAR FORMATION RATE AND DYNAMICAL MASS OF 108 SOLAR MASS BLACK HOLE HOST GALAXIES AT REDSHIFT 6

We present ALMA observations of two moderate-luminosity quasars at redshift 6. These quasars, from the Canada–France High-z Quasar Survey (CFHQS), have black hole masses of ∼ 10 8 M ⊙ ? > . Both quasars are detected in the [C ii] line and dust continuum. Combining these data with our previous study of two similar CFHQS quasars we investigate the population properties. We show that z > 6 ? > quasars have a significantly lower far-infrared (far-IR) luminosity than bolometric-luminosity-matched samples at lower redshift, inferring a lower star formation rate possibly correlated with lower black hole masses at z = 6. The ratios of [C ii] to far-IR luminosities in the CFHQS quasars are comparable to those of starbursts of similar star formation rate in the local universe. We determine the values of velocity dispersion and dynamical mass for the quasar host galaxies based on the [C ii] data. We find that there is no significant offset from the relations defined by nearby galaxies with similar black hole masses. There is, however, a marked increase in the scatter at z = 6, beyond the large observational uncertainties.
Positivity constraints for pseudolinear massive spin-2 and vector Galileons

We derive analyticity constraints on a nonlinear ghost-free effective theory of a massive spin-2 particle known as pseudolinear massive gravity, and on a generalized theory of a massive spin-1 particle, both of which provide simple IR completions of Galileon theories. For pseudolinear massive gravity we find that, unlike de Rham, Gabadadze, and Tolley massive gravity, there is no window of parameter space which satisfies the analyticity constraints. For massive vectors which reduce to Galileons in the decoupling limit, we find that no two-derivative actions are compatible with positivity but that higher derivative actions can be made compatible.
Absolute clock synchronisation and special relativity paradoxes

Solving special relativity paradoxes requires rigorous analysis of event timing, due to relative simultaneity in consequence of the Lorentz transformation. Since clock syn- chronisation is a convention in special theory of relativity, instead of the Einstein's procedure one may choose such that offers absolute simultaneity. We present in short the corresponding formalism in one spatial dimension. We show that paradoxes do not arise with this choice of synchronisation and descriptions of these issues are exceptionally simple and consistent for both observers involved.
A volume-limited sample of X-ray galaxy groups and clusters – I. Radial entropy and cooling time profiles

We present the first results of our study of a sample of 101 X-ray galaxy groups and clusters, which is volume-limited in each of three X-ray luminosity bins. The aim of this work is to study the properties of the innermost ICM in the cores of our groups and clusters, and to determine the effect of non-gravitational processes, such as active galactic nucleus (AGN) feedback, on the ICM. The entropy of the ICM is of special interest, as it bears the imprint of the thermal history of a cluster, and it also determines a cluster's global properties. Entropy profiles can therefore be used to examine any deviations from cluster self-similarity, as well as the effects of feedback on the ICM. We find that the entropy profiles are well-fitted by a simple powerlaw model, of the form $K(r) = \alpha\times(r/100 \rm{kpc})^{\beta}$, where $\alpha$ and $\beta$ are constants. We do not find evidence for the existence of an "entropy floor", i.e. our entropy profiles do not flatten out at small radii, as suggested by some previous studies.
A revisit to agglomerates of early-type Hipparcos stars

We study the spatial structure and sub-structure of regions rich in Hipparcos stars with blue B_T-V_T colours. These regions, which comprise large stellar complexes, OB associations, and young open clusters, are tracers of on-going star formation in the Galaxy. The DBSCAN (Density-Based Spatial Clustering of Applications with Noise) data clustering algorithm is used to look for spatial overdensities of early-type stars. Once an overdensity, "agglomerate", is identified, we carry out a data and bibliographic compilation of their star member candidates. The actual membership in agglomerate of each early-type star is studied based on its heliocentric distance, proper motion, and previous spectro-photometric information. We identify 35 agglomerates of early-type Hipparcos stars. Most of them are associated to previously known clusters and OB associations. The previously unknown P Puppis agglomerate is subject of a dedicated study with Virtual Observatory tools. It is actually a new, nearby, young open cluster (d ~ 470 pc, age ~ 20 Ma) with a clear radial density gradient. We list P Puppis and other six agglomerates (including NGC 2451 A, vdBH 23, and Trumpler 10) as new sites for substellar searches because of their youth, closeness, and spatial density. We investigate in detail the sub-structure in the Orion, CMa-Pup and Pup-Vel OB complexes ("super-agglomerates"). We confirm or discover some stellar overdensities in the Orion complex, like the 25 Ori group, the Horsehead region (including the sigma Orionis cluster), and the eta Orionis agglomerate. Finally, we derive accurate parallactic distances to the Pleiades, NGC 2451 A, and IC 2391, describe several field early-type stars at d < 200 pc, and discuss the incompleteness of our search.
Distributed finite‐time tracking of multiple Euler–Lagrange systems without velocity measurements

This paper investigates the distributed finite‐time tracking problem of networked agents with multiple Euler–Lagrange dynamics. To achieve finite‐time tracking, a distributed finite‐time protocol is first proposed on the basis of both relative position and relative velocity measurements. By using tools from homogeneous theory, it is theoretically shown that the proposed protocol can guarantee finite‐time tracking in the presence of control input constraints. On the basis of the state feedback analysis and with the aid of second‐order sliding‐mode observer approach, a new class of finite‐time tracking protocols based only on the relative position measurements is developed and employed. It is proved that the multiple agents equipped with the designed protocols can track the target location in finite time. Furthermore, a decentralized finite‐time protocol based on a distributed estimator is proposed to solve the finite‐time tracking problems with a dynamic leader. The effectiveness of the theoretical results is finally illustrated by numerical simulations. Copyright © 2014 John Wiley & Sons, Ltd.
Quantum point contact as a probe of a topological superconductor

We calculate the conductance of a ballistic point contact to a superconducting wire, produced by the s-wave proximity effect in a semiconductor with spin–orbit coupling in a parallel magnetic field. The conductance G as a function of contact width or Fermi energy shows plateaux at half-integer multiples of 4e2/h if the superconductor is in a topologically nontrivial phase. In contrast, the plateaux are at the usual integer multiples in the topologically trivial phase. Disorder destroys all plateaux except the first, which remains precisely quantized, consistent with previous results for a tunnel contact. The advantage of a ballistic contact over a tunnel contact as a probe of the topological phase is the strongly reduced sensitivity to finite voltage or temperature.
On the morphology of dust lanes in galactic bars

The aim of our study is to use dynamical simulations to explore the influence of two important dynamical bar parameters, bar strength and bar pattern speed, on the shape of the bar dust lanes. To quantify the shape of the dust lanes we have developed a new systematic method to measure the dust lane curvature. Previous numerical simulations have compared the curvature of bar dust lanes with the bar strength, predicting a relation between both parameters which has been supported by observational studies but with a large spread. We take into account the bar pattern speed to explore, simultaneously, the effect of both parameters on the dust lane shape. To that end, we separate our galactic bars in fast bars $\left(1 1.4 \right)$, obtaining, as previous simulations, an inverse relation between the dust lane curvature and the bar strength for fast bars. For the first time, we extend the study to slow bars, finding a constant curvature as a function of the bar strength. As a result, we conclude that weak bars with straight dust lanes are candidates for slow bars. Finally, we have analysed a pilot sample of ten S$^4$G galaxies, obtaining dust lane curvatures lying within the range covered by the simulations.
Vector Autoregressive and Vector Error Correction Models

Introduction The first step in constructing a model for a specific purpose or for a particular sector of an economy is to decide on the variables to be included in the analysis. At this stage it is usually important to take into account what economic theory has to say about the relations between the variables of interest. Suppose we want to analyze the transmission mechanism of monetary policy. An important relation in that context is the money demand function, which describes the link between the real and the monetary sector of the economy. In this relationship a money stock variable depends on the transactions volume and opportunity costs for holding money. As an example we consider German M3 as the money stock variable, GNP as a proxy for the transactions volume, a long-term interest rate R as an opportunity cost variable, and the inflation rate Dp = Δp, where p denotes the log of the GNP deflator. The latter variable may be regarded as a proxy for expected inflation, which may also be considered an opportunity cost variable. Because the quantity theory suggests a log linear relation, we focus on the variables m = log M3 and gnp = log GNP. Seasonally unadjusted quarterly series for the period 1972–98 are plotted in Figure 3.1. Of course, many more variables are related to the presently considered ones and, hence, could be included in a model for the monetary sector of the economy. However, increasing the number of variables and equations does not generally lead to a better model because doing so makes it more difficult to capture the dynamic, intertemporal relations between them.
Boundary Localized Terms in Universal Extra-Dimensional Models through a Dark Matter perspective

In universal extra dimension (UED) models with one compactified extra dimension, a Z2 symmetry, termed KK-parity, ensures the stability of the lightest Kaluza-Klein particle (LKP) which could be a viable dark matter candidate. This symmetry leads to two fixed points. In non-minimal versions of UED boundary-localized (kinetic or mass) terms (BLT) for different fields are included at these fixed points and KK-parity may be violated. However, BLTs with same strength at both points induce a new Z2 symmetry which restores the stability of the LKP. We show that the BLTs serve to relax the bounds set on the compactification scale in UED by the observed dark matter relic density. At the same time, the precision of the dark matter measurements severely correlates the BLT parameters of gauge bosons and fermions. Depending on the parameter values, the LKP can be chosen to be the level-1 photon, which is essentially the B (1) , or the level-1 Z-boson, basically the W (1) 3 . We find that in the latter case the relic density is too small if the W
Hydrocarbon degradation test among the microbial community in oil-contaminated soil of power generators in Kerbala city, Iraq

The present study was designed to isolate the microbial community from oil-contaminated sites and other non-oil-contaminated sites which served as control samples in Kerbala city. In addition to test the effect of hydrocarbons on the growth of some types of bacteria. Bacterial genera and species were identified based on their growth on nutrient agar and blood agar as well as biochemical tests. According to the high bacterial growth rate on crude oil, 5 bacterial isolates were selected for further study. Growth of some identified bacteria in Minimal salt medium amended with hydrocarbon as the sole carbon source was investigated. Acinetobacter sp. , Pseudomonas aeruginosa, Pseudomonas fluorescens, Pantoea sp. , Pasteurella pneumonia / haemolytica, Chryseobacterium meningosepticum, Bordetella sp. , and Enterobacter cloacae were the dominant phyla among all the soil samples. Although all tested bacteria were able to grow on mineral liquid media, P. aeruginosa had the most capacity for growth in this media. The present study showed that selected bacteria were able to grow and utilize MSM that contains different concentrations of gasoline. From this data, it can be concluded that oil-degrading bacteria are abundant in soils contaminated with spent oil. Consequently, these data suggest that these microbes could be useful for their application in the biodegradation of contaminated soils.
Suppression of gravitational instabilities by dominant dark matter halo in low surface brightness galaxies

The low-surface-brightness galaxies are gas rich and yet have a low star formation rate; this is a well-known puzzle. The spiral features in these galaxies are weak and difficult to trace, although this aspect has not been studied much. These galaxies are known to be dominated by the dark matter halo from the innermost regions. Here, we do a stability analysis for the galactic disc of UGC 7321, a low-surface-brightness, superthin galaxy, for which the various observational input parameters are available. We show that the disc is stable against local, linear axisymmetric and non-axisymmetric perturbations. The Toomre Q parameter values are found to be large (>> 1) mainly due to the low disc surface density, and the high rotation velocity resulting due to the dominant dark matter halo, which could explain the observed low star formation rate. For the stars-alone case, the disc shows finite swing amplification but the addition of dark matter halo suppresses that amplification almost completely. Even the inclusion of the low-dispersion gas which constitutes a high disc mass fraction does not help in causing swing amplification. This can explain why these galaxies do not show strong spiral features. Thus, the dynamical effect of a halo that is dominant from inner regions can naturally explain why star formation and spiral features are largely suppressed in low-surface-brightness galaxies, making these different from the high-surface-brightness galaxies.
Leopard density and interspecific spatiotemporal interactions in a hyena‐dominated landscape

Abstract Scavenging is widespread in the carnivore guild and can greatly impact food web structures and population dynamics by either facilitation or suppression of sympatric carnivores. Due to habitat loss and fragmentation, carnivores are increasingly forced into close sympatry, possibly resulting in more interactions such as kleptoparasitism and competition. In this paper, we investigate the potential for these interactions when carnivore densities are high. A camera trap survey was conducted in central Tuli, Botswana, to examine leopard Panthera pardus densities and spatiotemporal activity patterns of leopard and its most important competitors' brown hyena Parahyaena brunnea and spotted hyena Crocuta crocuta. Spatial capture–recapture models estimated leopard population density to be 12.7 ± 3.2 leopard/100 km2, which is one of the highest leopard densities in Africa. Time‐to‐event analyses showed both brown hyena and spotted hyena were observed more frequently before and after a leopard observation than expected by chance. The high spatiotemporal overlap of both hyena species with leopard is possibly explained by leopard providing scavenging opportunities for brown hyena and spotted hyena. Our results suggest that central Tuli is a high‐density leopard area, despite possible intense kleptoparasitism and competition.
Synchronization and anti-synchroniztion of dynamically coupled networks

We consider the coupling between two networks, each having N nodes whose individual dynamics is modeled by a two-state master equation. The intra-network interactions are all-to-all, whereas the inter-network interactions involve only a small percentage of the total number of nodes. We demonstrate that the dynamics of the mean field for a single network has an equivalent description in terms of a Langevin equation for a particle in a double-well potential. The coupling of two networks or equivalent coupling of two Langevin equations demonstrates synchronization or anti-synchronization between two systems, depending on the sign of the interaction. The anti-synchronized behavior is explained in terms of the potential function and the inter-network interaction. The relative entropy is used to establish that the conditions for maximum information transfer between the networks are consistent with the principle of complexity management and occurs when one system is near the critical state. The limitations of the Langevin modeling of the network coupling are also discussed.