Miracle-dz/UniFAR-FTUs huggingface dataset:
Testing emergent gravity with mass densities of galaxy clusters

We use a sample of 23 galaxy clusters to test the predictions of emergent gravity (EG) as alternative to dark matter. Our sample has both weak-lensing inferred total mass profiles as well as x-ray inferred baryonic gas mass profiles. Using nominal assumptions about the weak-lensing and x-ray mass profiles, we find that the EG predictions (based on no dark matter) are acceptable fits only near the virial radius. In the cores and in the outskirts, the mass profile shape differences allow us to confirm previous results that the EG model can be ruled out at $>5\sigma$. However, when we account for systematic uncertainties in the observed weak-lensing and x-ray profiles, we find good agreement for the EG predictions. For instance, if the weak-lensing total mass profiles are shallow in the core and the x-ray gas density profiles are steep in the outskirts, EG can predict the observed dark matter profile in $0.3 \le r \le 1$R$_{200}$, where R$_{200}$ is the radius which encloses 200$\times$ the critical density of the Universe. The required x-ray and lensing shapes are within the current observational systematics-limited errors on cluster profiles. We also show that EG itself allows flexibility in its predictions, which can allow for good agreement between the observations and the predictions. We conclude that we cannot formally rule our EG as an alternative to dark matter on the cluster scale and that we require better constraints on the weak-lensing and gas mass profile shapes in the region $0.3 \le r \le 1$R$_{200}$.
Magnetostrictive behaviour of thin superconducting disks

Flux-pinning-induced stress and strain distributions in a thin disk superconductor in a perpendicular magnetic field are analysed. We calculate the body forces, solve the magneto-elastic problem and derive formulae for all stress and strain components, including the magnetostriction ΔR/R. The flux and current density profiles in the disk are assumed to follow the Bean model. During a cycle of the applied field the maximum tensile stress is found to occur approximately midway between the maximum field and the remanent state. An effective relationship between this overall maximum stress and the peak field is found.
Water Resource Economics and Policy

A concise introduction to issues of water quality and quantity in both urban and agricultural settings, Water Resource Economics and Policy will be a valuable resource or text for students and researchers in the fields of agricultural economics, geography, law and hydrology. Those involved in water resource agencies and private utilities will also find the book a useful reference.
Phat ELVIS: The inevitable effect of the Milky Way’s disc on its dark matter subhaloes

We introduce an extension of the ELVIS project to account for the effects of the Milky Way galaxy on its subhalo population. Our simulation suite, Phat ELVIS, consists of 12 high-resolution cosmological dark matter-only (DMO) zoom simulations of Milky Way-size ΛCDM haloes [Mv = (0.7−2) × 1012 M⊙] along with 12 re-runs with embedded galaxy potentials grown to match the observed Milky Way disc and bulge today. The central galaxy potential destroys subhalos on orbits with small pericentres in every halo, regardless of the ratio of galaxy mass to halo mass. This has several important implications. (1) Most of the Disc runs have no subhaloes larger than Vmax = 4.5 km s−1 within 20 kpc and a significant lack of substructure going back ∼8 Gyr, suggesting that local stream-heating signals from dark substructure will be rare. (2) The pericentre distributions of Milky Way satellites derived from Gaia data are remarkably similar to the pericentre distributions of subhaloes in the Disc runs, while the DMO runs drastically overpredict galaxies with pericentres smaller than 20 kpc. (3) The enhanced destruction produces a tension opposite to that of the classic ‘missing satellites’ problem: in order to account for ultra-faint galaxies known within 30 kpc of the Galaxy, we must populate haloes with Vpeak ≃ 7 km s−1 (M ≃ 3 × 107 M⊙ at infall), well below the atomic cooling limit of $V_\mathrm{peak}\simeq 16 \,{\rm km} \, {\rm s}^{-1}$ (M ≃ 5 × 108M⊙ at infall). (4) If such tiny haloes do host ultra-faint dwarfs, this implies the existence of ∼1000 satellite galaxies within 300 kpc of the Milky Way.
Swift UVOT near-UV transit observations of WASP-121 b

Close-in gas planets are subject to continuous photoevaporation that can erode their volatile envelopes. Today, ongoing mass loss has been confirmed in a few individual systems via transit observations in the ultraviolet spectral range. We demonstrate that the Ultraviolet/Optical Telescope (UVOT) onboard the Neil Gehrels Swift Observatory enables photometry to a relative accuracy of about 0.5% and present the first near-UV (200–270 nm, NUV) transit observations of WASP-121 b, a hot Jupiter with one of the highest predicted mass-loss rates. The data cover the orbital phases 0.85–1.15 with three visits. We measure a broadband NUV transit depth of 2.10 ± 0.29%. While still consistent with the optical value of 1.55%, the NUV data indicate excess absorption of 0.55% at a 1. 9σ level. Such excess absorption is known from the WASP-12 system, and both of these hot Jupiters are expected to undergo mass loss at extremely high rates. With a Cloudy simulation, we show that absorption lines of Fe II in a dense extended atmosphere can cause broadband near-UV absorption at the 0.5% level. Given the numerous lines of low-ionization metals, the NUV range is a promising tracer of photoevaporation in the hottest gas planets.
The relationships between PM2.5 and AOD in China: About and behind spatiotemporal variations

Satellite aerosol products have been widely used to retrieve ground PM2.5 concentration because of its wide coverage and continuously spatial distribution. While more and more studies focus on the retrieval algorithm, we find that the relationship between PM2.5 concentration and satellite AOD has not been fully discussed in China. Is satellite AOD always a good indicator for PM2.5 in different regions and can AOD still be employed to retrieve PM2.5 with pollution conditions changing in these years remain unclear. In this study, the relationships between PM2.5 and AOD were investigated in 368 cities in China for a continuous period from February 2013 to December 2017, at different time and regional scales. Pearson correlation coefficients and PM2.5/AOD ratio were used as the indicator. Firstly, we concluded the relationship of PM2.5 and AOD in terms of spatiotemporal variations. Then the impact of meteorological factors, aerosol size and topography were discussed. Finally, a GWR retrieval experiment was conducted to find out how was the retrieval accuracy changing with the varying of PM2.5-AOD relationship. We found that spatially the correlation is higher in Beijing-Tianjin-Hebei and Chengyu region and weaker in coastal areas such as Yangtze River Delta and Pearl River Delta. The PM2.5/AOD ratio has obvious North-South difference with a high ratio in north China and a lower ratio in south China. Temporally, PM2.5/AOD ratio is higher in winter and lower in summer, the correlation coefficient tends to be higher in May and September. As for interannual variations from 2013 to 2017, we detected a declining tendency on PM2.5/AOD ratio. The accuracy of GWR retrievals were decreasing too, which may imply that AOD may not be a good indicator for PM2.5 in the future.
Statistical study of time intervals between murders for serial killers

We study the distribution of 2,837 inter-murder intervals (cooling off periods) for 1,012 American serial killers. The distribution is smooth, following a power law in the region of 10-10,000 days. The power law cuts off where inter-murder intervals become comparable with the length of human life. Otherwise there is no other characteristic scale in the distribution. In particular, we do not see any characteristic spree-killer interval or serial-killer interval, but only a monotonous smooth distribution lacking any features. This suggests that there is only a quantitative difference between serial killers and spree-killers, representing different samples generated by the same underlying phenomenon. The over decade long inter-murder intervals are not anomalies, but rare events described by the same power-law distribution and therefore should not necessarily be looked upon with suspicion, as has been done in a recent case involving a serial killer dubbed as the "Grim Sleeper. " This large-scale study supports the conclusions of a previous study, involving three prolific serial killers, and the associated neural net model, which can explain the observed power law distribution.
Lattice Boltzmann modelling of blood cell dynamics

Many diseases are a result of, or are associated with, abnormal blood flow. Usually, these abnormalities are caused by unhealthy red blood cells with modified shape which have difficulty traversing the microvessels. Unfortunately, experimental approaches to these problems are limited due to difficulties in isolating the critical determinants of flow in vivo or in vitro. Computer models overcome these problems, but most strive only to reproduce the macroscopic, continuum aspect of blood flow by making many simplifying assumptions. Unfortunately, these models cannot address the relationship between microscopic, cellular flow dynamics and macroscopic, bulk blood rheology. Here, we demonstrate the wide applicability of a novel, computational model for simulating blood flow that includes each blood cell explicitly. This fully 3D model accounts for cell membrane dynamics and reproduces rest shapes accurately. This model allows us to: (i) extract empirical relationships for use in macroscopic models and (ii) simulate various disease states to identify potential targets for therapy. We show here that the model accurately reproduces the well-documented flow relationships for healthy blood, and also predicts the abnormalities in blood rheology exhibited by malaria and sickle cell patients.
Simulating a single-qubit channel using a mixed-state environment

We analyze the class of single-qubit channels with the environment modeled by a one-qubit mixed state. The set of affine transformations for this class of channels is computed analytically, employing the canonical form for the two-qubit unitary operator. We demonstrate that (3/8) of the generalized depolarizing channels can be simulated by the one-qubit mixed-state environment by explicitly obtaining the shape of the volume occupied by this class of channels within the tetrahedron representing the generalized depolarizing channels. Further, as a special case, we show that the two-Pauli channel cannot be simulated by a one-qubit mixed-state environment.
Evidence for Solar Metallicities in Massive Star-forming Galaxies at z ≳ 2

We present results of near-IR spectroscopic measurements of seven star-forming galaxies at 2.1 < z < 2.5. Drawn from a large spectroscopic survey of galaxies photometrically preselected by their UnGℛ colors to lie at z ~ 2, these galaxies were chosen for their bright rest-frame optical luminosities (Ks ≤ 20.0). Most strikingly, the majority of the sample of seven galaxies exhibit [N II]/Hα nebular emission-line ratios indicative of at least solar H II region metallicities, at a look-back time of 10.5 Gyr. The broadband colors of the Ks-bright sample indicate that most have been forming stars for more than a gigayear at z ~ 2 and have already formed stellar masses in excess of 1011 M☉. The descendants of these galaxies in the local universe are most likely metal-rich and massive spiral and elliptical galaxies, while plausible progenitors for them can be found among the population of z ~ 3 Lyman break galaxies. While the Ks-bright z ~ 2 galaxies appear to be highly evolved systems, their large Hα luminosities and uncorrected Hα star formation rates of 24-60 M☉ yr-1 indicate that active star formation is still ongoing. The luminous UV-selected objects presented here comprise more than half of the high-redshift (z > 1.5) tails of current K-band-selected samples such as the K20 and Gemini Deep Deep surveys.
Synoptic conditions of snow occurrence in Budapest

Daily circulation patterns responsible for snow occurrence in Budapest were analysed. Three types of circulation patterns were distinguished, using a Principal Component Analysis and clustering technique, for days with snowfalls and snow cover persistence. Low pressure systems located over the Italian Peninsula (south-west of Budapest) are characteristic for days with snowfalls. Such lows coming from the west generate warm fronts and are a source of humidity necessary for the snowfalls. At the same time, higher pressure extends north or east of the Carpathian Basin and brings polar continental air masses and consequently low temperature. Snow persistence also requires temperature below zero. This condition is fulfilled at the airflow direction from the east (or south east) which brings frosty air from the interior of the continent. A winter high pressure system extending over the Carpathian Basin also generates low temperature, mainly due to the nocturnal radiation conditioned by a clear sky.
A zone of avoidance catalogue of 2MASS bright galaxies – I. Sample description and analysis

We present a homogeneous 2MASS bright galaxy catalogue at low Galactic latitudes ($|b| \le 10.0^{\rm o}$, called Zone of Avoidance) which is complete to a Galactic extinction-corrected magnitude of $K^o_s \le 11.25^{\rm m}$. It also includes galaxies in regions of high foreground extinctions ($E(B-V) > 0.95^{\rm m}$) situated at higher latitudes. This catalogue forms the basis of studies of large-scale structures, flow fields and extinction across the ZoA and complements the ongoing 2MASS Redshift and Tully-Fisher surveys. It comprises 3763 galaxies, 70% of which have at least one radial velocity measurement in the literature. The catalogue is complete up to star density levels of $\log N_*/{\rm deg}^2 <4.5$ and at least for $A_K < 0.6^{\rm m}$ and likely as high as $A_K = 20^{\rm m}$. Thus the ZoA in terms of bright NIR galaxies covers only $2.5-4$% of the whole sky. We use a diameter-dependent extinction correction to compare our sample with an unobscured, high-latitude sample. While the correction to the $K_s$ -band magnitude is sufficient, the corrected diameters are too small by about $4''$ on average. The omission of applying such a diameter-dependent extinction correction may lead to a biased flow field even at intermediate extinction values as found in the 2MRS survey. A slight dependence of galaxy colour with stellar density indicates that unsubtracted foreground stars make galaxies appear bluer. Furthermore, far-infrared sources in the DIRBE/IRAS extinction maps that were not removed at low latitudes affect the foreground extinction corrections of three galaxies and may weakly affect a further estimated $\approx 20$% of our galaxies.
BVRI Light Curves for 22 Type Ia Supernovae

We present 1210 Johnson/Cousins B, V, R, and I photometric observations of 22 recent Type Ia supernovae (SNe Ia): SNe 1993ac, 1993ae, 1994M, 1994S, 1994T, 1994Q, 1994ae, 1995D, 1995E, 1995al, 1995ac, 1995ak, 1995bd, 1996C, 1996X, 1996Z, 1996ab, 1996ai, 1996bk, 1996bl, 1996bo, and 1996bv. Most of the photometry was obtained at the Fred Lawrence Whipple Observatory of the Harvard-Smithsonian Center for Astrophysics in a cooperative observing plan aimed at improving the database for SNe Ia. The redshifts of the sample range from cz = 1200 to 37,000 km s-1 with a mean of cz = 7000 km s-1.
Field theoretical approach to gravitational waves

The aim of these notes is to give an accessible and self‐contained introduction to the theory of gravitational waves as the theory of a relativistic symmetric tensor field in a Minkowski background spacetime. This is the approach of a particle physicist: the graviton is identified with a particular irreducible representation of the Poincaré group, corresponding to vanishing mass and spin two. It is shown how to construct an action functional giving the linear dynamics of gravitons, and how General Relativity can be obtained from it. The Hamiltonian formulation of the linear theory is examined in detail. We study the emission of gravitational waves and apply the results to the simplest case of a binary Newtonian system.
Alternative string theory in twistor space for N=4 super-Yang-Mills theory

In this letter, an alternative string theory in twistor space is proposed for describing perturbative N=4 super-Yang-Mills theory. Like the recent proposal of Witten, this string theory uses twistor worldsheet variables and has manifest spacetime superconformal invariance. However, in this proposal, tree-level super-Yang-Mills amplitudes come from open string tree amplitudes as opposed to coming from D-instanton contributions.
Analysis of the Sutton Model for Aero-Optical Properties of Compressible Boundary Layers

In order to assess the capability of the Sutton model to evaluate aero-optical effects in a turbulent boundary layer, large-eddy simulation (LES) evolving spatially and Reynolds averaged Navier-Stokes (RANS) computations are carried out at Mach number equal to 0.9. First aerodynamic fields are proved to compare favorably with theoretical and experimental results. Once validated, the characteristics of the boundary layer allow us to obtain information concerning optical beam degradation. On the one hand, the density field is used to compute phase distortion directly and, on the other hand, by means of the Sutton model. Therefore, LES and RANS simulations allow us to study optical models and the validity of their assumptions. Finally, LES is proved to be considered as a reference tool to evaluate aero-optical effects.
Reflection from black holes

Black holes are presumed to have an ideal ability to absorb and keep matter. Whatever comes close to the event horizon, a boundary separating the inside region of a black hole from the outside world, inevitably goes in and remains inside forever. This work shows, however, that quantum corrections make possible a surprising process, reflection: a particle can bounce back from the event horizon. For low energy particles this process is efficient, black holes behave not as holes, but as mirrors, which changes our perception of their physical nature. Possible ways for observations of the reflection and its relation to the Hawking radiation process are outlined.
Absorption and emission features of 7Be ii in the outburst spectra of V838 Her (Nova Her 1991)

High and low resolution $IUE$ spectra of V838 Her in the early outburst stages exhibit a strong absorption feature shortward of $\lambda$3130. We discuss the nature of this spectral feature and provide convincing evidence that it corresponds to the blue-shifted resonance doublet of singly-ionized $^7$Be, recently discovered in other novae. During the evolution of the outburst the appearance of an emission feature close to $\lambda$3130 is also identified as $^7$Be II $\lambda$3132 because the usual identification as the O III $\lambda$3133.7 Bowen fluorescence line is hardly compatible with both the known oxygen under-abundance in the nova ejecta and the low optical depths in the nebula due to the high outflow velocity. The average $^7$Be abundance relative to hydrogen, estimated by four different methods, i.e. the $^7$Be II / Mg II absorption ratio, and the $^7$Be II / Mg II, $^7$Be II / He II$_{1640}$, and $^7$Be II / H$\beta$ emission ratios is N(Be)/N(H) $\approx$ 2.5 $\times 10^{-5}$ (by number), i.e. $\approx$ 1.7 $\times 10^{-4}$ by mass. This corresponds to an overproduction of $^7$Be by about 1 dex in comparison with the theoretical models of massive CO and ONe novae. Since $^7$Be all converts into $^7$Li, the $^7$Be/H abundance implies a $^7$Li/H overabundance of about 4 dex over the $^7$/H meteoritic value and indicates a total ejected mass of $^7$Li of $\approx$ 9.5$\times$10$^{-10}$ $M_{\odot}$. These data are in line with previous observations and indicate that large amounts of $^7$Li can be synthesized in a variety of novae, including very fast ONe novae.
Millisecond Pulsar Origin of the Galactic Center Excess and Extended Gamma-Ray Emission from Andromeda: A Closer Look

A new measurement of a spatially extended gamma-ray signal from the center of the Andromeda galaxy (M31) has recently been published by the Fermi-LAT collaboration, reporting that the emission broadly resembles the so-called Galactic center excess (GCE) of the Milky Way (MW). The weight of the evidence is steadily accumulating on a millisecond pulsar (MSPs) origin for the GCE. These elements prompt us to compare these observations with what is, perhaps, the simplest model for an MSP population, which is solely obtained by rescaling of the MSP luminosity function that is determined in the local MW disk via the respective stellar mass of the systems. Remarkably, we find that without free fitting parameters, this model can account for both the energetics and the morphology of the GCE within uncertainties. For M31, the estimated luminosity due to primordial MSPs is expected to only contribute about a quarter of the detected emission, although a stronger contribution cannot be excluded given the large uncertainties. If correct, the model predicts that the M31 disk emission due to MSPs is not far below the present upper bound. We also discuss additional refinements of this simple model. Using the correlation between globular cluster gamma-ray luminosity and stellar encounter rate, we gauge the dynamical MSP formation in the bulge. This component is expected to contribute to the GCE only at a level of ≲5%, it could affect the signal’s morphology. We also comment on the limitations of our model and on future perspectives for improved diagnostics.
Peaks in the Hartle-Hawking wavefunction from sums over topologies

Recent developments in 'Einstein Dehn filling' allow the construction of infinitely many Einstein manifolds that have different topologies but are geometrically close to each other. Using these results, we show that for many spatial topologies, the Hartle–Hawking wavefunction for a spacetime with a negative cosmological constant develops sharp peaks at certain calculable geometries. The peaks we find are all centred on spatial metrics of constant negative curvature, suggesting a new mechanism for obtaining local homogeneity in quantum cosmology.
Boundary value problem for five-dimensional stationary rotating black holes

We study the boundary value problem for stationary rotating black hole solutions to the five-dimensional vacuum Einstein equation. Assuming the existence of two additional commuting rotational Killing vector fields and sphericity of the horizon topology, we show that a black hole with a regular event horizon is uniquely characterized by its mass and a pair of angular momenta.
Stellar explosion in the weak field approximation of the Brans–Dicke theory

We treat a very crude model of an exploding star, in the weak field approximation of the Brans–Dicke theory, in a scenario that resembles some characteristic data of a type Ia supernova. The most noticeable feature, in the electromagnetic component, is the relationship between the absolute magnitude at maximum brightness of the star and the decline rate in one magnitude from that maximum. This characteristic has become one of the most accurate methods to measure luminosity distances to objects at cosmological distances (Phillips M M 1993 Astrophys. J. 413 L105; see www.all-science-fair-projects.com/science_fair_projects_encyclopedia/Supernova, for a brief description of supernovae types). An interesting result is that the active mass associated with the scalar field is totally radiated to infinity, representing a mass loss in the ratio of the ‘tensor’ component to the scalar component of 1 to (2ω + 3) (ω is the Brans–Dicke parameter), in agreement with a general result of Hawking (1972 Commun. Math. Phys. 25 167). Then, this model shows explicitly, in a dynamical case, the mechanism of the radiation of a scalar field, which is necessary to understand the Hawking result.