Miracle-dz/UniFAR-FTUs huggingface dataset:
Evaporating very small grains as tracers of the UV radiation field in photo-dissociation regions

Context. In photo-dissociation regions (PDRs), polycyclic aromatic hydrocarbons (PAHs) may be produced by evaporation of very small grains (VSGs) by the impinging UV radiation field from a nearby star. Aims. We quantitatively investigate the transition zone between evaporating VSGs (eVSGs) and PAHs in several PDRs. Methods. We studied the relative contribution of PAHs and eVSGs to the mid-IR emission in a wide range of excitation conditions. We fitted the observed mid-IR emission of PDRs by using a set of template band emission spectra of PAHs, eVSGs, and gas lines. The fitting tool PAHTAT (PAH Toulouse Astronomical Templates) is made available to the community as an IDL routine. From the results of the fit, we derived the fraction of carbon feVSG locked in eVSGs and compared it to the intensity of the local UV radiation field. Results. We show a clear decrease of feVSG with increasing intensity of the local UV radiation field, which supports the scenario of photo-destruction of eVSGs. Conversely, this dependence can be used to quantify the intensity of the UV radiation field for different PDRs, including unresolved ones. Conclusions. PAHTAT can be used to trace the intensity of the local UV radiation field in regions where eVSGs evaporate, which correspond to relatively dense (nH = [100, 10 5 ]c m −3 ) and UV irradiated PDRs (G0 = [100, 5 × 10 4 ]) where H2 emits in rotational
Visibility of Pulsar Emission: Motion of the Visible Point

Abstract A standard model for the visibility of pulsar radio emission is based on the assumption that the emission is confined to a narrow cone about the tangent to a dipolar field line. The widely accepted rotating vector model (RVM) is an approximation in which the line of sight is fixed and the field line is not strictly tangent to it. We refer to an exact treatment (Gangadhara, 2004) as the tangent model. In the tangent model (but not in the RVM) the visible point changes as a function of pulsar rotational phase, ψ, defining a trajectory on a sphere of radius r. We solve for the trajectory and for the angular velocity of the visible point around it. We note the recent claim that this motion is observable using interstellar holography (Pen et al., 2014). We estimate the error introduced by use of the RVM and find that it is significant for pulsars with emission over a wide range of ψ. The RVM tends to underestimate the range of ψ over which emission is visible. We suggest that the geometry alone strongly favors the visible pulsar radio being emitted at a heights more than ten percent of the light-cylinder distance, where our neglect of retardation effects becomes significant.
THE KENNICUTT–SCHMIDT RELATION IN EXTREMELY METAL-POOR DWARF GALAXIES

The Kennicutt–Schmidt (KS) relation between the gas mass and star formation rate (SFR) describes the star formation regulation in disk galaxies. It is a function of gas metallicity, but the low-metallicity regime of the KS diagram is poorly sampled. We have analyzed data for a representative set of extremely metal-poor galaxies (XMPs), as well as auxiliary data, and compared these to empirical and theoretical predictions. The majority of the XMPs possess high specific SFRs, similar to high-redshift star-forming galaxies. On the KS plot, the XMP H i data occupy the same region as dwarfs and extend the relation for low surface brightness galaxies. Considering the H i gas alone, a considerable fraction of the XMPs already fall off the KS law. Significant quantities of “dark” H2 mass (i.e., not traced by CO) would imply that XMPs possess low star formation efficiencies (SFEgas). Low SFEgas in XMPs may be the result of the metal-poor nature of the H i gas. Alternatively, the H i reservoir may be largely inert, the star formation being dominated by cosmological accretion. Time lags between gas accretion and star formation may also reduce the apparent SFEgas, as may galaxy winds, which can expel most of the gas into the intergalactic medium. Hence, on global scales, XMPs could be H i-dominated, high-specific-SFR (≳10−10 yr−1), low-SFEgas (≲10−9 yr−1) systems, in which the total H i mass is likely not a good predictor of the total H2 mass, nor of the SFR.
Accounting for transgenerational effects of toxicant exposure in population models alters the predicted long-term population status

Abstract Acute environmental stressors such as short-term exposure to pollutants can have lasting effects on organisms, potentially impacting future generations. Parental exposure to toxicants can result in changes to the epigenome (e.g., DNA methylation) that are passed down to subsequent, unexposed generations. However, it is difficult to gauge the cumulative population-scale impacts of epigenetic effects from laboratory experiments alone. Here, we developed a size- and age-structured delay-coordinate population model to evaluate the long-term consequences of epigenetic modifications on population sustainability. The model emulated changes in growth, mortality, and fecundity in the F0, F1, and F2 generations observed in experiments in which larval Menidia beryllina were exposed to environmentally relevant concentrations of bifenthrin (Bif), ethinylestradiol (EE2), levonorgestrel (LV), or trenbolone (TB) in the parent generation (F0) and reared in clean water up to the F2 generation. Our analysis suggests potentially dramatic population-level effects of repeated, chronic exposures of early-life stage fish that are not captured by models not accounting for those effects. Simulated exposures led to substantial declines in population abundance (LV and Bif) or near-extinction (EE2 and TB) with the exact trajectory and timeline of population decline dependent on the combination of F0, F1, and F2 effects produced by each compound. Even acute one-time exposures of each compound led to declines and recovery over multiple years due to lagged epigenetic effects. These results demonstrate the potential for environmentally relevant concentrations of commonly used compounds to impact the population dynamics and sustainability of an ecologically relevant species and model organism.
The nuclear cluster of the Milky Way: our primary testbed for the interaction of a dense star cluster with a massive black hole

This article intends to provide a concise overview, from an observational point-of-view, of the current state of our knowledge of the most relevant properties of the Milky Wayʼs nuclear star cluster (MWNSC). The MWNSC appears to be a typical specimen of nuclear star clusters, which are found at the centers of the majority of all types of galaxies. Nuclear clusters represent the densest and most massive stellar systems in the present-day Universe and frequently coexist with central massive black holes. They are therefore of prime interest for studying stellar dynamics, and the MWNSC is the only one that allows us to obtain data on milli-parsec scales. After discussing the main observational constraints, we start with a description of the overall structure and kinematics of the MWNSC, then focus on a comparison to extragalactic systems, summarize the properties of the young, massive stars in the immediate environment of the Milky Wayʼs central black hole, Sagittarius A*, and finally focus on the dynamics of stars orbiting the black hole at distances of a few to a few tens of milli parsecs.
Pulse-phase-resolved spectroscopy of continuum and reflection in SAX J1808.4-3658

We perform phase-resolved spectroscopy of the accreting millisecond pulsar, SAX J1808.4−3658, during the slow-decay phase of the 2002 outburst. Simple phenomenological fits to Rossi X-ray Timing Explorer Proportional Counter Array data reveal a pulsation in the iron line at the spin frequency of the neutron star. However, fitting more complex spectral models reveals a degeneracy between iron-line pulsations and changes in the underlying hotspot blackbody temperature with phase. By comparing with the variations in reflection continuum, which are much weaker than the iron-line variations, we infer that the iron line is not pulsed. The observed spectral variations can be explained by variations in blackbody temperature associated with rotational Doppler shifts at the neutron star surface. By allowing blackbody temperature to vary in this way, we also find a larger phase shift between the pulsations in the Comptonized and blackbody components than has been seen in previous work. The phase shift between the pulsation in the blackbody temperature and normalization is consistent with a simple model where the Doppler shift is maximized at the limb of the neutron star, ∼90° prior to maximization of the hotspot projected area.
College Students’ Perceptions of Relevance, Personal Interest, and Task Value

Abstract This study aimed to explore undergraduates’ perceptions of relevance in conjunction with two associated constructs, personal interest, and task value. To unearth these perceptions, American (n = 104) and Dutch (n = 79) students completed the Conceptualization of Relevance Task (CoRT). This task required them to: (a) select a graphic that best represented their view of the interplay of relevance, personal interest, and task value; (b) justify their selection and exemplify it with a personal experience (c) define each of these terms. We scored the quality and consistency between students’ graphic selection and their justification and exemplification of that selection using a 0–2 rubric. The definitions students wrote for each term were subjected to content analysis. Among the major contributions of this study was its demonstration of the merit of examining laypersons’ views of relevance; the finding that students conceived of relevance as multidimensional and both externally and internally influenced; and the noting of parallels between the views of these non-experts and those of experts in the field of motivation regarding the nature of relevance. Implications for future research and practice are forwarded.
Large-scale normal fluid circulation in helium superflows

We perform fully-coupled numerical simulations of helium II pure superflows in a channel, with vortex- line density typical of experiments. Peculiar to our model is the computation of the back-reaction of the superfluid vortex motion on the normal fluid and the presence of solid boundaries. We recover the uniform vortex-line density experimentally measured employing second sound resonators and we show that pure superflow in helium II is associated with a large-scale circulation of the normal fluid which can be detected using existing particle-tracking visualization techniques.
Confinement-induced metal-to-insulator transition in strained LaNiO3/LaAlO3 superlattices

Using density functional theory calculations including a Hubbard U termwe explore the effect of strain and confinement on the electronic groundstate of superlattices containing the band insulator LaAlO3 and thecorrelated metal LaNiO3. Besides a suppression of holes at the apicaloxygen, a central feature is the asymmetric response to strain in singleunit cell superlattices: For tensile strain a band gap opens due tocharge disproportionation at the Ni sites with two distinct magneticmoments of 1.45 mu(B) and 0.71 mu(B). Under compressive stain, chargedisproportionation is nearly quenched and the band gap collapses due tooverlap of d(3z2-r2) bands through a semimetallic state. This asymmetryin the electronic behavior is associated with the difference inoctahedral distortions and rotations under tensile and compressivestrain. The ligand hole density and the metallic state are quicklyrestored with increasing thickness of the (LaAlO3)(n)/(LaNiO3)(n)
The EFT of Large Scale Structures at all redshifts: analytical predictions for lensing

We study the prediction of the Effective Field Theory of Large Scale Structures (EFTofLSS) for the matter power spectrum at different redshifts. In previous work, we found that the two-loop prediction can match the nonlinear power spectrum measured from N-body simulations at redshift zero within approximately 2% up to k∼ 0.6 h Mpc-1 after fixing a single free parameter, the so-called “speed of sound”. We determine the time evolution of this parameter by matching the EFTofLSS prediction to simulation output at different redshifts, and find that it is well-described by a fitting function that only includes one additional parameter. After the two free parameters are fixed, the prediction agrees with nonlinear data within approximately 2% up to at least k∼ 1 h Mpc-1 at z⩾ 1, and also within approximately 5% up to k∼ 1.2 h Mpc-1 at z=1 and k∼ 2.3 h Mpc-1 at z=3, a major improvement with respect to other perturbative techniques. We also develop an accurate way to estimate where the EFTofLSS predictions at different loop orders should fail, based on the sizes of the next-order terms that are neglected, and find agreement with the actual comparisons to data. Finally, we use our matter power spectrum results to perform analytical calculations of lensing potential power spectra corresponding to both CMB and galaxy lensing. This opens the door to future direct applications of the EFTofLSS to observations of gravitational clustering on cosmic scales.
Preserving Local Gauge Invariance with t-Channel Regge Exchange

Photo- and electroproduction of mesons off baryons provide arguably the most direct routes to information about hadronic structure. At high energies, where multimeson production abounds, such processes can be described economically in terms of pomeron and Reggetrajectory exchanges [1–3]. At lower energies, singlemeson production provides a direct avenue for baryon spectroscopy [4], with theoretical descriptions that attempt to model the contributing mechanisms as detailed as possible in terms of Feynman-type exchange processes. The present work is concerned with an intermediateenergy transition region, where one starts within the Feynman-type picture and replaces some exchanges by Regge trajectories in an attempt to bring the economic features of the high-energy Regge approach to bear in the more traditional Feynman framework. Specifically, we will apply such a hybrid framework to the generic electromagnetic production process depicted in Fig. 1 of a meson (m) off an initial baryon (b) going over into a final baryon (b ′ ), i.e.,
EVOLVING GRAVITATIONALLY UNSTABLE DISKS OVER COSMIC TIME: IMPLICATIONS FOR THICK DISK FORMATION

Observations of disk galaxies at z ∼ 2 have demonstrated that turbulence driven by gravitational instability can dominate the energetics of the disk. We present a one-dimensional simulation code, which we have made publicly available, that economically evolves these galaxies from z ∼ 2 to z ∼ 0 on a single CPU in a matter of minutes, tracking column density, metallicity, and velocity dispersions of gaseous and multiple stellar components. We include an H2-regulated star formation law and the effects of stellar heating by transient spiral structure. We use this code to demonstrate a possible explanation for the existence of a thin and thick disk stellar population and the age–velocity-dispersion correlation of stars in the solar neighborhood: the high velocity dispersion of gas in disks at z ∼ 2 decreases along with the cosmological accretion rate, while at lower redshift the dynamically colder gas forms the low velocity dispersion stars of the thin disk.
A DEEP CHANDRA OBSERVATION OF OXYGEN-RICH SUPERNOVA REMNANT B0049–73.6 IN THE SMALL MAGELLANIC CLOUD

We report on the initial results from our deep Chandra observation (450 ks) of O-rich supernova remnant (SNR) B0049–73.6 in the Small Magellanic Cloud. We detect small metal-rich ejecta features extending out to the outermost boundary of B0049–73.6, which were not seen in the previous data with a shorter exposure. The central nebula is dominated by emission from reverse-shocked ejecta material enriched in O, Ne, Mg, and Si. O-rich ejecta distribution is relatively smooth throughout the central nebula. In contrast, the Si-rich material is highly structured. These results suggest that B0049–73.6 was produced by an asymmetric core-collapse explosion of a massive star. The estimated abundance ratios among these ejecta elements are in plausible agreement with the nucleosynthesis products from the explosion of a 13–15 M☉ progenitor. The central ring-like (in projection) ejecta nebula extends to ∼9 pc from the SNR center. This suggests that the contact discontinuity may be located at a further distance from the SNR center than the previous estimate. We estimate the Sedov age of ∼17,000 yr and an explosion energy of E0 ∼1.7 × 1051 erg for B0049–73.6. We place a stringent upper limit on the 2–7 keV band luminosity of LX ∼ 8.5 × 1031 erg s−1 for the embedded compact stellar remnant at the center of B0049–73.6.
The Impact of Price Preciseness, Price Reduction, and Lay Rationalism on Travelers’ Perceptions of Deal Attractiveness, Purchase Intention, and Choice

This research investigated the role of price preciseness (rounded vs. precise) in perceiving deal attractiveness, purchase intention, and choice in travel decision-making. Two competing hypotheses (price association vs. fluency) were proposed. Across five empirical studies, we found that the perceived attractiveness of a price promotion deal, along with purchase intention and relative preference, were higher when the original price was presented in a rounded (vs. precise) format (Studies 1A, 1B, and 3). This finding supports the price association-based explanation rather than the fluency-based explanation. In addition, the results were replicated in a consequential choice setting (Study 2). We further demonstrated that the effect of the price rounding is stronger for those with high (vs. low) lay rationalism, suggesting its moderating role (Study 4). The empirical findings of the current research have theoretical implications for various fields, including the behavioral pricing of travel and tourism, and practical implications for practitioners.
Action Principle and Dynamic Ensemble Theory for Non-equilibrium Markov Chains

An overarching action principle, the principle of minimal free action, exists for ergodic Markov chain dynamics. Using this principle and the Detailed Fluctuation Theorem, we construct a dynamic ensemble theory for non-equilibrium steady states (NESS) of Markov chains, which is in full analogy with equilibrium canonical ensemble theory. Concepts such as energy, free energy, Boltzmann macro-sates, entropy, and thermodynamic limit all have their dynamic counterparts. For reversible Markov chains, minimization of Boltzmann free action yields thermal equilibrium states, and hence provide a dynamic justification of the principle of minimal free energy. For irreversible Markov chains, minimization of Boltzmann free action selects the stable NESS, and determines its macroscopic properties, including entropy production. A quadratic approximation of free action leads to linear-response theory with reciprocal relations built-in. Hence, in so much as non-equilibrium phenomena can be modeled as Markov processes, minimal free action serves as a basic principle for both equilibrium and non-equilibrium statistical physics.
Measuring music-genre preferences: Discrepancies between direct and indirect methods

Preferences are essential in explaining consumer choice and have been studied from different standpoints. Some empirical studies aimed at measuring music preferences have used direct procedures (i.e., list of genres), while other studies have used indirect measures (i.e., listening to excerpts of music). This article focuses on analyzing music-genre preferences to identify whether they differ depending on the type of measure used (direct vs. indirect), studying their consistency. A survey was conducted among 753 individuals. The results highlight not only the discrepancies of using one measure or another but also the relevance of familiarity and experience, associated with individuals’ endowment of cultural capital. Findings explain the (in)consistency of reported preferences through direct and indirect means. All in all, the research suggests that direct and indirect methods to measure music preferences may be capturing different dimensions.
Structural and magnetic characterisation of iron oxyselenides Ce2O2Fe2OSe2 and Nd2O2Fe2OSe2

We present here an investigation of the magnetic ordering in the Mott insulating oxyselenide materials Ln2O2Fe2OSe2 (Ln = Ce, Nd). Neutron powder diffraction data are consistent with a non-collinear multi-k ordering on the iron sublattice structure and analysis indicates a reduced magnetic correlation length perpendicular to the [Fe2O]2+ layers. The magnetic role of the Ln3+ cations is investigated and Ce3+ moments are found to order for T < 16 K.
Bolometric luminosities and Eddington ratios of X-ray selected active galactic nuclei in the XMM-COSMOS survey

Bolometric luminosities and Eddington ratios of both X-ray selected broad-line (Type-1) and narrow-line (Type-2) active galactic nuclei (AGN) from the XMM–Newton survey in the Cosmic Evolution Survey field are presented. The sample is composed of 929 AGN (382 Type-1 AGN and 547 Type-2 AGN) and it covers a wide range of redshifts, X-ray luminosities and absorbing column densities. About 65 per cent of the sources are spectroscopically identified as either Type-1 or Type-2 AGN (83 and 52 per cent, respectively), while accurate photometric redshifts are available for the rest of the sample. The study of such a large sample of X-ray selected AGN with a high-quality multiwavelength coverage from the far-infrared (now with the inclusion of Herschel data at 100 and 160 μm) to the optical–ultraviolet allows us to obtain accurate estimates of bolometric luminosities, bolometric corrections and Eddington ratios. The kbol- Lbol relations derived in this work are calibrated for the first time against a sizable AGN sample, and rely on observed redshifts, X-ray luminosities and column density distributions. We find that kbol is significantly lower at high Lbol with respect to previous estimates by Marconi et al. and Hopkins et al. Black hole (BH) masses and Eddington ratios are available for 170 Type-1 AGN, while BH masses for Type-2 AGN are computed for 481 objects using the BH mass–stellar mass relation and the morphological information. We confirm a trend between kbol and λEdd, with lower hard X-ray bolometric corrections at lower Eddington ratios for both Type-1 and Type-2 AGN. We find that, on average, the Eddington ratio increases with redshift for all types of AGN at any given MBH, while no clear evolution with redshift is seen at any given Lbol.
Golgi Phosphoprotein 3 Mediates Radiation-Induced Bystander Effect via ERK/EGR1/TNF-α Signal Axis

The radiation-induced bystander effect (RIBE), an important non-targeted effect of radiation, has been proposed to be associated with irradiation-caused secondary cancers and reproductive damage beyond the irradiation-treated area after radiotherapy. However, the mechanisms for RIBE signal(s) regulation and transduction are not well understood. In the present work, we found that a Golgi protein, GOLPH3, was involved in RIBE transduction. Knocking down GOLPH3 in irradiated cells blocked the generation of the RIBE, whereas re-expression of GOLPH3 in knockdown cells rescued the RIBE. Furthermore, TNF-α was identified as an important intercellular signal molecule in the GOLPH3-mediated RIBE. A novel signal axis, GOLPH3/ERK/EGR1, was discovered to modulate the transcription of TNF-α and determine the level of released TNF-α. Our findings provide new insights into the molecular mechanism of the RIBE and a potential target for RIBE modulation.