Miracle-dz/UniFAR-FTUs huggingface dataset:
Pyramiding Submergence Tolerance and Three Bacterial Blight Resistance Genes in Popular Rice Variety Hasanta through Marker-Assisted Backcross Breeding

Flash flooding (FF) along with bacterial blight (BB) outbreak are very destructive for rice production in the rainfed shallow-lowland (RSL) ecosystem. The presence of dynamic Xoo races with varying levels of genetic diversity and virulence renders their management extremely challenging under RSL. In this context, the marker-assisted improvement of plant resistance/tolerance has been proven as one of the most promising strategies towards the development of sustainable cultivars. The present study demonstrates the marker-assisted introgression of the submergence tolerant (Sub1) and three bacterial blight resistant genes (Xa21 + xa13 + xa5) into the genetic background of Hasanta, a long duration popular rice variety in the eastern coastal region of India. The rice genotypes, Swarna Sub1 (carrying Sub1) and IRBB66 (carrying Xa21 + xa13 + Xa7 + xa5 + Xa4) had maximum genetic similarity (0.84 and 0.73, respectively) with Hasanta; recurrent parent (RP) was used as donor. The forward analysis of target genes in F1s, IC1F1s and backcross (BC) generations was performed by linked/genic markers (Sub1bc2; pTA248, xa13prom and RM122), whereas background recovery of RP in each BC and segregating generations was performed utilizing 108 hypervariable SSR markers. Intervened speed breeding (SB) strategy and intensive phenotyping could lead the development of near isogenic lines (NILs) as to the RP in all basic traits. The performance of the near isogenic lines (NILs, BC2F3 and BC2F4), HS 232-411-391-756-37, HS 232-411-391-809-8, HS 232-411-391-756-18, HS 110-224-197-10-36, HS 232-411-391-809-81, HS 110-224-197-10-41 and HS 232-411-391-809-63 establishes the utility of marker-assisted backcross-breeding (MAB) and SB in accelerated trait introgression. The introgressed lines carrying Sub1 + Xa21 + xa13 + xa5 showed 76% to 91% survival under 14 days of submergence and durable BB resistance (percent disease index-PDI of 2.68 ± 0.26 to 6.22 ± 1.08 and lesion length, LL of 1.29 ± 0.12 to 4.2 ± 0.64 cm). Physiological analysis revealed that improved NILs, carrying Sub1 gene conquered adaptive physiological modulations, had reduced the consumption of soluble sugar and the degradation of total chlorophyll contents (TCC), and an enhanced level of Alcohol Dehydrogenase activity (ADH) and proline accumulation in all submergence regimes. The pyramided lines attained complete product profile of RP, that will contribute to sustainable rice production under RSL, particularly in the coastal region that has substantial acreage under the variety Hasanta.
Implementing an institution-wide pedagogical change in an Israeli college: The AWpack advising system in support of academic writing

Universities and colleges around the globe struggle to find ways to improve students’ academic writing skills. With the goal of tackling students’ writing skills on an institutional level, we set out on a 6-year journey to seek ways of enhancing the teaching of academic writing on a wide selection of courses. Here we describe and analyze the challenges entailed in implementing an intervention in a teachers’ college in Israel. We found that as the implementation process evolved, a shift from a top-down approach to a bottom-up approach resolved three different challenges: (a) The management challenge, which comes into play when leading any type of change; (b) The challenges specific to the academic work environment; and (c) The challenges of providing effective pedagogical tools for the implementation of the change. The one-on-one advising system, constituting the final stage of the process brings about the desirable change in broader terms. Based on the Tpack model, we offer AWpack (Academic Writing—pedagogical and content knowledge) as a strategy for implementing an institutional pedagogic change in the case of academic writing. Moreover, we show that as a working strategy within an academic institution it may facilitate other sought-after pedagogic changes.
Stratigraphy, Tectonics and Hydrocarbon Habitat of the Abadan Plain Basin: A Geological Review of a Prolific Middle Eastern Hydrocarbon Province

The Abadan Plain Basin is located in the Middle East region which is host to some of the world’s largest oil and gas fields around the Persian Gulf. This basin is a foredeep basin to the southwest of the Zagros Fold-Thrust-Belt, bounded along its northern and eastern margins by the Dezful Embayment. Most of the rocks in this basin have been deposited in a carbonate environment, and existing fractures have made the formations a favourable place for hydrocarbon accumulations. The basin is enriched by oil and, therefore, gas reservoirs are few, and some of the explored reservoirs exhibit significant degrees of overpressure. This paper has compiled several aspects of the Abadan Plain Basin tectonics, structural geology and petroleum systems to provide a better understanding of the opportunities and risks of development activities in this region. In addition to the existing knowledge, this paper provides a basin-wide examination of pore pressure, vertical stress, temperature gradient, and wellbore stability issues.
Abell 315: reconciling cluster mass estimates from kinematics, X-ray, and lensing

Context. Determination of cluster masses is a fundamental tool for cosmology. Comparing mass estimates obtained by di ff erent probes allows to understand possible systematic uncertainties. Aims. The cluster Abell 315 is an interesting test case, since it has been claimed to be underluminous in X-ray for its mass (determined via kinematics and weak lensing). We have undertaken new spectroscopic observations with the aim of improving the cluster mass estimate, using the distribution of galaxies in projected phase space. Methods. We identified cluster members in our new spectroscopic sample. We estimated the cluster mass from the projected phasespace distribution of cluster members using the MAMPOSSt method. In doing this estimate we took into account the presence of substructures that we were able to identify. Results. We identify several cluster substructures. The main two have an overlapping spatial distribution, suggesting a (past or ongoing) collision along the line-of-sight. After accounting for the presence of substructures, the mass estimate of Abell 315 from kinematics is reduced by a factor 4, down to M-200 = 0.8(-0.4)(+0.6) x 10(14) M-circle dot. We also find evidence that the cluster mass concentration is unusually low, c200 r200 = r 2. 1. Using our new estimate of c200 we revise the weak lensing mass estimate down to M-200 = 1.8(-0.9)(+1.7) x 10(14) M-circle dot. Our new mass estimates are in agreement with that derived from the cluster X-ray luminosity via a scaling relation, M-200 = 0.9 +/- 0.2 x 10(14) M-circle dot. Conclusions. Abell 315 no longer belongs to the class of X-ray underluminous clusters. Its mass estimate was inflated by the presence of an undetected subcluster in collision with the main cluster. Whether the presence of undetected line-of-sight structures can be a general explanation for all X-ray underluminous clusters remains to be explored using a statistically significant sample.
Star Formation Rates in Faint Radio Galaxies

The decimetric radio continuum luminosity of a star-forming galaxy appears to be directly proportional to the rate of formation of supernovae in the galaxy. Since decimetric radiation does not suffer significant extinction and is not directive, radio luminosities may thus provide a particularly straightforward way to determine the current rate of star formation. Using a sample of over 700 local galaxies, we confirm the utility of the radio luminosity as a measure of star formation rate by showing concordance with the rates predicted by U-band, Hα, and far-infrared luminosities. We also show that there are systematic discrepancies between these various indicators, suggesting that the Hα luminosity may underestimate the star formation rate by approximately an order of magnitude when the star formation rate is ≳20 M☉ yr-1. We use this calibration and the measured radio luminosities of sub-mJy radio sources to infer the star formation rate in approximately 60 star-forming galaxies at moderate (z ≳ 0.1) redshifts, both as the actual rate and as the fraction of the existing mass of stars in the galaxy. For some of these objects, the inferred current rate of star formation could increase the stellar mass in the galaxy by approximately 10% over an interval of ≈ 30 Myr.
Understanding and Exploring the Concept of Fear, in the Work Context and Its Role in Improving Safety Performance and Reducing Well-Being in a Steady Job Insecurity Period

Job insecurity is attributable to the fear of being exploited by the organization and may have negative effects on employees. For example, it may lead employees to adopt non-compliant or deviant behaviors that harm individuals and their organization. However, knowledge about specific fears that have positive or negative effects on employees and organizations is limited. Therefore, this study aimed to detect the main fears related to job insecurity in an organization and the hidden meanings included in each of these fears that may cause negative and positive effects on important work-related outcomes. Further, we identified safety behaviors related to the previously identified fears. Notably, we investigated whether fears reduce well-being, the number of accidents and near misses, and behaviors related to safety and whether they increase the perceived probability of making mistakes. We conducted 65 focus groups with 37 managers/employees and 180 workers in separate groups. Furthermore, they completed a self-report questionnaire. We identified eleven fears and related meanings and ten safety behaviors. Multivariate regression analyses revealed that fears were significantly negatively associated with well-being and safety behaviors but not with the probability of making mistakes and causing accidents. Thus, fears play a key role in promoting behaviors, organizational strategies, and employees’ well-being. The analysis results show that fears are included in a main general factor and suggest a new way to consider fears at work. Given our findings, we propose a new definition of fear in the organization.
The Dawes Review 8: Measuring the Stellar Initial Mass Function

Abstract The birth of stars and the formation of galaxies are cornerstones of modern astrophysics. While much is known about how galaxies globally and their stars individually form and evolve, one fundamental property that affects both remains elusive. This is problematic because this key property, the birth mass distribution of stars, referred to as the stellar initial mass function, is a key tracer of the physics of star formation that underpins almost all of the unknowns in galaxy and stellar evolution. It is perhaps the greatest source of systematic uncertainty in star and galaxy evolution. The past decade has seen a growing variety of methods for measuring or inferring the initial mass function. This range of approaches and evolving definitions of the quantity being measured has in turn led to conflicting conclusions regarding whether or not the initial mass function is universal. Here I review this growing wealth of approaches, and highlight the importance of considering potential initial mass function variations, reinforcing the need to carefully quantify the scope and uncertainties of measurements. I present a new framework to aid the discussion of the initial mass function and promote clarity in the further development of this fundamental field.
Reply to the Comment on: “What is the Entanglement Length in a Polymer Melt ?“

In their comment on our paper [1] Wkhnewski and Richter provide new Neutron Spin Echo (IWE) data on longer PEB-2 polymer chains than in their recent publication [2]. They find that iinite chain length effects are rather small going from MW = 36000 to MW = 190000. In contrast our simulations showed rather strong finite size effects in the dynamic structure factor S(k, t) going from N = 700 to N = 10000 chains. The issue can be resolved by properly mapping their new data to the simulation. Such a mapping is ambiguous since a a unique definition of the entanglement length doea not exist. The definition using the plateau modulus gives an entanglemen~ length of ‘Ne,P = 72 for our bead-spring model & does a scaling analys~ of the diffusion constant D [1]. Defining N. by the crossover point of the monomer dkplacements, gl (t),from initial Rouse to local reptation regime, whkh is the concept used in the original reptation model, we obtain N= = 32. Since gl (~e) should be closely related to the tube dkneter, dT, we anticipated that dT measured from S(k, t) and gl (~e) give the same number. Apparently a good mapping to experiments is only obtained if one uses the model independent Ne,P value. Using N. ,P to map polyethylene onto our model a molecular weight of A&j = 36000 would correspond to N = 1150, which is twice as large than the mapping proposed in the comment based on Ne = 35. Jn Fig. 2 we show additional simulation data for N = 2000 and we find that the S(k, -t) data are irhstinguishable from the N = 10000 results. Hence the transitionrd range, where finite chain length eifects become negligible, is consistent with the PEB-2 NSE data. In the comment it is proposed to use the exact result for the long time decay of the reptation structure function since k119/27r = 1. Doing so improves the quality of the fits significantly and gives slightly larger values for d~ than before (dz’(20t)()) = 9.6a and dT(700) = 12.90, N – 150 was used for the fits se we argue below). However the overall finite size behavior of &(N) is not altered. To understand these finite size effects we calculated gl(t) as a function of the monomer position along the chain for N = 700. It can be seen from Fig. 1 that in the initial time regime the outer monomers (1/700) move twice aa fast the inner ones (75-625). Monomers between position (1) and (75) start to move faster in the observed time frame then the middle part of the chain. This faster Rouse-relaxation at the chain ends is neglected in the reptation model, but effects S(k, t) as well. The magnitude of this effect may be estimated by recalculating S(k, t) for a subchain of inner monomers where the first and the last 75 monomers are not taken into account. In Fig. 2 we can see that doing so increases S(k, t)by about 10%
A Low-Latitude Halo Stream around the Milky Way

We present evidence for a ring of stars in the plane of the Milky Way, extending at least from l = 180° to 227° with turnoff magnitude g ~ 19.5; the ring could encircle the Galaxy. We infer that the low Galactic latitude structure is at a fairly constant distance of R = 18 ± 2 kpc from the Galactic center above the Galactic plane and has R = 20 ± 2 kpc in the region sampled below the Galactic plane. The evidence includes 500 Sloan Digital Sky Survey spectroscopic radial velocities of stars within 30° of the plane. The velocity dispersion of the stars associated with this structure is found to be 27 km s-1 at (l, b) = (198°, - 27°), 22 km s-1 at (l, b) = (225°, 28°), 30 km s-1 at (l, b) = (188°, 24°), and 30 km s-1 at (l, b) = (182°, 27°). The structure rotates in the same prograde direction as the Galactic disk stars but with a circular velocity of 110 ± 25 km s-1. The narrow measured velocity dispersion is inconsistent with power-law spheroid or thick-disk populations. We compare the velocity dispersion in this structure with the velocity dispersion of stars in the Sagittarius dwarf galaxy tidal stream, for which we measure a velocity dispersion of 20 km s-1 at (l, b) = (165°, - 55°). We estimate a preliminary metallicity from the Ca II (K) line and color of the turnoff stars of [Fe/H] = -1.6 with a dispersion of 0.3 dex and note that the turnoff color is consistent with that of the spheroid population. We interpret our measurements as evidence for a tidally disrupted satellite of 2 × 107 to 5 × 108 M☉ that rings the Galaxy.
Anti-Inflammatory and Antimicrobial Activities of Portuguese Prunus avium L. (Sweet Cherry) By-Products Extracts

The bioactivity of natural by-products in food and pharmaceutical applications is the subject of numerous studies. Cherry production and processing generates large amounts of biowaste, most of which is not used. The recovery of these by-products is essential for promoting the circular economy and to improving sustainability in the food industry. In this work, we explored the anti-inflammatory and antimicrobial potential of two different extracts from stems, leaves, and flowers of Portuguese cherries. The anti-inflammatory potential was studied on lipopolysaccharide (LPS)-stimulated mouse macrophages (RAW 264.7) by evaluating the effect of by-products on cellular viability and nitric oxide (NO) production. Disc diffusion and minimum inhibitory concentration (MIC) were used to determine antimicrobial activity. The cherry by-products had no cytotoxic effect on RAW 264.7 cells, and were able to inhibit nitrite production in a dose-dependent manner. Moreover, all aqueous infusions showed good antioxidant activity against NO radicals. Moreover, leaf extracts showed the best activity against most of the strains studied. The results revealed, for the first time, interesting anti-inflammatory and antimicrobial properties of cherry by-products. This could potentially be of interest for their therapeutic use in the treatment of inflammation-related diseases or in controlling the growth of microorganisms.
The Fastest Galaxy Evolution in an Unbiased Compact Group Sample with WISE

We study the mid-infrared (MIR) properties of galaxies in compact groups and their environmental dependence using the Wide-field Infrared Survey Explorer (WISE) data. We use a volume-limited sample of 670 compact groups and their 2175 member galaxies with and , drawn from Sohn et al., which were identified using a friends-of-friends algorithm. Among the 2175 galaxies, 1541 galaxies are detected at WISE 12 with a signal-to-noise ratio greater than 3. Among the 1541 galaxies, 433 AGN-host galaxies are identified by using both optical and MIR classification schemes. Using the remaining 1108 non-AGN galaxies, we find that the MIR [3.4]–[12] colors of compact group early-type galaxies are on average bluer than those of cluster early-type galaxies. When compact groups have both early- and late-type member galaxies, the MIR colors of the late-type members in those compact groups are bluer than the MIR colors of cluster late-type galaxies. As compact groups are located in denser regions, they tend to have larger early-type galaxy fractions and bluer MIR color galaxies. These trends are also seen for neighboring galaxies around compact groups. However, compact group member galaxies always have larger early-type galaxy fractions and bluer MIR colors than their neighboring galaxies. Our findings suggest that the properties of compact group galaxies depend on both internal and external environments of compact groups, and that galaxy evolution is faster in compact groups than in the central regions of clusters.
The Angular Power Spectrum of BATSE 3B Gamma-Ray Bursts

We compute the angular power spectrum C(sub l) from the BATSE 3B catalog of 1122 gamma-ray bursts and find no evidence for clustering on any scale. These constraints bridge the entire range from small scales (which probe source clustering and burst repetition) to the largest scales (which constrain possible anisotropics from the Galactic halo or from nearby cosmological large-scale structures). We develop an analysis technique that takes the angular position errors into account. For specific clustering or repetition models, strong upper limits can be obtained down to scales l approx. equal to 30, corresponding to a couple of degrees on the sky. The minimum-variance burst weighting that we employ is visualized graphically as an all-sky map in which each burst is smeared out by an amount corresponding to its position uncertainty. We also present separate bandpass-filtered sky maps for the quadrupole term and for the multipole ranges l = 3-10 and l = 11-30, so that the fluctuations on different angular scales can be inspected separately for visual features such as localized 'hot spots' or structures aligned with the Galactic plane. These filtered maps reveal no apparent deviations from isotropy.
Bioaccessibility of Phenolic Compounds and Antioxidant Properties of Goat-Milk Powder Fortified with Grape-Pomace-Seed Extract after In Vitro Gastrointestinal Digestion

This study deals with the evaluation of the bioaccessibility and antioxidant properties of phenolic compounds from heat-treated skim goat-milk powder fortified with grape-pomace-seed extract, after in vitro gastrointestinal digestion. Ultra-high performance liquid chromatography coupled to diode array detection and mass spectrometry (UHPLC-DAD MS/MS) analysis confirmed the abundant presence of phenolic acids and flavan-3-ols in the grape-pomace-seed extract (SE) and heat-treated skim goat-milk/seed-extract powder (TME). After in vitro digestion of TME powder and recovery of total quantified phenolics, flavan-3-ols and phenolic acids were 18.11%, 24.54%, and 1.17%, respectively. Low recovery of grape-pomace-seed phenolics indicated strong milk protein–phenolic interactions. Electrophoretic analysis of a soluble fraction of digested heat-treated skim goat milk (TM) and TME samples showed the absence of bands originating from milk proteins, indicating their hydrolysis during in vitro gastrointestinal digestion. The digested TME sample had better antioxidant properties in comparison to the digested TM sample (except for the ferrous ion-chelating capacity, FCC), due to the presence of bioaccessible phenolics. Taking into account the contribution of the digestive cocktail, digested TME sample had lower values of total phenolic content (TPC), in vitro phosphomolybdenum reducing capacity (TAC) and ferric reducing power (FRP), compared to the undigested TME sample. These results could be attributed to low recovery of phenolic compounds. TME powder could be a good carrier of phenolics to the colon; thus, TME powder could be a promising ingredient in the formulation of functional food.
Descattering of Giant Pulses in PSR B1957+20

The interstellar medium scatters radio waves, which causes pulsars to scintillate. For intrinsically short bursts of emission, the observed signal should be a direct measurement of the impulse response function. We show that this is indeed the case for giant pulses from PSR B1957+20: from baseband observations at 327 MHz, we demonstrate that the observed voltages of a bright pulse allow one to coherently descatter nearby pulses. We find that while the scattering timescale is , the power in the descattered pulses is concentrated within a span almost two orders of magnitude shorter, of . This sets an upper limit to the intrinsic duration of the giant pulses. We verify that the response inferred from the giant pulses is consistent with the scintillation pattern obtained by folding the regular pulsed emission, and that it decorrelates on the same timescale, of . In principle, with large sets of giant pulses, it should be possible to constrain the structure of the scattering screen much more directly than with other current techniques, such as holography on the dynamic spectrum and cyclic spectroscopy.