Miracle-dz/UniFAR-FTUs huggingface dataset:
NuSTAR Hard X-Ray Data and Gemini 3D Spectra Reveal Powerful AGN and Outflow Histories in Two Low-redshift Lyα Blobs

We have shown that Lyα blobs (LABs) may still exist even at z ∼ 0.3 , about seven billion years later than most other LABs known (Shirmer et al.). Their luminous Lyα and [O iii] emitters at z ∼ 0.3 offer new insights into the ionization mechanism. This paper focuses on the two X-ray brightest LABs at z ∼ 0.3 , SDSS J0113+0106 (J0113) and SDSS J1155−0147 (J1155), comparable in size and luminosity to “B1,” one of the best-studied LABs at z ≳ 2 . Our NuSTAR hard X-ray (3–30 keV) observations reveal powerful active galactic nuclei (AGN) with L 2 – 10 keV = ( 0.5 – 3 ) × 10 44 erg s−1. J0113 also faded by a factor of ∼5 between 2014 and 2016, emphasizing that variable AGN may cause apparent ionization deficits in LABs. Joint spectral analyses including Chandra data constrain column densities of N H = 5.1 − 3.3 + 3.1 × 10 23 cm−2 (J0113) and N H = 6.0 − 1.1 + 1.4 × 10 22 cm−2 (J1155). J0113 is likely buried in a torus with a narrow ionization cone, but ionizing radiation is also leaking in other directions, as revealed by our Gemini/GMOS 3D spectroscopy. The latter shows a bipolar outflow over 10 kpc, with a peculiar velocity profile that is best explained by AGN flickering. X-ray analysis of J1155 reveals a weakly absorbed AGN that may ionize over a wide solid angle, consistent with our 3D spectra. Extinction-corrected [O iii] log-luminosities are high, ∼43.6. The velocity dispersions are low, ∼100–150 km s−1, even at the AGN positions. We argue that this is a combination of high extinction hiding the turbulent gas and previous outflows that have cleared the escape paths for their successors.
COMPARISON OF THE FRACTURE RESISTANCE BETWEEN INLAY RETAINED FIXED PARTIAL DENTURES FABRICATED FROM MILLED PEEK (BIOHPP) AND MONOLITHIC ZIRCONIA (In vitro study)

Aim: To evaluate the fracture resistance of veneered PEEK Inlay Retained Fixed Partial Dentures (IRFPDs) compared to those fabricated from monolithic zirconia. Materials and methods: Mandibular typodont with removed mandibular first molar was used to receive box inlay cavity preparation on mandibular second molar and second premolar. After tooth preparation, typodont was duplicated into fourteen epoxy models using silicone mold. Epoxy models were randomly divided into two equal groups (n= 7/group). Identical IRFPDs were fabricated from two different materials. For Group I (P/C): IRFPDs were fabricated from Bre. CAM BioHPP blanks and subsequently veneered with composite (Crea.lign). For Group II (MZ): IRFPDs were manufactured using industrially prefabricated monolithic zirconia blocks (Katana HTML). All IRFPDs were bonded to their corresponding epoxy models using adhesive resin cement (Theracem), and underwent thermal cycling (10,000 cycles). Fracture resistance testing was performed on the specimens using a universal testing machine with a crosshead speed of 0.5 mm/ min. Fractured samples were examined using a digital-microscope, with 35x magnification power, to determine failure mode pattern . Results : It was found that MZ group recorded statistically significant higher fracture resistance mean value (1876.198±218.039 N) than P/C group (1282.572±160.154 N). Most failures of MZ group were cohesive in nature, where connector fracture was the predominant failure mode. In P/C group, all failures were adhesive in nature between PEEK framework and composite veneering. Conclusion: When compared to Zirconia, PEEK IRFPDs veneered with composite exhibited sufficient resistance to fracture.
Three-dimensional Features of the Outer Heliosphere Due to Coupling between the Interstellar and Heliospheric Magnetic Field. V. The Bow Wave, Heliospheric Boundary Layer, Instabilities, and Magnetic Reconnection

The heliosphere is formed due to interaction between the solar wind (SW) and local interstellar medium (LISM). The shape and position of the heliospheric boundary, the heliopause, in space depend on the parameters of interacting plasma flows. The interplay between the asymmetrizing effect of the interstellar magnetic field and charge exchange between ions and neutral atoms plays an important role in the SW–LISM interaction. By performing three-dimensional, MHD plasma/kinetic neutral atom simulations, we determine the width of the outer heliosheath—the LISM plasma region affected by the presence of the heliosphere—and analyze quantitatively the distributions in front of the heliopause. It is shown that charge exchange modifies the LISM plasma to such extent that the contribution of a shock transition to the total variation of plasma parameters becomes small even if the LISM velocity exceeds the fast magnetosonic speed in the unperturbed medium. By performing adaptive mesh refinement simulations, we show that a distinct boundary layer of decreased plasma density and enhanced magnetic field should be observed on the interstellar side of the heliopause. We show that this behavior is in agreement with the plasma oscillations of increasing frequency observed by the plasma wave instrument onboard Voyager 1. We also demonstrate that Voyager observations in the inner heliosheath between the heliospheric termination shock and the heliopause are consistent with dissipation of the heliospheric magnetic field. The choice of LISM parameters in this analysis is based on the simulations that fit observations of energetic neutral atoms performed by Interstellar Boundary Explorer.
From cusps to cores: a stochastic model

The cold dark matter model of structure formation faces apparent problems on galactic scales. Several threads point to excessive halo concentration, including central densities that rise too steeply with decreasing radius. Yet, random fluctuations in the gaseous component can 'heat' the centres of haloes, decreasing their densities. We present a theoretical model deriving this effect from first principles: stochastic variations in the gas density are converted into potential fluctuations that act on the dark matter; the associated force correlation function is calculated and the corresponding stochastic equation solved. Assuming a power law spectrum of fluctuations with maximal and minimal cutoff scales, we derive the velocity dispersion imparted to the halo particles and the relevant relaxation time. We further perform numerical simulations, with fluctuations realised as a Gaussian random field, which confirm the formation of a core within a timescale comparable to that derived analytically. Non-radial collective modes enhance the energy transport process that erases the cusp, though the parametrisations of the analytical model persist. In our model, the dominant contribution to the dynamical coupling driving the cusp-core transformation comes from the largest scale fluctuations. Yet, the efficiency of the transformation is independent of the value of the largest scale and depends weakly (linearly) on the power law exponent; it effectively depends on two parameters: the gas mass fraction and the normalisation of the power spectrum. This suggests that cusp-core transformations observed in hydrodynamic simulations of galaxy formation may be understood and parametrised in simple terms, the physical and numerical complexities of the various implementations notwithstanding.
Levitation of a drop over a moving surface

Abstract We investigate the levitation of a drop gently deposited onto the inner wall of a rotating hollow cylinder. For a sufficiently large velocity of the wall, the drop steadily levitates over a thin air film and reaches a stable angular position in the cylinder, where the drag and lift balance the weight of the drop. Interferometric measurements yield the three-dimensional (3D) air film thickness under the drop and reveal the asymmetry of the profile along the direction of the wall motion. A two-dimensional (2D) model is presented which explains the levitation mechanism, captures the main characteristics of the air film shape and predicts two asymptotic regimes for the film thickness ${h}_{0} $ : for large drops ${h}_{0} \sim {\mathit{Ca}}^{2/ 3} { \kappa }_{b}^{- 1} $ , as in the Bretherton problem, where $\mathit{Ca}$ is the capillary number based on the air viscosity and ${\kappa }_{b} $ is the curvature at the bottom of the drop; for small drops ${h}_{0} \sim {\mathit{Ca}}^{4/ 5} {(a{\kappa }_{b} )}^{4/ 5} { \kappa }_{b}^{- 1} $ , where $a$ is the capillary length.
Dispersion engineered silicon nitride waveguides by geometrical and refractive-index optimization

Dispersion engineering in silicon nitride (SiXNY) waveguides is investigated through the optimization of the waveguide transversal dimensions and refractive indices in a multicladding arrangement. Ultraflat dispersion of −84.0±0.5 ps/nm/km between 1700 and 2440 nm and 1.5±3 ps/nm/km between 1670 and 2500 nm is numerically demonstrated. It is shown that typical refractive index fluctuations as well as dimension fluctuations during fabrication of the SiXNY waveguides are a limitation for obtaining ultraflat dispersion profiles. Single- and multicladding waveguides are fabricated and their dispersion profiles measured (over nearly 1000 nm) using a low-coherence frequency domain interferometric technique. By appropriate thickness optimization, the zero-dispersion wavelength is tuned over a large spectral range in single- and multicladding waveguides with small refractive index contrast (3%). A flat dispersion profile with ±3.2 ps/nm/km variation over 500 nm is obtained in a multicladding waveguide fabricated with a refractive index contrast of 37%. Finally, we generate a nearly three-octave supercontinuum in this dispersion flattened multicladding SiXNY waveguide.
Transiting exoplanets from the CoRoT space mission - XIV. CoRoT-11b: a transiting massive “hot-Jupiter” in a prograde orbit around a rapidly rotating F-type star

The CoRoT exoplanet science team announces the discovery of CoRoT-11b, a fairly massive hot-Jupiter transiting a V = 12.9 mag F6 dwarf star (M ∗ = 1.27 ± 0.05 M ⊙ , R ∗ = 1.37 ± 0.03 R ⊙ , T eff = 6440 ± 120 K), with an orbital period of P = 2.994329 ± 0.000011 days and semi-major axis a = 0.0436 ± 0.005 AU. The detection of part of the radial velocity anomaly caused by the Rossiter-McLaughlin effect shows that the transit-like events detected by CoRoT are caused by a planet-sized transiting object in a prograde orbit. The relatively high projected rotational velocity of the star (v sini ⋆ = 40 ± 5 km s-1 ) places CoRoT-11 among the most rapidly rotating planet host stars discovered so far. With a planetary mass of M p = 2.33 ± 0.34 M Jup and radius R p = 1.43 ± 0.03 R Jup , the resulting mean density of CoRoT-11b (ρ p = 0.99 ± 0.15 g/cm3 ) can be explained with a model for an inflated hydrogen-planet with a solar composition and a high level of energy dissipation in its interior.
CGM properties in VELA and NIHAO simulations; the OVI ionization mechanism: dependence on redshift, halo mass, and radius

We study the components of cool and warm/hot gas in the circumgalactic medium (CGM) of simulated galaxies and address the relative production of OVI by photoionization versus collisional ionization, as a function of halo mass, redshift, and distance from the galaxy halo center. This is done utilizing two different suites of zoom-in hydro-cosmological simulations, VELA (6 halos; $z>1$) and NIHAO (18 halos; to $z=0$), which provide a broad theoretical basis because they use different codes and physical recipes for star formation and feedback. In all halos studied in this work, we find that collisional ionization by thermal electrons dominates at high redshift, while photoionization of cool or warm gas by the metagalactic radiation takes over near $z\sim2$. In halos of $\sim 10^{12}M_{\odot}$ and above, collisions become important again at $z 3\times10^{11}~M_{\odot}$, at $z\sim 0$ most of the photoionized OVI is in a warm, not cool, gas phase ($T\lesssim 3\times 10^5$~K). We also find that collisions are dominant in the central regions of halos, while photoionization is more significant at the outskirts, around $R_{\textrm v}$, even in massive halos. This too may be explained by the presence of warm gas or, in lower mass halos, by cool gas inflows.
Semileptonic D-decays at BESIII

We present here three analyses of semileptonic $D$-meson decays based on the 2.92 fb$^{-1}$ of data collected by the BESIII experiment in 2010 and 2011 at the $\psi$(3770) peak. For the decay $D^{+}\to K^{-}\pi^{+}e^{+}\nu_{e}$, its branching fraction is measured over the whole $m_{K\pi}$ region and in the $\overline{K}^{*}(892)^{0}$ window, respectively. A partial wave analysis (PWA) is performed, indicating an \emph{S}-wave contribution of about 6\%. The \emph{S}-wave phase and the form factors are measured by the PWA and in a model-independent way. For the decay $D^{+}\to \omega e^{+}\nu_{e}$, an improved measurement of the branching fraction is performed and the form factors are determined for the first time. $D^{+}\to \phi e^{+}\nu_{e}$ is searched and an improved upper limit at 90\% confidence level is set. For the decay $D^{+}\to K_{L} e^{+}\nu_{e}$, its branching fraction is measured for the first time and the $CP$ asymmetry is presented. The product of the hadronic form factor and the CKM matrix element, $f_{+}^{K}(0)|V_{cs}|$, is also determined in this decay.
Chandra observation of two shock fronts in the merging galaxy cluster Abell 2146

We present a new Chandraobservation of the galaxy cluster Abell 2146 which has revealed a complex merging system with a gas structure that is remarkably similar to the Bullet cluster (eg. Markevitch et al. 2002). The X-ray image and temperature map show a cool 2− 3 keV subcluster with a ram pressure stripped tail of gas just exit ing the disrupted 6− 7 keV primary cluster. From the sharp jump in the temperature and density of the gas, we determine that the subcluster is preceded by a bow shock with a Mach number M = 2.2� 0.8, corresponding to a velocity v = 2200 +1000 −900 km s −1 relative to the main cluster. We estimate that the subcluste r passed through the primary core only 0.1− 0.3 Gyr ago. In addition, we observe a slower upstream shock propagating through the outer region of the primary cluster and calculate a Mach number M = 1.7� 0.3. Based on the measured shock Mach numbers M � 2 and the strength of the upstream shock, we argue that the mass ratio between the two merging clusters is between 3 and 4 to one. By comparing the Chandra observation with an archival HST observation, we find that a group of galaxies is located in fro nt of the X-ray subcluster core but the brightest cluster galaxy is located immediately behind the X-ray peak.
On the orbital parameters of Be/X‐ray binaries in the Small Magellanic Cloud

The orbital motion of a neutron star about its optical companion presents a window through which we can study the orbital parameters of that binary system. This has been used extensively in the Milky Way to calculate these parameters for several high-mass X-ray binaries. Using several years of Rossi X-ray Timing Explorer Proportional Counter Array data, we derive the orbital parameters of four Be/X-ray binary systems in the Small Magellanic Cloud (SMC), increasing the number of systems with orbital solutions by a factor of 3. We find one new orbital period, confirm a second and discuss the parameters with comparison to the Galactic systems. Despite the low metallicity in the SMC, these binary systems sit amongst the Galactic distribution of orbital periods and eccentricities, suggesting that metallicity may not play an important role in the evolution of high-mass X-ray binary systems. A plot of orbital period against eccentricity shows that the supergiant, Be and low-eccentricity OB transient systems occupy separate regions of the parameter space; akin to the separated regions on the Corbet diagram. Using a Spearman’s rank correlation test, we also find a possible correlation between the two parameters. The mass functions, inclinations and orbital semimajor axes are derived for the SMC systems based on the binary parameters and the spectral classification of the optical counterpart. As a by-product of our work, we present a catalogue of the orbital parameters for every high-mass X-ray binary in the Galaxy and Magellanic Clouds for which they are known.
Comparison of Adherence to Mediterranean Diet between Spanish and German School-Children and Influence of Gender, Overweight, and Physical Activity

Background: Poor dietary habits and low levels of physical activity (PA) have a strong tendency to track from childhood into adulthood. The Mediterranean Diet (MD) is known to be extremely healthy, associated with lower BMI and a lower risk of obesity in children and adolescents. Therefore, adherence to the MD was compared between Spanish (n = 182) and German (n = 152) children aged 10 to 13 years to examine a possible more “westernized” diet in Spain with a non-Mediterranean country, that traditionally prefers a “Western diet” and to determine the association between adherence to the MD and gender, body composition, and PA levels. Methods: In the German observational longitudinal cohort study and the Spanish cohort study, body composition and questionnaires (KIDMED, Diet Quality (IAES)) were obtained, and accelerometers (Actigraph) were applied to detect PA. Results: Girls had higher BMI-standard deviation score (SDS) than boys and Spanish girls were less active than boys. Differences were detected in MD habits, such as favorable fruit-, vegetables-, fish-intakes, and dairy products in Spanish children and unfavorable consumptions of fast food, processed bakery goods, candies, and sweet beverages in German children. Independently of country, girls, children with lower BMI-SDS and children with higher PA level were related with better diet quality. Conclusion: Spanish children showed higher adherence to MD and diet quality (IAES) compared to German children, but there was a trend toward a more “westernized” diet. Gender, body composition, and PA influenced nutrition regardless of country.
Compost fortification with lignocellulolytic fungi for wheat cultivation using fewer mineral fertilizers amount in sandy soil

Current study has focused on the hypothesis that augmentation of organic fertilizers with lignocellulolytic fungi could overcome the slow-release issue of nutrients and act as plant growth-promoting fungi (PGPF) for plants against synthetic fertilizers. Two factorial experiments were implemented to study the influence of compost, processed by the addition of lignocellulolytic fungi, against rates of NPK fertilizers on the growth and productivity of cultivated wheat in sandy soil. An inoculum consisted of two cellulolytic fungi, viz Trichoderma harzianum and Trichoderma viride and a ligninolytic fungus, viz Phanerochaete chrysosporium, was used for processing the compost before sowing. Three rates of NPK fertilizers, viz 100%, 75%, or 25% of the recommended dose were combined with processed compost or unprocessed. The results revealed an intensification of overall microbial count and associated activities in the rhizosphere of plants due to processed compost and a medium dose of NPK fertilizers. The dry weight of shoot generally increased in order 100% NPK> 75% NPK > 50% NPK , with a non-significant difference between 100% and 75% treatments when combined with processed compost. Despite the superiority of the full dose of NPK treatment, the divergence between them and 75% NPK fertilizers appeared non-significant when combined with processed compost for straw and grain yield, the weight of 1000 grains, or crude protein. Under the current situation, empowerment to diminish the applied amount of synthetic NPK fertilizers by 25% from the total dose by the incidence of saprobic fungi for more decomposition of organic matter doing a positive priming effect in wheat rhizobiome acting to improve the above- and below-ground parts of plants as a source capacity for high grain yield in eco-friendly and sustainable sound. The processed compost addition recorded 67.04 and 55.08; 27.57 and 25.24; 22.98 and 17.97 or 62.55 and 47.47% increases over unprocessed one for soil respiration, dehydrogenase enzymes, nitrogenase, or alkaline phosphatase during the first and second seasons, respectively. Mineral fertilization, in their main effect, also revealed significant differences based on the added rate with a superiority of 75% NPK to surpass the full or half doses for all estimated activities. Although significant differences are due to process compost with lignocellulolytic fungi, or NPK rates, the compost differences depend on NPK rate, except for nitrogenase activity during two seasons. The maximum activities were achieved in rhizospheres that received 75% NPK combined with processed compost, as indicated by soil respiration and alkaline phosphatase. While overall microbial activity was maximized by 50% NPK combined with processed compost, as indicated by dehydrogenase values. The heavy dose of NPK fertilizers hindered the biological activity in wheat rhizospheres.
Refractometric sensing of Li salt with visible-light Si3N4 microdisk resonators

We demonstrate aqueous refractive index sensing with 15 to 30 {\mu}m diameter silicon nitride microdisk resonators to detect small concentrations of Li salt. A dimpled-tapered fiber is used to couple 780 nm visible light to the microdisks, in order to perform spectroscopy their optical resonances. The dimpled fiber probe allows testing of multiple devices on a chip in a single experiment. This sensing system is versatile and easy to use, while remaining competitive with other refractometric sensors. For example, from a 20 {\mu}m diameter device we measure a sensitivity of 200 $\pm$ 30 nm/RIU with a loaded quality factor of 1.5 $\times$ 10$^4$, and a limit of detection down to (1.3 $\pm$ 0.1) $\times$ 10$^{-6}$ RIU.
THREE-DIMENSIONAL HYDRODYNAMIC SIMULATIONS OF MULTIPHASE GALACTIC DISKS WITH STAR FORMATION FEEDBACK. I. REGULATION OF STAR FORMATION RATES

The energy and momentum feedback from young stars has a profound impact on the interstellar medium (ISM), including heating and driving turbulence in the neutral gas that fuels future star formation. Recent theory has argued that this leads to a quasi-equilibrium self-regulated state, and for outer atomic-dominated disks results in the surface density of star formation ΣSFR varying approximately linearly with the weight of the ISM (or midplane turbulent + thermal pressure). We use three-dimensional numerical hydrodynamic simulations to test the theoretical predictions for thermal, turbulent, and vertical dynamical equilibrium, and the implied functional dependence of ΣSFR on local disk properties. Our models demonstrate that all equilibria are established rapidly, and that the expected proportionalities between mean thermal and turbulent pressures and ΣSFR apply. For outer disk regions, this results in , where Σ is the total gas surface density and ρsd is the midplane density of the stellar disk (plus dark matter). This scaling law arises because ρsd sets the vertical dynamical time in our models (and outer disk regions generally). The coefficient in the star formation law varies inversely with the specific energy and momentum yield from massive stars. We find proportions of warm and cold atomic gas, turbulent-to-thermal pressure, and mean velocity dispersions that are consistent with solar-neighborhood and other outer disk observations. This study confirms the conclusions of a previous set of simulations, which incorporated the same physics treatment but was restricted to radial-vertical slices through the ISM.