Miracle-dz/UniFAR-FTUs huggingface dataset:
Quantifying the global ”CMB tension” between the Atacama Cosmology Telescope and the Planck satellite in extended models of cosmology

We study the global agreement between the most recent observations of the Cosmic Microwave Background temperature and polarization anisotropies angular power spectra released by the Atacama Cosmology Telescope and the Planck satellite in various cosmological models that differ by the inclusion of different combinations of additional parameters. By using the Suspiciousness statistic, we show that the global ”CMB tension” between the two experiments, quantified at the Gaussian equivalent level of ∼2.5 σ within the baseline ΛCDM, is reduced at the level of 1. 8σ when the effective number of relativistic particles (Neff) is significantly less than the standard value, while it ranges between 2.3 σ and 3.5 σ in all the other extended models.
Erratum: Population synthesis on high-mass X-ray binaries: prospects and constraints from the universal X-ray luminosity function

Using an updated population synthesis code initially developed by Hurley et al. we modeled the synthetic X-ray binary (XRB) populations for direct comparison with the universal, featureless X-ray luminosity function (XLF) of high mass X-ray binaries (HMXBs) in star-forming galaxies. Our main goal is to use the universal XLF to constrain the model parameters, given the current knowledge of binary evolution. We find that the one-dimensional (1D) Maxwellian velocity dispersion of the natal kick can be constrained to be of the order of ~150km/s, supporting earlier findings that neutron stars (NSs) formed in binaries seem to receive significantly smaller natal kicks than the velocities of Galactic single pulsars would indicate. The super-Eddington accretion factor is further confirmed in the framework of stellar mass black holes (BHs), revealing the true origin of the most of the ultraluminous X-ray sources (ULXs) may indeed be the high-luminosity extension of ordinary HMXBs which harbor stellar-mass BHs rather than exotic intermediate-mass BHs or ones. We present the detail properties of the model-predicted present-day HMXBs, which may be investigated by future high-resolution X-ray and optical observations of sources in nearby star-forming galaxies.
On the Implicit Bias Towards Minimal Depth of Deep Neural Networks

Recent results in the literature suggest that the penultimate (second-to-last) layer representations of neural networks that are trained for classification exhibit a clustering property called neural collapse (NC). We study the implicit bias of stochastic gradient descent (SGD) in favor of low-depth solutions when training deep neural networks. We characterize a notion of effective depth that measures the first layer for which sample embeddings are separable using the nearest-class center classifier. Furthermore, we hypothesize and empirically show that SGD implicitly selects neural networks of small effective depths. Secondly, while neural collapse emerges even when generalization should be impossible - we argue that the \emph{degree of separability} in the intermediate layers is related to generalization. We derive a generalization bound based on comparing the effective depth of the network with the minimal depth required to fit the same dataset with partially corrupted labels. Remarkably, this bound provides non-trivial estimations of the test performance. Finally, we empirically show that the effective depth of a trained neural network monotonically increases when increasing the number of random labels in data.
Sparse source travel-time tomography of a laboratory target: accuracy and robustness of anomaly detection

This study concerned conebeam travel-time tomography. The focus was on a sparse distribution of signal sources that can be necessary in a challenging in situ environment such as in asteroid tomography. The goal was to approximate the minimum number of source positions needed for robust detection of refractive anomalies, e.g., voids within an asteroid or a casting defects in concrete. Experimental ultrasonic data were recorded utilizing as a target a 150 mm plastic cast cube containing three stones with diameter between 22 and 41 mm. A signal frequency of 55 kHz (35 mm wavelength) was used. Source counts from one to six were tested for different placements. Based on our statistical inversion approach and analysis of the results, three or four sources were found to lead to reliable inversion. The source configurations investigated were also ranked according to their performance. Our results can be used, for example, in the planning of planetary missions as well as in material testing.
Hierarchy of fillings for FQHE in monolayer and in bilayer graphene: Explanation of $\nu=-\frac{1}{2}$ fractional quantum Hall state in bilayer graphene

The commensurability condition is applied to determine the hierarchy of fractional fillings of Landau levels in monolayer and bilayer graphene. The filling rates for FQHE in graphene are found and illustrated in the first three Landau levels. The good agreement with the experimental data is achieved. The presence of even denominator filling fractions in the hierarchy for FQHE in bilayer graphene is explained.
Gravitational and mass distribution effects on stationary superwinds II. Extended dark matter haloes

In this second part, we generalize the results of the previous paper. We present an analytic superwind solution considering extended gravitationally-interacting dark-matter and baryonic haloes. The incorporation of the latter is critical, since they can have a substantial effect on the hydrodynamics of superwinds generated by massive galaxies. Although the presence of extended and massive haloes does not change the limit for the closed-box enrichment of galaxies established in the first paper, they can trigger an earlier activation of the open-box enrichment scenario, since their gravitational potentials can contribute to the inhibition of the free superwind. Moreover, the incorporation of the extended haloes will also enhance the physical setting behind the superwind model, as we consider mass distributions with properties that emulate the results of recent simulations of $\Lambda$CDM haloes.
Sulfur and zinc abundances of red giant stars

Sulfur and zinc are chemically volatile elements, which play significant roles as depletion-free tracers in studying galactic chemical evolution. However, regarding red giants having evolved off the main sequence, reliable abundance determinations of S and Zn seem to be difficult despite that a few studies have been reported so far. Given this situation, we tried to establish the abundances of these elements for an extensive sample of 239 field GK giants (-0.8 < [Fe/H] < +0.2), by applying the spectrum-fitting technique to S I 8694-5, S I 6757, and Zn I 6362 lines and by taking into account the non-LTE effect. Besides, similar abundance analysis was done for 160 FGK dwarfs to be used for comparison. The non-LTE corrections for the S and Zn abundances derived from these lines turned out < 0.1(-0.2) dex for most cases and not very significant. It revealed that the S I 6757 feature is more reliable as an abundance indicator than S I 8694-5 for the case of red giants, because the latter suffers blending of unidentified lines. The finally resulting [S/Fe]-[Fe/H] and [Zn/Fe]-[Fe/H] relations for GK giants were confirmed to be in good agreement with those for FGK dwarfs, indicating that S and Zn abundances of red giants are reliably determinable from the S I 6757 and Zn I 6362 lines. Accordingly, not only main-sequence stars but also evolved red giant stars are usable for tracing the chemical evolution history of S and Zn in the regime of disk metallicity by using these lines.
A system of financial indicators for assessing the risk of material misstatement of accounting information in the context of a continuous online audit

In the time of digitalization of the economy, the audit of financial reporting is bound to shift from periodic inspections (annual, semi-annual, quarterly) to continuous monitoring of financial information. Continuous monitoring ensures that the control results of activities are produced simultaneously or within the shortest period possible after discovering the relevant events. The risk of possible misstatement of financial statements in the process of this monitoring is assessed using analytical procedures. The source data for them are the values of financial indicators of the audited entity selected by the auditor. Analytical procedures are aimed at obtaining audit evidence and carried out through a number of actions taken to find out, study, analyze and assess the correlations between the financial-economic and other performance indicators of the organization in order to discover non-standard phenomena as well as facts and the causes of these discrepancies. The main purpose of the article was to develop a system of financial indicators, the continuous monitoring of which would allow for assessing the risk of material misstatement in real time. The methodological basis of the research is determined by the following fundamental techniques and principles: analysis, synthesis, attributive and proportional analogies, abstractions, descriptive generalizations, formulation and confirmation of working analytical hypotheses, economic/mathematical and mathematical/statistical methods. The paper analyzes the financial indicators, suggested for these purposes by a number of authors, and highlights the lack of substantiation of the former. The relationships between possible financial indicators and the items of financial statements are studied and a set of indicators has been formed. Their growth rate, if monitored in the online auditing process, makes it possible to assess the risk of material misstatement of accounting information and react accordingly.
The infrared-dark dust content of high redshift galaxies

We present a theoretical model aimed at explaining the IRX-$\beta$ relation for high redshift (z >5) galaxies. Recent observations (Capak+2015; Bouwens+2016) have shown that early Lyman Break Galaxies, although characterized by a large UV attenuation (e.g. flat UV beta slopes), show a striking FIR deficit, i.e. they are "infrared-dark". This marked deviation from the local IRX-beta relation can be explained by the larger molecular gas content of these systems. While dust in the diffuse ISM attains relatively high temperatures (Td = 45 K for typical size a=0.1 um; smaller grains can reach Td = 60 K), a sizable fraction of the dust mass is embedded in dense gas, and therefore remains cold. If confirmed, the FIR deficit might represent a novel, powerful indicator of the molecular content of high-z galaxies which can be used to pre-select candidates for follow-up deep CO observations. Thus, high-z CO line searches with ALMA might be much more promising than currently thought.
WIMPless Dark Matter from an AMSB Hidden Sector with No New Mass Parameters

We present a model with dark matter in an anomaly-mediated supersymmetry breaking hidden sector with a U(1)×U(1) gauge symmetry. The symmetries of the model stabilize the dark matter and forbid the introduction of new mass parameters. As a result, the thermal relic density is completely determined by the gravitino mass and dimensionless couplings. Assuming non-hierarchical couplings, the thermal relic density is ΩX ∼ 0.1, independent of the dark matter’s mass and interaction strength, realizing the WIMPless miracle. The model has several striking features. For particle physics, stability of the dark matter is completely consistent with R-parity violation in the visible sector, with implications for superpartner collider signatures; also the thermal relic’s mass may be ∼ 10 GeV or lighter, which is of interest given recent direct detection results. Interesting astrophysical signatures are dark matter self-interactions through a long-range force, and massless hidden photons and fermions that contribute to the number of relativistic degrees of freedom at BBN and CMB. The latter are particularly interesting, given current indications for extra degrees of freedom and near future results from the Planck observatory. PACS numbers: 95.35. +d, 12.60. Jv 1 ar X iv :1 11 1. 44 79 v1 [ he pph ] 1 8 N ov 2 01 1
A Personalised Approach to Audiovisual Humour Recognition and its Individual-level Fairness

Humour is one of the most subtle and contextualised behavioural patterns to study in social psychology and has a major impact on human emotions, social cognition, behaviour, and relations. Consequently, an automatic understanding of humour is crucial and challenging for a naturalistic human-robot interaction. Recent artificial intelligence (AI)-based methods have shown progress in multimodal humour recognition. However, such methods lack a mechanism in adapting to each individual's characteristics, resulting in a decreased performance, e.g., due to different facial expressions. Further, these models are faced with generalisation problems when being applied for recognition of different styles of humour. We aim to address these challenges by introducing a novel multimodal humour recognition approach in which the models are personalised for each individual in the Passau Spontaneous Football Coach Humour (Passau-SFCH) dataset. We begin by training a model on all individuals in the dataset. Subsequently, we fine-tune all layers of this model with the data from each individual. Finally, we use these models for the prediction task. Using the proposed personalised models, it is possible to significantly (two-tailed t-test, p < 0.05) outperform the non-personalised models. In particular, the mean Area Under the Curve (AUC) is increased from . 7573 to . 7731 for the audio modality, and from . 9203 to . 9256 for the video modality. In addition, we apply a weighted late fusion approach which increases the overall performance to an AUC of . 9308, demonstrating the complementarity of the features. Finally, we evaluate the individual-level fairness of our approach and show which group of subjects benefits most of using personalisation.
Merger-driven evolution of the effective stellar initial mass function of massive early-type galaxies

The stellar initial mass function (IMF) of early-type galaxies is the combination of the IMF of the stellar population formed in-situ and that of accreted stellar populations. Using as an observable the effective IMF $\alpha_{IMF}$, defined as the ratio between the true stellar mass of a galaxy and the stellar mass inferred assuming a Salpeter IMF, we present a theoretical model for its evolution as a result of dry mergers. We use a simple dry merger evolution model, based on cosmological $N$-body simulations, together with empirically motivated prescriptions for the IMF to make predictions for how the effective IMF of massive early-type galaxies changes from $z=2$ to $z=0$. We find that the IMF normalization of individual galaxies becomes lighter with time. At fixed velocity dispersion, $\alpha_{IMF}$ is predicted to be constant with redshift. Current constraints on the evolution of the IMF are in slight tension with this prediction, even though systematic uncertainties prevent a conclusive statement. The correlation of $\alpha_{IMF}$ with stellar mass becomes shallower with time, while the correlation between $\alpha_{IMF}$ and velocity dispersion is mostly preserved by dry mergers. We also find that dry mergers can mix the dependence of the IMF on stellar mass and velocity dispersion, making it challenging to infer, from $z=0$ observations of global galactic properties, what is the quantity that is originally coupled with the IMF.
Abundances in a sample of turnoff and subgiant stars in NGC 6121 (M 4)

Context. The stellar abundances observed in globular clusters show complex structures, currently not yet understood. Aims. The aim of this work is to investigate the relations between the abundances of different elements in the globular cluster M 4, selected for its uniform deficiency of iron, to explore the best models explaining the pattern of these observed abundances. Moreover, in turnoff stars, the abundances of the elements are not suspected to be affected by internal mixing. Methods. In M 4, using low and moderate resolution spectra obtained for 91 turnoff (and subgiant) stars with the ESO FLAMES-Giraffe spectrograph, we have extended previous measurements of abundances (of Li, C and Na) to other elements (C, Si, Ca, Sr and Ba), using model atmosphere analysis. We have also studied the influence of the choice of the microturbulent velocity. Results. Firstly, the peculiar turnoff star found to be very Li-rich in a previous paper does not show any other abundance anomalies relative to the other turnoff stars in M 4. Secondly, an anti-correlation between C and Na has been detected, the slope being significative at more than 3 σ . This relation between C and Na is in perfect agreement with the relation found in giant stars selected below the RGB bump. Thirdly, the strong enrichment of Si and of the neutron-capture elements Sr and Ba, already observed in the giants in M 4, is confirmed. Finally, the relations between Li, C, Na, Sr and Ba constrain the enrichment processes of the observed stars. Conclusions. The abundances of the elements in the turnoff stars appear to be compatible with production processes by massive AGBs, but are also compatible with the production of second generation elements (like Na) and low Li produced by, for example, fast rotating massive stars.
Magnetically elevated accretion disks in active galactic nuclei: broad emission line regions and associated star formation

We propose that the accretion discs fueling active galactic nuclei (AGN) are supported vertically against gravity by a strong toroidal (ϕ-direction) magnetic field that develops naturally as the result of an accretion disc dynamo. The magnetic pressure elevates most of the gas carrying the accretion flow at R to large heights z ≳ 0.1R and low densities, while leaving a thin dense layer containing most of the mass – but contributing very little accretion – around the equator. We show that such a disc model leads naturally to the formation of a broad emission-line region through thermal instability. Extrapolating to larger radii, we demonstrate that local gravitational instability and associated star formation are strongly suppressed compared to standard disc models for AGN, although star formation in the equatorial zone is predicted for sufficiently high mass supply rates. This new class of accretion disc models thus appears capable of resolving two longstanding puzzles in the theory of AGN fueling: the formation of broad emission-line regions and the suppression of fragmentation thought to inhibit accretion at the required rates. We show that the disc of stars that formed in the Galactic Center a few million years ago could have resulted from an episode of magnetically elevated accretion at ≳ 0.1 of the Eddington limit.
THE SPATIAL CLUSTERING OF ROSAT ALL-SKY SURVEY AGNs. I. THE CROSS-CORRELATION FUNCTION WITH SDSS LUMINOUS RED GALAXIES

We investigate the clustering properties of ∼1550 broad-line active galactic nuclei (AGNs) at 〈z〉 = 0.25 detected in the ROSAT All-Sky Survey (RASS) through their measured cross-correlation function with ∼46,000 luminous red galaxies (LRGs) in the Sloan Digital Sky Survey. By measuring the cross-correlation of our AGN sample with a larger tracer set of LRGs, we both minimize shot noise errors due to the relatively small AGN sample size and avoid systematic errors due to the spatially varying Galactic absorption that would affect direct measurements of the auto-correlation function (ACF) of the AGN sample. The measured ACF correlation length for the total RASS-AGN sample (〈L0.1–2.4 keVX〉 = 1.5 × 1044 erg s−1) is r0 = 4.3+0.4−0.5 h−1 Mpc and the slope γ = 1.7+0.1−0.1. Splitting the sample into low and high LX samples at L0.5–10 keVX = 1044 erg s−1, we detect an X-ray luminosity dependence of the clustering amplitude at the ∼2. 5σ level. The low LX sample has r0 = 3.3+0.6−0.8 h−1 Mpc (γ = 1.7+0.4−0.3), which is similar to the correlation length of blue star-forming galaxies at low redshift. The high LX sample has r0 = 5.4+0.7−1.0 h−1 Mpc (γ = 1.9+0.2−0.2), which is consistent with the clustering of red galaxies. From the observed clustering amplitude, we infer that the typical dark matter halo (DMH) mass harboring RASS-AGN with broad optical emission lines is log (MDMH/(h−1 M☉)) = 12.6+0.2−0.3, 11.8+0.6−∞, 13.1+0.2−0.4 for the total, low LX, and high LX RASS-AGN samples, respectively.
RADIALLY EXTENDED, STRATIFIED, LOCAL MODELS OF ISOTHERMAL DISKS

We consider local, stratified, numerical models of isothermal accretion disks. The novel feature of our treatment is that radial extent Lx and azimuthal extent Ly satisfy H ≪ Lx, Ly ≪ R, where H is the scale height and R is the local radius. This enables us to probe mesoscale structure in stratified thin disks. We evolve the model at several resolutions, sizes, and initial magnetic field strengths. Consistent with earlier work, we find that the saturated, turbulent state consists of a weakly magnetized disk midplane coupled to a strongly magnetized corona, with a transition at |z| ∼ 2H. The saturated α ≃ 0.01–0.02. A two-point correlation function analysis reveals that the central 4H of the disk is dominated by small-scale turbulence that is statistically similar to unstratified disk models, while the coronal magnetic fields are correlated on scales ∼10H. Nevertheless angular momentum transport through the corona is small. A study of magnetic field loops in the corona reveals few open field lines and predominantly toroidal loops with a characteristic distance between footpoints that is ∼H. Finally, we find quasi-periodic oscillations with characteristic timescale ∼30 Ω−1 in the magnetic field energy density. These oscillations are correlated with oscillations in the mean azimuthal field; we present a phenomenological, alpha-dynamo model that captures most aspects of the oscillations.
Microscopic Observation of the Light-Cone-Like Thermal Correlations in Cracking Excitations

Many seemingly intractable systems can be reduced to a system of interacting spins. Here, we introduce a system of artificial acoustic spins which are manipulated with ultrasound excitations associated with micro-cracking sources in thin sheets of crystals. Our spin-like system shows a peculiar relaxation mechanism after inducing an impulsive stress-ramp akin to splitting, or rupturing, of the system. Using real-time construction of correlations between spins states, we observe a clear emergence of the light cone effect. It has been proposed that equilibration horizon occurs on a local scale in systems where correlations between distant sites are established at a finite speed. The observed equilibration horizon in our observations defines a region where elements of the material are in elastic communication through excited elementary excitations. These results yield important insights into dynamic communication between failing elements in brittle materials during processes such as brittle fragmentation and dynamic stress triggering of earthquake-generating faults.