Miracle-dz/UniFAR-FTUs huggingface dataset:
Solar wind charge exchange X-ray emission from Mars Model and data comparison

Aims. We study the soft X-ray emission induced by charge exchange (CX) collisions between solar-wind, highly charged ions and neutral atoms of the Martian exosphere. Methods. A 3D multi species hybrid simulation model with improved spatial resolution (130 km) is used to describe the interaction between the solar wind and the Martian neutrals. We calculated velocity and density distributions of the solar wind plasma in the Martian environment with realistic planetary ions description, using spherically symmetric exospheric H and O profiles. Following that, a 3D test-particle model was developed to compute the X-ray emission produced by CX collisions between neutrals and solar wind minor ions. The model results are compared to XMM-Newton observations of Mars. Results. We calculate projected X-ray emission maps for the XMM-Newton observing conditions and demonstrate how the X-ray emission reflects the Martian electromagnetic structure in accordance with the observed X-ray images. Our maps confirm that X-ray images are a powerful tool for the study of solar wind - planetary interfaces. However, the simulation results reveal several quantitative discrepancies compared to the observations. Typical solar wind and neutral coronae conditions corresponding to the 2003 observation period of Mars cannot reproduce the high luminosity or the corresponding very extended halo observed with XMM-Newton. Potential explanations of these discrepancies are discussed.
Diagrammatic derivation of Lovelock densities

We discuss a method of calculating the various scalar densities encountered in Lovelock theory, which relies on diagrammatic, instead of algebraic manipulations. Taking advantage of the known symmetric and antisymmetric properties of the Riemann tensor that appears in the Lovelock densities, we map every quadratic or higher contraction into a corresponding permutation diagram. The derivation of the explicit form of each density is then reduced to identifying the distinct diagrams, from which we can also read off the overall combinatoric factors. The method is applied to the first Lovelock densities, of order two (Gauss-Bonnet term) and three.
Self-testing through EPR-steering

The verification of quantum devices is an important aspect of quantum information, especially with the emergence of more advanced experimental implementations of quantum computation and secure communication. Within this, the theory of device-independent robust self-testing via Bell tests has reached a level of maturity now that many quantum states and measurements can be verified without direct access to the quantum systems: interaction with the devices is solely classical. However, the requirements for this robust level of verification are daunting and require high levels of experimental accuracy. In this paper we discuss the possibility of self-testing where we only have direct access to one part of the quantum device. This motivates the study of self-testing via EPR-steering, an intermediate form of entanglement verification between full state tomography and Bell tests. Quantum non-locality implies EPR-steering so results in the former can apply in the latter, but we ask what advantages may be gleaned from the latter over the former given that one can do partial state tomography? We show that in the case of self-testing a maximally entangled two-qubit state, or ebit, EPR-steering allows for simpler analysis and better error tolerance than in the case of full device-independence. On the other hand, this improvement is only a constant improvement and (up to constants) is the best one can hope for. Finally, we indicate that the main advantage in self-testing based on EPR-steering could be in the case of self-testing multi-partite quantum states and measurements. For example, it may be easier to establish a tensor product structure for a particular party’s Hilbert space even if we do not have access to their part of the global quantum system.
Sunyaev–Zel’dovich effect and X-ray scaling relations from weak lensing mass calibration of 32 South Pole Telescope selected galaxy clusters

Uncertainty in mass–observable scaling relations is currently the limiting factor for galaxy-cluster-based cosmology. Weak gravitational lensing can provide direct mass calibration and reduce the mass uncertainty. We present new ground-based weak lensing observations of 19 South Pole Telescope (SPT) selected clusters at redshifts 0.29 ≤ $z$ ≤ 0.61 and combine them with previously reported space-based observations of 13 galaxy clusters at redshifts 0.576 ≤ $z$ ≤ 1.132 to constrain the cluster mass scaling relations with the Sunyaev–Zel’dovich effect (SZE), the cluster gas mass Mgas and YX, the product of Mgas and X-ray temperature. We extend a previously used framework for the analysis of scaling relations and cosmological constraints obtained from SPT-selected clusters to make use of weak lensing information. We introduce a new approach to estimate the effective average redshift distribution of background galaxies and quantify a number of systematic errors affecting the weak lensing modelling. These errors include a calibration of the bias incurred by fitting a Navarro–Frenk–White profile to the reduced shear using N-body simulations. We blind the analysis to avoid confirmation bias. We are able to limit the systematic uncertainties to 5.6% in cluster mass (68% confidence). Our constraints on the mass–X-ray observable scaling relation parameters are consistent with those obtained by earlier studies and our constraints for the mass–SZE scaling relation are consistent with the simulation-based prior used in the most recent SPT–SZ cosmology analysis. We can now replace the external mass calibration priors used in previous SPT–SZ cosmology studies with a direct, internal calibration obtained for the same clusters.
O ct 2 01 5 Demonstrating Universal Scaling in Quench Dynamics of a Yukawa One-Component Plasma

The Yukawa one-component plasma (OCP) is a paradigm model for describing plasmas that contain one component of interest and one or more other components that can be treated as a neutralizing, screening background. In appropriately scaled units, interactions are characterized entirely by a screening parameter, κ. As a result, systems of similar κ show the same dynamics, regardless of the underlying parameters (e.g., density and temperature). We demonstrate this behavior using ultracold neutral plasmas (UNP) created by photoionizing a cold (T ≤ 10mK) gas. The ions in UNP systems are well described by the Yukawa model, with the electrons providing the screening. Creation of the plasma through photoionization can be thought of as a rapid quench from κ0 = ∞ to a final κ value set by the electron density and temperature. We demonstrate experimentally that the post-quench dynamics are universal in κ over a factor of 30 in density and an order of magnitude in temperature. Results are compared with molecular dynamics simulations. We also demonstrate that features of the post-quench kinetic energy evolution, such as disorderinduced heating and kinetic-energy oscillations, can be used to determine the plasma density and the electron temperature.
Adaptive Approximation of Functions with Discontinuities

One of the basic principles of Approximation Theory is that the quality of approximations increase with the smoothness of the function to be approximated. Functions that are smooth in certain subdomains will have good approximations in those subdomains, and these {\em sub-approximations} can possibly be calculated efficiently in parallel, as long as the subdomains do not overlap. This paper proposes a class of algorithms that first calculate sub-approximations on non-overlapping subdomains, then extend the subdomains as much as possible and finally produce a global solution on the given domain by letting the subdomains fill the whole domain. Consequently, there will be no Gibbs phenomenon along the boundaries of the subdomains. Throughout, the algorithm works for fixed scattered input data of the function itself, not on spectral data, and it does not resample.
Phenomenological Description of the Interior of the Schwarzschild Black Hole

We discuss a sufficiently large 4-dimensional Schwarzschild black hole which is in equilibrium with a heat bath. In other words, we consider a black hole which has grown up from a small one in the heat bath adiabatically. We express the metric of the interior of the black hole in terms of two functions: One is the intensity of the Hawking radiation, and the other is the ratio between the radiation energy and the pressure in the radial direction. Especially in the case of conformal matters we check that it is a self-consistent solution of the semi-classical Einstein equation, $G_{\mu\nu}=8\pi G \langle T_{\mu\nu}\rangle$. It is shown that the strength of the Hawking radiation is proportional to the c-coefficient, that is, the coefficient of the square of the Weyl tensor in the 4-dimensional Weyl anomaly.
Spinorial geometry, horizons and superconformal symmetry in six dimensions

The spinorial geometry method of solving Killing spinor equations is reviewed as it applies to six-dimensional (1,0) supergravity. In particular, it is explained how the method is used to identify both the fractions of supersymmetry preserved by and the geometry of all supersymmetric backgrounds. Then two applications are described to systems that exhibit superconformal symmetry. The first is the proof that some six-dimensional black hole horizons are locally isometric to AdS3 × Σ3, where Σ3 is diffeomeorphic to S3. The second one is a description of all supersymmetric solutions of six-dimensional (1,0) superconformal theories and in particular of their brane solitons.
CHARACTERIZING THE EVOLVING X-RAY SPECTRAL FEATURES DURING A SUPERBURST FROM 4U 1636–536

Recent studies have shown that runaway thermonuclear burning of material accreted onto neutron stars, i.e., Type I X-ray bursts, may affect the accretion disk. We investigate this by performing a detailed time-resolved spectral analysis of the superburst from 4U 1636–536 observed in 2001 with the Rossi X-Ray Timing Explorer. Superbursts are attributed to the thermonuclear burning of carbon, and are approximately 1000 times more energetic than the regular short Type I bursts. This allows us to study detailed spectra for over 11 ks, compared to, at most, 100 s for regular bursts. A feature is present in the superburst spectra around 6.4 keV that is well fit with an emission line and an absorption edge, suggestive of reflection of the superburst off the accretion disk. The line and edge parameters evolve over time: the edge energy decreases from 9.4 keV at the peak to 8.1 keV in the tail, and both features become weaker in the tail. This is only the second superburst for which this has been detected and shows that this behavior is present even without strong radius expansion. Furthermore, we find the persistent flux more than doubles during the superburst and returns to the pre-superburst value in the tail. The combination of reflection features and increased persistent emission indicates that the superburst had a strong impact on the inner accretion disk and it emphasizes that X-ray bursts provide a unique probe of accretion physics.
Explicit secular equations for piezoacoustic surface waves: Rayleigh modes

The existence of a two-partial Rayleigh wave coupled to an electrical field in 2 mm piezoelectric crystals is known but has rarely been investigated analytically. It turns out that the Z cut X propagation problem can be fully solved, up to the derivation of the secular equation as a polynomial in the squared wave speed. For the metallized (unmetallized) boundary condition, the polynomial is of degree 10 (48). The relevant root is readily identified and the full description of the mechanical and electrical fields follows. The results are illustrated in the case of the superstrong piezoelectric crystal, potassium niobate, for which the effective piezoelectric coupling coefficient is calculated to be about 0.1.
EQUIVALENT NORMS WITH AN EXTREMELY NONLINEABLE SET OF NORM ATTAINING FUNCTIONALS

We present a construction that enables one to find Banach spaces $X$ whose sets $\operatorname{NA}(X)$ of norm attaining functionals do not contain two-dimensional subspaces and such that, consequently, $X$ does not contain proximinal subspaces of finite codimension greater than one, extending the results recently provided by Read [Banach spaces with no proximinal subspaces of codimension 2, Israel J. Math. (to appear)] and Rmoutil [Norm-attaining functionals need not contain 2-dimensional subspaces, J. Funct. Anal. 272 (2017), 918–928]. Roughly speaking, we construct an equivalent renorming with the requested properties for every Banach space $X$ where the set $\operatorname{NA}(X)$ for the original norm is not “too large”. The construction can be applied to every Banach space containing $c_{0}$ and having a countable system of norming functionals, in particular, to separable Banach spaces containing $c_{0}$ . We also provide some geometric properties of the norms we have constructed.
Compact sources in the Bologna Complete Sample: high-resolution VLA observations and optical data

Context. Among radio galaxies, compact sources are a class of objects that are not yet well understood, and most of them cannot be included in classical populations of compact radio sources (flat-spectrum or compact steep-spectrum sources). Aims. Our main goal is to analyze the radio and optical properties of a sample of compact sources and compare them with Faranoff-Riley I and II extended radio galaxies. Methods. We selected in the Bologna Complete Sample a subsample of compact sources, naming it the C BCS sample. We collected new and literature subarcsecond resolution multi-frequency VLA images and optical data. We compared total and nuclear radio power with optical emission line measurements. Results. The [OIII] luminosity − 408 MHz total power relation found in high- and low-excitation galaxies as well as in young (CSS) sources holds also for the C BCSs. However, C BCSs present higher [OIII] luminosity than expected at a given total radio power, and they show the same correlation as core radio galaxies, but with a higher radio power. Conclusions. The C BCSs appear to be the high-power tail of core radio galaxies. For most of the C BCSs, the morphology seems to be strongly dependent on the presence of dense environments (e.g., cluster or HI-rich galaxies) and on a young age or restarted radio activity.
On-chip single photon emission from an integrated semiconductor quantum dot into a photonic crystal waveguide

We demonstrate the in-plane emission of highly polarized single photons from an InAs quantum dot embedded into a photonic crystal waveguide. The spontaneous emission rates are Purcell-enhanced by the coupling of the quantum dot to a slow-light mode of the waveguide. Photon-correlation measurements confirm the sub-Poissonian statistics of the in-plane emission. Under optical pulse excitation, single photon emission rates of up to 19 MHz into the guided mode are demonstrated, which corresponds to a device efficiency of 24%. These results herald the monolithic integration of sources in photonic quantum circuits.
Diet and vegetation impacts of a reintroduced bison herd

DIET AND VEGETATION IMPACTS OF A REINTRODUCED BISON HERD Ryan Christopher Blackburn, M.S. Department of Biological Sciences Northern Illinois University, 2018 Dr. Holly P. Jones, Thesis Director To redress prairie loss, managers seed former agricultural lands and reinstate key ecosystem processes with prescribed fires and reintroduction of native grazers to create restored prairies. Bison (Bison bison) were almost hunted to extinction in the late 1800’s but are recovering and have recently been reintroduced to restored prairies for their ecosystemengineering roles. The effects bison and fire have on remnant (never-plowed) prairie vegetation are well documented. However, there is little known about how bison will affect and shape vegetation patterns in restored prairies. These effects may be largely driven by bison’s dietary preference to forage primarily on grasses. This study aims to quantify both bison diet and their effects on vegetation in a chronosequence of restored prairie with varied burning regimes. We used stable isotope analysis to quantify δ13C and δ15N in plants and bison hair to estimate the probability distributions for the proportional spread of bison diet constituents. Plant composition was measured across a chronosequence of restored prairie with varied grazing and fire regimes. We found that bison primarily grazed on C4 grass species throughout the late spring and early summer. However, bison foraged more on wetland species and high δN forbs in the late summer and fall. Plant diversity decreased with restoration age and did not differ among either grazing or fire treatments. However, grazed sites displayed a wider range of variation between plant communities. Older restorations tended to be more similar in species and functional group composition in comparison to the younger sites. The high contribution of wetland species in bison diet may be dampening their impacts on plant communities in the tallgrass prairie sites. Even though bison and fire did not have as important of a role as we predicted, changes in composition hint at bison impacts beginning to occur within these restored tallgrass prairies after three years of reintroduction. NORTHERN ILLINOIS UNIVERSITY DEKALB, ILLINOIS
PROBING THE TERRESTRIAL REGIONS OF PLANETARY SYSTEMS: WARM DEBRIS DISKS WITH EMISSION FEATURES

Observations of debris disks allow for the study of planetary systems, even where planets have not been detected. However, debris disks are often only characterized by unresolved infrared excesses that resemble featureless blackbodies, and the location of the emitting dust is uncertain due to a degeneracy with the dust grain properties. Here, we characterize the Spitzer Infrared Spectrograph spectra of 22 debris disks exhibiting 10 μm silicate emission features. Such features arise from small warm dust grains, and their presence can significantly constrain the orbital location of the emitting debris. We find that these features can be explained by the presence of an additional dust component in the terrestrial zones of the planetary systems, i.e., an exozodiacal belt. Aside from possessing exozodiacal dust, these debris disks are not particularly unique; their minimum grain sizes are consistent with the blowout sizes of their systems, and their brightnesses are comparable to those of featureless warm debris disks. These disks are in systems of a range of ages, though the older systems with features are found only around A-type stars. The features in young systems may be signatures of terrestrial planet formation. Analyzing the spectra of unresolved debris disks with emission features may be one of the simplest and most accessible ways to study the terrestrial regions of planetary systems.
Photometric study of open clusters Berkeley 96, Berkeley 97, King 12, NGC 7261, NGC 7296 and NGC 7788

We present BV RcIc CCD photometry in the fields of six Galactic open clusters toward the Perseus spiral arm. These data, complemented with J, H, and KS magnitudes from 2MASS, have been used to determine the ages, distances, and colour excesses E(B V ) for these clusters: 40 Myr, 3180 +440 380 pc, 0.54±0.03 mag (Berkeley 96); 250 Myr, 2410 +220 200 pc, 0.77±0.06 mag (Berkeley 97); 70 Myr, 2490 +180 170 pc, 0.51±0.05 mag (King 12); 160 Myr, 2830 +160 150 pc, 0.88 ± 0.09 mag (NGC 7261); 280 Myr, 2450 +190 170 pc, 0.24 ± 0.03 mag (NGC 7296); and 160 Myr, 2750 +220 210 pc, 0.49 ± 0.02 mag (NGC 7788). We found gaps in the mass function of clusters Be 97, King 12, and NGC 7788 in the mass intervals of [1.3–1.5], [1.4–1.6], and [1.5–1.7] solar masses, respectively.
Searching for the missing iron mass in the core of the Centaurus cluster

We re-analyse a combined 198 ks Chandra observation of NGC4696, the brightest galaxy of the Centaurus cluster. We extract temperature and metallicity profiles from the data, and we confirm the presence of a sharp drop in iron abundance, from ~1.8 Zsolar to ~0.4 Zsolar, within the central 5 kpc of the cluster. We estimate that this abundance drop corresponds to a total "missing" iron mass of 1.4e06 Msolar. We propose that part of this missing iron is locked up in cool (~19 K) far-IR emitting dust, as found by Spitzer and Herschel observations. This can occur if the iron injected by stellar mass loss in the central region is in grains, which remain in that form as the injected dusty cold gas mixes and joins the cold dusty filamentary nebula observed within the same region. The bubbling feedback process observed in the cluster core then drags filaments outward and dumps them at 10-20 kpc radius, where the metallicity is high.
HATS9-b AND HATS10-b: TWO COMPACT HOT JUPITERS IN FIELD 7 OF THE K2 MISSION

We report the discovery of two transiting extrasolar planets by the HATSouth survey. HATS-9b orbits an old (10.8 ± 1.5 Gyr) V = 13.3 G dwarf star with a period P ≈ 1.9153 ? > days. The host star has a mass of 1.03 M ☉ ? > , radius of 1.503 R ☉ ? > , and effective temperature 5366 ± 70 K. The planetary companion has a mass of 0.837 M J ? > and radius of 1.065 R J ? > , yielding a mean density of 0.85 g cm - 3 ? > . HATS-10b orbits a V = 13.1 G dwarf star with a period P ≈ 3.3128 ? > days. The host star has a mass of 1.1 M ☉ ? > , radius of 1.11 R ☉ ? > , and effective temperature 5880 ± 120 K. The planetary companion has a mass of 0.53 M J ? > and radius of 0.97 R J ? > , yielding a mean density of 0.7 g cm - 3 ? > . Both planets are compact in comparison with planets receiving similar irradiation from their host stars and lie in the nominal coordinates of Field 7 of K2, but only HATS-9b falls on working silicon. Future characterization of HATS-9b with the exquisite photometric precision of the Kepler telescope may provide measurements of its reflected light signature.
Dynamical linear modeling estimates of long-term ozone trends from homogenized Dobson Umkehr proﬁles

Six collocated spectrophotometers based in Arosa/Davos, Switzerland, have been measuring ozone proﬁles continuously since 1956 for the oldest Dobson instrument and since 2005 for the Brewer instruments. The datasets of these two ground-based triads (three Dobsons and three Brewers) allow for continuous intercom-parisons and derivation of long-term trend estimates. Mainly, two periods in