Miracle-dz/UniFAR-FTUs huggingface dataset:
X-RAY CONSTRAINTS ON THE LOCAL SUPERMASSIVE BLACK HOLE OCCUPATION FRACTION

Distinct seed formation mechanisms are imprinted upon the fraction of dwarf galaxies currently containing a central supermassive black hole. Seeding by Population III remnants is expected to produce a higher occupation fraction than is generated with direct gas collapse precursors. Chandra observations of nearby early-type galaxies can directly detect even low-level supermassive black hole activity, and the active fraction immediately provides a firm lower limit to the occupation fraction. Here, we use the volume-limited AMUSE surveys of ∼200 optically selected early-type galaxies to characterize simultaneously, for the first time, the occupation fraction and the scaling of LX with Mstar, accounting for intrinsic scatter, measurement uncertainties, and X-ray limits. For early-type galaxies with Mstar < 1010 M☉, we obtain a lower limit to the occupation fraction of >20% (at 95% confidence), but full occupation cannot be excluded. The preferred dependence of log LX upon log Mstar has a slope of ∼0.7–0.8, consistent with the “downsizing” trend previously identified from the AMUSE data set, and a uniform Eddington efficiency is disfavored at ∼2σ. We provide guidelines for the future precision with which these parameters may be refined with larger or more sensitive samples.
Teacher Appraisers' Perceptions of Teacher Appraisal

This study investigates teacher appraisers' perceptions of teacher appraisal in terms of its purpose, methods, and criteria. Fourteen teacher-appraisers were administered semi-structured interviews to gain an in-depth understanding of their perceptions of appraisal. Analysis of the responses revealed that participants seemed to advocate the use of teacher appraisal for both professional improvement and decision-making purposes. Participants also seemed to agree about the value of classroom observation as an objective method of evaluation. Still, they were divided regarding the use of student evaluation, student achievement, and other indi-rect observation methods, especially for decision-making purposes. As for evaluation criteria, the results revealed that while teacher-appraisers paid attention to all aspects of the teaching process in their evaluation, their focus remained mainly on those skills exhibited during the actual delivery of teaching.
MgB 2 Thin Films Fabricated by Pulsed Laser Deposition Using Nd:YAG Laser in an In Situ Two-Step Process

: Magnesium diboride (MgB 2 ) thin ﬁlms on r -cut sapphire ( r -Al 2 O 3 ) single crystals were fabricated by a precursor, which was obtained at room temperature via a pulsed laser deposition (PLD) method using a Nd:YAG laser, and an in situ postannealing process. The onset superconducting transition, T conset , and zero-resistivity transition, T czero , were observed at 33.6 and 31.7 K, respectively, in the MgB 2 thin ﬁlms prepared by a Mg-rich target with a ratio of Mg:B = 3:2. The critical current density, J c , calculated from magnetization measurements reached up to 0.9 × 10 6 A cm − 2 at 20 K and 0 T. The broad angular J c peak was found at 28 K when the magnetic ﬁelds were applied in a direction parallel to the ﬁlm surface ( θ = 90 ◦ ). This could be indicative of the granular structure with randomly oriented grains. Our results demonstrate that this process is a promising candidate for the fabrication of MgB 2 superconducting devices. peak around an H ⊥ ﬁlm surface. The other would be caused by the ﬁlm surface, the MgB 2 /substrate interface, or the layer structure of the crystals, leading to the strong peak around an H // ﬁlm surface. The MgB 2 ﬁlm on c -cut sapphire ( c -Al 2 O 3 ) single crystals fabricated by an ex situ PLD process has a broad and small peak at an H // ﬁlm surface [34]. This could be because of the granular structure with randomly oriented grains in the ﬁlms. MgB 2 ﬁlm #2 on r -Al 2 O 3 single crystals in this study has also a broad peak at an H // ﬁlm surface. These results indicate that the broad peak would arise from the granular grain structure. In addition, we found that the difference of the crystallographic orientation on an Al 2 O 3 substrate would contribute little to the peak position in J c ( θ ) curves for MgB 2 ﬁlms in this measurement.
Hartree-Fock computation of the high- T c cuprate phase diagram

A computation of the cuprate phase diagram is presented. Adiabatic deformability back to the density function band structure is assumed. Symmetry constraints lead to a fermi liquid theory with 5 interaction parameters. Two of these are forced to zero by experiment. The remaining 3 are fit to (1) the moment of the antiferromagnetic state at half filling, (2) the superconducting gap at optimal doping, and (3) the maximum pseudogap, which I identify as d-density wave. Solution of the Hartree-Fock equations gives, in quantitative agreement with experiment, (1) quantum phase transitions at 5% and 16% p-type doping, (2) insulation below 5%, (3) a d-wave pseudogap quasiparticle spectrum, (4) pseudogap and superconducting gap values as a function of doping, (5) superconducting Tc versus doping, (6) London penetration depth versus doping, (7) spin wave velocity. The fit points to superexchange mediated by the bonding O atom in the Cu-O plane as the causative agent of all three ordering phenomena.
The Role of N1-Src regulated splicing in neuronal differentiation

2 List of contents 3 List of figures 4 List of tables 4 Acknowledgements 5 Author’s declaration 5 Chapter 1: Introduction 6 1.1: Alternative splicing 6 1.2: Splicing and neural development 7 1.3: The Src family of non-receptor kinases 9 1.4: Cellular Functions of C-Src 10 1.5: C-Src Functions in the Brain 11 1.6: Neuronal Srcs 12 1.7: N1-Src and neuroblastoma 13 1.8: A role for N1-Src in Xenopus primary neurogenesis 14 1.9: Src and splicing during neurogenesis 15 Chapter 2: Methods 17 2.1: RNA-seq datasets and genome assemblies 17 2.2: Data preprocessing 18 2.3: Differential splicing analysis 18 2.4: Motif enrichment analysis 19 2.5: Functional enrichment analysis 20 2.6: Event clustering 21 2.7: Differential gene expression analysis 21 2.8: Summary of software and algorithms used in this study 21 Chapter 3: Results 23 3.1 Developing a data analysis pipeline to process RNA-Seq datasets for alternative splicing 24 3.1.1. Differential splicing analysis 24 3.1.2. Motif enrichment analysis 26 3.2: v-Src expression regulates a programme of alternative splicing in a human MCF10ER-Src cell line 27 3.4: Splicing is an important feature of Xenopus early development. 34 3.3: Xenopus neural plate and crest development are regulated by alternative splicing 38 3.4: N1-Src knockdown and v-Src expression cause changes in splicing of splicing factors TRA2A and HNRNPA1 43 Chapter 4: Discussion 45 4.1: Src regulates the splicing of splicing factors 45 4.2 : Regulation of splicing as a therapeutic strategy 47 Definitions and abbreviations 49 References 50
C + emission from the Magellanic Clouds. II. [C II] maps of star-forming regions LMC-N 11, SMC-N 66, and several others

Context. We study the λ 158 μm [CII] fine-structure line emission from star-forming regions as a function of metallicity. Aims. We have measured and mapped the [CII] emission from the very bright HII region complexes N 11 in the LMC and N 66 in the SMC; as well as the SMC HII regions N 25, N 27, N 83/N 84, and N 88 with the FIFI instrument on the Kuiper Airborne Observatory. Methods. In both LMC and SMC, the ratio of [CII] line to CO line and to the far-infrared continuum emission is much higher than seen almost anywhere else, including Milky Way star-forming regions, and whole galaxies. Results. In the low metallicity, low dust-abundance environment of the LMC and the SMC UV mean free path lengths are much greater than those in the higher-metallicity Milky Way. The increased photoelectric heating efficiencies cause significantly greater relative [CII] line emission strengths. At the same time, similar decreases in PAH abundances have the opposite effect by diminishing photoelectric heating rates. Consequently, in low-metallicity environments relative [CII] strengths are high but exhibit little further dependence on actual metallicity. Relative [CII] strengths are slightly higher in the LMC than in the SMC which has both lower dust and lower PAH abundances.
Gaussian Projection Deep Extreme Clustering and Chebyshev Reflective Correlation based Outlier Detection

Outlier detection or simply the task of point detection that are noticeably distinct and different from data sample is a predominant issue in deep learning. When a framework is constructed, these distinctive points can later lead to model training and compromise accurate predictions. Owing to this reason, it is paramount to recognize and eliminate them before constructing any supervised model and this is frequently the initial step when dealing with a deep learning issue. Over the recent few years, different numbers of outlier detector algorithms have been designed that ensure satisfactory results. However, their main disadvantages remain in the time and space complexity and unsupervised nature. In this work, a clusteringbased outlier detection called, Random Projection Deep Extreme Learning-based Chebyshev Reflective Correlation (RPDELCRC) is proposed. First, Gaussian Random Projection-based Deep Extreme Learning-based Clustering model is designed. Here, by applying Gaussian Random Projection function to the Deep Extreme Learning obtains the relevant and robust clusters corresponding to the data points in a significant manner. Next, with the robust clusters, outlier detection time is said to be reduced to a greater extent. In addition, a novel Chebyshev Temporal and Reflective Correlation-based Outlier Detection model is proposed to detect outliers therefore achieving high outlier detection accuracy. The proposed approach is validated with the NIFTY-50 stock market dataset. The performance of the RPDEL-CRC method is evaluated by applying it to NIFTY-50 Stock Market dataset. Finally, we compare the results of the RPDEL-CRC method to the state-of-the-art outlier detection methods using outlier detection time, accuracy, error rate and false positive rate evaluation metrics. Keywords—Outlier detection; clustering; Gaussian random projection; deep extreme learning; Chebyshev distance; temporal; reflective correlation
PP-Peripherality and Ambiguity in the Noun Phrase

4 Predictions arising from structural analyses 27 ∗I would like to thank my supervisor, Professor Ad Neeleman, for his help and support over the past year, and for encouraging me to stick with it. I would also like to thank my classmates, for their lively discussions and vigourous debates, especially Javi Fernandez and Georg Hoehn for their help connecting me with informants. My thanks also to all of my informants, for politely answering my at times ridiculous questions, and particularly to Professor Junko Shimoyama at McGill. Thanks to Allegra Fryxell for her help with proof-reading. Finally, I would like to thank Alan Belk and Isobel Heathcote for trying their best to understand my decision to study linguistics, as well as the linguistics itself. Any errors that remain are entirely the fault of the author.
Can Large Language Models Distinguish Cause from Effect?

Identifying the causal direction between two variables has long been an important but challenging task for causal inference. Existing work proposes to distinguish whether X → Y or Y → X by setting up an input-output learning task using the two variables, since causal and anticausal learning have different performances under semi-supervised learning and domain shift. This approach works for many task-specific models trained on the input-output pairs. However, with the rise of general-purpose large language models (LLMs), there are various challenges posed to this previous task-specific learning approach, since continued training of LLMs is less likely to be affordable for university labs, and LLMs are no longer trained on specific input-output pairs. In this work, we propose a new paradigm to distinguish cause from effect using LLMs. Specifically, we conduct post-hoc analysis using natural language prompts that describe different possible causal stories behind the X , Y pairs, and test their zero-shot performance. Through the experiments, we show that the natural language prompts that describe the same causal story as the ground-truth data generating direction achieve the highest zero-shot performance, with 2% margin over anticausal prompts. We highlight that it will be an interesting direction to identify more causal relations using LLMs. a
ON THE INTERPLAY BETWEEN STAR FORMATION AND FEEDBACK IN GALAXY FORMATION SIMULATIONS

We investigate the star formation–feedback cycle in cosmological galaxy formation simulations, focusing on the progenitors of Milky Way (MW)-sized galaxies. We find that in order to reproduce key properties of the MW progenitors, such as semi-empirically derived star formation histories (SFHs) and the shape of rotation curves, our implementation of star formation and stellar feedback requires (1) a combination of local early momentum feedback via radiation pressure and stellar winds, and subsequent efficient supernovae feedback, and (2) an efficacy of feedback that results in the self-regulation of the global star formation rate on kiloparsec scales. We show that such feedback-driven self-regulation is achieved globally for a local star formation efficiency per free fall time of ϵ ff ≈ 10 % ? > . Although this value is larger that the ϵ ff ∼ 1 % ? > value usually inferred from the Kennicutt–Schmidt (KS) relation, we show that it is consistent with direct observational estimates of ϵ ff ? > in molecular clouds. Moreover, we show that simulations with local efficiency of ϵ ff ≈ 10 % ? > reproduce the global observed KS relation. Such simulations also reproduce the cosmic SFH of the MW-sized galaxies and satisfy a number of other observational constraints. Conversely, we find that simulations that a priori assume an inefficient mode of star formation, instead of achieving it via stellar feedback regulation, fail to produce sufficiently vigorous outflows and do not reproduce observations. This illustrates the importance of understanding the complex interplay between star formation and feedback, and the detailed processes that contribute to the feedback-regulated formation of galaxies.
Linking Corporate Social Responsibility, Consumer Identification and Purchasing Intention

Apart from the broad oversight of a company’s supply chain practices, more businesses are recognizing the importance of corporate social responsibility (CSR) and its influence on societal well-being. In addition to their financial success, ratings are being developed to analyze how well most corporations perform regarding their CSR operations. This grade can then be used to determine the market success of each firm. This study’s objective was to examine the mechanisms of how customers intend to pay premium prices for companies’ CSR activities, i.e., how CSR affects consumer–company identification and purchasing intention. We employed a questionnaire-based study to evaluate our research model generated from the literature. Using PLS-SEM, a quantitative analysis based on responses from major businesses in Pakistan was conducted. The results indicate that CSR is significantly correlated with brand image, consumer–company identification and identity attractiveness, and further leads to higher consumer satisfaction and purchasing intention. This paper contributes to the literature by confirming that consumers in Pakistan intend to buy CSR-conscious products and are willing to sponsor companies’ CSR activities. It implies that investing in CSR may improve a company’s financial performance and competitive advantage. On the other hand, the stability of this association calls for additional testing and empirical investigation.
The Recent Development in Technologies for Attaining Doubled Haploid Plants In Vivo

Haploid plants with a doubled set of chromosomes (doubled haploid (DH)) significantly speed up the selection process by the fixation of genetic traits in each locus in the homozygous state within one generation. Doubled haploids are mainly attained by the formation of plants from the cultured gametophytic (haploid) tissues and cells in vitro, or by targeted reduction in the parent chromosome during intra- or interspecific hybridization. Since then, DH has become one of the most powerful tools to support various basic research studies, as well as applied research. This review is focused on the recent development of the production of doubled haploids in vivo and their fundamental bases. The various mechanisms and approaches responsible for the formation of haploids in vivo are discussed, particularly the induction of parthenogenesis by BBM-like proteins, the long constructed Salmon system of wheat, the usage of patatin-like phospholipases MTL/PLA1/NLD, the IG1 system, uniparental genome elimination during interspecific hybridization, and the perspective technology of centromeric histone 3 (CENH3) modification.
CHANDRA CHARACTERIZATION OF X-RAY EMISSION IN THE YOUNG F-STAR BINARY SYSTEM HD 113766

Using Chandra, we have obtained imaging X-ray spectroscopy of the 10–16 Myr old F-star binary HD 113766. We individually resolve the 1. ″4 separation binary components for the first time in the X-ray and find a total 0.3–2.0 keV luminosity of 2.2 × 1029 erg s−1, consistent with previous RASS estimates. We find emission from the easternmost, infrared-bright, dusty member HD 113766A to be only ∼10% that of the western, infrared-faint member HD 113766B. There is no evidence for a 3rd late-type stellar or substellar member of HD 113766 with Lx > 6 × 1025 erg s−1 within 2′ of the binary pair. The ratio of the two stars’ X-ray luminosity is consistent with their assignments as F2V and F6V by Pecaut et al. The emission is soft for both stars, kTApec = 0.30–0.50 keV, suggesting X-rays produced by stellar rotation and/or convection in young dynamos, but not accretion or outflow shocks, which we rule out. A possible 2.8 ± 0.15 (2σ) hr modulation in the HD 113766B X-ray emission is seen, but at very low confidence and of unknown provenance. Stellar wind drag models corresponding to Lx ∼ 2 × 1029 erg s−1 argue for a 1 mm dust particle lifetime around HD 113766B of only ∼90,0000 years, suggesting that dust around HD 113766B is quickly removed, whereas 1 mm sized dust around HD 113766A can survive for >1.5 × 106 years. At 1028–1029 erg s−1 X-ray luminosity, astrobiologically important effects, like dust warming and X-ray photolytic organic synthesis, are likely for any circumstellar material in the HD 113766 systems.
Continuum brightness of solar magnetic elements

Ratios between the Stokes V profiles of C I lines and Fe II lines are used to determine the temperature of the continuum-forming layers of solar magnetic features. From the derived temperature stratification the continuum intensity of the spatially unresolved magnetic features is obtained independently of spatial-resolution. First results suggest that whereas magnetic features have, on average, a brighter continuum than the quiet sun in a region of small magnetic filling, they are darker in a region with large filling factor. Consequences for flux-tube sizes and the interpretation of the global solar luminosity variation are discussed
GRAVITATIONAL INSTABILITIES IN TWO-COMPONENT GALAXY DISKS WITH GAS DISSIPATION

Growth rates for gravitational instabilities in a thick disk of gas and stars are determined for a turbulent gas that dissipates on the local crossing time. The scale heights are derived from vertical equilibrium. The accuracy of the usual thickness correction, (1 + kH)−1, is better than 6% in the growth rate when compared to exact integrations for the gravitational acceleration in the disk. Gas dissipation extends the instability to small scales, removing the minimum Jeans length. This makes infinitesimally thin disks unstable for all Toomre-Q values and reasonably thick disks stable at high Q primarily because of thickness effects. The conventional gas+star threshold, Qtot, increases from ∼1 without dissipation to 2 or 3 when dissipation has a rate equal to the crossing rate over a perturbation scale. Observations of Qtot ∼ 2–3 and the presence of supersonic turbulence suggest that disks are unstable over a wide range of scales. Such instabilities drive spiral structure if there is shear and clumpy structure if shear is weak; they may dominate the generation of turbulence. Feedback regulation of Qtot is complex because the stellar component does not cool; the range of spiral strengths from multiple arm to flocculent galaxies suggests that feedback is weak. Gravitational instabilities may have a connection to star formation even when the star formation rate scales directly with the molecular mass because the instabilities return dispersed gas to molecular clouds and complete the cycle of cloud formation and destruction. The mass flow to dense clouds by instabilities can be 10 times larger than the star formation rate.
Observation of the new emission line at ~3.5 keV in X-ray spectra of galaxies and galaxy clusters

The detection of an unidentified emission line in X-ray spectra of cosmic objects would be a 'smoking gun' signature for particle physics beyond the Standard Model. More than a decade of its extensive searches results in several narrow faint emission lines reported at 3.5, 8.7, 9.4 and 10.1 keV. The most promising of them is the emission line at ~3.5 keV reported in spectra of several nearby galaxies and galaxy clusters. Here I summarize its up-to-date status, overview its possible interpretations, including an intriguing connection with radiatively decaying dark matter, and outline future directions for its studies.
Nonperturbative aspects of Yang-Mills theory

In this thesis, several aspects of Yang-Mills theory are studied. It begins with the constrained quantization in the Coulomb gauge, using the Dirac bracket formalism. A nonperturbative analysis of the infrared asymptotics of propagators in any spatial dimension follows, and a connection to the Landau gauge is given. In the Coulomb gauge Hamiltonian approach, a linearly rising static color Coulomb potential is found, along with an infrared diverging gluon energy, both signaling confinement. The propagators and vertices in the entire momentum regime are calculated with the variational principle. In the ultraviolet, a nonperturbative running coupling constant is studied, and certain asymptotic forms of the propagators are postulated. Furthermore, the back reaction of the gauge sector to the inclusion of external charges is investigated.