Miracle-dz/UniFAR-FTUs huggingface dataset:
Gaps, rings, and non-axisymmetric structures in protoplanetary disks - Emission from large grains

Dust grains with sizes around (sub)mm are expected to couple only weakly to the gas motion in regions beyond 10 au of circumstellar disks. In this work, we investigate the influence of the spatial distribution of such grains on the (sub)mm appearance of magnetized protoplanetary disks. We perform non-ideal global 3D magneto-hydrodynamic stratified disk simulations including particles of different sizes (50 micron to 1 cm), using a Lagrangian particle solver. We calculate the spatial dust temperature distribution, including the dynamically coupled submicron-sized dust grains, and derive ideal continuum re-emission maps of the disk through radiative transfer simulations. Finally, we investigate the feasibility to observe specific structures in the thermal re-emission maps with the Atacama Large Millimeter/submillimeter Array (ALMA). The pressure bump close to the outer edge of the dead-zone leads to particle trapping in ring structures. More specifically, vortices in the disk concentrate the dust and create an inhomogeneous distribution of the solid material in the azimuthal direction. The large-scale disk perturbations are preserved in the (sub)mm re-emission maps. The observable structures are very similar to those expected to result from planet-disk interaction. The larger dust particles increase the brightness contrast between gap and ring structures. We find that rings, gaps and the dust accumulation in the vortex could be traced with ALMA down to a scale of a few astronomical units in circumstellar disks located in nearby star-forming regions. Finally, we present a brief comparison of these structures with those recently found with ALMA in the young circumstellar disks of HL Tau and Oph IRS 48.
MUSE deep-fields: the Ly α luminosity function in the Hubble Deep Field-South at 2.91 < z < 6.64

We present the first estimate of the Ly{\alpha} luminosity function using blind spectroscopy from the Multi Unit Spectroscopic Explorer, MUSE, in the Hubble Deep Field South. Using automatic source-detection software, we assemble a homogeneously-detected sample of 59 Ly{\alpha} emitters covering a flux range of -18.0 < log10 (F) < -16.3 (erg s^-1 cm^-2), corresponding to luminosities of 41.4 < log10 (L) < 42.8 (erg s^-1). As recent studies have shown, Ly{\alpha} fluxes can be underestimated by a factor of two or more via traditional methods, and so we undertake a careful assessment of each object's Ly{\alpha} flux using a curve-of-growth analysis to account for extended emission. We describe our self-consistent method for determining the completeness of the sample, and present an estimate of the global Ly{\alpha} luminosity function between redshifts 2.91 < z < 6.64 using the 1/Vmax estimator. We find the luminosity function is higher than many number densities reported in the literature by a factor of 2 - 3, although our result is consistent at the 1{\sigma} level with most of these studies. Our observed luminosity function is also in good agreement with predictions from semi-analytic models, and shows no evidence for strong evolution between the high- and low-redshift halves of the data. We demonstrate that one's approach to Ly{\alpha} flux estimation does alter the observed luminosity function, and caution that accurate flux assessments will be crucial in measurements of the faint end slope. This is a pilot study for the Ly{\alpha} luminosity function in the MUSE deep-fields, to be built on with data from the Hubble Ultra Deep Field which will increase the size of our sample by almost a factor of 10.
Collapse and three-body loss in a 85 Rb Bose-Einstein condensate

Collapsing Bose-Einstein condensates are rich and complex quantum systems for which quantitative explanation by simple models has proved elusive. We present experimental data on the collapse of high-density {sup 85}Rb condensates with attractive interactions and find quantitative agreement with the predictions of the Gross-Pitaevskii equation. The collapse data and measurements of the decay of atoms from our condensates allow us to put new limits on the value of the {sup 85}Rb three-body loss coefficient K{sub 3} at small positive and negative scattering lengths.
Theory of coupled spin-charge transport due to spin-orbit interaction in inhomogeneous two-dimensional electron liquids

Spin-orbit interactions in two-dimensional electron liquids are responsible for many interesting transport phenomena in which particle currents are converted to spin polarizations and spin currents and vice versa. Prime examples are the spin Hall effect, the Edelstein effect, and their inverses. By similar mechanisms, it is also possible to partially convert an optically induced electron-hole density wave to a spin density wave and vice versa. In this paper, we present a unified theoretical treatment of these effects based on quantum kinetic equations that include not only the intrinsic spin-orbit coupling from the band structure of the host material, but also the spin-orbit coupling due to an external electric field and a random impurity potential. The drift-diffusion equations we derive in the diffusive regime are applicable to a broad variety of experimental situations, both homogeneous and nonhomogeneous, and include on equal footing ``skew scattering'' and ``side jump'' from electron-impurity collisions. As a demonstration of the strength and usefulness of the theory we apply it to the study of several effects of current experimental interest: the inverse Edelstein effect, the spin-current swapping effect, and the partial conversion of an electron-hole density wave to a spin density wave in a two-dimensional electron gas with Rashba and Dresselhaus spin-orbit couplings, subject to an electric field.
Association Between Oncology Clinical Pathway Utilization and Toxicity and Cost Outcomes in Patients With Metastatic Solid Tumors

PURPOSE This retrospective observational study compared cancer care toxicity and cost outcomes for patients with metastatic cancer with nine different cancer types prescribed on- versus off-pathway regimens. METHODS This study used claims and authorization data from a national insurer between January 1, 2018, and October 31, 2021. Participants included adults with metastatic breast, lung, colorectal, pancreatic, melanoma, kidney, bladder, gastric, or uterine cancer, who were prescribed first-line anticancer regimens. Multivariable regressions were used to assess outcomes including counts of emergency room visits or hospitalizations, use of supportive care medications, immune-related adverse events (IRAEs), and health care costs. RESULTS Of the 8,357 patients in the study, 5,453 (65.3%) were prescribed on-pathway regimens. The on-pathway proportion trended downward, from 74.3% in 2018 to 59.8% in 2021. The on- and off-pathway groups had a similar proportion of patients with treatment-related hospitalization (adjusted odds ratio [aOR], 1.080; P = .201) and IRAEs (aOR, 0.961; P = .497). More all-cause hospitalizations (aOR, 1.679; P = .013) were observed among patients with melanoma treated on-pathway. The on-pathway group had higher use of supportive care drugs in bladder cancer (aOR, 4.602; P < .001) and colorectal cancer (aOR, 4.465; P < .001), and lower use in breast (aOR, 0.668; P = .001) and lung cancer (aOR, 0.550; P < .001). On average, on-pathway patients incurred $17,589 less total health care cost (P < .001), and $22,543 lower chemotherapy cost (P < .001) than those from the off-pathway group. CONCLUSION Our findings suggest that use of on-pathway regimens was associated with significant cost savings. Toxicity outcomes were variable by disease, but overall, there were similar numbers of treatment-related hospitalizations and IRAEs compared to off-pathway regimens. This cross-institutional study provides evidence to support the use of clinical pathway regimens for patients with metastatic cancer.
NONLINEAR FORCE-FREE FIELD MODELING OF A SOLAR ACTIVE REGION USING SDO/HMI AND SOLIS/VSM DATA

We use SDO/HMI and SOLIS/VSM photospheric magnetic field measurements to model the force-free coronal field above a solar active region, assuming magnetic forces dominate. We take measurement uncertainties caused by, e.g., noise and the particular inversion technique, into account. After searching for the optimum modeling parameters for the particular data sets, we compare the resulting nonlinear force-free model fields. We show the degree of agreement of the coronal field reconstructions from the different data sources by comparing the relative free energy content, the vertical distribution of the magnetic pressure, and the vertically integrated current density. Though the longitudinal and transverse magnetic flux measured by the VSM and HMI is clearly different, we find considerable similarities in the modeled fields. This indicates the robustness of the algorithm we use to calculate the nonlinear force-free fields against differences and deficiencies of the photospheric vector maps used as an input. We also depict how much the absolute values of the total force-free, virial, and the free magnetic energy differ and how the orientation of the longitudinal and transverse components of the HMI- and VSM-based model volumes compare to each other.
The redshift distribution of submillimetre galaxies at different wavelengths

Using simulations we demonstrate that some of the published redshift distributions of submillimetre galaxies (SMGs) at different wavelengths, which were previously reported to be statistically different, are consistent with a parent distribution of the same population of galaxies. The redshift distributions which peak at z_med=2.9, 2.6, 2.2, 2.2, and 2.0 for galaxies selected at 2 and 1.1 mm, and 870, 850, and 450 um respectively, can be derived from a single parent redshift distribution, in contrast with previous studies. The differences can be explained through wavelength selection, depth of the surveys, and to a lesser degree, angular resolution. The main differences are attributed to the temperature of the spectral energy distributions, as shorter-wavelength maps select a hotter population of galaxies. Using the same parent distribution and taking into account lensing bias we can also reproduce the redshift distribution of 1.4 mm-selected ultra-bright galaxies, which peaks at z_med=3.4. However, the redshift distribution of 450 um-selected galaxies in the deepest surveys, which peaks at z_med=1.4, cannot be reproduced from the same parent population with just these selection effects. In order to explain this distribution we have to add another population of galaxies or include different selection biases.
Opportunities for maser studies with the Square Kilometre Array

Abstract The Square Kilometre Array (SKA) is the radio telescope of the next generation, providing an increase in sensitivity and angular resolution of two orders of magnitude over existing telescopes. Currently, the SKA is expected to span the frequency range 0.1-25 GHz with capabilities including a wide field-of-view and measurement of polarised emission. Such a telescope has enormous potential for testing fundamental physical laws and producing transformational discoveries. Important science goals include using H2O megamasers to make precise estimates of H0, which will anchor the extragalactic distance scale, and to probe the central structures of accretion disks around supermassive black holes in AGNs, to study OH megamasers associated with extreme starburst activity in distant galaxies and to study with unprecedented precision molecular gas and star formation in our Galaxy.
Positron-impact ionization and positronium formation from helium

Detailed measurements of the total ionization cross-section by positron impact on He from threshold up to 850 eV are reported. Both the present total ionization cross-section and the direct ionization cross-section of Moxom et al (1996) and Ashley et al (1996) have been normalized to the latest electron-impact ionization cross-sections. The positronium formation cross-section for this target is thus extracted and compared with the existing experimental and theoretical data.
Large Convection Limits for KPP Fronts

This paper is concerned with the KPP equation with strong convection. The asymptotic behavior of the minimal speed of traveling fronts is derived for shear flow convection and for cellular flow convection. In the first case a new limit problem is derived and analyzed. For cellular flows new almost optimal upper bounds are obtained in terms of the wave speed of the homogenized problem. Thereby some conjectures on the asymptotic growth of front speeds are confirmed.
Predicting dust extinction properties of star-forming galaxies from Hα/UV ratio

Using star-forming galaxies sample in the nearby Universe (0.02<z<0.10) selected from the SDSS (DR7) and GALEX all-sky survey (GR5), we present a new empirical calibration for predicting dust extinction of galaxies from H-alpha-to-FUV flux ratio. We find that the H-alpha dust extinction (A(Ha)) derived with H-alpha/H-beta ratio (Balmer decrement) increases with increasing H-alpha/UV ratio as expected, but there remains a considerable scatter around the relation, which is largely dependent on stellar mass and/or H-alpha equivalent width (EW(Ha)). At fixed H-alpha/UV ratio, galaxies with higher stellar mass (or galaxies with lower EW(Ha)) tend to be more highly obscured by dust. We quantify this trend and establish an empirical calibration for predicting A(Ha) with a combination of H-alpha/UV ratio, stellar mass and EW(Ha), with which we can successfully reduce the systematic uncertainties accompanying the simple H-alpha/UV approach by ~15-30%. The new recipes proposed in this study will provide a convenient tool for predicting dust extinction level of galaxies particularly when Balmer decrement is not available. By comparing A(Ha) (derived with Balmer decrement) and A(UV) (derived with IR/UV luminosity ratio) for a subsample of galaxies for which AKARI FIR photometry is available, we demonstrate that more massive galaxies tend to have higher extra extinction towards the nebular regions compared to the stellar continuum light. Considering recent studies reporting smaller extra extinction towards nebular regions for high-redshift galaxies, we argue that the dust geometry within high-redshift galaxies resemble more like low-mass galaxies in the nearby Universe.
2FGL J1653.6−0159: A NEW LOW IN EVAPORATING PULSAR BINARY PERIODS

We have identified an optical binary with orbital period Pb = 4488 s as the probable counterpart of the Fermi source 2FGL J1653.6−0159. Although pulsations have not yet been detected, the source properties are consistent with an evaporating millisecond pulsar binary; this Pb = 75 minutes is the record low for a spin-powered system. The heated side of the companion shows coherent radial-velocity variations, with amplitude K = 666.9 ± 7.5 km s−1 for a large mass function of f(M) = 1.60 ± 0.05 M☉. This heating suggests a pulsar luminosity ∼3 × 1034 erg s−1. The colors and spectra show an additional blue component dominating at binary minimum. Its origin is, at present, unclear. This system is similar to PSR J1311−3430, with a low-mass H-depleted companion, a dense shrouding wind and, likely, a large pulsar mass.
New positron spectral features from supersymmetric dark matter: A way to explain the PAMELA data?

Department of Physics, Stockholm University, AlbaNova University Center, SE - 106 91 Stockholm, Sweden(Dated: August 27, 2008)The space-borne antimatter experiment PAMELA has recently reported a surprising rise in thepositron to electron ratio at high energies. It has also recently been found that electromagneticradiative corrections in some cases may boost the gamma-ray yield from supersymmetric darkmatter annihilations in the galactic halo by up to three or four orders of magnitude, providingdistinct spectral signatures for indirect dark matter searches to look for. Here, we investigatewhether the same type of corrections can also lead to sizeable enhancements in the positron yield.We ﬁnd that this is indeed the case, albeit for a smaller region of parameter space than for gammarays; selecting models with a small mass diﬀerence between the neutralino and sleptons, like inthe stau coannihilation region in mSUGRA, the eﬀect becomes more pronounced. The resulting,rather hard positron spectrum with a relatively sharp cutoﬀ may potentially ﬁt the rising positronratio measured by the PAMELA satellite. To do so, however, very large “boost factors” have tobe invoked that are not expected in current models of halo structure. If the predicted cutoﬀ wouldalso be conﬁrmed by later PAMELA data or upcoming experiments, one could either assume non-thermal production in the early universe or non-standard halo formation to explain such a spectralfeature as an eﬀect of dark matter annihilation. At the end of the paper, we brieﬂy comment onthe impact of radiative corrections on other annihilation channels, in particular antiprotons andneutrinos.
STRATOSPHERIC TEMPERATURES AND WATER LOSS FROM MOIST GREENHOUSE ATMOSPHERES OF EARTH-LIKE PLANETS

A radiative-convective climate model is used to calculate stratospheric temperatures and water vapor concentrations for ozone-free atmospheres warmer than that of modern Earth. Cold, dry stratospheres are predicted at low surface temperatures, in agreement with recent 3D calculations. However, at surface temperatures above 350 K, the stratosphere warms and water vapor becomes a major upper atmospheric constituent, allowing water to be lost by photodissociation and hydrogen escape. Hence, a moist greenhouse explanation for loss of water from Venus, or some exoplanet receiving a comparable amount of stellar radiation, remains a viable hypothesis. Temperatures in the upper parts of such atmospheres are well below those estimated for a gray atmosphere, and this factor should be taken into account when performing inverse climate calculations to determine habitable zone boundaries using 1D models.
A quantitative management support model of a certain production - supply system : boundary conditions

This article is dedicated to constructing a method for the probabilistic analysis of the functioning a certain production-supply system. We continue the research started in the article [8], where, among other things, we derived a set of partial differential equations satisfied by the joint density function of the state of a three-dimensional process characterizing the functioning of the system. In this article the operation of the system at the boundaries of the stock levels is analyzed. Two sets of differential equations are derived, one describing the operation of the system when the stock level is zero and one describing the operation of the system when the stocks are full.
KnowledgePit Meets BrightBox: A Step Toward Insightful Investigation of the Results of Data Science Competitions

We discuss the benefits of integrating the KnowledgePit data science competition platform with the BrightBox technology aimed at diagnostics of machine learning models embedded within complex software systems. We briefly recall the history of international challenges held at KnowledgePit and we also discuss in what sense such technologies as BrightBox can be helpful during the post-challenge analysis. In particular, we show how to combine solutions submitted by the competition participants in order to obtain even more accurate predictions. The discussed functionalities are of significant importance for the sponsors and organizers of data science / machine learning online contests because they support adoption of submissions while designing ultimate solutions of real-world problems.
Cannabinoid Therapeutic Effects in Inflammatory Bowel Diseases: A Systematic Review and Meta-Analysis of Randomized Controlled Trials

(1) Introduction: Inflammatory Bowel Disease (IBD) patients may benefit from cannabinoid administration supplementary therapy; currently no consensus on its effect has been reached. (2) Methods: a systematic review of RCTs on cannabinoid supplementation therapy in IBD has been conducted; data sources were MEDLINE, Scopus, ClinicalTrials. (3) Results: out of 974 papers found with electronic search, six studies have been included into the systematic review, and five of them, for a grand total of 208 patients, were included into the meta-analysis. (4) Conclusions: cannabinoid supplementation as adjuvant therapy may increase the chances of success for standard therapy of Crohn’s Disease during the induction period; no statement on its potential usage during maintenance period can be derived from retrieved evidence. Its usage in Ulcerative Colitis is not to be recommended. If ever, low-dose treatment may be more effective than higher dosage. Mean CDAI reduction was found stronger in patients treated with cannabinoids (mean CDAI reduction = 36.63, CI 95% 12.27–61.19) than placebo. In future studies, it is advisable to include disease activity levels, as well as patient-level information such as genetic and behavioral patterns.
HOST GALAXIES OF LUMINOUS TYPE 2 QUASARS AT z ∼ 0.5

We present deep Gemini GMOS optical spectroscopy of nine luminous quasars at redshifts z ∼ 0.5, drawn from the Sloan Digital Sky Survey type 2 quasar sample. Our targets were selected to have high intrinsic luminosities (MV < −26 mag) as indicated by the [O iii] λ5007 Å emission-line luminosity (L[O iii]). Our sample has a median black hole mass of ∼108.8 M☉ inferred assuming the local MBH–σ* relation and a median Eddington ratio of ∼0.7, using stellar velocity dispersions σ* measured from the G band. We estimate the contamination of the stellar continuum from scattered quasar light based on the strength of broad Hβ, and provide an empirical calibration of the contamination as a function of L[O iii]; the scattered-light fraction is ∼30% of L5100 for objects with L[O iii] = 109.5 L☉. Population synthesis indicates that young poststarburst populations (<0.1 Gyr) are prevalent in luminous type 2 quasars, in addition to a relatively old population (>1 Gyr) which dominates the stellar mass. Broad emission complexes around He ii λ4686 Å with luminosities up to 108.3 L☉ are unambiguously detected in three out of the nine targets, indicative of Wolf–Rayet (WR) populations. Population synthesis shows that ∼5 Myr poststarburst populations contribute substantially to the luminosities (>50% of L5100) of all three objects with WR detections. We find two objects with double cores and four with close companions. Our results may suggest that luminous type 2 quasars trace an early stage of galaxy interaction, perhaps responsible for both the quasar and the starburst activity.