Miracle-dz/UniFAR-FTUs huggingface dataset:
ON THE METHOD TO INFER AN ATMOSPHERE ON A TIDALLY LOCKED SUPER EARTH EXOPLANET AND UPPER LIMITS TO GJ 876d

We develop a method to infer or rule out the presence of an atmosphere on a tidally locked hot super Earth. The question of atmosphere retention is a fundamental one, especially for planets orbiting M stars due to the star's long-duration active phase and corresponding potential for stellar-induced planetary atmospheric escape and erosion. Tidally locked planets with no atmosphere are expected to show a Lambertian-like thermal phase curve, causing the combined light of the planet–star system to vary with planet orbital phase. We report Spitzer 8 μm IRAC observations of GJ 876 taken over 32 continuous hours and reaching a relative photometric precision of 3.9 × 10−4 per point for 25.6 s time sampling. This translates to a 3σ limit of 5.13 × 10−5 on a planet thermal phase curve amplitude. Despite the almost photon-noise-limited data, we are unable to conclusively infer the presence of an atmosphere or rule one out on the non-transiting short-period super Earth GJ 876d. The limiting factor in our observations was the miniscule, monotonic photometric variation of the slightly active host M star, because the partial sine wave due to the planet has a component in common with the stellar linear trend. The proposed method is nevertheless very promising for transiting hot super Earths with the James Webb Space Telescope and is critical for establishing observational constraints for atmospheric escape.
A sustainable development approach of silica recovery and treatment of semiconductor-industry wastewater using ceramic membranes

ABSTRACT The semiconductor sector generates a large amount of wastewater. If these wastewaters are not treated, they can be harmful to the environment. Wastewater often contains silicon particles, which could be recovered and repurposed. Membrane technology has grown significantly and offers benefits in treating wastewater. The objective of this study is to evaluate the performance of ceramic membrane as a sustainable development approach of silica recovery for the treatment of semiconductor-industry wastewater. Two ultrafiltration (UF) ceramic membranes with different molecular weight cutoff were used in this study. UF membrane with pore diameter smaller than hydrodynamic particle size of the silica colloids (124.3 nm to 126.7 nm) was able to recover silica colloids. Membrane B has the best performance in terms of color rejection (98.95%), SS rejection (97.76%), TDS rejection (92.75%), NH3-N rejection (92.86%), turbidity rejection (99.53%), COD rejection (99.34%), and BOD rejection (93.75%). Besides, the usage of 0.1 M NaOCl for alkaline cleaning was most prominent in membrane cleaning with a high FRR value (78.39–80.77%). Furthermore, the blocking mechanisms were determined, as proven by the Hermia model, which is standard blocking for both membranes. This innovation serves as a new revolution in semiconductor-industry wastewater treatment where wastewater treatment process comes along with simultaneous recovery of silica for recycle and reuse.
Plant functional diversity is affected by weed management through processes of trait convergence and divergence

Weed management involving tillage and/or herbicides has generally led to a decline of plant diversity in agroecosystems, with negative impacts on ecosystem services provision. The use of plant covers has become the predominant alternative in vineyard management, with numerous studies focusing on analyzing the advantages and disadvantages of plant covers compared to the aforementioned management. Although the impacts of weed management on taxonomic diversity have been widely studied, many gaps remain on their effects on plant functional diversity. As plant functional diversity is linked to the delivery of key ecosystem services in agroecosystems, understanding these effects could enable the development of more sustainable practices. From 2008 to 2018, a long-term trial was carried out in a Mediterranean vineyard to assess different agricultural practices. In this article, we examined how weed management, as well as irrigation use, could affect plant functional diversity. Based on 10 functional traits, such as plant height, specific leaf area or seed mass, we measured different indices of functional diversity and used null models to detect processes of trait convergence and divergence. Our results revealed that weed management and irrigation use had a significant effect on plant functional diversity. Mown plots showed the highest functional richness but were functionally convergent, since mowing was a strong functional filter on most of the traits. Tillage also behaved as a functional filter on some vegetative traits, but favored the divergence of certain reproductive traits. Herbicide-treated and irrigated plots showed the highest values of functional divergence by promoting more competitive species with more divergent trait values. The effect of weed management on these community assembly processes was shaped by the use of irrigation in vineyard rows, leading to functional divergence in those vegetative traits related to resource acquisition and seed mass. These results suggest that greater functional diversity may be associated with the bias caused by higher occurrence of competitive species (e.g. Convolvulus arvensis, Sonchus asper) with contrasting values for certain traits. Therefore, since these species are considered harmful to crops, higher plant functional diversity might not be a desirable indicator in agroecosystems.
HUBBLE SPACE TELESCOPE OBSERVATIONS OF AN OUTER FIELD IN OMEGA CENTAURI: A DEFINITIVE HELIUM ABUNDANCE

We revisit the problem of the split main sequence (MS) of the globular cluster ω Centauri, and report the results of two-epoch Hubble Space Telescope observations of an outer field, for which proper motions give us a pure sample of cluster members, and an improved separation of the two branches of the MS. Using a new set of stellar models covering a grid of values of helium and metallicity, we find that the best possible estimate of the helium abundance of the bluer branch of the MS is Y = 0.39 ± 0.02. For the cluster center, we apply new techniques to old observations: we use indices of photometric quality to select a high-quality sample of stars, which we also correct for differential reddening. We then superpose the color–magnitude diagram of the outer field on that of the cluster center, and suggest a connection of the bluer branch of the MS with one of the more prominent among the many sequences in the subgiant region. We also report a group of undoubted cluster members that are well to the red of the lower MS.
Treatment patterns and burden of complications associated with sickle cell disease: A US retrospective claims analysis

Complications associated with sickle cell disease (SCD) that are highly impactful for patients but until recently have been less understood include priapism, nephropathy, and neurologic injury. We conducted a retrospective study using US administrative claims data from July 01, 2013 through March 31, 2020 to analyze incidence of these complications, SCD treatment patterns, and healthcare resource utilization (HCRU) and costs among 2524 pediatric and adult patients with SCD (mean [SD] age 43.4 [22.4] years). The most common treatments during follow‐up were short‐acting opioids (54.0% of patients), red blood cell transfusion (15.9%), and hydroxyurea (11.0%). SCD complications occurred frequently; in the overall population, the highest follow‐up incidences per 1000 person‐years were for acute kidney injury (53.1), chronic kidney disease (40.6), and stroke (39.0). Complications occurred across all age groups but increased in frequency with age; notably, acute kidney injury was 69.7 times more frequent among ages 65+ than ages 0–15 (p < 0.001). Follow‐up per‐patient‐per‐month HCRU also increased with age; however, all‐cause healthcare costs were similarly high for all age groups and were driven primarily by inpatient stays. Patients with SCD across the age spectrum have a high burden of complications with the use of current treatments, suggesting unmet needs for treatment management.
ZAREMBA, SALEM AND THE FRACTAL NATURE OF GHOST DISTRIBUTIONS

Abstract Motivated by near-identical graphs of two increasing continuous functions—one related to Zaremba’s conjecture and the other due to Salem—we provide an explicit connection between fractals and regular sequences by showing that the graphs of ghost distributions, the distribution functions of measures associated to regular sequences, are sections of self-affine sets. Additionally, we provide a sufficient condition for such measures to be purely singular continuous. As a corollary, and analogous to Salem’s strictly increasing singular continuous function, we show that the ghost distributions of the Zaremba sequences are singular continuous.
Measurement of the intracluster light at z ∼ 1

A significant fraction of the total photospheric light in nearby galaxy clusters is thought to be contained within the diffuse intracluster light (ICL), which extends hundreds of kpc from cluster cores. The study of the ICL can reveal details of the evolutionary histories and processes occurring within galaxy clusters; however, since it has a very low surface brightness, it is often difficult to detect. We present here the first measurements of the ICL as a fraction of the total cluster light at z ∼ 1 using deep J-band (1.2 μm) imaging from a high-acuity wide-field K-band imager on the Very Large Telescope. We investigate the ICL in six X-ray selected galaxy clusters at 0.8 ≤ z ≤ 1.2 and find that the ICL below isophotes μ J = 22 magarcsec -2 constitutes 1-4 per cent of the total cluster light within a radius R 500. This is broadly consistent with simulations of the ICL at a similar redshift and when compared to nearby observations suggests that the fraction of the total cluster light that is in the ICL has increased by a factor of 2-4 since z ∼ 1. We also find the fraction of the total cluster light contained within the brightest cluster galaxy (BCG) to be 2.0-6.3 per cent at these redshifts, which in five out of six cases is larger than the fraction of the ICL component, in contrast to the results from nearby clusters. This suggests that the evolution in cluster cores involves substantial stripping activity at late times, in addition to the early build-up of the BCG stellar mass through merging. The presence of significant amount of stellar light at large radii from these BCGs may help towards solving the recent disagreement between the semi-analytic model predictions of BCG mass growth and the observed large masses and scale sizes reported for BCGs at high redshift.
Detailed cluster mass and light profiles of A1703, A370 and RXJ1347−11 from deep Subaru imaging★

Weak lensing work can be badly compromised by unlensed foreground and cluster members which dilute the true lensing signal. We show how the lensing amplitude in multicolour space can be harnessed to securely separate cluster members from the foreground and background populations for three massive clusters, A1703 (z= 0.258), A370 (z= 0.375) and RXJ1347−11 (z= 0.451) imaged with Subaru. The luminosity functions of these clusters when corrected for dilution show similar faint-end slopes, α≃− 1.0, with no marked faint-end upturn to our limit of MR≃− 15.0, and only a mild radial gradient. In each case, the radial profile of the mass-to-light ratio (M/L) peaks at intermediate radius, ≃ 0.2rvir, at a level of 300–500(M/LR)⊙, and then falls steadily towards ∼ 100(M/LR)⊙ at the virial radius, similar to the mean field level. This behaviour is likely due to the relative paucity of central late-type galaxies, whereas for the E/S0 sequence only a mild radial decline in M/L is found for each cluster. We discuss this behaviour in the context of detailed simulations where predictions for tidal stripping may now be tested accurately with observations.
Correlated versus Ferromagnetic State in Repulsively Interacting Two-Component Fermi Gases

Whether a spin-1/2 Fermi gas will become ferromagnetic as the strength of repulsive interaction increases is a long-standing controversial issue. Recently this problem has been studied experimentally by Jo et al. [Science 325, 1521 (2009)] in which the authors claim a ferromagnetic transition is observed. This work is to point out the results of this experiment cannot distinguish whether the system is in a ferromagnetic state or in a nonmagnetic but strongly short-range correlated state. A conclusive experimental demonstration of ferromagnetism relies on the observation of ferromagnetic domains.
The Wave Nature Of The Electron

When in 1920 I resumed my studies of theoretical physics which had long been interrupted by circumstances beyond my control, I was far from the idea that my studies would bring me several years later to receive such a high and envied prize as that awarded by the Swedish Academy of Sciences each year to a scientist: the Nobel Prize for Physics. What at that time drew me towards theoretical physics was not the hope that such a high distinction would ever crown my work; I was attracted to theoretical physics by the mystery enshrouding the structure of matter and the structure of radiations, a mystery which deepened as the strange quantum concept introduced by Planck in 1900 in his research on black-body radiation continued to encroach on the whole domain of physics. To assist you to understand how my studies developed, I must first depict for you the crisis which physics had then been passing through for some twenty years.
Probing the photoionised outflow in the NLS1 Ark 564: An XMM-Newton view

We present a detailed analysis of xmm X-ray observations of the Narrow line Seyfert-1 (NLS1) galaxy Ark 564 taken between 2000 and 2011. High-resolution X-ray spectroscopy is carried out on the resultant high signal-to-noise stacked spectrum. We find three separate photoionised warm absorbers outflowing at velocities unusually lower than typical NLS1s. Using recombination timescale estimates, improved constraints on the location of these clouds show they could be located beyond 4 pc from the central source. Our estimates of the outflow kinetics suggest that the AGN in Ark 564 is unlikely to affect the host galaxy in its current state but over typical lifetime of 10^7 years the ISM could be affected. The individual observations used here suggest the luminosity varies over weekly timescales and in addition we find evidence of gas response to changes in the ionising radiation.
High-resolution Spectroscopy and Spectropolarimetry of Some Late F- / Early G-type Sun-like Stars as Targets for Zeeman Doppler Imaging

Abstract High-resolution spectroscopy and spectropolarimetry have been undertaken at the Anglo-Australian Telescope in order to identify suitable targets for magnetic studies of young Sun-like stars, for the proxy study of early solar evolution. This study involved the investigation of some variable late F- / early G-type Sun-like stars originally identified by the Hipparcos mission. Of the 38 stars observed for this study, HIP 31021, HIP 64732, HIP 73780 were found to be spectroscopic binary stars, while HIP 19072, HIP 67651 and HIP 75636 are also likely to be binaries and HIP 33111 could even be a triple system. Magnetic fields were detected on a number of the survey stars: HIP 21632, HIP 43720, HIP 48770, HIP 62517, HIP 71933, HIP 77144, HIP 89829, HIP 90899 and HIP 105388, making these stars good candidates for follow-up Zeeman Doppler imaging studies.
PROBING OUTFLOWS IN z = 1 ∼ 2 GALAXIES THROUGH Fe ii/Fe ii* MULTIPLETS

We report on a study of the 2300–2600 Å Fe ii/Fe ii* multiplets in the rest-UV spectra of star-forming galaxies at 1.0 < z < 2.6 as probes of galactic-scale outflows. We extracted a mass-limited sample of 97 galaxies at z ∼ 1.0–2.6 from ultra-deep spectra obtained during the GMASS spectroscopic survey in the GOODS South field with the Very Large Telescope and FORS2. We obtain robust measures of the rest equivalent width of the Fe ii absorption lines down to a limit of Wr > 1.5 Å and of the Fe ii* emission lines to Wr > 0.5 Å. Whenever we can measure the systemic redshift of the galaxies from the [O ii] emission line, we find that both the Fe ii and Mg ii absorption lines are blueshifted, indicating that both species trace gaseous outflows. We also find, however, that the Fe ii gas has generally lower outflow velocity relative to that of Mg ii. We investigate the variation of Fe ii line profiles as a function of the radiative transfer properties of the lines, and find that transitions with higher oscillator strengths are more blueshifted in terms of both line centroids and line wings. We discuss the possibility that Fe ii lines are suppressed by stellar absorptions. The lower velocities of the Fe ii lines relative to the Mg ii doublet, as well as the absence of spatially extended Fe ii* emission in two-dimensional stacked spectra, suggest that most clouds responsible for Fe ii absorption lie close (3 ∼ 4 kpc) to the disks of galaxies. We show that the Fe ii/Fe ii* multiplets offer unique probes of the kinematic structure of galactic outflows.
Operational approach to Bell inequalities: Application to qutrits

Bell inequalities can be studied both as constraints in the space of probability distributions and as expectation values of multipartite operators. The latter approach is particularly useful when considering outcomes as eigenvalues of unitary operators. This brings the possibility of exploiting the complex structure of the coefficients in the Bell operators. We investigate this avenue of though in the known case of two outcomes, and find new Bell inequalities for the cases of three outcomes and $n=3,4,5$ and $6$ parties. We find their corresponding classical bounds and their maximum violation in the case of qutrits. We further propose a novel way to generate Bell inequalities based on a mapping from maximally entangled states to Bell operators and produce examples for different outcomes and number of parties.
Fe and Al Abundances for 180 Red Giants in the Globular Cluster Omega Centauri (NGC 5139)

We present radial velocities and Fe and Al abundances for 180 red giant branch (RGB) stars in the Galactic globular cluster Omega Centauri (ω Cen). The majority of our data lie in the range 11.0 < V < 13.5, which covers the RGB from about 1 mag above the horizontal branch to the RGB tip. The selection procedures are biased toward preferentially observing the more metal-poor and luminous stars of ω Cen. Abundances were determined using equivalent width measurements and spectrum synthesis analyses of moderate resolution spectra (R ≈ 13,000) obtained with the Blanco 4 m telescope and Hydra multifiber spectrograph. Our results are in agreement with previous studies as we find at least four different metallicity populations with [ Fe/H ] = − 1.75, –1.45, –1.05, and –0.75, with a full range of –2.20≲ [ Fe/H ] ≲ − 0.70. [Al/Fe] ratios exhibit large star-to-star scatter for all populations, with the more than 1.0 dex range of [Al/Fe] decreasing for stars more metal-rich than [ Fe/H ] ∼ − 1.4. The minimum [Al/Fe] abundance observed for all metallicity populations is [ Al/Fe ] ∼ + 0.15. The maximum abundance of log ϵ (Al) is reached for stars with [ Fe/H ] ∼ − 1.4 and does not increase further with stellar metallicity. We interpret these results as evidence for Type II SNe providing the minimum [Al/Fe] ratio and a mass spectrum of intermediate-mass asymptotic giant branch stars causing the majority of the [Al/Fe] scatter. These results seem to fit in the adopted scheme that star formation occurred in ω Cen over >1 Gyr.
The ATLAS 3D project - XXIV. The intrinsic shape distribution of early-type galaxies

We use the ATLAS^(3D) sample to perform a study of the intrinsic shapes of early-type galaxies, taking advantage of the available combined photometric and kinematic data. Based on our ellipticity measurements from the Sloan Digital Sky Survey Data Release 7, and additional imaging from the Isaac Newton Telescope, we first invert the shape distribution of fast and slow rotators under the assumption of axisymmetry. The so-obtained intrinsic shape distribution for the fast rotators can be described with a Gaussian with a mean flattening of q = 0.25 and standard deviation σ_q = 0.14, and an additional tail towards rounder shapes. The slow rotators are much rounder, and are well described with a Gaussian with mean q = 0.63 and σ_q = 0.09. We then checked that our results were consistent when applying a different and independent method to obtain intrinsic shape distributions, by fitting the observed ellipticity distributions directly using Gaussian parametrizations for the intrinsic axis ratios. Although both fast and slow rotators are identified as early-type galaxies in morphological studies, and in many previous shape studies are therefore grouped together, their shape distributions are significantly different, hinting at different formation scenarios. The intrinsic shape distribution of the fast rotators shows similarities with the spiral galaxy population. Including the observed kinematic misalignment in our intrinsic shape study shows that the fast rotators are predominantly axisymmetric, with only very little room for triaxiality. For the slow rotators though there are very strong indications that they are (mildly) triaxial.
THE STELLAR-TO-HALO MASS RELATION OF LOCAL GALAXIES SEGREGATES BY COLOR

By means of a statistical approach that combines different semi-empirical methods of galaxy–halo connection, we derive the stellar-to-halo mass relations (SHMR) of local blue and red central galaxies. We also constrain the fraction of halos hosting blue/red central galaxies and the occupation statistics of blue and red satellites as a function of halo mass, Mh. For the observational input we use the blue and red central/satellite galaxy stellar mass functions and two-point correlation functions in the stellar mass range of 9 < log(M*/M☉) <12. We find that: (1) the SHMR of central galaxies is segregated by color, with blue centrals having a SHMR above that of red centrals; at log(Mh/M☉) ∼12, the M*-to-Mh ratio of the blue centrals is ≈0.05, which is ∼1.7 times larger than the value of red centrals. (2) The constrained scatters around the SHMRs of red and blue centrals are ≈0.14 and ≈0.11 dex, respectively. The scatter of the average SHMR of all central galaxies changes from ∼0.20 dex to ∼0.14 dex in the 11.3 < log(Mh/M☉) <15 range. (3) The fraction of halos hosting blue centrals at M☉ is 87%, but at 2 × 1012 M☉ decays to ∼20%, approaching a few percent at higher masses. The characteristic mass at which this fraction is the same for blue and red galaxies is M☉. Our results suggest that the SHMR of central galaxies at large masses is shaped by mass quenching. At low masses processes that delay star formation without invoking too strong supernova-driven outflows could explain the high M*-to-Mh ratios of blue centrals as compared to those of the scarce red centrals.
Sandpiles and absorbing-state phase transitions: Recent results and open problems

We review some recent results on the relations between sandpiles and a class of absorbing state phase transitions. We use the concept of fixed energy sandpiles (FES), in which external driving and dissipation are absent. FES are shown to exhibit an absorbing state transition with critical properties coinciding with those of the corresponding sandpile model. We propose a set of Langevin equations capturing the relevant features of this transition. These equations characterize the universality class of systems with an infinite number of absorbing states and a static conserved field coupled to the order parameter. Different models in this class are identified, and strong evidence is presented showing that the Manna sandpile, as well as some other stochastic sandpiles, belong in this universality class. Finally some open problems and questions are discussed.