Miracle-dz/UniFAR-FTUs huggingface dataset:
Potassium balance in paddy fields under conventional rice straw recycling versus cow dung compost application in mixed crop–livestock systems in Japan

ABSTRACT Potassium (K) fertilizer consumption in rice production has increased in developing countries where negative K balance was observed, but it has recently decreased in Japan. This situation raises a question of how K fertilization is managed in Japanese paddy fields and how it affects soil K balance and soil K status. Rice straw (RS) is a good source of K, and RS recycling after harvesting is a common practice in Japan. However, in mixed crop–livestock systems, RS is taken at harvesting time to use as the feed for cows and substituted with the application of cow dung compost (CDC) to the fields. We investigated soil K balance and soil K status in 8 (2017) and 10 (2018) pairs of adjacent RS- and CDC-treated fields in Mamurogawa, Yamagata, Japan. The K balance was calculated from K inputs (RS or CDC, fertilizer, and irrigation water) and K outputs (plant uptake and leaching). K fertilizer application varied widely in both treatments, with no significant difference between RS and CDC fields. K fertilizer was applied in amounts lower than those recommended for paddy rice in the study area in 56% of the fields in both treatments. The K balance was positive in most fields with RS recycling even if K fertilizer application was lower than recommended, but it was negative in half of the fields where RS was substituted with CDC. Most fields in the RS treatment had higher soil exchangeable K than the standard value for fertile soil. Therefore, K input through RS is sufficient for maintaining positive K balance, whereas K input in the CDC treatment from CDC or fertilizer may need to be increased to ensure positive K balance.
A Search for the Host Galaxy of FRB 171020

We report on a search for the host galaxy of FRB 171020, the fast radio burst (FRB) with the smallest recorded dispersion measure (DM; DM = 114 pc cm−3) of our ongoing ASKAP survey. The low DM confines the burst location within a sufficiently small volume to rigorously constrain the identity of the host galaxy. We identify 16 candidate galaxies in the search volume and single out ESO 601–G036, an Sc galaxy at redshift z = 0.00867, as the most likely host galaxy. Ultraviolet and optical imaging and spectroscopy reveal that this galaxy has a star formation rate of approximately 0.1 M⊙ yr−1 and oxygen abundance 12 + log(O/H) = 8.3 ± 0.2, properties that are remarkably consistent with the galaxy hosting the repeating FRB 121102. However, in contrast to FRB 121102, follow-up radio observations of ESO 601–G036 show no compact radio emission above a 5σ limit of L2.1GHz = 3.6 × 1019 W Hz−1. Using radio continuum observations of the field, combined with archival optical imaging data, we find no analog to the persistent radio source associated with FRB 121102 within the localization region of FRB 171020 out to z = 0.06. These results suggest that FRBs are not necessarily associated with a luminous and compact radio continuum source.
Circumstellar molecular composition of the oxygen-rich AGB star IK Tauri - I. Observations and LTE chemical abundance analysis

Context. Molecular lines in the (sub)millimeter wavelength range can provide important information about the physical and chemical conditions in the circumstellar envelopes around asymptotic giant branch stars. Aims. The aim of this paper is to study the molecular composition in the circumstellar envelope around the oxygen-rich star IK Tau. Methods. We observed IK Tau in several (sub)millimeter bands using the APEX telescope during three observing periods. To determine the spatial distribution of the 12 CO(3-2) emission, mapping observations were performed. To constrain the physical conditions in the circumstellar envelope, multiple rotational CO emission lines were modeled using a nonlocal thermodynamic equilibrium radiative transfer code. The rotational temperatures and the abundances of the other molecules were obtained assuming local thermodynamic equilibrium. Results. An oxygen-rich asymptotic giant branch star has been surveyed in the submillimeter wavelength range. Thirty four transitions of twelve molecular species, including maser lines, were detected. The kinetic temperature of the envelope was determined, and the molecular abundance fractions of the molecules were estimated. The deduced molecular abundances were compared with observations and modeling from the literature and agree within a factor of 10, except for SO 2 , which is found to be almost a factor 100 stronger than predicted by chemical models. Conclusions. From this study, we found that IK Tau is a good laboratory for studying the conditions in circumstellar envelopes around oxygen-rich stars with (sub)millimeter-wavelength molecular lines. We could also expect from this study that the molecules in the circumstellar envelope can be explained more faithfully by non-LTE analysis with lower and higher transition lines than by simple LTE analysis with only lower transition lines. In particular, the observed CO line profiles could be well reproduced by a simple expanding envelope model with a power-law structure.
RELICS: High-resolution Constraints on the Inner Mass Distribution of the z = 0.83 Merging Cluster RXJ0152.7-1357 from Strong Lensing

Strong gravitational lensing (SL) is a powerful means of mapping the distribution of dark matter. In this work, we perform an SL analysis of the prominent X-ray cluster RXJ0152.7-1357 (z = 0.83, also known as CL0152.7-1357) in Hubble Space Telescope images, taken in the framework of the Reionization Lensing Cluster Survey (RELICS). On top of a previously known z = 3.93 galaxy multiply imaged by RXJ0152.7-1357, for which we identify an additional multiple image, guided by a light-traces-mass approach, we identify seven new sets of multiply imaged background sources lensed by this cluster, spanning the redshift range [1.79–3.93]. A total of 25 multiple images are seen over a small area of ∼0.4 arcmin2, allowing us to put relatively high-resolution constraints on the inner matter distribution. Although modestly massive, the high degree of substructure, together with its very elongated shape, makes RXJ0152.7-1357 a very efficient lens for its size. This cluster also comprises the third-largest sample of z ∼ 6–7 candidates in the RELICS survey. Finally, we present a comparison of our resulting mass distribution and magnification estimates with those from a Lenstool model. These models are made publicly available through the Mikulski Archive for Space Telescopes.
Ice structures, patterns, and processes: A view across the icefields

European Science Foundation workshop Euroice 2008 held in Granada, Spain from 1–4 October 2008; Spanish national project, Hielocris, ﬁnanced by the Consejo Superior de Investigaciones Cientiﬁcas; funding from FWF, Austria (No. P23027); MINCINN, Spain (No. FIS2010-16455, No. PR2010-0012, and No. FIS2010-22322-528C02-02); and SNSF, Switzerland (No. 200021121857)
RING STAR FORMATION RATES IN BARRED AND NONBARRED GALAXIES

Nonbarred ringed galaxies are relatively normal galaxies showing bright rings of star formation in spite of lacking a strong bar. This morphology is interesting because it is generally accepted that a typical galactic disk ring forms when material collects near a resonance, set up by the pattern speed of a bar or bar-like perturbation. Our goal in this paper is to examine whether the star formation properties of rings are related to the strength of a bar or, in the absence of a bar, to the non-axisymmetric gravity potential in general. For this purpose, we obtained Hα emission line images and calculated the line fluxes and star formation rates (SFRs) for 16 nonbarred SA galaxies and four weakly barred SAB galaxies with rings. For comparison, we combine our new observations with a re-analysis of previously published data on five SA, seven SAB, and 15 SB galaxies with rings, three of which are duplicates from our sample. With these data, we examine what role a bar may play in the star formation process in rings. Compared to barred ringed galaxies, we find that the inner ring SFRs and Hα+[N ii] equivalent widths in nonbarred ringed galaxies show a similar range and trend with absolute blue magnitude, revised Hubble type, and other parameters. On the whole, the star formation properties of inner rings, excluding the distribution of H ii regions, are independent of the ring shapes and the bar strength in our small samples. We confirm that the deprojected axis ratios of inner rings correlate with maximum relative gravitational force Qg; however, if we consider all rings, a better correlation is found when a local bar forcing at the radius of the ring, Qr, is used. Individual cases are described and other correlations are discussed. By studying the physical properties of these galaxies, we hope to gain a better understanding of their placement in the scheme of the Hubble sequence and how they formed rings without the driving force of a bar.
Research on Neural Graph Collaborative Filtering Recommendation Model Fused With Item Temporal Sequence Relationships

Graph neural network-based recommender systems are blossoming recently, and it can explicitly express user-item high-order connectivity information, so it can significantly improve the recommendation performance. However, the existing methods usually assume that the users’ interests are invariant, but temporal relationships is left insufficient exploration to charactertize the user’s dynamic interest. In this paper, we propose a Neural Graph Collaborative Filtering recommendation model fused with Item Temporal Sequence relationships (NGCF-ITS), that is, a hybrid recommendation model that fuses with user-item interactions information and item temporal sequence relationships. It divides the item temporal sequences into several groups of subsequences through the sliding window strategy, then constructs the item temporal sequence relationships graph and aggregates the characteristics of item temporal sequences information. At the last, deeply depicts the dynamic changes of users’ interests, and uses the bipartite graph neural network to map the high-dimensional information of user-item and item-item into the low-dimensional space. The hybrid embedding of user-item historical interactions and item temporal sequence relationships are realized, and the expression of user-item interactions is enhanced. In this way, the heterogeneous multi-relational graphs are fused for the feature propagation, which largely refines the user and item representation for model prediction. Extensive experiments demonstrate the our proposed model significantly improve the recommendation performance compared to the state-of-the-art GNN-based models both in accuracy and training efficiency.
The three-point function in large-scale structure: redshift distortions and galaxy bias

We study the behaviour of the three-point correlation function ζ of dark matter and mock galaxies, concentrating on the effects of redshift-space distortions and the determination of galaxy bias parameters in current redshift galaxy surveys. On large scales, redshift-space distortions tend to wash out slightly the configuration dependence of the reduced three-point function Q 3 ∼ζ/ξ 2 . O nsmaller scales (10 h −1 Mpc), Q 3 develops a characteristic U-shape anisotropy between elongated and open triangles due to the effects of velocity dispersion. We show that this shape is quite universal, very weakly dependent on scale, initial spectral index or cosmological parameters and should be detectable in current galaxy surveys even if affected by shot noise or galaxy bias. We present a detailed method for obtaining constraints on galaxy bias parameters from measurements of Q3 in current galaxy redshift surveys, based on the eigenmode analysis similar to that developed for the bispectrum. We show that our method recovers the bias parameters introduced into mock galaxies by a halo occupation distribution prescription and is also able to handle potential systematics in the case when a smaller number than is ideal for mock catalogues is used to estimate the covariance matrix. We find that current redshift surveys (e.g. SDSS or 2dFGRS) are just about large enough to obtain interesting new constraints on bias. Ke yw ords: galaxies: statistics ‐ large-scale structure of Universe.
Hadronic vacuum polarization in QCD and its evaluation in Euclidean spacetime

We discuss a new technique to evaluate integrals of QCD Green's functions in the Euclidean based on their Mellin-Barnes representation. We present as a first application the evaluation of the lowest order Hadronic Vacuum Polarization (HVP) contribution to the anomalous magnetic moment of the muon $\frac{1}{2}(g_{\mu}-2)_{\rm\tiny HVP}\equiv a_{\mu}^{\rm HVP}$. It is shown that with a precise determination of the slope and curvature of the HVP function at the origin from lattice QCD (LQCD), one can already obtain a result bfor $a_{\mu}^{\rm HVP}$ which may serve as a test of the determinations based on experimental measurements of the $e^+ e^-$ annihilation cross-section into hadrons.
Finsler space–time can explain both parity asymmetry and power deficit seen in CMB temperature anisotropies

We propose a framework of Finsler space-time to explain the observed parity asymmetry and the power deficit in the low-$\ell$ ($2\leqslant \ell \leqslant 29$) multipole range of cosmic microwave background (CMB) temperature anisotropies. In the $3+1$ dimensional space-time, the three-dimensional space is described by a Randers-Finsler space, which is spatially irreversible, inducing the parity asymmetry in the CMB angular power spectrum. We estimate the constraints on the two parameters introduced by Finsler space-time via analyzing the low-$\ell$ angular power spectrum in PLANCK 2015 CMB temperature data. We see that the low-$\ell$ power suppression in the CMB temperature anisotropies can also be resolved in this scenario. Our study shows that the two low-$\ell$ anomalies, i.e., parity asymmetry and power deficit, may have a common origin.
Solar Polar Brightening and Radius at 100 and 230 GHz Observed by ALMA

Polar brightening of the Sun at radio frequencies has been studied for almost 50 years and yet a disagreement persists between solar atmospheric models and observations. Some observations reported brightening values much smaller than the expected values obtained from the models, with discrepancies being particularly large at millimeter wavelengths. New clues to calibrate the atmospheric models can be obtained with the advent of the Atacama Large Millimeter/submillimeter Array (ALMA) radio interferometer. In this work, we analyzed the lower limit of the polar brightening observed at 100 and 230 GHz by ALMA, during its Science Verification period, 2015 December 16–20. We find that the average polar intensity is higher than the disk intensity at 100 and 230 GHz, with larger brightness intensities at the south pole in eight of the nine maps analyzed. The observational results were compared with calculations of the millimetric limb brightening emission for two semi-empirical atmospheric models, FAL-C and SSC. Both models presented larger limb intensities than the average observed values. The intensities obtained with the SSC model were closer to the observations, with polar brightenings of 10.5% and 17.8% at 100 and 230 GHz, respectively. This discrepancy may be due to the presence of chromospheric features (like spicules) at regions close to the limb.
Arp 202: a TDG formed in a parent's extended dark matter halo?

We report on H${\alpha}$ + [NII] imaging of the Arp 202 interacting pair and its tidal dwarf galaxy (TDG) candidate as well as a GMOS long slit spectrum from the TDG candidate, observed with the Gemini North telescope. Our H${\alpha}$ + [NII] imaging reveals the TDG to have an elongated structure, $\sim$ 1.9 kpc in length with the two principal star forming knots at either end. Our observations also show the TDG candidate has a recessional V$_{H\alpha}$ $\sim$ 3032 km s$^{-1}$, within 100 km s$^{-1}$ of the parent pair's mean velocity and an oxygen abundance of 12+log(O/H) = 8.10$\pm$0.41. The TDG's oxygen abundance is in good agreement with that of a star forming region in NGC 2719A, one of the parent galaxies, which has an estimated oxygen abundance of 12+log(O/H) = 8.05$\pm$0.41. The TDG's V$_{H\alpha}$ and oxygen abundance confirm previous results validating the candidate as a TDG. The absence of detectable emission from the TDG in $\textit{Spitzer}$ 3.6 $\mu$m and 4.5 $\mu$m images together with the lack of absorption lines and weak continuum in the spectrum is consistent with absence of an old population ($\gtrsim$ 0.5 Gyr). The location of the TDG within the interaction debris and the absence of indicators of an old stellar population in the TDG are consistent with a scenario in which the TDG is formed from HI stripped from the parent galaxies and within the extended dark matter halo of one of the parents as proposed by (Bournaud et al. 2003; Duc et al. 2004).
The Use and Efficacy of Biological Therapies for Inflammatory Bowel Disease in a Danish Tertiary Centre 2010–2020

Abstract Background Patients with inflammatory bowel disease (IBD) who receive biologicals frequently experience lack or loss of response. Our aim was to describe the use and efficacy of biological therapy in a tertiary IBD center. Methods We included all bio-naive IBD patients who initiated biological therapy between 2010 and 2020 at our centre. Their medical records were reviewed. Results The population consisted of 327 Crohn’s disease (CD) patients, 291 ulcerative colitis (UC) patients, and 3 patients with IBD unclassified (IBDU). The median follow-up was 3 years (interquartile range = 2–5) after initiating therapy. The annual number of patients initiating biological therapy rose from 29 (2010) to 85 (2019). Most patients (457, 73.6%) received 1 biological drug; 164 (26.4%) patients received 2 or more biologicals. Primary lack of response was observed in 36.4% (106/291) and 17.4% (57/327) of UC and CD patients; loss of response was observed in 27.1% (79/291) and 31.5% (103/327) of UC and CD patients, respectively. The 5-year surgery rates were 26.6% and 20.4% in UC and CD patients, respectively. Multivariate Cox regression showed that treatment with thiopurine reduced the likelihood of needing to switch biological therapy, requiring surgery or corticosteroids in UC patients (HR: 0.745, 95% CI: 0.559–0.993), but not in CD patients (HR: 0.996, 95% CI: 0.736–1.349). Conclusions The annual number of IBD patients initiated on biological therapy increased considerably between 2010 and 2020. One-quarter of these patients required surgery after 5 years. Our findings suggest a beneficial effect of concurrent thiopurines for UC patients receiving biologicals, but this was not found for CD patients. This effect in UC patients was not observed when we included patients initiating thiopurines up to 6 months after the introduction of biological therapy.
Elemental abundances in the Galactic bulge from microlensed dwarf stars

Abstract We present elemental abundances of 13 microlensed dwarf and subgiant stars in the Galactic bulge, which constitute the largest sample to date. We show that these stars span the full range of metallicity from Fe/H= −0.8 to +0.4, and that they follow well-defined abundance trends, coincident with those of the Galactic thick disc.
Perturbations in quantum cosmology: The continuum limit in Fourier space

We analyze the passage to a continuum limit of the mode spectrum of primordial perturbations around flat cosmological spacetimes in hybrid Loop Quantum Cosmology, showing that this limit can be reached even if one starts by considering a finite fiducial cell as spatial slice. We focus our attention on regimes in which the background cosmology follows the effective dynamics of Loop Quantum Cosmology, although we comment on extensions of our arguments beyond this regime, as well as to some formalisms other than the hybrid approach. Whereas the perturbed system can be described in an invariant way under changes of the fiducial volume using the standard variables of the improved prescription for Loop Quantum Cosmology, we show that the desired continuum limit can be established by means of scaling transformations of the physical volume when this volume grows unboundedly. These transformations lead to a model with a continuum of modes and independent of any scale of reference for the physical volume. For the sake of comparison, we also consider an alternative road to the continuum in Fourier space that has been employed in geometrodynamics and is based on the use of scaling transformations of the fiducial volume, together with variables that are independent of them.
EXPLOSIVE NUCLEOSYNTHESIS IN THE NEUTRINO-DRIVEN ASPHERICAL SUPERNOVA EXPLOSION OF A NON-ROTATING 15 M☉ STAR WITH SOLAR METALLICITY

We investigate explosive nucleosynthesis in a non-rotating 15 M☉ star with solar metallicity that explodes by a neutrino-heating supernova (SN) mechanism aided by both standing accretion shock instability (SASI) and convection. To trigger explosions in our two-dimensional hydrodynamic simulations, we approximate the neutrino transport with a simple light-bulb scheme and systematically change the neutrino fluxes emitted from the protoneutron star. By a post-processing calculation, we evaluate abundances and masses of the SN ejecta for nuclei with a mass number ⩽70, employing a large nuclear reaction network. Aspherical abundance distributions, which are observed in nearby core-collapse SN remnants, are obtained for the non-rotating spherically symmetric progenitor, due to the growth of a low-mode SASI. The abundance pattern of the SN ejecta is similar to that of the solar system for models whose masses range between (0.4–0.5) M☉ of the ejecta from the inner region (⩽10, 000 km) of the precollapse core. For the models, the explosion energies and the 56Ni masses are ≃ 1051erg and (0.05–0.06) M☉, respectively; their estimated baryonic masses of the neutron star are comparable to the ones observed in neutron-star binaries. These findings may have little uncertainty because most of the ejecta is composed of matter that is heated via the shock wave and has relatively definite abundances. The abundance ratios for Ne, Mg, Si, and Fe observed in the Cygnus loop are reproduced well with the SN ejecta from an inner region of the 15 M☉ progenitor.
The dynamical evolution of transiting planetary systems including a realistic collision prescription

Planet–planet collisions are a common outcome of instability in systems of transiting planets close to the star, as well as occurring during in-situ formation of such planets from embryos. Previous N-body studies of instability amongst transiting planets have assumed that collisions result in perfect merging. Here, we explore the effects of implementing a more realistic collision prescription on the outcomes of instability and in-situ formation at orbital radii of a few tenths of an au. There is a strong effect on the outcome of the growth of planetary embryos, so long as the debris thrown off in collisions is rapidly removed from the system (which happens by collisional processing to dust, and then removal by radiation forces) and embryos are small (<0.1 M⊕). If this is the case, then systems form fewer detectable (≥1 M⊕) planets than systems evolved under the assumption of perfect merging in collisions. This provides some contribution to the ‘Kepler dichotomy’: the observed overabundance of single-planet systems. The effects of changing the collision prescription on unstable mature systems of super-Earths are less pronounced. Perfect mergers only account for a minority of collision outcomes in such systems, but most collisions resulting in mass loss are grazing impacts in which only a few per cent of mass is lost. As a result, there is little impact on the final masses and multiplicities of the systems after instability when compared to systems evolved under the assumption that collisions always result in perfect merging. (Less)