Miracle-dz/UniFAR-FTUs huggingface dataset:
Zodiacal Exoplanets in Time (ZEIT). V. A Uniform Search for Transiting Planets in Young Clusters Observed by K2

Detection of transiting exoplanets around young stars is more difficult than for older systems owing to increased stellar variability. Nine young open cluster planets have been found in the K2 data, but no single analysis pipeline identified all planets. We have developed a transit search pipeline for young stars that uses a transit-shaped notch and quadratic continuum in a 12 or 24 hr window to fit both the stellar variability and the presence of a transit. In addition, for the most rapid rotators ( days) we model the variability using a linear combination of observed rotations of each star. To maximally exploit our new pipeline, we update the membership for four stellar populations observed by K2 (Upper Scorpius, Pleiades, Hyades, Praesepe) and conduct a uniform search of the members. We identify all known transiting exoplanets in the clusters, 17 eclipsing binaries, one transiting planet candidate orbiting a potential Pleiades member, and three orbiting unlikely members of the young clusters. Limited injection recovery testing on the known planet hosts indicates that for the older Praesepe systems we are sensitive to additional exoplanets as small as 1–2 R⊕, and for the larger Upper Scorpius planet host (K2-33) our pipeline is sensitive to ∼4 R⊕ transiting planets. The lack of detected multiple systems in the young clusters is consistent with the expected frequency from the original Kepler sample, within our detection limits. With a robust pipeline that detects all known planets in the young clusters, occurrence rate testing at young ages is now possible.
Identification of regenerating island-derived protein 3E in dogs

Regenerating islet-derived protein (REG) 1A (aka pancreatic stone protein) and REG3A (aka pancreatitis-associated protein) are upregulated in humans with sepsis, pancreatitis, and gastrointestinal diseases, but little is known about this protein family in dogs. Our aim was to identify REG1 and REG3 family members in dogs. REG-family genes were computationally annotated in the canine genome and proteome, with verification of gene expression using publicly available RNA-seq data. The presence of the protein in canine pancreatic tissue and plasma was investigated with Western blot and immunohistochemistry, using anti-human REG1A and REG3A antibodies. Protein identity was confirmed with mass spectrometry. Two members of the REG3 subfamily were found in the canine genome, REG3E1 and REG3E2, both encoding for the same 176 AA protein, subsequently named REG3E. Anti-human REG3A antibodies demonstrated cross-reactivity with the canine REG3E protein in pancreas homogenates. In canine plasma, a protein band of approximately 17 kDa was apparent. Mass spectrometry confirmed this protein to be the product of the two annotated REG3E genes. Strong immunoreactivity to anti-human REG3A antibodies was found in sections of canine pancreas affected with acute pancreatitis, but it was weak in healthy pancreatic tissue. Recombinant canine REG3E protein underwent a selective trypsin digestion as described in other species. No evidence for the presence of a homolog of REG1A in dogs was found in any of the investigations. In conclusion, dogs express REG3E in the pancreas, whose role as biomarker merits further investigations. Homologs to human REG1A are not likely to exist in dogs.
Deformations and D-branes

I discuss the relation of Hochschild cohomology to the physical states in the closed topological string. This allows a notion of deformation intrinsic to the derived category. I use this to identify deformations of a quiver gauge theory associated to a D-branes at a singularity with generalized deformations of the geometry of the resolution of the singularity. An explicit map is given from noncommutative deformations (ie, B-fields) to terms in the superpotential.
Fusion-Fission Hybrid Using a D-D Cylindrical Inertial Electrostatic Confinement (IEC) Driver

Recent progress in fusion development combined with the rebirth of nuclear fission power has regenerated interest in fusion-fission hybrid reactors. Such systems could be applied to both low power research reactors for use in University and industrial research assemblies and power reactors. However most attention has been directed at D-T fusion drivers using Tokamak, ICF or various alternate confinement systems like FRCs. However, the necessity to have large devices and breed tritium in the blanket complicates the concept. Here we propose the inertial electrostatic confinement (IEC) fusion approach since it offers the advantages of simple structural, high power density and a non-Maxwellian beam dominated plasma suited for burning advanced fuels to minimize tritium involvement. The cylindrical IEC allows a small compact unit which can be inserted into fuel element slots in the fission reactor core, thus providing a compact overall system and excellent neutronic coupling. The basic physics for the IEC has been demonstrated in small-scale laboratory experiments close to levels needed for driving a subcritical assembly for use in student teaching labs. However, for use in future high power hybrids significant scale-up in source strength is required. Scale up using an external ion source (e.g. a Helicon) so the background gas pressure is minimized in the reaction zone potentially offers a route to the required neutron source strength.
Water Footprint for Garlic under Irrigation Levels and Agrispon Application

Field experiment was conducted in Giza, Egypt, during two growing seasons of 2017-2018 and 2018-2019 on garlic crop, with the objective of investigating the effect of different irrigation levels (60, 80 and 100 % of water requirements and their combination with the foliar spraying applications of agrispon (with 0.5 and 1.0 ml/ liter) on growth and yield. The results indicated that increased irrigation level up to 100% led to increased vegetative characters of garlic and that the lowest growth and productivity was obtained by 60% irrigation level. When considering spray application of agrispon; with 1.0 ml/L increased growth and productivity followed by 0.5 ml/L; while control treatment gave the lowest productivity during the both seasons. Interaction effect between irrigation level and agrispon treatments indicated that 100% irrigation level combined with 1.0 ml/L spray application of agrispon gave the highest garlic productivity followed by 100% irrigation level combined with 0.5 ml/L spray application. The chemical analysis showed that the highest NPK was obtained by 100% irrigation level combined with 1.0 ml/L agrispon application during the both seasons. Regarding water footprint, the highest irrigation water footprint was obtained by 80% irrigation level followed by 60% irrigation level, while the lowest footprint was obtained by 100% irrigation level due to high garlic productivity under 100% irrigation level. The estimate water footprint for garlic was 525 m3/ton. The blue water footprint for garlic was 422 m3/ton about 80% form total water footprint, while gray water percentage about 20% with value of 103 m3/ton.
The weight of the crowd, social information credibility, and firm strategy

When considering a purchase, consumers often augment their private information about a product with anonymous online social information (reviews, etc.). We examine the impact on firm strategy of how consumers weight these two information sources—private and social—in their purchase decisions. An increase in weight on private information always results in higher prices at the interior equilibrium. However, the effects on profits, consumer, and total surplus are nonmonotonic: all increasing with the weight on private information when weight is high but decreasing when weight is low. Profit and surplus decrease with weight when weight is low because a marginal increase in a low weighting leads to a contraction of demand. The dynamic reverses when weight is high. Besides weighting of information sources, our model incorporates the questionable credibility of social information. A firm's optimal investment to improve social information credibility depends on whether consumers process information in a Bayesian or non‐Bayesian manner. We show that, compared to Bayesian consumers, non‐Bayesian consumers endogenously trust (distrust) social information from firms with high(low)‐positivity ratings. This distinction in information processing results in a stark contrast in how firms manage social information credibility: when facing Bayesian consumers, with an increase in the positivity of its social information, a firm with high(low) positivity spends less (more) to improve credibility. On the contrary, when facing non‐Bayesian consumers, a firm with high(low) positivity spends more (less) to improve credibility. Product quality also affects optimal credibility investment, following an inverted U‐shape.
The effect of star formation on the redshift evolution of interstellar metals, atomic and molecular gas in galaxies

We examine how the atomic and molecular gas components of galaxies evolve to higher redshifts using the semi-analytic galaxy formation models of Fu et al. in which we track the surface density profiles of gas in discs. We adopt two different prescriptions based either on gas surface density and metallicity or on interstellar pressure, to compute the molecular fraction as a function of radius in each disc. We demonstrate that the adopted star formation law determines how the balance between gas, stars and metals changes with time in the star-forming galaxy population, but does not influence the total mass in stars formed into galaxies at redshifts below z similar to 2.5. The redshift evolution of the massmetallicity relation places strong constraints on the time-scale over which cold gas is converted into stars in high-redshift galaxies, and favours models where this remains constant at values around 12 Gyr. Future observations of the evolution of the average molecular-to-atomic gas ratio in galaxies as a function of stellar mass and redshift will constrain models of the atomic-to-molecular transition.
Lax-Halmos Type Theorems in H^p Spaces

In this paper we characterize for 0 < p \leq \infty, the closed subspaces of Hp that are invariant under multiplication by all powers of a finite Blaschke factor B, except the first power. Our result clearly generalizes the invariant subspace theorem obtained by Paulsen and Singh [9] which has proved to be the starting point of important work on constrained Nevanlinna-Pick interpolation. Our method of proof can also be readily adapted to the case where the subspace is invariant under all positive powers of B (z). The two results are in the mould of the classical Lax-Halmos Theorem and can be said to be Lax-Halmos type results in the finitre multiplicity case for two commuting shifts and for a single shift respectively.
CONSERVATION GENETICS OF NABALUS SERPENTARIUS AND CONSERVATION GENETICS OF NABALUS SERPENTARIUS AND ITS COMMON CONGENER, NABALUS TRIFOLIOLATUS ITS COMMON CONGENER, NABALUS TRIFOLIOLATUS (ASTERACEAE) WITH IMPLICATIONS ON CONSERVATION (ASTERACEAE) WITH IMPLICATIONS ON CONSERVATION

Nabalus serpentarius (Pursh) Hooker is a species of concern to conservation management on the island of Nantucket, MA where four populations have been recently observed. A comparative population genetic study was carried out on N. serpentarius and a common congener, N. trifoliolatus using genetic markers developed from Taraxacum kok-saghyz and Nabalus serpentarius . Evaluations of genetic diversity and population structure of both Nabalus species on Nantucket were conducted. Nabalus serpentarius showed no reduction in population genetic variation as compared to the common congener, and the two species demonstrated similar and very low levels of population genetic structure. These data indicate that genetic threats to the rare species are not an immediate concern. However, given the small numbers of populations and the potential for stochastic demographic threats such as disease and weather phenomena, we recommend protection of all populations and encourage any programs that bolster population number.
Title : Diversification dynamics in the Neotropics through time , clades and biogeographic 1 regions

| EPHE), Place Eugène Bataillon, 34095 Montpellier, France; 10 Real Jardín Botánico de Madrid (RJB-CSIC), Madrid, Spain; 11 Department of Anthropology, University of California, Davis. 12 Royal Botanic Gardens, Kew, TW9 3AE, Richmond, Surrey, United Kingdom 13 Ecology and Evolutionary Biology, University of Sheffield, Western Bank, Sheffield; 14 Gothenburg Global Biodiversity Centre, Department of Biological and Environmental 15
Manual of Leaf Architecture

1. Introduction 2. General Definitions 3. Leaf Characters 4. Vein Definitions 5. Vein Characters 6. Tooth Definitions 7. Tooth Characters References Appendix A: Summary of Characters and Character States Appendix B: Examples of Scored Leaves Appendix C: Vouchers Appendix D: Instructions for Clearing Leaves.
Reply to anonymous reviewer 2

We thank the reviewer for taking the time to carefully read through the manuscript and the generally positive comments. The work presented here is a culmination of almost five years of effort, and it is gratifying to know that others in the community consider it a step forward. We are happy that the reviewer thinks this work is an important contribution to the field and appreciate the suggestions for improvement. Please find below the reviewer’s comments italicized, with our responses in normal font.
CONSTRAINING THE ABUNDANCES OF COMPLEX ORGANICS IN THE INNER REGIONS OF SOLAR-TYPE PROTOSTARS

The high abundances of Complex Organic Molecules (COMs) with respect to methanol, the most abundant COM, detected toward low-mass protostars, tend to be underpredicted by astrochemical models. This discrepancy might come from the large beam of the single-dish telescopes, encompassing several components of the studied protostar, commonly used to detect COMs. To address this issue, we have carried out multi-line observations of methanol and several COMs toward the two low-mass protostars NGC 1333-IRAS 2A and -IRAS 4A with the Plateau de Bure interferometer at an angular resolution of 2″, resulting in the first multi-line detection of the O-bearing species glycolaldehyde and ethanol and of the N-bearing species ethyl cyanide toward low-mass protostars other than IRAS 16293. The high number of detected transitions from COMs (more than 40 methanol transitions for instance) allowed us to accurately derive the source size of their emission and the COM column densities. The COM abundances with respect to methanol derived toward IRAS 2A and IRAS 4A are slightly, but not substantitally, lower than those derived from previous single-dish observations. The COM abundance ratios do not vary significantly with the protostellar luminosity, over five orders of magnitude, implying that low-mass hot corinos are quite chemically rich as high-mass hot cores. Astrochemical models still underpredict the abundances of key COMs, such as methyl formate or di-methyl ether, suggesting that our understanding of their formation remains incomplete.
On the Assembly Bias of Cool Core Clusters Traced by Hα Nebulae

Do cool-core (CC) and non-cool-core (NCC) clusters live in different environments? We make novel use of Hα emission lines in the central galaxies of redMaPPer clusters as proxies to construct large (1000's) samples of CC and NCC clusters and measure their relative assembly bias using both clustering and weak lensing. We increase the statistical significance of the bias measurements from clustering by cross-correlating the clusters with an external galaxy redshift catalog from the Sloan Digital Sky Survey III, the LOWZ sample. Our cross-correlations can constrain assembly bias up to a statistical uncertainty of 6%. Given our Hα criteria for CC and NCC, we find no significant differences in their clustering amplitude. Interpreting this difference as the absence of halo assembly bias, our results rule out the possibility of having different large-scale (tens of Mpc) environments as the source of diversity observed in cluster cores. Combined with recent observations of the overall mild evolution of CC and NCC properties, such as central density and CC fraction, this would suggest that either the cooling properties of the cluster core are determined early on solely by the local (<200 kpc) gas properties at formation or that local merging leads to stochastic CC relaxation and disruption in a periodic way, preserving the average population properties over time. Studying the small-scale clustering in clusters at high redshift would help shed light on the exact scenario.
Energy decay estimates for wave equations with a fractional damping

We consider the Cauchy problem in ${\bf R}^{n}$ for wave equations with a fractional damping. We generalize partially the previous results due to[12], and derive sharp decay estimates for the total energy and the $L^{2}$-norm of solutions based on the energy method in the Fourier space.
GAMA/G10-COSMOS/3D-HST: Evolution of the galaxy stellar mass function over 12.5 Gyr

Using a combined and consistently analysed GAMA, G10-COSMOS, and 3D-HST dataset we explore the evolution of the galaxy stellar-mass function over lookback times $t_{\rm L} \in \left[0.2,12.5\right] {\rm h^{-1}_{70} Gyr}$. We use a series of volume limited samples to fit Schechter functions in bins of $\sim\! $constant lookback time and explore the evolution of the best-fit parameters in both single and two-component cases. In all cases, we employ a fitting procedure that is robust to the effects of Eddington bias and sample variance. Surprisingly, when fitting a two-component Schechter function, we find essentially no evidence of temporal evolution in $M_\star$, the two $\alpha$ slope parameters, or the normalisation of the low-mass component. Instead, our fits suggest that the various shape parameters have been exceptionally stable over cosmic time, as has the normalisation of the low-mass component, and that the evolution of the stellar-mass function is well described by a simple build up of the high-mass component over time. When fitting a single component Schechter function, there is an observed evolution in both $M_\star$ and $\alpha$, however this is interpreted as being an artefact. Finally, we find that the evolution of the stellar-mass function, and the observed stellar mass density, can be well described by a simple model of constant growth in the high-mass source density over the last $11 {\rm h^{-1}_{70} Gyr}$.
DENSITY WAVES EXCITED BY LOW-MASS PLANETS IN PROTOPLANETARY DISKS. II. HIGH-RESOLUTION SIMULATIONS OF THE NONLINEAR REGIME

We investigate numerically the propagation of density waves excited by a low-mass planet in a protoplanetary disk in the nonlinear regime, using two-dimensional local shearing box simulations with the grid-based code Athena at high spatial resolution (256 grid points per scale height h). The nonlinear evolution results in the wave steepening into a shock, causing damping and angular momentum transfer to the disk. On long timescales this leads to spatial redistribution of the disk density, causing migration feedback and potentially resulting in gap opening. Previous numerical studies concentrated on exploring these secondary phenomena as probes of the nonlinear wave evolution. Here we focus on exploring the evolution of the basic wave properties, such as its density profile evolution, shock formation, and post-shock wave behavior, and provide comparison with analytical theory. The generation of potential vorticity at the shock is computed analytically and is subsequently verified by simulations and used to pinpoint the shock location. We confirm the theoretical relation between the shocking length and the planet mass (including the effect of the equation of state), and the post-shock decay of the angular momentum flux carried by the wave. The post-shock evolution of the wave profile is explored, and we quantitatively confirm its convergence to the theoretically expected N-wave shape. The accuracy of various numerical algorithms used to compute the nonlinear wave evolution is also investigated: we find that higher order spatial reconstruction and high resolution are crucial for capturing the shock formation correctly.
The giant radio flare of Cygnus X-3 in September 2016

In the long-term multi-frequency monitoring program of the microquasars with RATAN-600 we discovered the giant flare from the X-ray binary Cygnus X-3 on 13 September 2016. It happened after 2000 days of the 'quiescent state' of the source passed after the former giant flare (~18 Jy) in March 2011. We have found that during this quiet period the hard X-ray flux (Swift/BAT, 15-50 keV) and radio flux (RATAN-600, 11 GHz) have been strongly anti-correlated. Both radio flares occurred after transitions of the microquasar to a 'hypersoft' X-ray state that occurred in February 2011 and in the end of August 2016. The giant flare was predicted by us in the first ATel #9416. Indeed after dramatic decrease of the hard X-ray Swift 15-50 keV flux and RATAN 4-11 GHz fluxes (a 'quenched state') a small flare (0.7 Jy at 4-11 GHz) developed on MJD 57632 and then on MJD 57644.5 almost simultaneously with X-rays radio flux rose from 0.01 to 15 Jy at 4.6 GHz during few days. The rise of the flaring flux is well fitted by a exponential law that could be a initial phase of the relativistic electrons generation by internal shock waves in the jets. Initially spectra were optically thick at frequencies lower 2 GHz and optically thin at frequencies higher 8 GHz with typical spectral index about -0.5. After maximum of the flare radio fluxes at all frequencies faded out with the exponential law (~ exp(-(t-t0)/2d) for 21.7 GHz).