Miracle-dz/UniFAR-FTUs huggingface dataset:
The impact of global environment on galaxy mass functions at low redshift

We study the galaxy stellar mass function in different environments in the local Universe, considering both the total mass function and that of individual galaxy morphological types. We compare the mass functions of galaxies with $\rm log_{10} M_{\star}/M_{\odot} \geq 10.25$ in the general field and in galaxy groups, binary and single galaxy systems from the Padova-Millennium Galaxy and Group Catalogue at $z=0.04-0.1$ with the mass function of galaxy clusters of the WIde-field Nearby Galaxy-Cluster Survey at $z=0.04-0.07$. Strikingly, the variations of the mass function with global environment, overall, are small and subtle. The shapes of the mass functions of the general field and clusters are indistinguishable, and only small, statistically insignificant variations are allowed in groups. Only the mass function of our single galaxies, representing the least massive haloes and comprising less than a third of the general field population, is proportionally richer in low-mass galaxies than other environments. The most notable environmental effect is a progressive change in the upper galaxy mass, with very massive galaxies found only in the most massive environments. This environment-dependent mass cut-off is unable to affect the Schechter parameters and the K-S test, and can only be revealed by an ad-hoc analysis. Finally, we show how, in each given environment, the mass function changes with morphological type, and that galaxies of the same morphological type can have different mass functions in different environments.
A new approach to simulating collisionless dark matter fluids

Recently, we have shown how current cosmological N-body codes already follow the fine grained phase-space information of the dark matter fluid. Using a tetrahedral tesselation of the three-dimensional manifold that describes perfectly cold fluids in six-dimensional phase space, the phase-space distribution function can be followed throughout the simulation. This allows one to project the distribution function into configuration space to obtain highly accurate densities, velocities, and velocity dispersions. Here, we exploit this technique to show first steps on how to devise an improved particle-mesh technique. At its heart, the new method thus relies on a piecewise linear approximation of the phase space distribution function rather than the usual particle discretisation. We use pseudo-particles that approximate the masses of the tetrahedral cells up to quadrupolar order as the locations for cloud-in-cell (CIC) deposit instead of the particle locations themselves as in standard CIC deposit. We demonstrate that this modification already gives much improved stability and more accurate dynamics of the collisionless dark matter fluid at high force and low mass resolution. We demonstrate the validity and advantages of this method with various test problems as well as hot/warm-dark matter simulations which have been known to exhibit artificial fragmentation. This completely unphysical behaviour is much reduced in the new approach. The current limitations of our approach are discussed in detail and future improvements are outlined.
Calculation of Skin Dose Rate Conversion Factors Due to Surface Contamination from Frequently used Radionuclides in Local Nuclear and Medical Facilities

Purpose: The use of nonsealed radioactive sources can lead to skin contamination due to radiological accidents and staff oversight. This contamination has been shown to contribute considerably to the total skin dose received by nuclear medicine technicians and can easily exceed the limit of 500 mSv/year established by the current regulations. To assess the severity of contamination, it is necessary to estimate the skin dose through the use of suitable skin dose rate conversion factors. To determine the appropriate factors, it is important to study the influence of the contamination area, the epidermal thickness, and the percutaneous absorption on them. Materials and Methods: Monte Carlo simulations using the code PHITS 3.02 were carried out to study and quantify the dosimetry conversion factors of 15 frequently used radionuclides (11C, 18F, 36Cl, 54Mn, 60Co, 90Sr, 99 mTc, 123I, 131I, 137Cs, 153Sm, 177 Lu, 223Ra, 226Ra, and 241Am). Results: The absorbed dose to the skin is significantly influenced by epidermal thickness and percutaneous absorptions and can differ by up to two orders of magnitude with respect to the operational magnitude H'(0.07,0°). Conclusions: Skin dosimetry after a contamination incident may be complex because the absorbed dose delivered to the basal layer is influenced by the contamination area, the epidermal thickness, and the percutaneous absorption. Therefore, when an accident occurs, the dose should be quantified taking into account these parameters, especially the epidermal thickness, and the possible percutaneous absorption should be evaluated in cases where the contamination involves a dose approximately equivalent to the established limits.
The $m–z$ relation for Type Ia supernovae, locally inhomogeneous cosmological models, and the nature of dark matter

The $m$-$z$ relation for type Ia supernovae is one of the key pieces of evidence supporting the cosmological `concordance model' with $\lambda_0 \approx 0.7$ and $\Omega_0 \approx 0.3$. However, it is well known that the $m$-$z$ relation depends not only on $\lambda_0$ and $\Omega_0$ (with $H_0$ as a scale factor) but also on the density of matter along the line of sight, which is not necessarily the same as the large-scale density. I investigate to what extent the measurement of $\lambda_0$ and $\Omega_0$ depends on this density when it is characterized by the parameter $\eta$ ($0 \le \eta \le 1$), which describes the ratio of density along the line of sight to the overall density. I also discuss what constraints can be placed on $\eta$, both with and without constraints on $\lambda_0$ and $\Omega_0$ in addition to those from the $m$-$z$ relation for type~Ia supernovae.
RADIO DIAGNOSTICS OF ELECTRON ACCELERATION SITES DURING THE ERUPTION OF A FLUX ROPE IN THE SOLAR CORONA

Electron acceleration in the solar corona is often associated with flares and the eruption of twisted magnetic structures known as flux ropes. However, the locations and mechanisms of such particle acceleration during the flare and eruption are still subject to much investigation. Observing the exact sites of particle acceleration can help confirm how the flare and eruption are initiated and how they evolve. Here we use the Atmospheric Imaging Assembly to analyze a flare and erupting flux rope on 2014 April 18, while observations from the Nançay Radio Astronomy Facility allow us to diagnose the sites of electron acceleration during the eruption. Our analysis shows evidence of a pre-formed flux rope that slowly rises and becomes destabilized at the time of a C-class flare, plasma jet, and the escape of ≳75 keV electrons from the rope center into the corona. As the eruption proceeds, continued acceleration of electrons with energies of ∼5 keV occurs above the flux rope for a period over 5 minutes. At the flare peak, one site of electron acceleration is located close to the flare site, while another is driven by the erupting flux rope into the corona at speeds of up to 400 km s−1. Energetic electrons then fill the erupting volume, eventually allowing the flux rope legs to be clearly imaged from radio sources at 150–445 MHz. Following the analysis of Joshi et al. (2015), we conclude that the sites of energetic electrons are consistent with flux rope eruption via a tether cutting or flux cancellation scenario inside a magnetic fan-spine structure. In total, our radio observations allow us to better understand the evolution of a flux rope eruption and its associated electron acceleration sites, from eruption initiation to propagation into the corona.
Integrating Microfluidics and Electronics in Point-of-Care Diagnostics: Current and Future Challenges

Point-of-Care (POC) diagnostics have gained increasing attention in recent years due to its numerous advantages over conventional diagnostic approaches. As proven during the recent COVID-19 pandemic, the rapidity and portability of POC testing improves the efficiency of healthcare services and reduces the burden on healthcare providers. There are hundreds of thousands of different applications for POC diagnostics, however, the ultimate requirement for the test is the same: sample-in and result-out. Many technologies have been implemented, such as microfluidics, semiconductors, and nanostructure, to achieve this end. The development of even more powerful POC systems was also enabled by merging multiple technologies into the same system. One successful example is the integration of microfluidics and electronics in POC diagnostics, which has simplified the sample handling process, reduced sample usage, and reduced the cost of the test. This review will analyze the current development of the POC diagnostic systems with the integration of microfluidics and electronics and discuss the future challenges and perspectives that researchers might have.
Dark Energy and Consciousness

One of the most important concepts in logic and the foundations of mathematics may be useful in providing an explanation for the cosmological constant problem. A connection between self-reference and consciousness has been previously discussed due to their similar nature of making a reference to itself. Vacuum observation has the property of self-reference and consciousness in the sense that the observer is observing one's own reference frame of energy. In this paper, the cyclical loop model of self-reference is applied to the vacuum observation, such that the discrepancy between the energy density resulting from the first part of the causal loop (i.e., the classical irreversible computation of the observer's reference frame) and the other part of the causal loop (i.e., nondeterministic quantum evolution) corresponds to 10^(123). This effectively provides a consistent explanation of the difference between the observed and the theoretical values of the vacuum energy, namely, the cosmological constant problem.
Microbes-Assisted Arsenate Reduction Activity in Bangladesh Drinking Water Wells as Revealed by Enrichment Cultivation

Abstract Arsenate-reducing microorganisms may mobilize arsenic into groundwater. Phylogenetic DNA sequence information cannot exclusively be used to infer arsenate reduction, as the spotted homologies may not translate to biochemical activities. We here develop a cultivation-based metagenomic strategy for inferring actual activities: we complement a cultivation-independent microbial community survey covering 22 arsenic-contaminated drinking water wells in Bangladesh, with the characterization of enrichments of anaerobic arsenate reducers. All investigated samples revealed microbial arsenate reduction activity. The enriched microbial communities were phylogenetically diverse within and between the enrichments. The enrichment also unveiled species: the arsenate-reducing enrichments held 16S rRNA gene sequences closest to Dechloromonas sp. , Azonexus fungiphilus, Youngiibacter fragile, Methanogenic prokaryote and Fusibacter sp. , in addition to arsenate-reducing Sulfurospirillum strains NP4, b10 and dissimilatory iron-reducing Geobacter species. The enriched arsenate reductase gene (arrA) sequences were closest to sequences in known arsenate reducing Sulfurospirillum barnesii. This study bridges the knowledge gap between cultivation-independent and cultivation-dependent analyses. It clarifies the mechanism for arsenic mobilization and redistribution in rural drinking water wells, as a balance between bioremediation and harmful activities. The identified, potentially dissimilatory arsenate and iron-reducing microbes, constitute a risk for arsenic bioremediation. Appropriate metagenomic and dynamic analyses should help design and maintain safer, effective bioremediation.
DEVELOPMENT OF AN INTEGRATED GIS BASED METHODOLOGY FOR THE SELECTION OF SOLID WASTES DISPOSAL SITES FOR KHULNA CITY

Solid waste management system is a global concern today. As sustainable management of the environment is necessary to keep a safe and livable world for the next generation, the continuous process of environmental degradation must be stopped or at least minimized immediately. Improperly managed or unmanaged solid waste can create adverse impact on environment through air pollution, water pollution, land contamination etc. It is really a serious threat to the environment. In order to minimize the impact, environmental consideration is incorporated in solid waste management system in developed countries but it is a new practice in developing countries. This paper examines a GIS based location finding approaches combined with multi-criteria evaluation for solid waste dumping for Khulna city in Bangladesh. It attempts to develop a methodology that can be applied in finding suitable sites for solid waste disposal for most of the major cities.
ENVIRONMENTAL EFFECTS ON STAR FORMATION ACTIVITY AT z ∼ 0.9 IN THE COSMOS FIELD

We investigated the fraction of [O ii] emitters in galaxies at z ∼ 0.9 as a function of the local galaxy density in the Hubble Space Telescope (HST) COSMOS 2 deg2 field. [O ii] emitters are selected by the narrowband excess technique with the NB711-band imaging data taken with Suprime-Cam on the Subaru telescope. We carefully selected 614 photo-z-selected galaxies with MU3500 < −19.31 at z = 0.901 – 0.920, which includes 195 [O ii] emitters, to directly compare the results with our previous study at z ∼ 1.2. We found that the fraction is almost constant at 0.3 Mpc−2 < Σ10th < 10 Mpc−2. We also checked the fraction of galaxies with blue rest-frame colors of NUV − R < 2 in our photo-z-selected sample, and found that the fraction of blue galaxies does not significantly depend on the local density. On the other hand, the semi-analytic model of galaxy formation predicted that the fraction of star-forming galaxies at z ∼ 0.9 decreases with increasing projected galaxy density even if the effects of the projection and the photo-z error in our analysis were taken into account. The fraction of [O ii] emitters decreases from ∼60% at z ∼ 1.2 to ∼30% at z ∼ 0.9 independent of galaxy environment. The decrease of the [O ii] emitter fraction could be explained mainly by the rapid decrease of star formation activity in the universe from z ∼ 1.2 to z ∼ 0.9.
A DEEP XMM-NEWTON SURVEY OF M33: POINT-SOURCE CATALOG, SOURCE DETECTION, AND CHARACTERIZATION OF OVERLAPPING FIELDS

We have obtained a deep 8 field XMM-Newton mosaic of M33 covering the galaxy out to the D25 isophote and beyond to a limiting 0.2–4.5 keV unabsorbed flux of 5 × 10−16 erg cm−2 s−1 (L > ? > 4 × 1034 erg s−1 at the distance of M33). These data allow complete coverage of the galaxy with high sensitivity to soft sources such as diffuse hot gas and supernova remnants (SNRs). Here, we describe the methods we used to identify and characterize 1296 point sources in the 8 fields. We compare our resulting source catalog to the literature, note variable sources, construct hardness ratios, classify soft sources, analyze the source density profile, and measure the X-ray luminosity function (XLF). As a result of the large effective area of XMM-Newton below 1 keV, the survey contains many new soft X-ray sources. The radial source density profile and XLF for the sources suggest that only ∼15% of the 391 bright sources with L > ? > 3.6 × 1035 erg s−1 are likely to be associated with M33, and more than a third of these are known SNRs. The log(N)–log(S) distribution, when corrected for background contamination, is a relatively flat power law with a differential index of 1.5, which suggests that many of the other M33 sources may be high-mass X-ray binaries. Finally, we note the discovery of an interesting new transient X-ray source, which we are unable to classify.
Lipid Rafts and Plant Gravisensitivity

The necessity to include plants as a component of a Bioregenerative Life Support System leads to investigations to optimize plant growth facilities as well as a better understanding of the plant cell membrane and its numerous activities in the signaling, transport, and sensing of gravity, drought, and other stressors. The cell membrane participates in numerous processes, including endo- and exocytosis and cell division, and is involved in the response to external stimuli. Variable but stabilized microdomains form in membranes that include specific lipids and proteins that became known as (detergent-resistant) membrane microdomains, or lipid rafts with various subclassifications. The composition, especially the sterol-dependent recruitment of specific proteins affects endo- and exo-membrane domains as well as plasmodesmata. The enhanced saturated fatty acid content in lipid rafts after clinorotation suggests increased rigidity and reduced membrane permeability as a primary response to abiotic and mechanical stress. These results can also be obtained with lipid-sensitive stains. The linkage of the CM to the cytoskeleton via rafts is part of the complex interactions between lipid microdomains, mechanosensitive ion channels, and the organization of the cytoskeleton. These intricately linked structures and functions provide multiple future research directions to elucidate the role of lipid rafts in physiological processes.
In-beam evaluation of a medium-size Resistive-Plate WELL gaseous particle detector

In-beam evaluation of a fully-equipped medium-size 30 × 30 cm2 Resistive Plate WELL (RPWELL) detector is presented. It consists here of a single element gas-avalanche multiplier with Semitron ESD225 resistive plate, 1 cm2 readout pads and APV25/SRS electronics. Similarly to previous results with small detector prototypes, stable operation at high detection efficiency (> 98%) and low average pad multiplicity (∼ 1.2) were recorded with 150 GeV muon and high-rate pion beams, in Ne/(5%CH4), Ar/(5%CH4) and Ar/(7%CO2). This is an important step towards the realization of robust detectors suitable for applications requiring large-area coverage; among them Digital Hadron Calorimetry.
Supply Chain Finance Arrangements and Shareholder Benefits

ABSTRACT Supply chain finance (SCF) is a buyer-led financial innovation used to optimize working capital and increase liquidity within the supply chain. Advertised as win-win, little is known of the benefits to firms or shareholders. I explore whether these arrangements are beneficial to the initiating firm and whether such benefits percolate to the buyer’s investors. I find that although a firm’s days payable outstanding increases post-adoption, SCF arrangements are not beneficial to all firms. Liquidity and profitability decrease post-adoption. I also find that shareholders respond negatively to SCF adoptions, but this response may be attenuated by some firms increasing share repurchases.
Modeling the effect of small-scale magnetic turbulence on the X-ray properties of Pulsar Wind Nebulae

Pulsar Wind Nebulae (PWNe) constitute an ideal astrophysical environment to test our current understanding of relativistic plasma processes. It is well known that magnetic fields play a crucial role in their dynamics and emission properties. At present, one of the main issues concerns the level of magnetic turbulence present in these systems, which in the absence of space resolved X-ray polarization measures cannot be directly constrained. In this work we investigate, for the first time using simulated synchrotron maps, the effect of a small scale fluctuating component of the magnetic field on the emission properties in X-ray. We illustrate how to include the effects of a turbulent component in standard emission models for PWNe, and which consequences are expected in terms of net emissivity and depolarization, showing that the X-ray surface brightness maps can provide already some rough constraints. We then apply our analysis to the Crab and Vela nebulae and, by comparing our model with Chandra and Vela data, we found that the typical energies in the turbulent component of the magnetic field are about 1.5 to 3 times the one in the ordered field.
DISCOVERY OF AN Hα EMITTING DISK AROUND THE SUPERMASSIVE BLACK HOLE OF M31

Due to its proximity, the mass of the supermassive black hole in the nucleus of the Andromeda galaxy (M31), the most massive black hole in the Local Group of galaxies, has been measured by several methods involving the kinematics of a stellar disk which surrounds it. We report here the discovery of an eccentric Hα emitting disk around the black hole at the center of M31 and show how modeling this disk can provide an independent determination of the mass of the black hole. Our model implies a mass of 5.0+0.8− 1.0 × 107 M☉ for the central black hole, consistent with the average of determinations by methods involving stellar dynamics, and compatible (at 1σ level) with measurements obtained from the most detailed models of the stellar disk around the central black hole. This value is also consistent with the M–σ relation. In order to make a comparison, we applied our simulation on the stellar kinematics in the nucleus of M31 and concluded that the parameters obtained for the stellar disk are not formally compatible with the parameters obtained for the Hα emitting disk. This result suggests that the stellar and the Hα emitting disks are intrinsically different from each other. A plausible explanation is that the Hα emission is associated with a gaseous disk. This hypothesis is supported by the detection of traces of weaker nebular lines in the nuclear region of M31. However, we cannot exclude the possibility that the Hα emission is, at least partially, generated by stars.
HOW STARLESS ARE STARLESS CORES?

In this paper, we present the results of Combined Array for Research in Millimeter-wave Astronomy continuum and spectral line observations of the dense core Per-Bolo 45. Although this core has previously been classified as starless, we find evidence for an outflow and conclude that Per-Bolo 45 is actually an embedded, low-luminosity protostar. We discuss the impact of newly discovered, low-luminosity, embedded objects in the Perseus molecular cloud on starless core and protostar lifetimes. We estimate that the starless core lifetime has been overestimated by 4%–18% and the Class 0/I protostellar lifetime has been underestimated by 5%–20%. Given the relatively large systematic uncertainties involved in these calculations, variations on the order of 10% do not significantly change either core lifetimes or the expected protostellar luminosity function. Finally, we suggest that high-resolution (sub)millimeter surveys of known cores lacking near-infrared and mid-infrared emission are necessary to make an accurate census of starless cores.