Miracle-dz/UniFAR-FTUs huggingface dataset:
DARK MATTER SEARCH USING XMM-NEWTON OBSERVATIONS OF WILLMAN 1

We report the results of a search for an emission line from radiatively decaying dark matter in the ultra-faint dwarf spheroidal galaxy Willman 1 based on analysis of spectra extracted from XMM-Newton X-ray Observatory data. The observation follows up our analysis of Chandra data of Willman 1 that resulted in line flux upper limits over the Chandra bandpass and evidence of a 2.5 keV feature at a significance below the 99% confidence threshold used to define the limits. The higher effective area of the XMM-Newton detectors, combined with application of recently developing methods for extended-source analysis, allows us to derive improved constraints on the combination of mass and mixing angle of the sterile neutrino dark matter candidate. We do not confirm the Chandra evidence for a 2.5 keV emission line.
Self-consistent 2D models of fast-rotating early-type stars

Aims. This work aims at presenting the first two-dimensional model s of an isolated rapidly rotating star that include the deriv ation of the differential rotation and meridional circulation in a self-con sistent way. Methods. We use spectral methods in multidomains, together with a Newton algorithm to determine the steady state solutions including differential rotation and meridional circulation for an isolat ed non-magnetic, rapidly rotating early-type star. In part icular we devise an asymptotic method for small Ekman numbers (small viscosities) that removes the Ekman boundary layer and lifts the degeneracy of the inviscid baroclinic solutions. Results. For the first time, realistic two-dimensional models of fast -rotating stars are computed with the actual baroclinic flow s that predict the differential rotation and the meridional circulation for inter mediate-mass and massive stars. These models nicely compare with available data of some nearby fast-rotating early-typ e stars like Ras Alhague (α Oph), Regulus (α Leo), and Vega (α Lyr). It is shown that baroclinicity drives a differential rotation with a slow pole, a fast equator, a fast cor e, and a slow envelope. The differential rotation is found to increase with mass, with evolution (her e measured by the hydrogen mass fraction in the core), and with metallicity. The core-envelope interface is found to be a place of strong shear where mixing will be effi cient. Conclusions. Two-dimensional models offer a new view of fast-rotating stars, especially of their differential rotation, which turns out to be strong at the core-envelope interface. They also offer more accurate models for interpreting the interferometr ic and spectroscopic data of early-type stars.
GOODS-Herschel: the impact of galaxy-galaxy interactions on the far-infrared properties of galaxies

Aims. We study the impact of galaxy-galaxy interactions on the far-infrared properties of galaxies and its evolution at 0 \textless z \textless 1.2. Methods. Using the high-z galaxies in the fields of Great Observatories Origins Deep Survey (GOODS) observed by the Herschel Space Observatory in the framework of the GOODS-Herschel key program and the local IRAS or AKARI-selected galaxies in the field of Sloan Digital Sky Survey Data Release 7, we investigate the dependence of galaxy properties on the morphology of and the distance to the nearest neighbor galaxy. Results. We find that the star-formation rates (SFRs) and the specific SFRs (SSFRs) of galaxies on average depend on the morphology of and the distance to the nearest neighbor galaxy in this redshift range. When a late-type galaxy has a close neighbor galaxy, the SFR and the SSFR increase as it approaches a late-type neighbor, which is supported by Kolmogorov-Smirnov (K-S) and Monte Carlo (MC) tests with a significance level of \textgreater99%. However, the SFR and the SSFR decrease or do not change much as the galaxy approaches an early-type neighbor. The bifurcations of SFRs and SSFRs depending on the neighbor's morphology seem to occur at R-n approximate to 0.5r(vir,nei) (virial radius of the neighbor), which is supported by K-S and MC tests with a significance level of \textgreater98%. For all redshift bins, the SSFRs of late-type galaxies interacting with late-type neighbors are increased by factors of about 1.8 +/- 0.7 and 4.0 +/- 1.2 compared to those of non-interacting galaxies when the pair separation is smaller than 0.5rvir, nei and 0.1r(vir),(nei), respectively. The dust temperature of both local and high-z late-type galaxies that strongly interact with late-type neighbors (i.e. R-n = 0.1(rvir,nei)) appears to be higher than that of non-interacting galaxies with a significance level of 96-99%. However, the dust temperature of local late-type galaxies that strongly interact with early-type neighbors seems to be lower than or similar to that of non-interacting galaxies. Conclusions. Our results suggest that galaxy-galaxy interactions and mergers have been strongly affecting the SFR and the dust properties of star-forming galaxies over at least 8 billion years.
The Nature of Deeply Buried Ultraluminous Infrared Galaxies: A Unified Model for Highly Obscured Dusty Galaxy Emission

We present models of deeply buried ultraluminous infrared galaxy (ULIRG) spectral energy distributions (SEDs) and use them to construct a three-dimensional diagram for diagnosing the nature of observed ULIRGs. Our goal is to construct a suite of SEDs for a very simple model ULIRG structure, and to explore how well this simple model can (by itself) explain the full range of observed ULIRG properties. We use our diagnostic to analyze archival Spitzer Space Telescope Infrared Spectrograph data of ULIRGs and find that: (1) in general, our model does provide a comprehensive explanation of the distribution of mid-IR ULIRG properties; (2) >75% (in some cases 100%) of the bolometric luminosities of the most deeply buried ULIRGs must be powered by a dust-enshrouded active galactic nucleus; (3) an unobscured “keyhole” view through ≲10% of the obscuring medium surrounding a deeply buried ULIRG is sufficient to make it appear nearly unobscured in the mid-IR; (4) the observed absence of deeply buried ULIRGs with large polycyclic aromatic hydrocarbon (PAH) equivalent widths is naturally explained by our models, showing that deep absorption features are “filled-in” by small quantities of foreground unobscured PAH emission (e.g., from the host galaxy disk) at the level of ∼1% the bolometric nuclear luminosity. The modeling and analysis we present will also serve as a powerful tool for interpreting the high angular resolution spectra of high-redshift sources to be obtained with the James Webb Space Telescope.
Discrimination between ΛCDM, quintessence, and modified gravity models using wide area surveys

In the past decade or so observations of supernovae, Large Scale Structures (LSS), and the Cosmic Microwave Background (CMB) have confirmed the presence of what is called dark energy - the cause of accelerating expansion of the Universe. They have also measured its density as well as the value of other cosmological parameters according to the concordance $\Lambda$CDM model with few percent uncertainties. Next generation of surveys should allow to constrain this model with better precisions, or distinguish between a LCDM and alternative models such as modified gravity and (interacting)-quintessence models. In this work we parametrize both homogeneous and anisotropic components of matter density in the context of interacting dark energy models with the goal of discriminating between f(R) modified gravity and its generalizations, and interacting dark energy models, for which we also propose a phenomenological description of energy-momentum conservation equations inspired by particle physics. It is based on the fact that the simplest interactions between particles/fields are elastic scattering and decay. The parametrization of growth rate proposed here is nonetheless general and can be used to constrain other interactions. As an example of applications, we present an order of magnitude estimation of the accuracy of the measurement of these parameters using Euclid and Planck surveys data, and leave a better estimation to a dedicated work.
Two-loop integrand decomposition into master integrals and surface terms

Loop amplitudes are conveniently expressed in terms of master integrals whose coefficients carry the process dependent information. Similarly before integration, the loop integrands may be expressed as a linear combination of propagator products with universal numerator-tensors. Such a decomposition is an important input for the numerical unitarity approach, which constructs integrand coefficients from on-shell tree amplitudes. We present a new method to organise multi-loop integrands into a direct sum of terms that integrate to zero (surface terms) and remaining master integrands. This decomposition facilitates a general, numerical unitarity approach for multi-loop amplitudes circumventing analytic integral reduction. Vanishing integrals are well known as integration-by-parts identities. Our construction can be viewed as an explicit construction of a complete set of integration-by-parts identities excluding doubled propagators. Interestingly, a class of 'horizontal' identities is singled out which hold as well for altered propagator powers.
DIFFUSIVE SHOCK ACCELERATION SIMULATIONS OF RADIO RELICS

Recent radio observations have identified a class of structures, so-called radio relics, in clusters of galaxies. The radio emission from these sources is interpreted as synchrotron radiation from GeV electrons gyrating in μG-level magnetic fields. Radio relics, located mostly in the outskirts of clusters, seem to associate with shock waves, especially those developed during mergers. In fact, they seem to be good structures to identify and probe such shocks in intracluster media (ICMs), provided we understand the electron acceleration and re-acceleration at those shocks. In this paper, we describe time-dependent simulations for diffusive shock acceleration at weak shocks that are expected to be found in ICMs. Freshly injected as well as pre-existing populations of cosmic-ray (CR) electrons are considered, and energy losses via synchrotron and inverse Compton are included. We then compare the synchrotron flux and spectral distributions estimated from the simulations with those in two well-observed radio relics in CIZA J2242.8+5301 and ZwCl0008.8+5215. Considering that CR electron injection is expected to be rather inefficient at weak shocks with Mach number M ≲ a few, the existence of radio relics could indicate the pre-existing population of low-energy CR electrons in ICMs. The implication of our results on the merger shock scenario of radio relics is discussed.
Measures for a transdimensional multiverse

The multiverse/landscape paradigm that has emerged from eternal inflation and string theory, describes a large-scale multiverse populated by ``pocket universes'' which come in a huge variety of different types, including different dimensionalities. In order to make predictions in the multiverse, we need a probability measure. In (3+1)d landscapes, the scale factor cutoff measure has been previously shown to have a number of attractive properties. Here we consider possible generalizations of this measure to a transdimensional multiverse. We find that a straightforward extension of scale factor cutoff to the transdimensional case gives a measure that strongly disfavors large amounts of slow-roll inflation and predicts low values for the density parameter Ω, in conflict with observations. A suitable generalization, which retains all the good properties of the original measure, is the ``volume factor'' cutoff, which regularizes the infinite spacetime volume using cutoff surfaces of constant volume expansion factor.
Gravitational-radiation losses from the pulsar-white-dwarf binary PSR J1141-6545

Pulsars in close binary systems with white dwarfs or other neutron stars make ideal laboratories for testing the predictions of gravitational radiation and self-gravitational effects. We report new timing measurements of the pulsar-white-dwarf binary PSR J1141-6545. The orbit is found to be decaying at a rate of 1.04{+-}0.06 times the general relativistic prediction and the Shapiro delay is consistent with the orbital inclination angle derived from scintillation measurements. The system provides a unique testbed for tensor-scalar theories of gravity. Our measurements place stringent constraints in the theory space, with a limit of {alpha}{sub 0}{sup 2}<2.1x10{sup -5} for weakly nonlinear coupling and an asymptotic limit of {alpha}{sub 0}{sup 2}<3.4x10{sup -6} for strongly nonlinear coupling (where {alpha}{sub 0} is the linear coupling strength of matter to an underlying scalar field), which is nearly 3 times smaller than the Cassini bound ({alpha}{sub 0}{sup 2}{approx_equal}10{sup -5})
Ab Initio Phonon Structure of h-YMnO3 in Low-Symmetry Ferroelectric Phase

We present a systematic first-principles study of the phonon spectrum of hexagonal YMnO3 in ferroelectric (multiferroic) phase. We investigated in detail the low-energy phonon modes, their dispersion, symmetry, as well as the infrared optical properties of the crystal and determined the phonon density of states.
Knowledge, attitude and first aid of epilepsy among school teachers in Saudi Arabia

Background: epilepsy is a common neurological disorder among school children. While school teachers are the most and available caregivers for these students. The researchers found it necessary to search and review the current knowledge, attitude and first aid toward epilepsy among school teachers in Saudi Arabia. Methods: in this article, we review a state of art of over view about knowledge, attitude and first aid toward epilepsy among school teachers in Saudi Arabia. Results: this review confirmed a low to moderate knowledge, positive attitude and need for training about first aids. Conclusion: the researches emphasize the important role of school teachers in reducing epilepsy related physical, social, psychological and academic problems among students. Therefore, it is necessary to increase the teachers' level of knowledge, attitude and practices regarding epilepsy and its consequences. were less likely to have negative attitudes including minding to have an epileptic child in their class (p = 0.028) or thinking that they should be placed in a special classroom (p = 0.029). The study also concluded that Primary school teacher’s knowledge about epilepsy needs improvements. Their attitudes correlated highly with their knowledge. Educational campaigns about epilepsy are needed to develop a well informed and tolerant community.
Ripple formation on silver after irradiation with radially polarized ultrashort-pulsed lasers

We report on the morphological effects induced by the inhomogeneous absorption of cylindrically polarized femtosecond laser irradiation of silver (Ag) in sub-ablation conditions. A theoretical prediction of the role of surface plasmon excitation in the production of self-formed periodic ripples structures is evaluated. Furthermore, a combined hydrodynamical and thermoelastic model is presented to account for the influence of temperature-related lattice movements in laser beam conditions that are sufficient to produce material melting. The ability to control the size of the morphological changes via modulating the beam polarization aims to provide a systematic methodology for controlling and optimizing the outcome of laser micro-processing.
ORBITAL SUPPORT OF FAST AND SLOW INNER BARS IN DOUBLE-BARRED GALAXIES

We analyze how the orbital support of the inner bar in a double-barred galaxy (nested bars) depends on the angular velocity (i.e., pattern speed) of this bar. We study orbits in seven models of double bars using the method of invariant loops. The range of pattern speed is covered exhaustively. We find that not all pattern speeds are allowed when the inner bar rotates in the same direction as the outer bar. Below a certain minimum pattern speed orbital support for the inner bar abruptly disappears, while at high values of this speed the orbits indicate an increasingly round bar that looks more like a twist in the nuclear isophotes than a dynamically independent component. For values between these two extremes, orbits supporting the inner bar extend further out as the bar's pattern speed decreases, their corresponding loops become more eccentric, pulsate more, and their rotation becomes increasingly non-uniform, as they speed up and slow down in their motion. Lower pattern speeds also lead to a less coherent bar, as the pulsation and acceleration increasingly varies among the loops supporting the inner bar. The morphologies of fast and slow inner bars expected from the orbital structure studied here have been recently recovered observationally by decomposition of double-barred galaxies. Our findings allow us to link the observed morphology to the dynamics of the inner bar.
COSMIC ORIGINS SPECTROGRAPH AND FUSE OBSERVATIONS OF T ∼ 105 K GAS IN A NEARBY GALAXY FILAMENT

We present a clear detection of a broad Lyα absorber (BLA) with a matching O vi line in the nearby universe. The BLA is detected at in the high signal-to-noise ratio spectrum of Mrk 290 obtained using the Cosmic Origins Spectrograph. The Lyα absorption has two components, with km s−1 and km s−1, separated in velocity by v ∼ 115 km s−1. The O vi, detected by the Far-Ultraviolet Spectroscopic Explorer at , has a km s−1 and is kinematically well aligned with the broader H i component. The non-detection of other ions such as C ii, Si ii, Fe ii, C iii, Si iii, C iv, Si iv, and N v at the same velocity as the BLA and the O vi implies that the absorber is tracing highly ionized gas. The different line widths of the BLA and O vi suggest a temperature of T = 1.4 × 105 K in the absorber. Photoionization, collisional ionization equilibrium as well as non-equilibrium collisional ionization models do not explain the ion ratios at this temperature. The observed line strength ratios and line widths favor an ionization scenario in which both ion–electron collisions and UV photons contribute to the ionization in the gas. Such a model requires a low metallicity of ∼−1.7 dex, ionization parameter of log U ∼ −1.4, a large total hydrogen column density of N(H) ∼ 4 × 1019 cm−2, and a path length of ∼400 kpc. The line of sight to Mrk 290 intercepts at the redshift of the absorber, a megaparsec scale filamentary structure extending over ∼20° in the sky, with several luminous galaxies distributed within ∼1.5 h−1 Mpc projected distance from the absorber. The collisionally ionized gas phase of this absorber is most likely tracing a shock-heated gaseous structure, consistent with a few different scenarios for the origin including an overdense region of the warm-hot intergalactic medium in the galaxy filament or highly ionized gas in the extended halo of one of the galaxies in the filament. In general, BLAs with metals provide an efficient means to study T ∼ 105–106 K gas in galaxy halos and in the intergalactic medium. A substantial fraction of the baryons missing from the present universe is predicted to be in such environments in the form of highly ionized plasma.
The Economics of Financial Stress

We study the psychological costs of financial constraints and their economic consequences. Using a representative survey of U.S. households, we document the prevalence of financial stress in U.S. households and a strong relationship between financial stress and measures of financial constraints. We incorporate financial stress into an otherwise standard dynamic model of consumption and labor supply. We emphasize two key results. First, a psychologybased theory of poverty traps requires two equally important components: financial stress itself and naivete about financial stress. Specifically, sophisticates save enough to escape highstress states, because they understand that doing so alleviates the economic consequences of financial stress. On the other hand, naifs dis-save, fall into a poverty trap, and incur high welfare losses. Second, the financial stress channel can reverse the counterfactual negative wealth effect on labor supply because relieving stress frees up cognitive resources for productive work. Financial stress also has macroeconomic implications on wealth inequality and fiscal multipliers. *Sergeyev: Bocconi University, CEPR, and IGIER, dmytro.sergeyev@unibocconi.it; Lian: UC Berkeley and NBER, chen_lian@berkeley.edu; Gorodnichenko: UC Berkeley and NBER, ygorodni@econ.berkeley.edu. For helpful comments and suggestions, we are grateful to Marios Angeletos, Abhijit Banerjee, Nicholas Barberis, David Berger, Tito Boeri, Leonardo Bursztyn, James Choi, Stefano Dellavigna, Eliana La Ferrara, Pierre-Olivier Gourinchas, Joel Flynn, Jonathon Hazell, Supreet Kaur, Yueran Ma, Anandi Mani, Gonzalo Maturana, Peter Maxted, Tim Mcquade, Sendhil Mullainathan, Emi Nakamura, Gautam Rao, Dmitry Taubinsky, Neil Thakral (discussant), Ricardo Perez-Truglia, Gautam Rao, Christopher Roth, Karthik Sastry, Jon Steinsson, Frank Schilbach, Benjamin Schoefer, and seminar participants at Behavioral Economics Annual Meeting, NBER Behavioral Finance Meeting, Bocconi, Miami Behavioral Finance Conference, TSE, Stanford, SED, UC Berkeley, UC Davis, Biennial Consumer Finance and Macroeconomics Conference, Psychology and Economics of Poverty Annual Convening, and the 16th CSEF-IGIER Symposium on Economics and Institutions. The survey was approved by UC Berkeley IRB 2021-1114868. We thank Zhuoran Lyu, Jack Mannion, Emily Martell, Bruno Smaniotto, and Laura Waring for excellent research assistance and the BB90 fund for financial support.
Phase-asymmetry resource interconversion via estimation

Practical implementations of quantum information-theoretic applications rely on phase coherences between systems. These coherences are disturbed by misalignment between phase references. Quantum states carrying phase-asymmetry act as resources to counteract this misalignment. In this paper, we construct protocols for interconverting these resources by first estimating the misalignment. Our method achieves sublinear, but otherwise arbitrarily high, asymptotic rate of conversion of pure resource states to mixed ones. No other method is known for asymptotic pure-to-mixed state conversion. Our method also has the advantage of achieving phase reference alignment in addition to resource conversion.