Miracle-dz/UniFAR-FTUs huggingface dataset:
Successive lettuce cultivation on organic substrates

Abstract The purpose of the present work was to evaluate i the influence of organic compost and soil proportions on lettuce growth in greenhouse and ii - the residual effect of organic fertilization in successive lettuce crops. Six compost:soil proportions were evaluated (100:0, 80:20, 60:40, 40:60, 20:80 and 0:100) in three successive lettuce (cultivar “Monica”) crops under randomized blocks design. Stem and crown diameter, plant height, number of leaves, volume of roots, fresh weight of leaves and the aerial portion, dry weight of leaves, stem, aerial portion, roots and the total dry weight; chlorophyll A, B and total chlorophyll were evaluated. There was a significant interaction between the organic compost dosages and the successive cultivation. The effect of the cultivation periods according to the proportions showed, in a general manner, a tendency to produce higher values of CLB, ALP and DMC in the first cultivation period for the majority of proportions. The best proportion of organic compost:soil was of 60:40, in the first crop. For all successive crops, although a residual effect of the compost was detected, the proportion of 60:40 was not enough to sustain the productivity level of the first crop and therefore requiring supplementing fertilization.
Investigating the dusty torus of Seyfert galaxies using SOFIA/FORCAST photometry

We present 31.5 micron imaging photometry of 11 nearby Seyfert galaxies observed from the Stratospheric Observatory For Infrared Astronomy (SOFIA) using the Faint Object infraRed CAmera for the SOFIA Telescope (FORCAST). We tentatively detect extended 31 micron emission for the first time in our sample. In combination with this new data set, subarcsecond resolution 1-18 micron imaging and 7.5-13 micron spectroscopic observations were used to compute the nuclear spectral energy distribution (SED) of each galaxy. We found that the turnover of the torus emission does not occur at wavelengths <31.5 micron, which we interpret as a lower-limit for the wavelength of peak emission. We used CLUMPY torus models to fit the nuclear infrared (IR) SED and infer trends in the physical parameters of the AGN torus for the galaxies in the sample. Including the 31.5 micron nuclear flux in the SED 1) reduces the number of clumpy torus models compatible with the data, and 2) modifies the model output for the outer radial extent of the torus for 10 of the 11 objects. Specifically, six (60%) objects show a decrease in radial extent while four (40%) show an increase. We find torus outer radii ranging from <1pc to 8.4 pc
A proposed chemical scheme for HCCO formation in cold dense clouds

The ketenyl radical (HCCO) has recently been discovered in two cold dense clouds with a non-negligible abundance of a few 10-11 (compared to H2). Until now, no chemical network has been able to reproduce this observation. We propose here a chemical scheme that can reproduce HCCO abundances together with HCO, H2CCO and CH3CHO in the dark clouds Lupus-1A and L486. The main formation pathway for HCCO is the OH + CCH → HCCO + H reaction as suggested by Agundez et al. but with a much larger rate coefficient than used in current models. Since this reaction has never been studied experimentally or theoretically, this larger value is based on a comparison with other similar systems.
The Diet of the Imperial Shag Phalacrocorax atriceps at Vintter Lake, Patagonia, Argentina

Abstract. The diet of the Imperial Shag (Phalacrocorax atriceps) at Vintter Lake, Patagonia, Argentina, was investigated through analysis of 157 regurgitate pellets collected during the summer seasons of 2008–2010 and 2016–2017. The native fish Galaxias platei was the main prey throughout the study period, accompanied only by a few gastropod species (2010) and coleopterans (2009 and 2016). Our results markedly differ from those previously reported for Imperial shags breeding at Vintter Lake and other sites. The results are discussed in relation to the population decline observed in shags at Vintter Lake throughout the study period.
THE CONTRIBUTION OF X-RAY BINARIES TO THE EVOLUTION OF LATE-TYPE GALAXIES: EVOLUTIONARY POPULATION SYNTHESIS SIMULATIONS

X-ray studies of normal late-type galaxies have shown that non-nuclear X-ray emission is typically dominated by X-ray binaries and provides a useful measure of star formation activity. We have modeled the X-ray evolution of late-type galaxies over the ∼14 Gyr of cosmic history, with an evolutionary population synthesis code developed by Hurley et al. Our calculations reveal a decrease in the X-ray luminosity-to-mass ratio LX/M with time, in agreement with observations. We show that this decrease is a natural consequence of stellar and binary evolution and the mass accumulating process in galaxies. The X-ray-to-optical luminosity ratio LX/LB is found to be fairly constant (around ∼1030 erg s−1L−1B,☉) and insensitive to the star formation history in the galaxies. The nearly constant value of LX/LB is in conflict with the observed increase in LX/LB from z = 0 to 1.4. The discrepancy may be caused by intense obscured star formation activity that leads to a nonlinear relationship between X-ray and B-band emission.
The role of residual symmetries in dark matter stability and the neutrino nature

We consider the class of models where Dirac neutrino masses at one loop and the dark matter stability can be obtained using only the global $U(1)_{B-L}$ symmetry already present in Standard Model. We discuss how the residual $\mathcal{Z}_n$ subgroup, left unbroken after the breaking of $U(1)_{B-L}$, dictates the neutrino nature, namely if they are Dirac or Majorana particles, as well as determines the stability of the dark matter candidate in such models. In particular, we show that without the correct breaking of $U(1)_{B-L}$ to an appropriate residual $\mathcal{Z}_n$ symmetry, the Dirac nature of neutrinos and/or dark matter stability might be lost. For completeness we also provide some examples where the dark matter stability is accidental or lost completely. Finally, we discuss one example model where the Dirac neutrinos with naturally small one loop masses as well as dark matter stability, are both protected by the same residual $\mathcal{Z}_6$ subgroup, without need for adding any new explicit or accidental symmetries beyond the Standard Model symmetries.
GAMMA-RAY BURST AND STAR FORMATION RATES: THE PHYSICAL ORIGIN FOR THE REDSHIFT EVOLUTION OF THEIR RATIO

Gamma-ray bursts (GRBs) and galaxies at high redshift represent complementary probes of the star formation history of the universe. In fact, both the GRB rate and the galaxy luminosity density are connected to the underlying star formation. Here, we combine a star formation model for the evolution of the galaxy luminosity function from z = 0 to z = 10 with a metallicity-dependent efficiency for GRB formation to simultaneously predict the comoving GRB rate. Our model sheds light on the physical origin of the empirical relation often assumed between GRB rate and luminosity density-derived star formation rate: , with ε(z)∝(1 + z)1.2. At z ≲ 4, ε(z) is dominated by the effects of metallicity evolution in the GRB efficiency. Our best-fitting model only requires a moderate preference for low-metallicity, that is a GRB rate per unit stellar mass about four times higher for log (Z/Z☉) < −3 compared to log (Z/Z☉) > 0. Models with total suppression of GRB formation at log (Z/Z☉) ≳ 0 are disfavored. At z ≳ 4, most of the star formation happens in low-metallicity hosts with nearly saturated efficiency of GRB production per unit stellar mass. However, at the same epoch, galaxy surveys miss an increasing fraction of the predicted luminosity density because of flux limits, driving an accelerated evolution of ε(z) compared to the empirical power-law fit from lower z. Our findings are consistent with the non-detections of GRB hosts in ultradeep imaging at z > 5, and point toward current galaxy surveys at z > 8 only observing the top 15%–20% of the total luminosity density.
NUMERICAL STUDY OF COSMIC RAY DIFFUSION IN MAGNETOHYDRODYNAMIC TURBULENCE

We study the diffusion of cosmic rays (CRs) in turbulent magnetic fields using test particle simulations. Electromagnetic fields are produced in direct numerical MHD simulations of turbulence and used as an input for particle tracing, particle feedback on turbulence being ignored. Statistical transport coefficients from the test particle runs are compared with earlier analytical predictions. We find qualitative correspondence between them in various aspects of CR diffusion. In the incompressible case that we consider in this paper, the dominant scattering mechanism is the non-resonant mirror interactions with the slow-mode perturbations. Perpendicular transport roughly agrees with being produced by magnetic field wandering.
The outer profile of dark matter haloes: an analytical approach

A steepening feature in the outer density profiles of dark matter halos indicating the splashback radius has drawn much attention recently. Possible observational detections have even been made for galaxy clusters. Theoretically, Adhikari et al. have estimated the location of the splashback radius by computing the secondary infall trajectory of a dark matter shell through a growing dark matter halo with an NFW profile. However, since they imposed a shape of the halo profile rather than computing it consistently from the trajectories of the dark matter shells, they could not provide the full shape of the dark matter profile around the splashback radius. We improve on this by extending the self-similar spherical collapse model of Fillmore \& Goldreich to a $\Lambda$CDM universe. This allows us to compute the dark matter halo profile and the trajectories simultaneously from the mass accretion history. Our results on the splashback location agree qualitatively with Adhikari et al. but with small quantitative differences at large mass accretion rates. We present new fitting formulae for the splashback radius $R_{\rm sp}$ in various forms, including the ratios of $R_{\rm sp} / R_{\rm 200c}$ and $R_{\rm sp} / R_{\rm 200m}$. Numerical simulations have made the puzzling discovery that the splashback radius scales well with $R_{\rm 200m}$ but not with $R_{\rm 200c}$. We trace the origin of this to be the correlated increase of $\Omega_{\rm m}$ and the average halo mass accretion rate with an increasing redshift.
Editors' Note: Relationship Between Headache Characteristics and a Remote History of TBI in Veterans: A 10-Year Retrospective Chart Review

Dr. Coffman et al. examined the association between deployment-related traumatic brain injury (TBI) severity, frequency, and other injury characteristics with headache outcomes in 594 veterans evaluated at a Veterans Administration polytrauma support clinic. They found a dose-dependent relationship between TBI severity and headache outcomes, with a history of multiple mild TBIs and a longer duration of alteration of consciousness and post-traumatic amnesia being important risk factors for poor headache outcomes in the veterans. In addition to highlighting the poor headache outcomes associated with subconcussive exposure, the authors concluded that past TBI characteristics should be considered in the development of headache management guidelines for veterans. In response, Dr. Gupta argues that the TBI phenotypes do not offer insights into salient aspects of migraine pathophysiology and questions the biological plausibility of epidemiologic relationships reported in headache research. He suggests that vasopressin may play a role in advancing the pathophysiologic understanding of headache in TBI. Responding to these comments, the authors disagree and among other things point out that not all headaches reported by patients in their study had migraine-like features. They appropriately point out that specific aspects of migraine pathophysiology were beyond the scope of their study, although they acknowledge that cortical spreading depression is a hallmark of both migraine and acute TBI and may relate to injury severity and outcomes. Nevertheless, they advocate for a cautious approach when extrapolating migraine research to the TBI population, given the differences between migraine and post-traumatic headache patients seen on structural and functional neuroimaging studies. This exchange highlights important similarities and differences in the characteristics of migraine and TBI-related headaches that are worth bearing in mind for both clinical and research pursuits in this area.
Farmer adoption of efficient inorganic nitrogen fertilizer management practices in South Dakota

Nitrogen (N) fertilizer use has led to reductions in air and water quality but is essential for increasing crop production. Following the 4Rs of nutrient management (right: source, rate, timing, and placement), specifically following university N rate guidelines, proper urea fertilizer management, use of enhanced efficiency fertilizers, and splitting up inorganic fertilizer-N applications can minimize potential negative environmental effects. Data from a 2019 probability sample survey of 465 South Dakota farmers were used to examine how local and operational characteristics (geographic location, tillage practice, and farm size) are related to the adoption of these four Rs of nutrient management practices. Factors included in inorganic N rate decisions from most to least were use of preplant soil test N (74%), yield potential (68%), previous crop credit (48%), manure credit (25%), and tillage type (16%). Of all the factors used to make fertilizer-N rate decisions, only the use of previous crop and manure credit factors were influenced by farm location and tillage method but not farm size. Of all respondents, 30% used urease inhibitors to minimize ammonia (NH3) loss and 31% applied urea before predicted precipitation. However, farms in drier, central South Dakota and no-till farms used urease inhibitors and applied before predicted precipitation more often than farms in wetter, eastern South Dakota and conventional- and reduced-tillage farms, who were more likely to use tillage to incorporate urea. To minimize leaching and denitrification loss, farms in eastern South Dakota where normal rainfall is greater used nitrification inhibitors or slow-release fertilizers and split-N applications (48% and 53%, respectively), while fewer farms in central South Dakota where normal rainfall is less used these technologies (34% and 36%, respectively). Larger farms more frequently used urease and nitrification inhibitors, and/or slow-release fertilizer technologies to minimize N loss. These results indicate that local and operational characteristics including geographic location, tillage, and farm size influence on-farm decisions concerning the adoption of these 4R management practices and should be considered when investigating and promoting 4R practices.
Radio pulsar variability

Abstract Pulsars are potentially the most remarkable physical laboratories we will ever use. Although in many senses they are extremely clean systems there are a large number of instabilities and variabilities seen in the emission and rotation of pulsars. These need to be recognised in order to both fully understand the nature of pulsars, and to enable their use as precision tools for astrophysical investigations. Here I describe these effects, discuss the wide range of timescales involved, and consider the implications for precision pulsar timing.
AN EXTRAORDINARY OUTBURST OF THE MAGNETAR SWIFT J1822.3–1606

The 2011 outburst of Swift J1822.3–1606 was extraordinary; periodic modulations at the spin period of the underlying neutron star were clearly visible, remarkably similar to what is observed during the decaying tail of magnetar giant flares. We investigated the temporal characteristics of X-ray emission during the early phases of the outburst. We performed a periodicity search with the spectral hardness ratio (HR) and found a coherent signal near the spin period of the neutron star, but with a lag of about 3 radians. Therefore, the HR is strongly anti-correlated with the X-ray intensity, which is also seen in the giant flares. We studied the time evolution of the pulse profile and found that it evolves from a complex morphology to a much simpler shape within about a month. Pulse profile simplification also takes place during the giant flares, but on a much shorter timescale of about a few minutes. We found that the amount of energy emitted during the first 25 days of the outburst is comparable to what was detected in minutes during the decaying tail of giant flares. Based on these similarities, we suggest that the triggering mechanisms of the giant flares and the magnetar outbursts are likely the same. We propose that the trapped fireball that develops in the magnetosphere at the onset of the outburst radiates away efficiently in minutes in magnetars exhibiting giant flares, while in other magnetars, such as Swift J1822.3–1606, the efficiency of radiation of the fireball is not as high and, therefore, lasts much longer.
Quantum and classical aspects of scalar and vector fields around black holes

This thesis presents recent studies on test scalar and vector fields around black holes. It is separated in two parts according to the asymptotic properties of the spacetime under study. In the first part, we investigate scalar and Proca fields on an asymptotically flat background. For the Proca field, we obtain a complete set of equations of motion in higher dimensional spherically symmetric backgrounds. These equations are solved numerically, both to compute Hawking radiation spectra and quasi-bound states. In the former case, we carry out a precise study of the longitudinal degrees of freedom induced by the field mass. This can be used to improve the model in the black hole event generators currently used at the Large Hadron Collider. Regarding quasi-bound states, we find arbitrarily long lived modes for a charged Proca field, as well as for a charged scalar field, in a Reissner-Nordstr\"om black hole. The second part of this thesis presents research on superradiant instabilities of scalar and Maxwell fields on an asymptotically anti-de Sitter background. For the scalar case, we introduce a charge coupling between the field and the background, and show that superradiant instabilities do exist for all $\ell$ modes, in higher dimensions. For the Maxwell case, we first propose a general prescription to impose boundary conditions on the Kerr-anti-de Sitter spacetime, and obtain two Robin boundary conditions. Then these two conditions are implemented to study superradiant unstable modes and vector clouds. In particular, we find that the new branch of quasinormal modes may be unstable in a larger parameter space. Furthermore, the existence of vector clouds indicates that one may find a vector hairy black hole solution for the Einstein-Maxwell-anti-de Sitter system at the nonlinear level, which implies that, in such system, the Kerr-Newman-anti-de Sitter black hole is not a unique solution.
TERRESTRIAL PLANETS ACROSS SPACE AND TIME

The study of cosmology, galaxy formation, and exoplanets has now advanced to a stage where a cosmic inventory of terrestrial planets (TPs) may be attempted. By coupling semianalytic models of galaxy formation to a recipe that relates the occurrence of planets to the mass and metallicity of their host stars, we trace the population of TPs around both solar-mass (FGK type) and lower-mass (M dwarf) stars throughout all of cosmic history. We find that the mean age of TPs in the local universe is for FGK hosts and for M dwarfs. We estimate that hot Jupiters have depleted the population of TPs around FGK stars by no more than , and that only of the TPs at the current epoch are orbiting stars in a metallicity range for which such planets have yet to be confirmed. The typical TP in the local universe is located in a spheroid-dominated galaxy with a total stellar mass comparable to that of the Milky Way. When looking at the inventory of planets throughout the whole observable universe, we argue for a total of and TPs around FGK and M stars, respectively. Due to light travel time effects, the TPs on our past light cone exhibit a mean age of just 1.7 ± 0.2 Gyr. These results are discussed in the context of cosmic habitability, the Copernican principle, and searches for extraterrestrial intelligence at cosmological distances.
CO J=3-2 Emission from the "Water Fountain" Sources IRAS 16342-3814 and IRAS 18286-0959

We observed CO J=3-2 emission from the "water fountain" sources, which exhibit high-velocity collimated stellar jets traced by water maser emission, with the Atacama Submillimeter Telescope Experiment (ASTE) 10 m telescope. We detected the CO emission from two sources, IRAS 16342-3814 and IRAS 18286-0959. The IRAS 16342-3814 CO emission exhibits a spectrum that is well fit to a Gaussian profile, rather than to a parabolic profile, with a velocity width (FWHM) of 158+/-6 km/s and an intensity peak at VLSR = 50+/-2 km/s. The mass loss rate of the star is estimated to be ~2.9x10^-5 M_sun/yr. Our morpho-kinematic models suggest that the CO emission is optically thin and associated with a bipolar outflow rather than with a (cold and relatively small) torus. The IRAS 18286-0959 CO emission has a velocity width (FWHM) of 3.0+/-0.2 km/s, smaller than typically seen in AGB envelopes. The narrow velocity width of the CO emission suggests that it originates from either an interstellar molecular cloud or a slowly-rotating circumstellar envelope that harbors the water maser source.
CALIBRATING STELLAR POPULATION MODELS WITH MAGELLANIC CLOUD STAR CLUSTERS

Stellar population models are commonly calculated using star clusters as calibrators for those evolutionary stages that depend on free parameters. However, discrepancies exist among different models, even if similar sets of calibration clusters are used. With the aim of understanding these discrepancies, and of improving the calibration procedure, we consider a set of 43 Magellanic Cloud (MC) clusters, taking age and photometric information from the literature. We carefully assign ages to each cluster based on up-to-date determinations, ensuring that these are as homogeneous as possible. To cope with statistical fluctuations, we stack the clusters in five age bins, deriving for each of them integrated luminosities and colors. We find that clusters become abruptly red in optical and optical–infrared colors as they age from ∼0.6 to ∼1 Gyr, which we interpret as due to the development of a well-populated thermally pulsing asymptotic giant branch (TP-AGB). We argue that other studies missed this detection because of coarser age binnings. Maraston and Girardi et al. models predict the presence of a populated TP-AGB at ∼0.6 Gyr, with a correspondingly very red integrated color, at variance with the data; Bruzual & Charlot and Conroy models run within the error bars at all ages. The discrepancy between the synthetic colors of Maraston models and the average colors of MC clusters results from the now obsolete age scale adopted. Finally, our finding that the TP-AGB phase appears to develop between ∼0.6 and 1 Gyr is dependent on the adopted age scale for the clusters and may have important implications for stellar evolution.