Miracle-dz/UniFAR-FTUs huggingface dataset:
THE EFFECT OF DISSIPATION ON THE SHAPES OF DARK HALOS

The dissipative infall of gas during the formation of a galaxy modifies the density profile and shape of the dark halo. Gas dissipates energy radiatively and sinks to the center of the dark halo forming the luminous part of a galaxy. The resulting central density enhancement can alter the halo's orbital distribution. We simulate dissipative infall inside of an initially triaxial N-body dark halo by slowly growing a potential in the center of the particle distribution. The dark halo transforms from a prolate-triaxial halo ($T \sim 0.8$) to an oblate-triaxial halo ($T \sim 0.5$) while approximately preserving the flattening ($c/a \sim 0.5$). The main implication is that dark halos are rounder and more oblate than previous predictions of purely collisionless simulations with the new constraint that $b/a \gapp 0.7$. At the same time, the distribution of intrinsic flattenings of dark halos ($\langle c/a \rangle = 0.5$, $\langle (c/a)^2 \rangle ^{1/2} = 0.15$) is preserved during the period of baryonic infall. The oval distortions of disk galaxies should therefore be slightly less than original predictions from collisionless dark halos. The predicted distribution of shapes for dark halos from cosmological N-body simulations is in better agreement with distribution of ellipticities of elliptical galaxies if we assume all halos and galaxies become oblate-triaxial in response to baryonic dissipation. The observed distribution of kinematic misalignment angles is also consistent with this shape distribution if
Predictors of Gastrin Elevation Following Proton Pump Inhibitor Therapy

Supplemental Digital Content is available in the text. Goals: The goal of this study was to elucidate the most important predictors for elevation of gastrin in patients on long-term PPI therapy through analysis of data from 2 published studies in Icelandic patients with erosive GERD. Background: Gastrin elevation is a known but variable consequence of proton pump inhibitor (PPI) therapy. Concerns have been raised about the clinical importance of chronic PPI induced gastrin elevation. Study: This cross-sectional analysis included patients with endoscopically verified erosive esophagitis receiving long-term PPI therapy. PPI exposure in dosage over weight (mg/kg) and dosage over body surface area (mg/m2) was compared with fasting gastrin levels in two separate multiple linear regression models. Data was collected on age, gender, weight, H. pylori infection, smoking, PPI duration and type. Results: Overall data from 157 patients (78 females) were analyzed. Median serum gastrin levels were higher in females than males (92 vs. 60 pg/mL; P=0.001). Simple linear regression showed a correlation between serum gastrin levels and gender (P=0.0008) as well as PPI exposure in mg/kg (P=0.0001) and mg/m2 (P=0.0001). Multiple linear regression analysis showed that PPI exposure, both in mg/kg (β=0.95 [CI=0.4-1.5]; P=0.001) and mg/m2 (β=0.02 [CI=0.0-0.0]; P=0.0015) along with female gender (β=0.2 [CI=0.0-0.4]; P=0.02) predicted higher gastrin values. Conclusions: Dosage and female gender seem to play an important role in the development of gastrin elevation on PPI therapy. A significant correlation was found between fasting serum gastrin and dosage of PPIs over weight and body surface area.
A Python Calculator for Supernova Remnant Evolution

A freely available Python code for modeling supernova remnant (SNR) evolution has been created. This software is intended for two purposes: to understand SNR evolution and to use in modeling observations of SNR for obtaining good estimates of SNR properties. It includes all phases for the standard path of evolution for spherically symmetric SNRs. In addition, alternate evolutionary models are available, including evolution in a cloudy ISM, the fractional energy-loss model, and evolution in a hot low-density ISM. The graphical interface takes in various parameters and produces outputs such as shock radius and velocity versus time, as well as SNR surface brightness profile and spectrum. Some interesting properties of SNR evolution are demonstrated using the program.
Light–matter interactions in multi-element resonators

We investigate light–matter interactions in multi-element optical resonators and provide a roadmap for the identification of structural resonances and the description of the interaction of single extended cavity modes with quantum emitters or mechanical resonators. Using a first principle approach based on the transfer matrix formalism we analyze, both numerically and analytically, the static and dynamical properties of three- and four-mirror cavities. We investigate in particular conditions under which the confinement of the field in specific subcavities allows for enhanced light–matter interactions in the context of cavity quantum electrodynamics and cavity optomechanics.
Tidally induced bars in Illustris galaxies

We study barred galaxies selected from the Illustris cosmological simulation, focusing on tidally induced bars formed from flyby interactions. To guarantee high enough resolution we focus on high mass disc galaxies ($M_*>8.3 \times 10^{10} M_{\odot}$). We find that the fraction of barred galaxies among those (21% at redshift $z=0$) is lower in Illustris than observed in the local Universe, and the fraction grows slightly with redshift. The bar fraction also increases with the stellar mass and decreases with the amount of gas in the disc. Only very few bars at redshift $z=0$ are formed in secular evolution ($\sim$ 7%) and most of them are triggered by external perturbers in mergers or flybys. Many of these bars disappear over time, mostly during secular evolution, which leads to a lower fraction of bars at redshift $z=0$. We then focus on the effect of flyby interactions on the disc and look at tidally induced bars created by a flyby, or pre-existing bars influenced by the passage of a perturber. In the latter case, the interaction can enhance or weaken the bar. During the interaction, the change in the bar strength occurs right after the pericentre passage. The resulting tidally induced bars tend to be stronger than the overall bar sample in Illustris. The preferred scenario to create or enhance a bar seems to be with a strong interaction involving a perturber on a prograde orbit. Furthermore, the strength of the created bar grows with the strength of the interaction.
Dynamical ionization ignition of clusters in intense short laser pulses

The electron dynamics of rare-gas clusters in laser fields is investigated quantum mechanically by means of time-dependent density-functional theory. The mechanism of early inner and outer ionization is revealed. The formation of an electron wave packet inside the cluster shortly after the first removal of a small amount of electron density is observed. By collisions with the cluster boundary the wave-packet oscillation is driven into resonance with the laser field, hence leading to higher absorption of laser energy. Inner ionization is increased because the electric field of the bouncing electron wave packet adds up constructively to the laser field. The fastest electrons in the wave packet escape from the cluster as a whole so that outer ionization is increased as well.
3D modelling of HCO + and its isotopologues in the low-mass proto-star IRAS16293-2422

Ions and electrons play an important role in various stages of the star formation process. By following the magnetic field of their environment and interacting with neutral species, they slow down the gravitational collapse of the proto-star envelope. This process (known as ambipolar diffusion) depends on the ionisation degree, which can be derived from the \hco abundance. We present a study of \hco and its isotopologues (H$^{13}$CO$^+$, HC$^{18}$O$^+$, DCO$^+$, and H$^{13}$CO$^+$) in the low-mass proto-star IRAS16293$-$2422. The structure of this object is complex, and the HCO$^+$ emission arises from the contribution of a young NW-SE outflow, the proto-stellar envelope and the foreground cloud. We aim at constraining the physical parameters of these structures using all the observed transitions. For the young NW-SE outflow, we derive $T_{\rm kin}=180-220$ K and $n({\rm H_2})=(4-7)\times10^6$ cm$^{-3}$ with an HCO$^+$ abundance of $(3-5)\times10^{-9}$. Following previous studies, we demonstrate that the presence of a cold ($T_{\rm kin}$$\leqslant$30 K) and low density ($n({\rm H_2})\leqslant1\times10^4$ cm$^{-3}$) foreground cloud is also necessary to reproduce the observed line profiles. We have used the gas-grain chemical code \textsc{nautilus} to derive the HCO$^+$ abundance profile across the envelope and the external regions where X(HCO$^+$)$\gtrsim1\times10^{-9}$ dominate the envelope emission. From this, we derive an ionisation degree of $10^{-8.9}\,\lesssim\,x(e)\,\lesssim\,10^{-7.9}$. The ambipolar diffusion timescale is $\sim$5 times the free-fall timescale, indicating that the magnetic field starts to support the source against gravitational collapse and the magnetic field strength is estimated to be $6-46 \mu$G.
Evidence for a maximum mass cut-off in the neutron star mass distribution and constraints on the equation of state

We infer the mass distribution of neutron stars in binary systems using a flexible Gaussian mixture model and use Bayesian model selection to explore evidence for multi-modality and a sharp cut-off in the mass distribution. We find overwhelming evidence for a bimodal distribution, in agreement with previous literature, and report for the first time positive evidence for a sharp cut-off at a maximum neutron star mass. We measure the maximum mass to be $2. 0M_\odot 2M_\odot$ neutron stars, our inference of $m_\mathrm{max}$ is able to distinguish between models at odds ratios of up to $12:1$, whilst under a flexible piecewise polytropic equation of state model our maximum mass measurement improves constraints on the pressure at $3-7\times$ the nuclear saturation density by $\sim 30-50\%$ compared to simply requiring $m_\mathrm{max}> 2M_\odot$. We obtain a lower bound on the maximum sound speed attained inside the neutron star of $c_s^\mathrm{max} > 0.63c$ (99.8\%), ruling out $c_s^\mathrm{max} < c/\sqrt{3}$ at high significance. Our constraints on the maximum neutron star mass strengthen the case for neutron star-neutron star mergers as the primary source of short gamma-ray bursts.
3D Topological Kondo Insulators

Topological Kondo insulators (TKIs) are new type of symmetry-protected topological insulators, which develop through the interplay of strong correlations and spin-orbit interactions. In these materials, the bulk is a perfect band insulator due to Kondo screening of localized moments via conduction electrons. Furthermore, strong spin-orbit coupling (SOC) and crystal field effect (CFE) of the localized moments result in a nonlocal odd-parity, time-reversal invariant hybridization between the local-moments and conduction bands, which creates a ground-state with nontrivial topology and gapless surface excitations (Physical Review Letters 104 (2010) 106408). In the present work, we develop a self-consistent theory to study topological Kondo insulators at the mean-field level. To achieve this, we apply slave-boson mean-field theory for a system with and without periodic boundary conditions, in order to study the system at bulk and slab geometry configuration. This enables us to observe a clear signature of protected edge states through band structure and calculation of spectral functions.
CRIRES high-resolution infrared spectroscopy of the long-period Cepheid l Carinae

Context. The dynamical structure of the atmosphere of Cepheids has been well studied in the optical. Several authors have found very interesting spectral features in the J band, but little data have been secured beyond 1.6 μm. However, such observations can probe different radial velocities and line asymmetry regimes, and are able to provide crucial insights into stellar physics. Aims. Our goal was to investigate the infrared line-forming region in the K-band domain, and its impact on the projection factor and the k-term of Cepheids. Methods. We secured CRIRES observations for the long-period Cepheid l Car, with a focus on the unblended spectral line NaI 2208.969 nm. We measured the corresponding radial velocities (by using the first moment method) and the line asymmetries (by using the bi-Gaussian method). These quantities are compared to the HARPS visible spectra we previously obtained on l Car. Results. The optical and infrared radial velocity curves show the same amplitude (only about 3% of difference), with a slight radial velocity shift of about 0.5 ± 0.3 km s−1 between the two curves. Around the minimum radius (phase ≃ 0.9) the visible radial velocity curve is found in advance compared to the infrared one (phase lag), which is consistent with an infrared line forming higher in the atmosphere (compared to the visible line) and with a compression wave moving from the bottom to the top of the atmosphere during maximum outward velocity. The asymmetry of the K-band line is also found to be significantly different from that of the optical line.
Small Groups of Galaxies: a Clue to a Critical Universe

We study the formation and the evolution of galaxy groups in a critical universe, showing the importance of secondary infall for their dynamical evolution. Merging is only slightly accelerated if galaxies have massive halos, because the mass initially associated to the individual galaxies is soon tidally stripped. Stripping is particularly effective for infalling galaxies, which thus avoid merging. We find that, as a rule, merging is effectively terminated when infall becomes dominant. We look for compact groups in our ensemble of simulations, and compare their statistical properties with Hickson's compact groups. We then discuss in terms of the Press & Schechter formalism the statistics of such groups and their evolution in different cosmological scenarios. We show that compact group formation is an ongoing and frequent process in a critical universe. Our model reconciles the contradiction between the observed absence of young merger remnants and the high rate of galaxy interactions expected in compact groups. In open universes, instead, earlier formation of groups and suppression of secondary infall makes it more unlikely that compact groups survive as such until the present. We conclude that the existence of dense and dynamically young groups of galaxies like HCGs points towards a high-density universe.
Defining patterns of care in the management of patients with brain metastases in a large oncology centre: A single-centre retrospective audit of 236 cases.

AIMS The role of selected treatments for brain metastases (BM) is well documented; however, the prevalence of these is not. We report on the patterns of care in the management of BM in a large oncology centre. MATERIALS AND METHODS We retrospectively audited 236 cases of newly diagnosed BM from January 2016 to December 2017 by looking at 2 years of radiology reports and gathered data on primary site, survival, treatment received, palliative care input and brain metastases-related admissions. RESULTS Eighty-two per cent of cases were related to lung, breast and melanoma primaries. Half of patients received a form of treatment with the other half receiving best supportive care. Of these, whole-brain radiotherapy (39%) and stereotactic radiosurgery (40%) were the most common treatment modalities. Most common reasons for admissions were headaches, seizures, weakness and confusion. CONCLUSION This is the first study in the UK that gives an in-depth overview of the real-world management of brain metastases. We have demonstrated the prevalence of treatment across the spectrum of brain metastases patients. Radiotherapy is the mainstay of treatment in nearly 80% of cases; however, care needs to be taken in ensuring that SRS is offered to those who are suitable.
A Systematic Comparison of Tropical Waves over Northern Africa. Part I: Influence on Rainfall

Low-latitude rainfall variability on the daily to intraseasonal time scale is often related to tropical waves, including convectively coupled equatorial waves, the Madden–Julian oscillation (MJO), and tropical disturbances (TDs). Despite the importance of rainfall variability for vulnerable societies in tropical Africa, the relative influence of tropical waves for this region is largely unknown. This article presents the first systematic comparison of the impact of six wave types on precipitation over northern tropical Africa during the transition and full monsoon seasons, using two satellite products and a dense rain gauge network. Composites of rainfall anomalies in the different datasets show comparable modulation intensities in the West Sahel and at the Guinea Coast, varying from less than 2 to above 7 mm day−1 depending on the wave type. African easterly waves (AEWs) and Kelvin waves dominate the 3-hourly to daily time scale and explain 10%–30% locally. On longer time scales (7–20 days), only the MJO and equatorial Rossby (ER) waves remain as modulating factors and explain about up to one-third of rainfall variability. Eastward inertio-gravity waves and mixed Rossby–gravity (MRG) waves are comparatively unimportant. An analysis of wave superposition shows that low-frequency waves (MJO, ER) in their wet phase amplify the activity of high-frequency waves (TD, MRG) and suppress them in the dry phase. The results stress that more attention should be paid to tropical waves when forecasting rainfall over northern tropical Africa.
Fault-tolerant Quantum Computation with Highly Verified Logical Cluster States

We investigate a scheme of fault-tolerant quantum computation based on the cluster model. Logical qubits are encoded by a suitable code such as the Steane's 7-qubit code. Cluster states of logical qubits are prepared by post-selection through verification at high fidelity level, where the unsuccessful ones are discarded without recovery operation. Then, gate operations are implemented by transversal measurements on the prepared logical cluster states. The noise threshold is improved significantly by making the high fidelity preparation and transversal measurement. It is estimated to be about 3% by a numerical simulation.
Unit root tests using semi-parametric estimators of the long-memory parameter

Time series where the mean-level changes with time are known as non-stationary processes or processes having a unit root. In this context, for a series to be stationary it needs to be differentiated a sufficient number of times, where the number of differences is known as the integration order I(d). Classical tests for unit root processes consider an integer order of integration, where the null and alternative hypotheses are I(1) and I(0), respectively. However, recently, some research has shown a refinement of these hypotheses where 0≤d≤1. This kind of analysis can be obtained through fractional processes, also known as long-memory models. In this work, we propose, for testing unit roots, the use of the semi-parametric estimator of the fractional parameter of the ARFIMA model suggested by Geweke and Porter-Hudak [Geweke, J. and Porter-Hudak, S. , 1983, The estimation and application of long memory time series model. Journal of Time Series Analysis, 4(4), 221–238. ], GPH, and a bootstrap version of this test, GPH*. Through Monte Carlo experiments, we observed that the GPH and GPH* tests presented higher power than the classic ADF test [Said, S.E. and Dickey, D.A. , 1984, Testing for unit roots in autoregressive moving average models of unknown order. Biometrika, 71, 599–607. ] to unit roots, when in the alternative hypothesis d is fractional.
SILVERRUSH. III. Deep Optical and Near-Infrared Spectroscopy for Lya and UV-Nebular Lines of Bright Lya Emitters at z=6-7

We present Lya and UV-nebular emission line properties of bright Lya emitters (LAEs) at z=6-7 with a luminosity of log L_Lya/[erg s-1] = 43-44 identified in the 21-deg2 area of the SILVERRUSH early sample developed with the Subaru Hyper Suprime-Cam (HSC) survey data. Our optical spectroscopy newly confirm 21 bright LAEs with clear Lya emission, and contribute to make a spectroscopic sample of 96 LAEs at z=6-7 in SILVERRUSH. From the spectroscopic sample, we select 7 remarkable LAEs as bright as Himiko and CR7 objects, and perform deep Keck/MOSFIRE and Subaru/nuMOIRCS near-infrared spectroscopy reaching the 3sigma-flux limit of ~ 2x10^{-18} erg s-1 for the UV-nebular emission lines of He II1640, C IV1548,1550, and O III]1661,1666. Except for one tentative detection of C IV, we find no strong UV-nebular lines down to the flux limit, placing the upper limits of the rest-frame equivalent widths (EW_0) of ~2-4 A for He II, C IV, and O III] lines. Here we also investigate the VLT/X-SHOOTER spectrum of CR7 whose 6 sigma detection of He II is claimed by Sobral et al. Although two individuals and the ESO-archive service carefully re-analyze the X-SHOOTER data that are used in the study of Sobral et al., no He II signal of CR7 is detected, supportive of weak UV-nebular lines of the bright LAEs even for CR7. Spectral properties of these bright LAEs are thus clearly different from those of faint dropouts at z~7 that have strong UV-nebular lines shown in the various studies. Comparing these bright LAEs and the faint dropouts, we find anti-correlations between the UV-nebular line EW_0 and UV-continuum luminosity, which are similar to those found at z~2-3.
Intra-Brillouin-zone bandgaps due to periodic misalignment in one-dimensional magnetophotonic crystals

One-dimensional (1D) magnetophotonic crystals (MPCs) can incorporate optical gyrotropy induced by a bias magnetic field, crystalline misalignment, and differential linear birefringence in a single photonic-crystal structure. A 1D MPC whose unit cell contains two layers—one magnetophotonic, the other not—displays intra-Brillouin-zone photonic bandgaps (PBGs) in the Brillouin diagram. While the optical gyrotropy makes the PBG bandwidths tunable by a bias magnetic field, the bicrystalline misalignment modifies and can even trump this magnetic tunability. Magnetic tunability is greatly affected by a proper selection of the two materials; e.g., a large birefringence ratio between the two layers can dramatically enhance the magnetic tunability of the MPC. We also expect our 1D MPCs to be useful for detecting magnetic fields.
CROSS-CORRELATING THE γ-RAY SKY WITH CATALOGS OF GALAXY CLUSTERS

We report the detection of a cross-correlation signal between Fermi Large Area Telescope diffuse γ-ray maps and catalogs of clusters. In our analysis, we considered three different catalogs: WHL12, redMaPPer, and PlanckSZ. They all show a positive correlation with different amplitudes, related to the average mass of the objects in each catalog, which also sets the catalog bias. The signal detection is confirmed by the results of a stacking analysis. The cross-correlation signal extends to rather large angular scales, around 1°, that correspond, at the typical redshift of the clusters in these catalogs, to a few to tens of megaparsecs, i.e., the typical scale-length of the large-scale structures in the universe. Most likely this signal is contributed by the cumulative emission from active galactic nuclei (AGNs) associated with the filamentary structures that converge toward the high peaks of the matter density field in which galaxy clusters reside. In addition, our analysis reveals the presence of a second component, more compact in size and compatible with a point-like emission from within individual clusters. At present, we cannot distinguish between the two most likely interpretations for such a signal, i.e., whether it is produced by AGNs inside clusters or if it is a diffuse γ-ray emission from the intracluster medium. We argue that this latter, intriguing, hypothesis might be tested by applying this technique to a low-redshift large-mass cluster sample.