Miracle-dz/UniFAR-FTUs huggingface dataset:
Novel constraints on noncold, nonthermal dark matter from Lyman-
α
 forest data

In this paper we present an efficient method for constraining both thermal and non-thermal Dark Matter (DM) scenarios with the Lyman-$\alpha$ forest, based on a simple and flexible parametrisation capable to reproduce the small scale clustering signal of a large set of non-cold DM (nCDM) models. We extract new limits on the fundamental DM properties, through an extensive analysis of the high resolution, high redshift data obtained by the MIKE/HIRES spectrographs. By using a large suite of hydrodynamical simulations, we determine constraints on both astrophysical, cosmological, and nCDM parameters by performing a full Monte Carlo Markov Chain (MCMC) analysis. We obtain a marginalised upper limit on the largest possible scale at which a power suppression induced by nearly any nCDM scenario can occur, i.e. $\alpha<0.03~{\rm{Mpc}}/h$ (2$\sigma$ C.L.). We explicitly describe how to test several of the most viable nCDM scenarios without the need to run any specific numerical simulations, due to the novel parametrisation proposed, and due to a new scheme that interpolates between the cosmological models explored. The shape of the linear matter power spectrum for standard thermal warm DM models appear to be in mild tension ($\sim 2\sigma$ C.L.) with the data, compared to non-thermal scenarios. We show that a DM fluid composed by both a warm (thermal) and a cold component is also in tension with the Lyman-$\alpha$ forest, at least for large $\alpha$ values. This is the first study that allows to probe the linear small scale shape of the DM power spectrum for a large set of nCDM models.
Challenges and Changes of the Breast Cancer Screening Paradigm

Since four decades mammography is used for early breast cancer detection in asymptomatic women and still remains the gold standard imaging modality. However, population screening programs can be personalized and women can be divided into different groups based on risk factors and personal preferences. The availability of new and evolving imaging modalities, for example, digital breast tomosynthesis, dynamic‐contrast‐enhanced magnetic resonance imaging (MRI), abbreviated MRI protocols, diffusion‐weighted MRI, and contrast‐enhanced mammography leads to new challenges and perspectives regarding the feasibility and potential harms of breast cancer screening. The aim of this review is to discuss the current guidelines for different risk groups, to analyze the recent published studies about the diagnostic performance of the imaging modalities and to discuss new developments and future perspectives.
On the evolution of the intrinsic scatter in black hole versus galaxy mass relations

We present results on the evolution of the intrinsic scatter of black hole masses considering different implementations of a model in which black holes only grow via mergers. We demonstrate how merger driven growth affects the correlations between black hole mass and host bulge mass. The simple case of an initially log-normal distributed scatter in black hole and bulge masses combined with random merging within the galaxy population results in a decreasing scatter with merging generation/number as predicted by the Central-limit theorem. In general we find that the decrease in scatter σ is well approximated by σmerg(m) � σini × (m + 1) a/2 with a = 0.42 for a range of mean number of mergers m 100) we find a convergence to a = 0.61. This is valid for a wide range of different initial distributions, refill-scenarios or merger mass-ratios. Growth scenarios based on halo merger
The tight subgiant branch of the intermediate-age star cluster NGC 411 implies a single-aged stellar population

The presence of extended main-sequence turn-off (eMSTO) regions in intermediate-age star clusters in the Large and Small Magellanic Clouds is often interpreted as resulting from extended star formation histories (SFHs), lasting >= 300 Myr. This strongly conflicts with the traditional view of the dominant star formation mode in stellar clusters, which are thought of as single-aged stellar populations. Here we present a test of this interpretation by exploring the morphology of the subgiant branch (SGB) of NGC 411, which hosts possibly the most extended eMSTO among all known intermediate-age star clusters. We show that the width of the NGC 411 SGB favours the single-aged stellar population interpretation and rules out an extended SFH. In addition, when considering the red clump (RC) morphology and adopting the unproven premise that the widths of all features in the colour-magnitude diagram are determined by an underlying range in ages, we find that the SFH implied is still very close to that resulting from a single-aged stellar population, with a minor fraction of stars scattering to younger ages compared with the bulk of the population. The SFHs derived from the SGB and RC are both inconsistent with the SFH derived from the eMSTO region. NGC 411 has a very low escape velocity and it has unlikely undergone significant mass-loss at an early stage, thus indicating that it may lack the capacity to capture most of its initial, expelled gas from stellar evolutionary processes, a condition often required for extended SFHs to take root.
Day Type and Start Time May Influence Sleep in Adolescent Professional Football Players

Abstract This study assessed whether scheduling (start time and day type) and workload variables influenced sleep markers (activity monitor) in professional academy footballers (n=11; 17.3±0.7 yrs) over a 10-week in-season period. Separate linear mixed regressions were used to describe the effect of start time on the previous nights sleep, and the effect of day type (match day, match day+1) and workload on subsequent sleep. Workload variables were modelled by day (day), 7-day (acute), and 28-day (chronic) periods. Sleep duration following match day+1 (400 mins; 95%CI:368–432) was significantly reduced compared to all other day types (p<0.001). Sleep onset time following match day (00:35; CI:00:04–01:12) and wake time on match day+1 (09:00; CI:08:37–09:23) were also significantly later compared to all other day types (p<0.001). Sleep duration (19.1 mins; CI:9.4–28.79), wake time (18 mins; CI:9.3–26.6), and time in bed (16.8 mins; CI:2.0–31.5) were significantly increased per hour delay in start time. When no activity was scheduled, sleep duration (37 mins; CI:18.1–55.9), sleep onset (42.1 mins; CI:28.8–56.2), and wake times (86 mins; CI:72–100) were significantly extended, relative to a 09:00 start time. Day, acute, and chronic workloads were associated with sleep onset and wake times only. Scheduled start times were associated with changes in sleep duration. Therefore, delaying start times may increase sleep in this population.
The mass, luminosity and mass-loss rate of the donor of the V1487 Aql/GRS 1915+105 binary system

The donor in the microquasar GRS 1915+105 is a low-mass giant. Such a star consists of a degenerate helium core and a hydrogen-rich envelope. Both components are separated by a hydrogen burning shell. The structure of such an object is relatively simple and easy to model. Making use of the observational constraints on the luminosity and the radius of the donor, we constrain the mass of this star with evolutionary models. We find a very good agreement between the constraints from those models and from the observed rotational broadening and the NIR magnitude. Combining the constraints, we find solutions with stripped giants of the mass of $\geq\! 0.28{\rm M}_{\odot}$ and of the spectral class K5 III, independent of the distance to the system, and a distance-dependent upper limit, $\lesssim\! 1{\rm M}_{\odot}$. We also calculate the average mass transfer rate and the duty cycle of the system as a function of the donor mass. This rate is much below the critical rate (at which the system would become persistent), and the duty cycle is less than 20 per cent.
LONG-TERM EVOLUTION OF PROTOSTELLAR AND PROTOPLANETARY DISKS. II. LAYERED ACCRETION WITH INFALL

We use one-dimensional two-zone time-dependent accretion disk models to study the long-term evolution of protostellar disks subject to mass addition from the collapse of a rotating cloud core. Our model consists of a constant surface density magnetically coupled active layer, with transport and dissipation in inactive regions only via gravitational instability. We start our simulations after a central protostar has formed, containing ∼10% of the mass of the protostellar cloud. Subsequent evolution depends on the angular momentum of the accreting envelope. We find that disk accretion matches the infall rate early in the disk evolution because much of the inner disk is hot enough to couple to the magnetic field. Later infall reaches the disk beyond ∼10 AU, and the disk undergoes outbursts of accretion in FU Ori-like events as described by Zhu et al. If the initial cloud core is moderately rotating, most of the central star's mass is built up by these outburst events. Our results suggest that the protostellar “luminosity problem” is eased by accretion during these FU Ori-like outbursts. After infall stops, the disk enters the T Tauri phase. An outer, viscously evolving disk has a structure that is in reasonable agreement with recent submillimeter studies and its surface density evolves from Σ ∝ R−1 to R−1.5. An inner, massive belt of material—the “dead zone”—would not have been observed yet but should be seen in future high angular resolution observations by EVLA and ALMA. This high surface density belt is a generic consequence of low angular momentum transport efficiency at radii where the disk is magnetically decoupled, and would strongly affect planet formation and migration.
DAMPING OF MAGNETOHYDRODYNAMIC TURBULENCE IN PARTIALLY IONIZED GAS AND THE OBSERVED DIFFERENCE OF VELOCITIES OF NEUTRALS AND IONS

Theoretical and observational studies on the turbulence of the interstellar medium developed fast in the past decades. The theory of supersonic magnetized turbulence, as well as the understanding of the projection effects of observed quantities, is still in progress. In this work, we explore the characterization of the turbulent cascade and its damping from observational spectral line profiles. We address the difference of ion and neutral velocities by clarifying the nature of the turbulence damping in the partially ionized. We provide theoretical arguments in favor of the explanation of the larger Doppler broadening of lines arising from neutral species compared to ions as arising from the turbulence damping of ions at larger scales. Also, we compute a number of MHD numerical simulations for different turbulent regimes and explicit turbulent damping, and compare both the three-dimensional distributions of velocity and the synthetic line profile distributions. From the numerical simulations, we place constraints on the precision with which one can measure the three-dimensional dispersion depending on the turbulence sonic Mach number. We show that no universal correspondence between the three-dimensional velocity dispersions measured in the turbulent volume and minima of the two-dimensional velocity dispersions available through observations exist. For instance, for subsonic turbulence the correspondence is poor at scales much smaller than the turbulence injection scale, while for supersonic turbulence the correspondence is poor for the scales comparable with the injection scale. We provide a physical explanation of the existence of such a two-dimensional to three-dimensional correspondence and discuss the uncertainties in evaluating the damping scale of ions that can be obtained from observations. However, we show that the statistics of velocity dispersion from observed line profiles can provide the spectral index and the energy transfer rate of turbulence. Also, by comparing two similar simulations with different viscous coefficients, it was possible to constrain the turbulent cut-off scale. This may especially prove useful since it is believed that ambipolar diffusion may be one of the dominant dissipative mechanisms in star-forming regions. In this case, the determination of the ambipolar diffusion scale may be used as a complementary method for the determination of magnetic field intensity in collapsing cores. We discuss the implications of our findings in terms of a new approach to magnetic field measurement proposed by Li & Houde.
OGLE-ing the Magellanic System: Photometric Metallicity from Fundamental Mode RR Lyrae Stars

In an era of extensive photometric observations, the catalogs of RR Lyr type variable stars number tens of thousands of objects. The relation between the iron abundance [Fe/H] and the Fourier parameters of the stars light curve allows us to investigate mean metallicities and metallicity gradients in various stellar environments, independently of time-consuming spectroscopic observations. In this paper we use almost 6500 $V$- and $I$-band light curves of fundamental mode RR Lyr stars from the OGLE-IV survey to provide a relation between the $V$- and $I$-band phase parameter $\varphi_{31}$ used to estimate [Fe/H]. The relation depends on metallicity, which limits its applicability. We apply this relation to metallicity formulae developed for the Johnson $V$- and the Kepler $Kp$-band to obtain the relation between [Fe/H] and $\varphi_{31}$ for the $I$-band photometry. Last, we apply the new relation of Nemec to the OGLE-IV fundamental mode RR Lyr stars data and construct a metallicity map of the Magellanic Clouds. Median [Fe/H] is $-1.39\pm0.44$ dex for the LMC and $-1.77\pm0.48$ dex for the SMC, on the Jurcsik metallicity scale. We also find a metallicity gradient within the LMC with a slope of $-0.029\pm0.002$ dex/kpc in the inner 5 kpc and $-0.030 \pm0.003$ dex/kpc beyond 8 kpc, and no gradient in-between ($-0.019\pm0.002$ dex/kpc integrally). We do not observe a metallicity gradient in the SMC, although we show that the metal-rich RRab stars are more concentrated toward the SMC center than the metal-poor.
Search for the rare decays B^{+}\rightarrow\mu^{+}\mu^{-}K^{+}, B^{0}\rightarrow\mu^{+}\mu^{-}K^{*}(892)^{0}, and B_{s}^{0}\rightarrow\mu^{+}\mu^{-}\phi at CDF

We search for b to s\mu^+\mu^- transitions in B meson (B^+, B^0, or B^0_s) decays with 924pb^{-1} of p pbar collisions at sqrt(s)=1.96 TeV collected with the CDF II detector at the Fermilab Tevatron. We find excesses with significances of 4.5, 2.9, and 2.4 standard deviations in the B^+ to \mu^+\mu^-K^+, B^0 to \mu^+\mu^-K^*(892)^0, and B_s^0 to \mu^+\mu^-\phi decay modes, respectively. Using B to J/psi h (h = K^+, K^*(892)^0, phi) decays as normalization channels, we report branching fractions for the previously observed B^+ and B^0 decays, BR(B^+ to \mu^+\mu^-K^+)=(0.59\pm0.15\pm0.04) x 10^{-6}, and BR(B^0 to \mu^+\mu^-K^*(892)^0)=(0.81\pm0.30\pm0.10) x 10^{-6}, where the first uncertainty is statistical, and the second is systematic. These measurements are consistent with the world average results, and are competitive with the best available measurements. We set an upper limit on the relative branching fraction BR(B_s^0 to \mu^+\mu^-\phi)/BR(B_s^0 to J/\psi\phi)<2.6(2.3)\times10^{-3} at the 95(90)% confidence level, which is the most stringent to date.
Digital health experiences reported in chronic disease management: An umbrella review of qualitative studies

Introduction Digital health interventions can be useful for the management of chronic disease. The aim of this study was to draw out universal themes to understand how people with chronic conditions experience digital health services, programmes, and interventions, and consequently, better inform future digital health delivery. Methods An umbrella review was conducted to identify qualitative systematic reviews reporting digital health experiences in chronic disease. Themes for each included review were independently extracted and appraised by two review authors. Data analysis was conducted using the Constant Comparative method. Results Twenty-two systematic reviews containing 240 individual studies were selected for inclusion. Mental health was the most common condition (n = 5, 23%), followed by cancer (n = 4, 18%) or a combination of chronic diseases (n = 4, 18%). Common themes across the conditions were categorised under nine headings, including: (i) participation and engagement (strong usability and engagement vs reluctance to use digital health when these concepts are ignored), (ii) trust, confidence, and competence (users felt reassured, however technology illiteracy led to a perceived lack of control), (iii) perceived value, perceived effectiveness, transaction cost (gained from efficient aspects of digital health, but also lost through the burden of keeping up with data entry), (iv) perceived care quality (requiring tailoring and fostering motivation), (v) barriers and threats (related to technology risks and challenges), (vi) health outcomes (improved self-management capability), (vii) relationships (improved participant-health professional interaction, but interpersonal aspects such as face-to-face contact were lacking), (viii) unplanned benefit (where digital health often led to users feeling more empowered in their health journey), and (ix) diversity of experiences (reflecting ambivalence of experiences and discipline-specific experiences). Conclusion People with chronic conditions perceive digital health provides feelings of reassurance and the ability to self-manage their condition. While there is ambivalence across the participant experiences reported within the major themes, this umbrella review has outlined a need for future interventions that are user-friendly, flexible, and tailored to individual users. This will be best achieved through a co-design model, with the consumer actively involved in the planning and design of digital health products and services.
Multicomponent Superfluids and Superconductors in Dense Nuclear and Quark Matter

Matter at intermediate baryon densities and low temperatures is notoriously hard to tackle theoretically. Whereas lattice methods cannot cover more than rather small densities, perturbative methods are only applicable at much higher densities. The regime of intermediate chemical potential at low temperatures in the QCD-phase diagram is therefore out of reach of first-principle methods, thus we have to rely on stellar objects to investigate dense nuclear and quark matter at low temperatures. Compact stars can serve as an unique laboratory for this regime. Due to their fast rotation and high magnetic field, phenomena like hydrodynamic instabilities and the formation of vortices/flux tubes become of phenomenological interest. In my thesis, I investigate these multicomponent systems in a consistent multi-fluid treatment. By starting from a fieldtheoretical, bosonic model, the phase structure of a two-fluid system, e.g. consisting of superfluid neutrons and superconducting protons, is explored. Consequently, hydrodynamic instabilities, which might serve as trigger for pulsar glitches, are calculated for these two-fluid systems. By incorporating a gauge field and taking into account the charge of one scalar field, the influence of a superfluid on the magnetic phase structure of a superconductor is studied. In the last part, color superconducting quark matter, which can effectively be described as a multicomponent (color-)supercondcutor, is investigated.
Dirac dynamical resonance states around Schwarzschild black holes

Recently, a novel kind of scalar wigs around Schwarzschild black holes\char22{}scalar dynamical resonance states\char22{}was introduced in [Phys. Rev. D 84, 083008 (2011)] and [Phys. Rev. Lett. 109, 081102 (2012)]. In this paper, we investigate the existence and evolution of Dirac dynamical resonance states. First, we look for stationary resonance states of a Dirac field around a Schwarzchild black hole by using the Schro\ifmmode \ddot{}\else \"{}\fi{}dinger-like equations reduced from the Dirac equation in Schwarzschild spacetime. Then Dirac pseudostationary configurations are constructed from the stationary resonance states. We use these configurations as initial data and investigate their numerical evolutions and energy decay. These dynamical solutions are the so-called ``Dirac dynamical resonance states. '' It is found that the energy of the Dirac dynamical resonance states shows an exponential decay. The decay rate of energy is affected by the resonant frequency, the mass of the Dirac field, the total angular momentum, and the spin-orbit interaction. In particular, for an ultralight Dirac field, the corresponding particles can stay around a Schwarzschild black hole for a very long time, even for cosmological time scales.
DYNAMICS OF ELECTRIC CURRENTS, MAGNETIC FIELD TOPOLOGY, AND HELIOSEISMIC RESPONSE OF A SOLAR FLARE

The solar flare on 2011 July 30 was of a modest X-ray class (M9.3), but it made a strong photospheric impact and produced a “sunquake,” which was observed with the Helioseismic and Magnetic Imager on board NASA's Solar Dynamics Observatory. In addition to the helioseismic waves, the flare caused a large expanding area of white-light emission and was accompanied by the rapid formation of a sunspot structure in the flare region. The flare produced hard X-ray (HXR) emission less then 300 keV and no coronal mass ejection (CME). The absence of CME rules out magnetic rope eruption as a mechanism of helioseismic waves. The sunquake impact does not coincide with the strongest HXR source, which contradicts the standard beam-driven mechanism of sunquake generation. We discuss the connectivity of the flare energy release with the electric currents dynamics and show the potential importance of high-speed plasma flows in the lower solar atmosphere during the flare energy release.
SUPERMASSIVE SEEDS FOR SUPERMASSIVE BLACK HOLES

Recent observations of quasars powered by supermassive black holes (SMBHs) out to z ≳ 7 constrain both the initial seed masses and the growth of the most massive black holes (BHs) in the early universe. Here we elucidate the implications of the radiative feedback from early generations of stars and from BH accretion for popular models for the formation and growth of seed BHs. We show that by properly accounting for (1) the limited role of mergers in growing seed BHs as inferred from cosmological simulations of early star formation and radiative feedback, (2) the sub-Eddington accretion rates of BHs expected at the earliest times, and (3) the large radiative efficiencies ϵ of the most massive BHs inferred from observations of active galactic nuclei at high redshift (ϵ ≳ 0.1), we are led to the conclusion that the initial BH seeds may have been as massive as ≳ 105 M☉. This presents a strong challenge to the Population III seed model, which calls for seed masses of ∼100 M☉ and, even with constant Eddington-limited accretion, requires ϵ ≲ 0.09 to explain the highest-z SMBHs in today's standard ΛCDM cosmological model. It is, however, consistent with the prediction of the direct collapse scenario of SMBH seed formation, in which a supermassive primordial star forms in a region of the universe with a high molecule-dissociating background radiation field, and collapses directly into a 104–106M☉ seed BH. These results corroborate recent cosmological simulations and observational campaigns which suggest that these massive BHs were the seeds of a large fraction of the SMBHs residing in the centers of galaxies today.