Miracle-dz/UniFAR-FTUs huggingface dataset:
CHANGES IN THE BACTERIAL COMMUNITY STRUCTURE AND DIVERSITY OF CHAGAN LAKE SEDIMENTS, NORTHEASTERN CHINA

This study employed Illumina MiSeq high-throughput sequencing to explore the composition of the bacterial community of Chagan Lake sediments and its response to soil physicochemical properties. Our findings indicated that bacterial abundance and diversity are significantly correlated with water depth. Particularly, the bacterial alpha diversity and phyla relative abundance increased with water depth. Furthermore, the five dominant bacterial phyla in the bacterial community according to all plots were Proteobacteria, Chloroflexi, Acidobacteriota, and Actinobacteriota. Moreover, our findings indicated that electrical conductivity (EC), pH, and total carbon (TC) in sediments are important factors that affect the bacterial community structure and diversity of sediments. In summary, the bacterial community structure and diversity varied significantly in different plot sediments of Chagan Lake, which were regulated by soil nutrients and physical properties. The results of this study can be used to further explore the potential relationship between bacterial communities and the environment, and provide a scientific basis for the prediction of ecosystem structure and function of alpine inland wetlands. Bacteria are a major component of lake microbial communities and are the main decomposers of organic compounds. Several studies have evaluated the microbial community structure of lake sediments and have reported that the microbial community composition of sediments varies depending on location, season, and sediment depth. the composition of bacterial communities in the sediments Taihu Lake in summer, and found that the dominant bacterial phyla in different lake areas varied depending on the region. found that the composition of eukaryotic microbial communities in Meiliang Bay and the lake center of Taihu exhibited obvious seasonal changes, and different lake areas responded differently to environmental factors. Meiliang Bay and the lake center were affected by total phosphorus (TP), total nitrogen (TN), and electrical conductivity (EC). However, Wan found that, rather than lake location, season was the most important determinant of microbial community structure in sediments. Ye et found that although the vertical distribution of bacterial communities in the sediments of Meiliang Bay in Taihu Lake was similar, the composition of archaeal communities varied significantly depending on water depth. few studies have explored the microbial community composition of Chagan Lake sediments. Therefore, our study collected sediments from a 10–15 cm depth in the coastal areas of Chagan Lake and the center of the lake in 2017. The bacterial community structure of the sediments was then characterized via high-throughput sequencing technology to explore its relationship with different sediment properties. Collectively, our findings provide insights into the formation mechanism of sediment bacterial communities in Chagan Lake, which can serve as a theoretical basis for maintaining the stability of the Chagan Lake ecosystem.
Spectroscopy of z∼ 5 Lyman break galaxies in the ESO Remote Galaxy Survey

We present the global results of a large spectroscopic survey carried out in order to identify z∼ 5 Lyman break galaxies (LBGs) across 10 widely separated ∼45 arcmin2 fields to a depth of IAB= 26.3. The redshifts of seventy 4.6 3, the typical z∼ 5 LBGs have metallicities a factor of 3 lower than those of LBGs at z∼ 3. Hubble Space Telescope imaging of a subset of the LBGs indicates that a large majority of the spectroscopically confirmed LBGs in our sample are members of multiple systems (on ∼ arcsec scales) and/or show disturbed morphology. Using local LBG analogues as a model, this multiplicity could be explained either by super-starburst regions within a larger unseen structure or by a high incidence of merging events at this epoch. The current data cannot distinguish between these two possibilities. The surface density of z∼ 5 LBGs in two of the 10 fields is considerably higher than in the rest. Both show clear spikes in their redshift distributions indicating strong three-dimensional clustering in these fields. Against an expectation of about one source per 0.1 in redshift between 4.8 < z < 5.6, one field has seven identified objects between 5.11 < z < 5.21 and the other has 17 between 4.95 < z < 5.15. Neither structure can be bound given their depth in redshift and probably extend beyond the observed fields. The three-dimensional distances between LBGs in the structures are too large for them to have triggered their starbursts through mutual gravitational interaction, and so it is likely that the short-lived LBGs represent only a small fraction of the baryons in the structures.
Study of LINER sources with broad H(alpha) emission. X-ray properties and comparision to luminous AGN and X-ray binaries

We study the X-ray properties of LINER sources with definite detection of a broad H(alpha) emission line in their optical spectra, LINER 1s from Ho et al. sample. These objects preferentially harbor a low luminosity active nucleus at the center and show small or no intrinsic absorption (<10^(22) cm^(-1)). We analyzed all available X-ray archived XMM-Newton and Chandra observations of 13 LINER 1s satisfying the above criterion in a systematic homogeneous way. We looked for any correlations between the X-ray properties and the intrinsic parameters of our sample of LINER 1s. An absorbed power-law gave a good fit to the spectra of 9 out of the 13 sources. A thermal component and an absorbed power-law were required in the remaining 4 sources. We found a photon index between 1.3\pm0.2 for the hardest source and 2.4^(+0.2)_(-0.3) for the softest one with a mean value of 1.9\pm0.2 and a dispersion sigma=0.3. The thermal component had a mean temperature kT~0.6 keV. Significant short (hours to days) time-scale variability is not common in the present sample and was observed in only 2 sources (NGC 3226 and NGC 4278). Three other sources indicate a possible variability with a low K-S test probability (2%-4%) that the nuclear emission originates from a constant source. Significant variability on months to years time-scales is detected in 7 out of the 9 sources observed more than once. No significant Fe K(alpha) emission line at 6.4 keV was detected and upper limits were derived for the 4 sources with a high enough signal to noise ratio around 6 keV. Finally, we established, for the first time for a sample of LINER 1s, that the photon index is significantly anticorrelated to L_(2-10 keV)/L_(Edd). This anticorrelation is similar to the one seen in XRBs in their low/hard state where a radiatively inefficient accretion flow is thought to be responsible for the X-ray emitted energy.
THE SIZE OF THE NARROW-LINE-EMITTING REGION IN THE SEYFERT 1 GALAXY NGC 5548 FROM EMISSION-LINE VARIABILITY

The narrow [O iii] λλ4959, 5007 emission-line fluxes in the spectrum of the well-studied Seyfert 1 galaxy NGC 5548 are shown to vary with time. From this we show that the narrow-line-emitting region has a radius of only 1–3 pc and is denser (n e ∼ 105 cm−3) than previously supposed. The [O iii] line width is consistent with virial motions at this radius given previous determinations of the black hole mass. Since the [O iii] emission-line flux is usually assumed to be constant and is therefore used to calibrate spectroscopic monitoring data, the variability has ramifications for the long-term secular variations of continuum and emission-line fluxes, though it has no effect on shorter-term reverberation studies. We present corrected optical continuum and broad Hβ emission-line light curves for the period 1988–2008.
Family of non-Abelian Kitaev models on a lattice: Topological condensation and confinement

We study a family of non-Abelian topological models in a lattice that arise by modifying the Kitaev model through the introduction of single-qudit terms. The effect of these terms amounts to a reduction in the discrete gauge symmetry with respect to the original systems, which corresponds to a generalized mechanism of explicit symmetry breaking. The topological order is either partially lost or completely destroyed throughout the various models. The systems display condensation and confinement of the topological charges present in the standard non-Abelian Kitaev models, which we study in terms of ribbon operator algebras.
DISCOVERY OF AN ∼23 MJup BROWN DWARF ORBITING ∼700 AU FROM THE MASSIVE STAR HIP 78530 IN UPPER SCORPIUS

We present the discovery of a substellar companion on a wide orbit around the ∼ 2.5 M☉ star HIP 78530, which is a member of the 5 Myr old Upper Scorpius association. We have obtained follow-up imaging over two years and show that the companion and primary share common proper motion. We have also obtained JHK spectroscopy of the companion and confirm its low surface gravity, in accordance with the young age of the system. A comparison with Drift-Phoenix synthetic spectra indicates an effective temperature of 2800 ± 200 K and a comparison with template spectra of young and old dwarfs indicates a spectral type of M8 ± 1. The mass of the companion is estimated to be 19–26 MJup based on its bolometric luminosity and the predictions of evolutionary models. The angular separation of the companion is 4. ″5, which at the distance of the primary star, 156.7 pc, corresponds to a projected separation of ∼710 AU. This companion features one of the lowest mass ratios (∼0.009) of any known companion at separations greater than 100 AU.
On combining galaxy clustering and weak lensing to unveil galaxy biasing via the halo model

We formulate the concept of non-linear and stochastic galaxy biasing in the framework of halo occupation statistics. Using two-point statistics in projection, we define the galaxy bias function, bg(rp), and the galaxy-dark matter cross-correlation function, Rgm(rp), where rp is the projected distance. We use the analytical halo model to predict how the scale dependence of bg and Rgm, over the range 0.1h 1 Mpc < � rp < � 30h 1 Mpc, depends on the non-linearity and stochasticity in halo occupation models. In particular we quantify the effect due to the presence of central galaxies, the assumption for the radial distribution of satellite galaxies, the richness of the halo, and the Poisson character of the probability to have a certain number of satellite galaxies in a halo of a certain mass. Overall, brighter galaxies reveal a stronger scale dependence, and out to a larger radius. In real-space, we find that galaxy bias becomes scale independent, with Rg = 1, for radii r � 1 5h 1 Mpc, depending on luminosity. However, galaxy bias is scale-dependent out to much larger radii when one uses the projected quantities defined in this paper. These projected bias functions have the advantage that they are more easily accessible observationally and that their scale dependence carries a wealth of information regarding the properties of galaxy biasing. To observationally constrain the parameters of the halo occupation statistics and to unveil the origin of galaxy biasing we propose the use of the bias function gm(rp) � bg(rp)/Rgm(rp). This function is obtained via a combination of weak gravitational lensing and galaxy clustering, and it can be measured using existing and forthcoming imaging and spectroscopic galaxy surveys.
PSR J0737−3039B: A PROBE OF RADIO PULSAR EMISSION HEIGHTS

In the double pulsar system PSR J0737−3039A/B, the strong wind produced by pulsar A distorts the magnetosphere of pulsar B. The influence of these distortions on the orbital-dependent emission properties of pulsar B can be used to determine the location of the coherent radio emission generation region in the pulsar magnetosphere. Using a model of the wind-distorted magnetosphere of pulsar B and the well-defined geometrical parameters of the system, we determine the minimum emission height to be ∼20RNS in the two bright orbital longitude regions. We can determine the maximum emission height by accounting for the amount of deflection of the polar field line with respect to the magnetic axis using the analytical magnetic reconnection model of Dungey and the semi-empirical numerical model of Tsyganenko. Both of these models estimate the maximum emission height to be ∼2500RNS. The minimum and maximum emission heights we calculate are consistent with those estimated for normal isolated pulsars.
TRIHALOMETHANES REMOVAL FROM DRINKING WATER BY HEATING: A CASE STUDY

Trihalomethanes (THMs) specially Chloroform is the most significant and well-known by-products of chlorine disinfection. In light of the alleged carcinogenic effects of THMs in drinking water, the goal of this study was to investigate the consequences of heating the chlorinated water, to lower its THM content, if any, in the drinking water of Dhaka. In this experiment, three individual samples from three separate locations in the same water supply system were investigated in 2019. Chloroform concentrations decreased noticeably (from 42% to 100%) due to heating during the trials. The results revealed that in sample 1, chloroform decreased from 199 to 79.7 20 μg/l (60% removal) after one minute of boiling of water, to 20 μg/l (90% elimination) after two minutes, and finally to 0 μg/l (100% removal) after three minutes. The comparable reductions in samples 2 and 3 were also similar: 70 to 24.5 μg/l (65% removal), 8.5 μg/l (88% removal), and zero μg/l (100% removal) and 153 to 89 μg/l (41.83% removal), 41 μg/l (73.2% removal), and to 40 μg/l (73.86% removal). According to experimental findings, if THM precursors and chlorine residuals are present, there may be a further considerable synthesis of THMs during the heating of drinking water. The generation and volatilization rates of THMs were responsible for the overall fluctuation in THM content in water during heating. Temperature and reaction time were major determinants of the rate of THMs synthesis, in addition to the amounts of THMs precursors and residual chlorine.
FORMATION AND PLASMA CIRCULATION OF SOLAR PROMINENCES

Solar prominences are long-lived cool and dense plasma curtains in the hot and rarefied outer solar atmosphere or corona. The physical mechanism responsible for their formation and especially for their internal plasma circulation has been uncertain for decades. The observed ubiquitous downflows in quiescent prominences are difficult to interpret because plasma with high conductivity seems to move across horizontal magnetic field lines. Here we present three-dimensional numerical simulations of prominence formation and evolution in an elongated magnetic flux rope as a result of in situ plasma condensations fueled by continuous plasma evaporation from the solar chromosphere. The prominence is born and maintained in a fragmented, highly dynamic state with continuous reappearance of multiple blobs and thread structures that move mainly downward, dragging along mass-loaded field lines. The circulation of prominence plasma is characterized by the dynamic balance between the drainage of prominence plasma back to the chromosphere and the formation of prominence plasma via continuous condensation. Plasma evaporates from the chromosphere, condenses into the prominence in the corona, and drains back to the chromosphere, establishing a stable chromosphere–corona plasma cycle. Synthetic images of the modeled prominence with the Solar Dynamics Observatory Atmospheric Imaging Assembly closely resemble actual observations, with many dynamical threads underlying an elliptical coronal cavity.
Validity of the Effective Fisher matrix for parameter estimation analysis: Comparing to the analytic Fisher matrix

The effective Fisher matrix method recently introduced by Cho et al. is a semi-analytic approach to the Fisher matrix, in which a local overlap surface is fitted by using a quadratic fitting function. Mathematically, the effective Fisher matrix should be consistent with the analytic one at the infinitesimal fitting scale. In this work, using the frequency-domain waveform (TaylorF2), we give brief comparison results between the effective and analytic Fisher matrices for several non-spinning binaries consisting of binary neutron stars with masses of (1.4, 1.4)M_sun, black hole-neutron star of (1.4, 10)M_sun, and binary black holes of (5, 5) and (10, 10)M_sun for a fixed signal to noise ratio (SNR=20) and show a good consistency between two methods. We also give a comparison result for an aligned-spin black hole-neutron star binary with a black hole spin of \chi=1, where we define new mass parameters (Mc, \eta^-1, \chi^7/2) to find good fitting functions to the overlap surface. The effective Fisher matrix can also be computed by using the time-domain waveforms which are generally more accurate than frequency-domain waveform. We show comparison results between the frequency-domain and time-domain waveforms (TaylorT4) for both the non-spinning aligned-spin binaries.
Self-Reported Sensory Decline in Older Adults Is Longitudinally Associated With Both Modality-General and Modality-Specific Factors

Abstract Background and Objectives Self-reported sensory data provide important insight into an individual’s perception of sensory ability. It remains unclear what factors predict longitudinal change in self-reported sensory ability across multiple modalities during healthy aging. This study examined these associations in a cohort of older adults for vision, hearing, taste, and smell. Research Design and Methods Data on self-report sensory ability were drawn from 5,065 participants of The Irish Longitudinal Study on Ageing (mean age at baseline = 61.6, SD = 9.5, range 32–93 years; 59% female; resident in the Republic of Ireland) across 6 waves of data collection (2009–2021). Covariates included demographics, lifestyle factors, and measures of sensory, physical, mental, and cognitive health. Independent discrete survival analyses were performed for each sensory modality. Results A transition to self-reported fair/poor hearing was most prevalent (21% of the sample), followed by fair/poor vision (19%), smell (11%), and taste (6%). Participants who self-reported fair/poor function in one sensory modality were likely to report fair/poor ability in another sensory modality, although not for all pairings. Only self-rated fair/poor health was associated with increased odds of self-reported fair/poor ability across all sensory modalities. Age was associated with increased odds of self-reported fair/poor hearing, smell, and taste, as was current smoker status (vision, smell, and taste). Several other sensory (e.g., eye disease, hearing aid use) and nonsensory covariates (e.g., education, depression) were associated with the odds of self-reported fair/poor ability in one or two sensory modalities only. Discussion and Implications Over time, older adults perceive associations in fair/poor ability for multiple sensory modalities, albeit somewhat inconsistently. Both modality-general and modality-specific factors are associated with a transition from normal to fair/poor sensory ability. These results suggest the need for more routine testing of multiple senses with increasing age.
Teacher –Students Relationship as a Tool for Positive Academic Performance in Nigeria

The paper examined the concept of teacher-students relationship as a tool for positive academic performance. It examined the essential components of student –teacher relationship such as the learners, teachers, cooperative learning, and reciprocal learning and so on. The paper also talks about the importance of teacher-students relationship which stated that good teachers’ students’ relationship creates many advantages between both the teachers and students. For instance, a good relationship produces a good environment within the classroom. It also highlights the causes of poor teachers’ students’ relationship, such as insensitivity to student needs, teachers’ bullying, troublesome behaviour and so on. Lastly, the paper proffers solution to poor teachers’ students’ relationship that, teachers should avoid the use of complete authority in handling students. Since the students are under the care of the teacher, the teacher is expected to show good example to them, his authority and discipline over the students should be personal rather than official and also parents’ show of concern for their children’s welfare is crucial.
MODELING INDICATIONS OF TECHNOLOGY IN PLANETARY TRANSIT LIGHT CURVES—DARK-SIDE ILLUMINATION

We analyze potential effects of an extraterrestrial civilization’s use of orbiting mirrors to illuminate the dark side of a synchronously rotating planet on planetary transit light curves. Previous efforts to detect civilizations based on side effects of planetary-scale engineering have focused on structures affecting the host star output (e.g., Dyson spheres). However, younger civilizations are likely to be less advanced in their engineering efforts, yet still capable of sending small spacecraft into orbit. Since M dwarfs are the most common type of star in the solar neighborhood, it seems plausible that many of the nearest habitable planets orbit dim, low-mass M stars, and will be in synchronous rotation. Logically, a civilization evolving on such a planet may be inspired to illuminate their planet’s dark side by placing a single large mirror at the L2 Lagrangian point, or launching a fleet of small thin mirrors into planetary orbit. We briefly examine the requirements and engineering challenges of such a collection of orbiting mirrors, then explore their impact on transit light curves. We incorporate stellar limb darkening and model a simplistic mirror fleet’s effects for transits of Earth-like (R = 0.5 to 2 R Earth ? > ) planets which would be synchronously rotating for orbits within the habitable zone of their host star. Although such an installation is undetectable in Kepler data, the James Webb Space Telescope will provide the sensitivity necessary to detect a fleet of mirrors orbiting Earth-like habitable planets around nearby stars.
Grocery loyalty cards: Do they work? A customer-centred investigation

Orientation: Research into the effectiveness of loyalty programmes is fragmented and paradoxical. Some authors showed that loyalty programmes are effective, while others demonstrated the contrary.Motivation for the study: This study draws on two previous studies and argues that theories compiled in developed economies are not applicable in emerging economies and that the success of loyalty programmes is a multidimensional topic.Research purpose: This study aimed to investigate the effectiveness of grocery loyalty programmes within an emerging economy and investigate various areas to get a customer-centric perspective on this marketing tool.Research design, approach and method: This study used a qualitative methodology with an abductive mindset and proposed several hunches that arose from the findings. Ten online interviews were conducted with customers of grocery loyalty programmes, and issues were probed such as the customers’ purchase frequency, their price sensitivity, their advocacy of loyalty programmes and the quality and length of their relationship. The interview were transcribed and the content was analysed inductively.Main findings: Findings suggest that the customers of grocery loyalty programmes are generally uncertain about the benefits of loyalty programmes and a sense of disengagement is observed.Managerial/practical implications: Several suggestions are made to improve the practicality of loyalty programmes. These suggestions focus on ways to get the customers more engaged.Contribution of study: This study contributes to the academic knowledge within an emerging economy and provides some practical managerial suggestions for effective implementation. This study proposes that the effectiveness of loyalty programmes is not a simple issue and requires input from several disciplines, such as psychology.