Miracle-dz/UniFAR-FTUs huggingface dataset:
Spitzer deep and wide legacy mid- and far-infrared number counts and lower limits of cosmic infrared background

Aims. We aim to place stronger lower limits on the cosmic infrared background (CIB) brightness at 24 μm, 70 μm and 160 μ ma nd measure the extragalactic number counts at these wavelengths in a homogeneous way from various surveys. Methods. Using Spitzer legacy data over 53.6 deg 2 of various depths, we build catalogs with the same extraction method at each wavelength. Completeness and photometric accuracy are estimated with Monte-Carlo simulations. Number count uncertainties are estimated with a counts-in-cells moment method to take galaxy clustering into account. Furthermore, we use a stacking analysis to estimate number counts of sources not detected at 70 μm and 160 μm. This method is validated by simulations. The integration of the number counts gives new CIB lower limits. Results. Number counts reach 35 μJy, 3.5 mJy and 40 mJy at 24 μm, 70 μm, and 160 μm, respectively. We reach deeper flux densities of 0.38 mJy at 70, and 3.1 at 160 μm with a stacking analysis. We confirm the number count turnover at 24 μm and 70 μm, and observe it for the first time at 160 μm at about 20 mJy, together with a power-law behavior below 10 mJy. These mid- and far-infrared counts: 1) are homogeneously built by combining fields of different depths and sizes, providing a legacy over about three orders of magnitude in flux density; 2) are the deepest to date at 70 μm and 160 μm; 3) agree with previously published results in the common measured flux density range; 4) globally agree with the Lagache et al. (2004) model, except at 160 μm, where the model slightly overestimates the counts around 20 and 200 mJy. Conclusions. These counts are integrated to estimate new CIB firm lower limits of 2.29 +0.09 −0.09 nW m −2 sr −1 ,5 . 4 +0.4 −0.4 nW m −2 sr −1 ,a nd 8.9 +1.1 −1.1 nW m −2 sr −1 at 24 μm, 70 μm, and 160 μm, respectively, and extrapolated to give new estimates of the CIB due to galaxies of 2.86 +0.19 −0.16 nW m −2 sr −1 ,6 . 6 +0.7 −0.6 nW m −2 sr −1 , and 14.6 +7.1 −2.9 nW m −2 sr −1 , respectively. Products (point spread function, counts, CIB contributions, software) are publicly available for download at http://www.ias. u-psud.fr/irgalaxies/
SDSS-III Baryon Oscillation Spectroscopic Survey: Analysis of Potential Systematics in Fitting of Baryon Acoustic Feature

Extraction of the Baryon Acoustic Oscillations (BAO) to percent level accuracy is challenging and demands an understanding of many potential systematic to an accuracy well below 1 per cent, in order ensure that they do not combine significantly when compared to statistical error of the BAO measurement. Sloan Digital Sky Survey (SDSS)-III Baryon Oscillation Spectroscopic Survey (BOSS) SDSS Data Release Eleven (DR11) reaches a distance measurement with $\sim 1\%$ statistical error and this prompts an extensive search for all possible sub-percent level systematic errors which could be safely ignored previously. In this paper, we analyze the potential systematics in BAO fitting methodology using mocks and data from BOSS DR10 and DR11. We demonstrate the robustness of the fiducial multipole fitting methodology to be at $0.1\%-0.2\%$ level with a wide range of tests in mock galaxy catalogs pre- and post-reconstruction. We also find the DR10 and DR11 data from BOSS to be robust against changes in methodology at similar level. This systematic error budget is incorporated into the the error budget of Baryon Oscillation Spectroscopic Survey (BOSS) DR10 and DR11 BAO measurements. Of the wide range of changes we have investigated, we find that when fitting pre-reconstructed data or mocks, the following changes have the largest effect on the best fit values of distance measurements both parallel and perpendicular to the line of sight: (a) Changes in non-linear correlation function template; (b) Changes in fitting range of the correlation function; (c) Changes to the non-linear damping model parameters. The priors applied do not matter in the estimates of the fitted errors as long as we restrict ourselves to physically meaningful fitting regions. [abridged]
Cold gas properties of the herschel reference survey: III. Molecular gas stripping in cluster galaxies

The Herschel Reference Survey is a complete volume-limited, K-band-selected sample of nearby objects including Virgo cluster and isolated objects. Using a recent compilation of Hi and CO data for this sample we study the effects of the cluster environment on the molecular gas content of spiral galaxies. With the subsample of unperturbed field galaxies, we first identify the stel lar mass as the scaling variable that traces the total molecular gas mas s of galaxies better. We show that, on average, Hi-deficient galaxies are significantly o ffset (4 �) from the M(H2) vs. Mstar relation for Hi-normal galaxies. We use the M(H2) vs. Mstar scaling relation to define the H 2-deficiency parameter as the di fference, on logarithmic scale, between the expected and observed molecular gas mass for a galaxy of given stellar mass. The H2-deficiency parameter shows a weak and scattered relation wi th the Hi-deficiency parameter, here taken as a proxy for galaxy interactions with the surrounding cluster environment. We also show that, as for the atomic gas, the extent of the molecular disc decreases with increasing Hi-deficiency. All together, these results show that cluster g alaxies have, on average, a lower molecular gas content than similar objects in the field. Our analysis indicates that ram pressure stri pping is the physical process responsible for this molecular gas deficie ncy. The slope of the H2− de f vs. Hi− de f relation is less than unity, while the D(Hi)/D(i) vs. Hi− de f relation is steeper than the D(CO)/D(i) vs. Hi− de f relation, thereby indicating that the molecular gas is removed less effi ciently than the atomic gas. This result can be understood if the atomic gas is distributed on a relatively flat disc that is more extended than the stellar disc. It is thus le ss anchored to the gravitational potential well of the galax y than the molecular gas phase, which is distributed on an exponential disc with a scalelength rCO≃ 0.2r24. 5(g). There is a clear trend between the NUV− i colour index, which is a proxy for the specific star formation activity, and the H2-deficiency parameter, which suggests that molecular gas removal quenches the activity of star formation. This causes galaxies migrate from the blue cloud to the green valley and, eventually, to the red sequence. The total gas-c onsumption timescale of gas deficient cluster galaxies is co mparable to that
SOLAR FLARE PREDICTION USING SDO/HMI VECTOR MAGNETIC FIELD DATA WITH A MACHINE-LEARNING ALGORITHM

We attempt to forecast M- and X-class solar flares using a machine-learning algorithm, called support vector machine (SVM), and four years of data from the Solar Dynamics Observatory's Helioseismic and Magnetic Imager, the first instrument to continuously map the full-disk photospheric vector magnetic field from space. Most flare forecasting efforts described in the literature use either line-of-sight magnetograms or a relatively small number of ground-based vector magnetograms. This is the first time a large data set of vector magnetograms has been used to forecast solar flares. We build a catalog of flaring and non-flaring active regions sampled from a database of 2071 active regions, comprised of 1.5 million active region patches of vector magnetic field data, and characterize each active region by 25 parameters. We then train and test the machine-learning algorithm and we estimate its performances using forecast verification metrics with an emphasis on the true skill statistic (TSS). We obtain relatively high TSS scores and overall predictive abilities. We surmise that this is partly due to fine-tuning the SVM for this purpose and also to an advantageous set of features that can only be calculated from vector magnetic field data. We also apply a feature selection algorithm to determine which of our 25 features are useful for discriminating between flaring and non-flaring active regions and conclude that only a handful are needed for good predictive abilities.
An Abundance Analysis of Bright Giants in the Globular Cluster NGC 1851

We present the chemical compositions for eight bright giants in the globular cluster NGC 1851. Our analysis reveals large star-to-star abundance variations and correlations of the light elements O, Na, and Al, a feature found in every well-studied globular cluster. However, NGC 1851 also exhibits large star-to-star abundance variations of the s-process elements Zr and La. These s-process elements are correlated with Al and anticorrelated with O. Furthermore, the Zr and La abundances appear to cluster around two distinct values. A recent study revealed a double subgiant branch in NGC 1851. Our data reinforce the notion that there are two stellar populations in NGC 1851 and indicate that this cluster has experienced a complicated formation history with similarities to ω Centauri.
Self-consistent field theory of density correlations in classical fluids

More than half of a century has passed since the free energy of classical fluids defined by second Legendre transform was derived as a functional of density-density correlation function. It is now becoming an increasingly significant issue to develop the correlation functional theory that encompasses the liquid state theory, especially for glassy systems where out of equilibrium correlation fields are to be investigated. Here we have formulated a field theoretic perturbation theory that incorporates two-body fields (both of density-density correlation field and its dual field playing the role of two-body interaction potential) into a density functional integral representation of the Helmholtz free energy. Quadratic density fluctuations are only considered in the saddle-point approximation of two-body fields as well as density field. We have obtained a set of self-consistent field equations with respect to these fields, which simply reads a modified mean-field equation of density field where the bare interaction potential in the thermal energy unit is replaced by minus the direct correlation function given in the mean spherical approximation. Such replacement of the interaction potential in the mean-field equation belongs to the same category as the local molecular field theory proposed by Weeks and co-workers. Notably, it has been shown that even the mean-field part of the free energy functional given by the self-consistent field theory includes information on short-range correlations between fluid particles, similarly to the formulation of the local molecular field theory. The advantage of our field theoretic approach is not only that the modified mean-field equation can be improved systematically, but also that fluctuations of two-body fields in nonuniform fluids may be considered, which would be relevant especially for glass-forming liquids.
Journal Pre-proof Distinct molecular profiles of sporadic early onset colorectal cancer: a population-based cohort and systematic review

Background and aims: The observed increase in incidence of early onset colorectal cancer (EOCRC) is being driven by sporadic cases, but the molecular characteristics of these tumours are not fully understood. Our objective was to investigate the prevalence of microsatellite instability (MSI) and selected mutations in sporadic EOCRC, and their association with survival. Methods: Firstly, we compared the prevalence of molecular characteristics and survival within a population-based cohort study of 652 Stage II and III colon cancer patients in Northern Ireland, comparing sporadic early onset (<50 years, n=35) with older (60-69 years, n=179) patients. Secondly, a systematic review for studies reporting the prevalence of MSI, mismatch repair deficiency (dMMR) or BRAF , KRAS , NRAS , PIK3CA and TP53 mutations in sporadic EOCRC was conducted. Meta-analysis was performed to calculate pooled estimates of the prevalence of molecular features in sporadic EOCRC. The molecular characteristics of sporadic EOCRC differ from those of older adults, particularly regarding reduced prevalence of BRAF mutations. Ten percent of sporadic EOCRC display MSI-H/dMMR. Further studies are needed to address survival in sporadic EOCRC and whether molecular profiles influence EOCRC outcomes in this patient group.
Live Proof-by-Induction

Refinement types are a powerful formalism with many applications in program verification, compiler optimization, etc. We present our work-in-progress on MachineArithmetic, an implementation of refinement types in Smalltalk. Our current results are empirical, successfully running tests in the LiquidHaskell benchmark suite. They say you do not understand a topic in mathematics until you can teach it. And you do not really understand it until you can prove it in Coq. And you do not really really understand it until you can prove it in Agda.
Parametric Landau damping of space charge modes

Landau damping is the mechanism of plasma and beam stabilization; it arises through energy transfer from collective modes to the incoherent motion of resonant particles. Normally this resonance requires the resonant particle's frequency to match the collective mode frequency. We have identified an important new damping mechanism, {\it parametric Landau damping}, which is driven by the modulation of the mode-particle interaction. This reveals new possibilities for stability control through manipulation of both particle and mode-particle coupling spectra. We demonstrate the existence of parametric Landau damping in a simulation of transverse coherent modes of bunched accelerator beams with space charge.
Robust Ensemble Adversarial Model-Based Reinforcement Learning

Model-Based Reinforcement Learning (MBRL) algorithms solve sequential decision-making problems, usually formalized as Markov Decision Processes, using a model of the environment dynamics to compute the optimal policy. When dealing with complex environments, the environment dynamics are frequently approximated with function approximators (such as Neural Networks) that are not guaranteed to converge to an optimal solution. As a consequence, the planning process using samples generated by an imperfect model is also not guaranteed to converge to the optimal policy. In fact, the mismatch between source and target dynamics distribution can result in compounding errors, leading to poor algorithm performance during testing. To mitigate this, we combine the Robust Markov Decision Processes (RMDPs) framework and an ensemble of models to take into account the uncertainty in the approximation of the dynamics. With RMDPs, we can study the uncertainty problem as a two-player stochastic game where Player 1 aims to maximize the expected return and Player 2 wants to minimize it. Using an ensemble of models, Player 2 can choose the worst model to carry out the transitions when performing rollout for the policy improvement. We present Robust Ensemble AdversariaL (REAL) MBRL, an ensemble-based algorithm leveraging the use of an Ad-versarial agent to compute a policy more robust to model errors. We propose two adversarial approaches: one with a greedy adversary and one with an 𝜖 -random adversary. We experimentally show that finding a maximin strategy for this two-player game results in a policy robust to model errors leading to better performance when compared to assuming the learned dynamics to be correct. 1
Evolution of multiple supernova remnants

(Abridged) Heating of the interstellar medium by multiple supernovae (SNe) explosions is at the heart of producing galaxy-scale outflows. We use hydrodynamical simulations to study the efficiency of multiple SNe in heating the interstellar medium (ISM) and filling the volume with gas of high temperatures. We argue that it is important for SNe remnants to have a large filling factor {\it and} a large heating efficiency. For this, they have to be clustered in space and time, and keep exploding until the hot gas percolates through the whole region, in order to compensate for the radiative loss. In the case of a limited number of SNe, we find that although the filling factor can be large, the heating efficiency declines after reaching a large value. In the case of a continuous series of SNe, the hot gas ($T \ge 3 \times 10^6$ K) can percolate through the whole region after the total volume filling factor reaches a threshold of $\sim 0.3$. The efficiency of heating the gas to X-ray temperatures can be $\ge 0.1$ after this percolation epoch, which occurs after a period of $\approx 10$ Myr for a typical starburst SNe rate density of $\nu_{\rm SN} \approx 10^{-9}$ pc$^{-3}$ yr$^{-1}$ and gas density of $n\approx 10$ cm$^{-3}$ in starburst nuclei regions. This matches the recent observations of a time delay of similar order between the onset of star formation and galactic outflows. The efficiency to heat gas up to X-ray temperatures ($\ge 10^{6.5}$ K) roughly scales as $\nu_{\rm SN}^{0.2} n^{-0.6}$. For a typical SNe rate density and gas density in starburst nuclei, the heating efficiency is $\sim 0.15$, also consistent with previous interpretations from X-ray observations. We discuss the implications of our results with regard to observational diagnostics of ionic ratios and emission measures in starburst nuclei regions.
Improving approximate-optimized effective potentials by imposing exact conditions: Theory and applications to electronic statics and dynamics

We develop a method that can constrain any local exchange-correlation potential to preserve ba-sic exact conditions. Using the method of Lagrange multipliers, we calculate for each set of given Kohn-Sham orbitals, a constraint-preserving potential which is closest to the given exchange-correlation potential. The method is applicable to both the time-dependent (TD) and independent cases. The exact conditions that are enforced for the time-independent case are: Galilean covariance, zero net force and torque, and Levy-Perdew virial theorem. For the TD case we enforce translational covariance, zero net force, the Levy-Perdew virial theorem and energy balance. We test our method on the exchange Krieger-Li-Iafrate (xKLI) approximate-optimized effective potential (AOEP), for both cases. For the time-independent case, we calculated the ground state properties of some hydrogen chains and small sodium clusters, for some constrained xKLI potentials and Hartree-Fock (HF) exchange. The results indicate that enforcing the exact conditions is not important for these cases. On the other hand, in the case, constraining both energy balance and zero net force yields improved results relative to TDHF calculations. We explored the electron dynamics in small sodium clusters driven by CW laser pulses. For each laser pulse we compared calculations from TD constrained xKLI, TD partially constrained xKLI and TDHF. We found that electron dynamics like elec-tron ionization and moment of inertia dynamics for the constrained xKLI are most similar to the TDHF results. Also, energy conservation is better by at least an order of magnitude with respect to the unconstrained xKLI. We also discuss the problems that arise in satisfying constraints in the TD case with a non CW driving force.
The warm absorber and X-ray variability of the Seyfert 1 galaxy NGC 3516 as seen by the XMM-Newton RGS

Aims. We present a new analysis of the soft and medium energy X-ray spectrum of the Seyfert 1 galaxy NGC3516 taken with the Reflection Grating Spectrometer (RGS) and European Photon Imaging Camera (EPIC) on board the XMM-Newton observatory. We examine four observations made in October 2006. We investigate whether the observed variability is due to absorption by the warm absorber and/or is intrinsic to the source emission. Methods. We analyse in detail the EPIC-pn and RGS spectra of each observation separately. Results. The warm absorber in NGC3516 is found to consist of three phases of ionisation, two of which have outflow velocities of more than 1000 kms −1 . The third phase (the least ionised one) is much slower at 100 kms −1 . One of the high ionisation phases, with log ξ of 2.4, is found to have a partial covering fraction of about 60%. It has previously been suggested that the passage of a cloud, part of a disc wind, in front of the source (producing a change in the covering fraction) was the cause of a significant dip in the lightcurve during one of the observations. From our modelling of the EPIC-pn and RGS spectra, we find that variation in the covering fraction cannot be solely responsible for this. We show that intrinsic change in the source continuum plays a much more significant role in explaining the observed flux and spectral variability than originally thought.
EFFICACY AND UTILITY OF BRONCHIAL CYTOLOGY IN DIAGNOSING LUNG LESIONS AND ITS HISTOPATHOLOGICAL CORRELATION

Background: Lung cancer is the leading cause of cancer mortality. Presently, various cytologic diagnostic techniques are being used in the evaluation of suspected lung neoplasms. Though the initial diagnosis of malignancy can be made based on clinico-radiological grounds, but the definitive diagnosis needs cytological or histopathological examinations of the specimens from the respiratory tract. Materials and Methods: The present study is a retrospective study done in the Department of Pathology for a period of 1 year (August 2019 to August 2020). A total of 100 reported cases of bronchial brushing cytology were included and correlated with the histopathology; wherever available. Rest of the respiratory cytological samples like sputum, bronchoalveolar lavage, bronchial washings, fine needle aspiration cytology was excluded from the study. Result: Out of the total 100 bronchial brushing cytology specimens, 69 were males and rest 31were females. The age of the patients ranged from 17 to 84 years, with mean age of 50.2 years. None of the cases were unsatisfactory on bronchial brushing cytology. Out of the 100 cases, histological findings were present in 50 cases (50/100). A total of 22 cases (22/ 100) were reported as malignant on bronchial brushings. The various diagnosis given on bronchial brushings were; 1) NSCLC favouring either squamous cell carcinoma, adenocarcinoma or poorly differentiated,
Rescue-Prime Optimized

This note specifies two instances of a hash function obtained from applying the Marvellous design strategy [1] to a specific context. The context in question is native hashing in a STARK [2] Virtual Machine such as Miden [9]. This context induces unique design constraints, which this specification addresses. The hash function must be defined over the same field that the VM is defined over, which is the prime field with p = 2 − 2 + 1 elements. One of the main use cases is Merkle tree hashing, and so the hash function must support an interface for efficient two-to-one hashing. There are two parameter sets, targeting security level 128 and 160, respectively.