Miracle-dz/UniFAR-FTUs huggingface dataset:
The luminosity function and the rate of Swift's Gamma Ray Bursts

We invert directly the redshift-luminosity distribution of observed long Swift gamma-ray bursts (GRBs) to obtain their rate and luminosity function. Our best-fitting rate is described by a broken power law that rises like (1 + 2) 2.1+0.5 -0.6 for 0 3. The local rate is ρ 0 ≃ 1.3 +0.6 -0.7 (Gpc -3 yr -1 ). The luminosity function is well described by a broken power law with a break at L* ≃ 10 52.5±0.2 (erg s -1 ) and with indices α = 0.2 +0.2 -0.1 and β = 1.4 +0.3 -0.6 . The recently detected GRB 090423, with z ≈ 8, fits nicely into the model's prediction, verifying that we are allowed to extend our results to high redshifts. While the GRB rate may follow the star formation rate (SFR) for z < 3, the high-redshift slope is shallower than the steep decline in the SFR for 4 < z. However, we cannot rule out a GRB rate that follows one of the recent SFR models.
A STRING OF RADIO EMISSION ASSOCIATED WITH IRAS 16562−3959: A COLLIMATED JET EMANATING FROM A LUMINOUS MASSIVE YOUNG STELLAR OBJECT

We report the discovery, made using the Australia Telescope Compact Array, of a remarkable string of radio emission toward IRAS 16562−3959, a luminous infrared source with a bolometric luminosity of 7.0 × 104 L☉. The radio emission arises from a compact, bright central component, two inner lobes which are separated by about 7″ and symmetrically offset from the central source, and two outer lobes which are separated by about 45″. The emission from the central object has a spectral index between 1.4 and 8.6 GHz of 0.85 ± 0.15, consistent with free–free emission from a thermal jet. The radio emission from the lobes has spectral indices in the range characteristic of thermal emission. We suggest that the emission from the lobes arises in shocks resulting from the interaction of a collimated wind with the surrounding medium. The radio string is located within a massive dense molecular core, and is associated with extended green emission (Spitzer three-color), Herbig–Haro-type emission (2MASS Ks band), and OH maser sites—all phenomena readily observed toward sites of massive star formation. We conclude that the massive core hosts a high-mass star in an early stage of evolution in which it is undergoing the ejection of a powerful collimated stellar wind, showing that jets found in the formation of low-mass stars are also produced in high-mass stars.
AN X-RAY AND MULTIWAVELENGTH SURVEY OF HIGHLY RADIO-LOUD QUASARS AT z > 4: JET-LINKED EMISSION IN THE BRIGHTEST RADIO BEACONS OF THE EARLY UNIVERSE

We present a systematic study of the X-ray and multiwavelength properties of a sample of 17 highly radio-loud quasars (HRLQs) at z > 4 with sensitive X-ray coverage from new Chandra and archival Chandra, XMM–Newton, and Swift observations. Eight of the new and archival observations are reported in this work for the first time. New Chandra observations of two moderately radio-loud and highly optically luminous quasars at z ≳ 4 are also reported. Our HRLQ sample represents the top ∼5% of radio-loud quasars (RLQs) in terms of radio loudness. We found that our HRLQs have an X-ray emission enhancement over HRLQs at lower redshifts (by a typical factor of ≈3), and this effect, after controlling for several factors which may introduce biases, has been solidly estimated to be significant at the 3σ–4σ level. HRLQs at z = 3–4 are also found to have a similar X-ray emission enhancement over z < 3 HRLQs, which further supports the robustness of our results. We discuss models for the X-ray enhancement's origin including a fractional contribution from inverse Compton scattering of cosmic microwave background photons. No strong correlations are found between the relative X-ray brightness and optical/UV emission-line rest-frame equivalent widths (REWs) for RLQs. However, the line REWs are positively correlated with radio loudness, which suggests that relativistic jets make a negligible contribution to the optical/UV continua of these HRLQs (contrary to the case where the emission lines are diluted by the relativistically boosted continuum). Our HRLQs are generally consistent with the known anti-correlation between radio loudness and X-ray power-law photon index. We also found that the two moderately radio-loud quasars appear to have the hardest X-ray spectra among our objects, suggesting that intrinsic X-ray absorption (NH ∼ 1023 cm−2) may be present. Our z > 4 HRLQs generally have higher X-ray luminosities than those for the composite broadband spectral energy distributions of HRLQs at lower redshift, which further illustrates and supports the X-ray emission enhancement of z > 4 HRLQs. Some of our HRLQs also show an excess of mid-infrared emission which may originate from the synchrotron emission of the relativistic jets. None of our z > 4 HRLQs is detected by the Fermi-LAT two-year survey, which provides constraints on jet-emission models.
Thermal Spraying of Thin Metallic Coatings

Metallic coatings can be produced easily with thermal spray and cold gas spray processes. However, when coating thicknesses below 50 μm are required for economical or technological reasons, the use of these well-established processes becomes more challenging. The company OBZ Innovation GmbH has developed spray processes that can produce metallic coatings with thicknesses of less than 20 μm. Such coatings are of interest for applications such as cold gas sprayed silver coatings with high purity and good electrical conductivity. Thinner sprayed coatings of such valuable materials have economic advantages, and the process may be competitive with commonly used thin film coating methods.
FORMING CIRCUMBINARY PLANETS: N-BODY SIMULATIONS OF KEPLER-34

Observations of circumbinary planets orbiting very close to the central stars have shown that planet formation may occur in a very hostile environment, where the gravitational pull from the binary should be very strong on the primordial protoplanetary disk. Elevated impact velocities and orbit crossings from eccentricity oscillations are the primary contributors to high energy, potentially destructive collisions that inhibit the growth of aspiring planets. In this work, we conduct high-resolution, inter-particle gravity enabled N-body simulations to investigate the feasibility of planetesimal growth in the Kepler-34 system. We improve upon previous work by including planetesimal disk self-gravity and an extensive collision model to accurately handle inter-planetesimal interactions. We find that super-catastrophic erosion events are the dominant mechanism up to and including the orbital radius of Kepler-34(AB)b, making in situ growth unlikely. It is more plausible that Kepler-34(AB)b migrated from a region beyond 1.5 AU. Based on the conclusions that we have made for Kepler-34, it seems likely that all of the currently known circumbinary planets have also migrated significantly from their formation location with the possible exception of Kepler-47(AB)c.
THE ORIGIN OF THE MOST IRON-POOR STAR

We investigate the origin of carbon-enhanced metal-poor (CEMP) stars starting from the recently discovered [Fe/H] < -7.1 star SMSS J031300. We show that the elemental abundances observed on the surface of SMSS J031300 can be well fit by the yields of faint, metal-free, supernovae (SNe). Using properly calibrated faint SN explosion models, we study, for the first time, the formation of dust grains in such carbon-rich, iron-poor SN ejecta. Calculations are performed assuming both unmixed and uniformly mixed ejecta and taking into account the partial destruction by the SN reverse shock. We find that, due to the paucity of refractory elements beside carbon, amorphous carbon is the only grain species to form, with carbon condensation efficiencies that range between (0.15 and 0.84), resulting in dust yields in the range (0.025–2.25) M☉. We follow the collapse and fragmentation of a star-forming cloud enriched by the products of these faint SN explosions and we explore the role played by fine structure line cooling and dust cooling. We show that even if grain growth during the collapse has a minor effect of the dust-to-gas ratio, due to C depletion into CO molecules at an early stage of the collapse, the formation of CEMP low-mass stars, such as SMSS J031300, could be triggered by dust cooling and fragmentation. A comparison between model predictions and observations of a sample of C-normal and C-rich metal-poor stars supports the idea that a single common pathway may be responsible for the formation of the first low-mass stars.
NUMERICAL SIMULATIONS OF QUIET SUN MAGNETISM: ON THE CONTRIBUTION FROM A SMALL-SCALE DYNAMO

We present a series of radiative MHD simulations addressing the origin and distribution of the mixed polarity magnetic field in the solar photosphere. To this end, we consider numerical simulations that cover the uppermost 2–6 Mm of the solar convection zone and we explore scales ranging from 2 km to 25 Mm. We study how the strength and distribution of the magnetic field in the photosphere and subsurface layers depend on resolution, domain size, and boundary conditions. We find that 50% of the magnetic energy at the τ = 1 level comes from fields with the less than 500 G strength and that 50% of the energy resides on scales smaller than about 100 km. While the probability distribution functions are essentially independent of resolution, properly describing the spectral energy distribution requires grid spacings of 8 km or smaller. The formation of flux concentrations in the photosphere exceeding 1 kG requires a mean vertical field strength greater than 30–40 G at τ = 1. The filling factor of kG flux concentrations increases with overall domain size as the magnetic field becomes organized by larger, longer-lived flow structures. A solution with a mean vertical field strength of around 85 G at τ = 1 requires a subsurface rms field strength increasing with depth at the same rate as the equipartition field strength. We consider this an upper limit for the quiet Sun field strength, which implies that most of the convection zone is magnetized close to the equipartition. We discuss these findings in view of recent high-resolution spectropolarimetric observations of quiet Sun magnetism.
Dynamical versus stellar masses of ultracompact dwarf galaxies in the Fornax cluster

The origin of ultracompact dwarf (UCD) galaxies, compact extragalactic stellar systems, is still a puzzle for present galaxy formation models. We present the comprehensive analysis of high-resolution multi-object spectroscopic data for a sample of 24 Fornax cluster UCDs obtained with VLT with Fibre Large Array Multi Element Spectrograph (FLAMES). It comprises previously published data for 19 objects which we re-analysed, including 13 with available Hubble Space Telescope (HST) photometric data. Using Virtual Observatory technologies we found archival HST images for two more UCDs and then determined their structural properties. For all objects we derived internal velocity dispersions, stellar population parameters and stellar mass-to-light ratios (M/L) * by fitting individual simple stellar population (SSP) synthetic spectra convolved with a Gaussian against the observed spectra using the NBURSTS full spectral fitting technique. For 14 objects we estimated dynamical masses suggesting no dark matter (DM) in 12 of them and no more than 40per cent DM mass fraction in the remaining two, in contrast to findings for several UCDs in the Virgo cluster. Some Fornax UCDs even have too high values of (M/L) * estimated using the Kroupa stellar initial mass function (IMF) resulting in negative formally computed DM mass fractions. The objects with too high (M/L) * ratios compared to the dynamical ones have relatively short dynamical relaxation time-scales, close to the Hubble time or below. We therefore suggest that their lower dynamical ratios (M/L) dyn are caused by low-mass star depletion due to dynamical evolution. Overall, the observed UCD characteristics suggest at least two formation channels: tidal threshing of nucleated dwarf galaxies for massive UCDs (≃10 8 M ⊙ ), and a classical scenario of red globular cluster formation for lower-mass UCDs (≲10 7 M ⊙ ).
Routine Use of Pressure Wire as an Adjunct to Diagnostic Angiography; Comparison of Resources Utilization in the Catheterization Laboratory: A Sub-Study of RIPCORD 2

Background: The RIPCORD 2 trial randomized patients undergoing coronary angiography to strategy of routine measurement of fractional flow reserve (FFR) in all vessels or to angiography alone. Objectives: We compared, for the randomized groups, the catheter laboratory procedure costs to diagnosis. Methods: This is a sub-study of the RIPCORD2 trial. We excluded patients with follow-on PCI to better reflect procedural costs of the diagnostic phase. We compared resource utilization and, from this, derived an estimated procedure cost for UK practice. We examined the association between cost and the number of vessels examined with pressure wire (PW) technology. Results: We included 249/552 (45%) patients randomized to angiography and 261/548 (48%) patients to systematic FFR measurement. The median (IQR) procedure cost was higher in the FFR group £1392 (1126 – 1686) versus £411 (308 – 586); P < 0.001. In the FFR group, 86.6% of procedures were completed with a single pressure wire; two and three PWs were used in 10.7% and 1.5% of cases respectively. The procedure duration (median, IQR; mins) was longer in the FFR group; 52 (39 – 66) versus 20 (15 – 30) as was the use of radiographic contrast (median, IQR; mls); 140 (110 – 189) versus 70 (60 – 94). In the FFR group, it seems that the additional cost was associated with the cost of the PW and laboratory set up for the performance of FFR measurement; the incremental cost of examining additional vessels, beyond the first, was modest. Conclusion: The procedural cost associated with a strategy of systematic measurement of FFR in all vessels is higher than that of angiography alone.
THE PROGRESSION OF STAR FORMATION IN THE ROSETTE MOLECULAR CLOUD

Using Spitzer Space Telescope and Chandra X-Ray Observatory data, we identify young stellar objects (YSOs) in the Rosette Molecular Cloud (RMC). By being able to select cluster members and classify them into YSO types, we are able to track the progression of star formation locally within the cluster environments and globally within the cloud. We employ the nearest neighbor method analysis to explore the density structure of the clusters and YSO ratio mapping to study age progressions in the cloud. We find a relationship between the YSO ratios and extinction that suggests star formation occurs preferentially in the densest parts of the cloud and that the column density of gas rapidly decreases as the region evolves. This suggests rapid removal of gas may account for the low star formation efficiencies observed in molecular clouds. We find that the overall age spread across the RMC is small. Our analysis suggests that star formation started throughout the complex around the same time. Age gradients in the cloud appear to be localized and any effect the H ii region has on the star formation history is secondary to that of the primordial collapse of the cloud.
Realizable Reduction of Multi-Port RCL Networks by Block Elimination

In this paper a block circuit elimination method is proposed for realizable reduction of resistor-capacitor-inductor (RCL) networks. It is an extension of a recently published realizable RC reduction method, called HD-TICER (high-dimensional time-constant equilibration reduction), to reduction of multi-port RCL networks. A modified nodal analysis (MNA) formulation is adopted in a setting for dealing with the inductive elements, which is suited for developing a realizable high-dimensional reduction scheme. A new matrix-based method is presented to establish the basic computation scheme, which seems more intuitive than the previously employed driving point impedance (DPI) method. Furthermore, a pole-zero based low-order moment matching method is introduced for the purpose of circuit recovery after reduction. The main advantages of the proposed reduction method include: 1) an intuition-based topological formulation and reduction computation method, 2) a natural port preserving reduction method, and 3) an easy-to-implement circuit recovery procedure. Experimental numerical implementation has validated the effectiveness of the proposed reduction method. Comparison to other existing methods further highlights multiple benefits of this new circuit reduction method.
Shape Fidelity Evaluation of Alginate-Based Hydrogels through Extrusion-Based Bioprinting

Extrusion-based 3D bioprinting is a promising technique for fabricating multi-layered, complex biostructures, as it enables multi-material dispersion of bioinks with a straightforward procedure (particularly for users with limited additive manufacturing skills). Nonetheless, this method faces challenges in retaining the shape fidelity of the 3D-bioprinted structure, i.e., the collapse of filament (bioink) due to gravity and/or spreading of the bioink owing to the low viscosity, ultimately complicating the fabrication of multi-layered designs that can maintain the desired pore structure. While low viscosity is required to ensure a continuous flow of material (without clogging), a bioink should be viscous enough to retain its shape post-printing, highlighting the importance of bioink properties optimization. Here, two quantitative analyses are performed to evaluate shape fidelity. First, the filament collapse deformation is evaluated by printing different concentrations of alginate and its crosslinker (calcium chloride) by a co-axial nozzle over a platform to observe the overhanging deformation over time at two different ambient temperatures. In addition, a mathematical model is developed to estimate Young’s modulus and filament collapse over time. Second, the printability of alginate is improved by optimizing gelatin concentrations and analyzing the pore size area. In addition, the biocompatibility of proposed bioinks is evaluated with a cell viability test. The proposed bioink (3% w/v gelatin in 4% alginate) yielded a 98% normalized pore number (high shape fidelity) while maintaining >90% cell viability five days after being bioprinted. Integration of quantitative analysis/simulations and 3D printing facilitate the determination of the optimum composition and concentration of different elements of a bioink to prevent filament collapse or bioink spreading (post-printing), ultimately resulting in high shape fidelity (i.e., retaining the shape) and printing quality.
A MULTI-WAVELENGTH VIEW OF THE STAR FORMATION ACTIVITY AT z ∼ 3

We present a multi-wavelength, UV-to-radio analysis for a sample of massive (M* ∼ 1010 M☉) IRAC- and MIPS 24 μm detected Lyman break galaxies (LBGs) with spectroscopic redshifts z ∼ 3 in the GOODS-North field. For LBGs without individual 24 μm detections, we employ stacking techniques at 24 μm, 1.1 mm, and 1.4 GHz to construct the average UV-to-radio spectral energy distribution and find it to be consistent with that of a luminous infrared galaxy with LIR = 4.5+1.1−2.3 × 1011 L☉ and a specific star formation rate of 4.3 Gyr−1 that corresponds to a mass doubling time ∼230 Myr. On the other hand, when considering the 24 μm detected LBGs we find among them galaxies with LIR>1012 L☉, indicating that the space density of z ∼ 3 UV-selected ultra-luminous infrared galaxies (ULIRGs) is ∼(1.5 ± 0.5) × 10−5 Mpc−3. We compare measurements of star formation rates from data at different wavelengths and find that there is tight correlation (Kendall's τ>99.7%) and excellent agreement between the values derived from dust-corrected UV, mid-IR, millimeter, and radio data for the whole range of LIR up to LIR ∼ 1013 L☉. This range is greater than that for which the correlation is known to hold at z ∼ 2, possibly due to the lack of significant contribution from polycyclic aromatic hydrocarbons to the 24 μm flux at z ∼ 3. The fact that this agreement is observed for galaxies with LIR>1012 L☉ suggests that star formation in UV-selected ULIRGs, as well as the bulk of star formation activity at this redshift, is not embedded in optically thick regions as seen in local ULIRGs and submillimeter-selected galaxies at z = 2.
X-ray Absorption Spectroscopy Study of Iron Site Manganese Substituted Yttrium Orthoferrite

In this work, manganese (Mn)-doped YFeO3, i.e., YFMxO powders with 0 ≤ x ≤ 0.1, was synthesized by a hydrothermal method to study the influences of doping on its structural, morphological, optical, magnetic, and local electrical properties. The experimental results show that all the samples exhibit an orthorhombic structure with space group Pnma. Refined structure parameters are presented. Morphology images show the shape evolution from layered to multilayered with increasing Mn content. Infrared spectra reveal the characteristic vibrations of the obtained YFMxO samples. From the magnetic study, an increased magnetic moment in the range of 0 ≤ x ≤ 0.075 is observed. The Fe and Y K-edge local structure studies indicate that the valency of Fe and Y is mainly found in the trivalent state, which also indicates that the substitution of Mn ions not only affects the nearest neighbor atomic shell of Fe but also affects the nearest neighbor’s local structure of Y atoms. Our results show that the addition of Mn exhibits an evident influence on the local structural and magnetic properties.
Household water storage containers: Aedes aegypti larval breeding site and high risk of transmission of arboviruses in Abidjan, Côte d'Ivoire

Dengue 3 epidemic was declared in Abidjan in 2018. Vector control was directed towards management of breeding sites to reduce proliferation of mosquitoes. Thus, characterization was carried out through larval prospecting in 100 households in six communes of Abidjan in February and August (large and small dry season) of 2018, before and after mosquito control. 3,809 larval breeding sites were inventoried, including 2,289 before and 1,520 after (p-value > 0.05). 76% of sites (2,909), consisted of water storage (1,380) and abandoned containers (1,529). These two categories were most abundant in households (p-value <0.0001). Greatest number of storage containers were observed in Attécoubé (n = 312) and Abobo (n = 296). Abandoned containers were abundant in Port-Bouet (n = 416). Number of abandoned containers was reduced from 1,016 before to 513 after operation (p-value < 0.01). However, water storage containers have increased slightly. It went from 686 before operation to 694 after. Positive storage containers (255) were also the most numerous (53%). Their proportions were 151 (41%) and 104 (55%) before and after mosquito control. They were very productive in Aedes aegypti. Household water storage containers could lead to reconstitution, maintenance of mosquitoes and increased risk of arboviruses spread in Abidjan.