Miracle-dz/UniFAR-FTUs huggingface dataset:
STAR FORMATION ASSOCIATED WITH THE SUPERNOVA REMNANT IC443

We have performed submillimeter and millimeter observations in CO lines toward supernova remnant (SNR) IC443. The CO molecular shell coincides well with the partial shell of the SNR detected in radio continuum observations. Broad emission lines and three 1720 MHz OH masers were detected in the CO molecular shell. The present observations have provided further evidence in support of the interaction between the SNR and the adjoining molecular clouds (MCs). The total mass of the MCs is 9.26 × 103 M☉. The integrated CO line intensity ratio for the whole MC is between 0.79 and 3.40. The average value is 1.58, which is much higher than previous measurements of individual Galactic MCs. Higher line ratios imply that shocks have driven into the MCs. We conclude that high is identified as a good signature of the SNR–MC interacting system. Based on the IRAS Point Source Catalog and the Two Micron All Sky Survey near-infrared database, 12 protostellar object and 1666 young stellar object (YSO) candidates (including 154 classical T Tauri stars and 419 Herbig Ae/Be stars) are selected. In the interacting regions, the significant enhancement of the number of protostellar objects and YSOs indicates the presence of some recently formed stars. After comparing the characteristic timescales of star formation with the age of IC443, we conclude that the protostellar objects and YSO candidates are not triggered by IC443. For the age of the stellar winds shell, we have performed our calculation on the basis of a stellar wind shell expansion model. The results and analysis suggest that the formation of these stars may be triggered by the stellar winds of the IC443 progenitor.
Galaxy evolution in groups and clusters: star formation rates, red sequence fractions and the persistent bimodality

Using galaxy group/cluster catalogues created from the Sloan Digital Sky Survey Data Release 7, we examine in detail the specific star formation rate (SSFR) distribution of satellite galaxies and its dependence on stellar mass, host halo mass and halo-centric radius. All galaxies, regardless of central satellite designation, exhibit a similar bimodal SSFR distribution, with a strong break at SSFR ≈ 10−11 yr−1 and the same high SSFR peak; in no regime is there ever an excess of galaxies in the ‘green valley’. Satellite galaxies are simply more likely to lie on the quenched (‘red sequence’) side of the SSFR distribution. Furthermore, the satellite quenched fraction excess above the field galaxy value is nearly independent of galaxy stellar mass. An enhanced quenched fraction for satellites persists in groups with halo masses down to 3 × 1011 M⊙ and increases strongly with halo mass and towards halo centre. We find no detectable quenching enhancement for galaxies beyond ∼2 Rvir around massive clusters once these galaxies have been decomposed into centrals and satellites. These trends imply that (1) galaxies experience no significant environmental effects until they cross within ∼Rvir of a more massive host halo; (2) after this, star formation in active satellites continues to evolve in the same manner as active central galaxies for several Gyr; and (3) once begun, satellite star formation quenching occurs rapidly. These results place strong constraints on satellite-specific quenching mechanisms, as we will discuss further in companion papers.
DETERMINING THE LARGE-SCALE ENVIRONMENTAL DEPENDENCE OF GAS-PHASE METALLICITY IN DWARF GALAXIES

We study how the cosmic environment affects galaxy evolution in the universe by comparing the metallicities of dwarf galaxies in voids with dwarf galaxies in more dense regions. Ratios of the fluxes of emission lines, particularly those of the forbidden [O iii] and [S ii] transitions, provide estimates of a region’s electron temperature and number density. From these two quantities and the emission line fluxes [O ii] λ3727, [O iii] λ4363, and [O iii] λλ4959, 5007, we estimate the abundance of oxygen with the direct Te method. We estimate the metallicity of 42 blue, star-forming void dwarf galaxies and 89 blue, star-forming dwarf galaxies in more dense regions using spectroscopic observations from the Sloan Digital Sky Survey Data Release 7, as reprocessed in the MPA-JHU value-added catalog. We find very little difference between the two sets of galaxies, indicating little influence from the large-scale environment on their chemical evolution. Of particular interest are a number of extremely metal-poor dwarf galaxies that are less prevalent in voids than in the denser regions.
Eulerian dynamics with a commutator forcing II: Flocking

We continue our study of one-dimensional class of Euler equations, introduced in [ 11 ], driven by a forcing with a commutator structure of the form \begin{document} $[{\mathcal L}_φ, u](ρ)$ \end{document} , where \begin{document} $u$ \end{document} is the velocity field and \begin{document} ${\mathcal L}_φ$ \end{document} belongs to a rather general class of convolution operators depending on interaction kernels \begin{document} $φ$ \end{document} . In this paper we quantify the large-time behavior of such systems in terms of fast flocking, for two prototypical sub-classes of kernels: bounded positive \begin{document} $φ$ \end{document} 's, and singular \begin{document} $φ(r) = r^{-(1+α)}$ \end{document} of order \begin{document} $α∈ [1, 2)$ \end{document} associated with the action of the fractional Laplacian \begin{document} ${\mathcal L}_φ=-(-\partial_{xx})^{α/2}$ \end{document} . Specifically, we prove fast velocity alignment as the velocity \begin{document} $u(·, t)$ \end{document} approaches a constant state, \begin{document} $u \to \bar{u}$ \end{document} , with exponentially decaying slope and curvature bounds \begin{document} $|{u_x}( \cdot ,t){|_\infty } + |{u_{xx}}( \cdot ,t){|_\infty }\lesssim{e^{ - \delta t}}$ \end{document} . The alignment is accompanied by exponentially fast flocking of the density towards a fixed traveling state \begin{document} $ρ(·, t) -{ρ_{∞}}(x -\bar{u} t) \to 0$ \end{document} .
Orbital migration models under test

Abstract Planet-disk interaction predicts a change in the orbital elements of an embedded planet. Through linear and fully hydrodynamical studies it has been found that migration is typically directed inwards. Hence, this migration process gives natural explanation for the presence of the ’hot’ planets orbiting close to the parent star, and it plays a mayor role in explaining the formation of resonant planetary systems. However, standard migration models for locally isothermal disks indicate a too rapid inward migration for small mass planets, and a large number of massive planets are found very far away from the star. Recent studies, including more complete disk physics, have opened up new paths to slow down or even reverse migration. The new findings on migration are discussed and connected to the observational properties of planetary systems.
X-RAY DIPS IN THE SEYFERT GALAXY FAIRALL 9: COMPTON-THICK “COMETS” OR A FAILED RADIO GALAXY?

We investigate the spectral variability of the Seyfert galaxy Fairall 9 using almost 6 years of monitoring with the Rossi X-ray Timing Explorer with an approximate time resolution of 4 days. We discover the existence of pronounced and sharp dips in the X-ray flux, with a rapid decline of the 2–20 keV flux of a factor of two or more followed by a recovery to pre-dip fluxes after ∼10 days. These dips skew the flux distribution away from the commonly observed lognormal distribution. Dips may result from the eclipse of the central X-ray source by broad-line region clouds, as has recently been found in NGC 1365 and Mrk 766. Unlike these other examples, however, the clouds in Fairall 9 would need to be Compton-thick, and the non-dip state is remarkably free of any absorption features. A particularly intriguing alternative is that the accretion disk is undergoing the same cycle of disruption/ejection as seen in the accretion disks of broad-line radio galaxies such as 3C120 but, for some reason, fails to create a relativistic jet. This suggests that a detailed comparison of Fairall 9 and 3C120 with future high-quality data may hold the key to understanding the formation of relativistic jets in active galactic nucleus.
The Evolution of Cluster Early-Type Galaxies over the Past 8 Gyr

We present the Fundamental Plane (FP) of early-type galaxies in the clusters of galaxies RXJ1415.1+3612 at z=1.013. This is the first detailed FP investigation of cluster early-type galaxies at redshift z=1. The distant cluster galaxies follow a steeper FP relation compared to the local FP. The change in the slope of the FP can be interpreted as a mass-dependent evolution. To analyse in more detail the galaxy population in high redshift galaxy clusters at 0.8 2x10^{11}M_{\sun}) the bulk of their stellar populations have been formed earlier z_{form}>~1.6. Our results confirm previous findings by Jorgensen et al. This suggests that the less massive galaxies in the distant clusters have much younger stellar populations than their more massive counterparts. One explanation is that low-mass cluster galaxies have experienced more extended star formation histories with more frequent bursts of star formation with shorter duration compared to the formation history of high-mass cluster galaxies.
Quantum Ising chains with boundary fields

We present a detailed study of the finite one-dimensional quantum Ising chain in a transverse field in the presence of boundary magnetic fields coupled with the order-parameter spin operator. We consider two magnetic fields located at the boundaries of the chain that have the same strength and that are aligned in the same or in the opposite direction. We derive analytic expressions for the gap in all phases for large values of the chain length L, as a function of the boundary field strength. We also investigate the behaviour of the chain in the quantum ferromagnetic phase for oppositely aligned fields, focusing on the magnet-to-kink transition that occurs at a finite value of the magnetic field strength. At this transition we compute analytically the finite-size crossover functions for the gap, the magnetisation profile, the two-point correlation function, and the density of fermionic modes. As the magnet-to-kink transition is equivalent to the wetting transition in two-dimensional classical Ising models, our results provide new analytic predictions for the finite-size behaviour of Ising systems in a strip geometry at this transition.
Quantitative plant taphonomy: the cosmopolitan Mesozoic fern Weichselia reticulata as a case study

A quantitative approach to plant taphonomy focusing on preservation type and fragment size is tested by comparing 3338 Weichselia reticulata fragments from 25 Lower Cretaceous localities of different ages and depositional environments. Moreover, palaeobiological insights are also obtained from the taphonomic analyses. In the case of the specimens of Weichselia reticulata included in this work, charred remains are the most frequent preservation type, and are the smallest and most homogeneous in size, probably due to the fragmentation of the fronds while burning and to the fact that burnt fragments are more fragile and break easily during the initial abrasion and attrition produced by transport. The size of charred fragments varies depending on the depositional environment, suggesting that biostratinomic processes, and not fire temperature, are the main cause for size differences, and providing valuable insight into the distance the remains might have travelled from production to final deposition. The taphonomic analysis suggests that Weichselia reticulata is allochthonous in all the localities analysed, and that its habitat would have been prone to fire and not far from freshwater systems. This case study shows promising results that can be implemented on different plant groups and chronostratigraphic ages, allowing for the proposal of a taphonomic model.
A first study of the galaxy HRG 2304 and its companion AM 1646-795 (NED01)

Aims. We report the first study of the peculiar ring-like galaxy HRG 2304 (NED02), which was previously classified as a ring galaxy with an elliptical smooth ring. This object was selected to prove that it is a candidate for the Solitaire-type ring galaxies in an early stage of ring formation. The main goal of this work is to provide the spectral characteristics of the current object and its companion AM 1646-795 (NED01). Methods. The study is based on spectroscopic observations in the optical band to highlight the characteristics of this interacting galaxy. To investigate the star formation history of HRG 2304 we used the stellar population synthesis code STARLIGHT. The direct V and B broad band images were used to enhance some fine structures. Results. Along the entire long-slit signal, the spectra of HRG 2304 and its companion resemble that of an early-type galaxy. We estimated a heliocentric systemic redshift of z = 0.0415, corresponding to heliocentric velocities of 12 449 km s −1 for HRG 2304 (NED02) and 12 430 km s −1 for AM1646-795 (NED01). The spatial variation in the contribution of the stellar population components for both objects are dominated by an old stellar population 2 × 10 9 < t ≤ 13 × 10 9 yr. The observed radial-velocity distribution and the fine structures around HRG 2304 suggest an ongoing tidal interaction of both galaxies. Conclusions. The spectroscopic results and the morphological peculiarities of HRG 2304 can be adequately interpreted as an ongoing interaction with the companion galaxy. Both galaxies are early-type, the companion is elliptical, and the smooth distribution of the material around HRG 2304 and its off-center nucleus in the direction of AM1646-795 (NED01) characterize HRG 2304 as a Solitairetype galaxy candidate in an early stage of ring formation.
Enhancement of thermal photon production in event-by-event hydrodynamics

Thermal photon emission is widely believed to reflect properties of the earliest, hottest evolution stage of the medium created in ultrarelativistic heavy-ion collisions. Previous computations of photon emission have been carried out using a hydrodynamical medium description with smooth, averaged initial conditions. Recently, more sophisticated hydrodynamical models that calculate observables by averaging over many evolutions with event-by-event fluctuating initial conditions (ICs) have been developed. Given their direct connection to the early time dynamics, thermal photon emission appears to be an ideal observable to probe fluctuations in the medium initial state. In this work, we demonstrate that including fluctuations in the ICs may lead to an enhancement of the thermal photon yield of about a factor of 2 in the region 2<p{sub T}<4 GeV/c (where thermal photon production dominates the direct photon yield) compared to a scenario using smooth, averaged ICs. Consequently, a much better agreement with PHENIX data is found. This can be understood in terms of the strong temperature dependence of thermal photon production, translating into a sensitivity to the presence of hotspots in an event and thus establishing thermal photons as a suitable probe to characterize IC fluctuations.
DIFFUSE HARD X-RAY EMISSION IN STARBURST GALAXIES AS SYNCHROTRON FROM VERY HIGH ENERGY ELECTRONS

The origin of the diffuse hard X-ray (2–10 keV) emission from starburst galaxies is a long-standing problem. We suggest that synchrotron emission of 10–100 TeV electrons and positrons (e±) can contribute to this emission, because starbursts have strong magnetic fields. We consider three sources of e± at these energies: (1) primary electrons directly accelerated by supernova remnants, (2) pionic secondary e± created by inelastic collisions between cosmic ray (CR) protons and gas nuclei in the dense interstellar medium of starbursts, and (3) pair e± produced between the interactions between 10 and 100 TeV γ-rays and the intense far-infrared (FIR) radiation fields of starbursts. We create one-zone steady-state models of the CR population in the Galactic center (R ⩽ 112 pc), NGC 253, M82, and Arp 220's nuclei, assuming a power-law injection spectrum for electrons and protons. We consider different injection spectral slopes, magnetic field strengths, CR acceleration efficiencies, and diffusive escape times, and include advective escape, radiative cooling processes, and secondary and pair e±. We compare these models to extant radio and GeV and TeV γ-ray data for these starbursts, and calculate the diffuse synchrotron X-ray and inverse Compton (IC) luminosities of these starbursts in the models which satisfy multiwavelength constraints. If the primary electron spectrum extends to ∼PeV energies and has a proton/electron injection ratio similar to the Galactic value, we find that synchrotron emission contributes 2%–20% of their unresolved, diffuse hard X-ray emission. However, there is great uncertainty in this conclusion because of the limited information on the CR electron spectrum at these high energies. IC emission is likewise a minority of the unresolved X-ray emission in these starbursts, from 0.1% in the Galactic center to 10% in Arp 220's nuclei, with the main uncertainty being the starbursts' magnetic field. We also model generic starbursts, including submillimeter galaxies, in the context of the FIR–X-ray relation, finding that anywhere between 0% and 16% of the total hard X-ray emission is synchrotron for different parameters, and up to 2% in the densest starbursts assuming an E−2.2 injection spectrum and a diffusive escape time of 10 Myr (E/3 GeV)−1/2 (h/100 pc). Neutrino observations by IceCube and TeV γ-ray data from HESS, VERITAS, and CTA can further constrain the synchrotron X-ray emission of starbursts. Our models do not constrain the possibility of hard, second components of primary e± from sources like pulsars in starbursts, which could enhance the synchrotron X-ray emission further.
ROTATIONAL SPLITTING OF PULSATION MODES

Mode splittings produced by uniform rotation and a particular form of differential rotation are computed for two-dimensional rotating 10 M☉ zero-age main sequence stellar models. The change in the character of the mode splitting is traced as a function of uniform rotation rate, and it is found that only relatively slow rotation rates are required before the mode splitting becomes asymmetric about the azimuthally symmetric (m = 0) mode. Increased rotation produces a progressively altered pattern of the individual modes with respect to each other. Large mode splittings begin to overlap with the mode splittings produced by different radial and latitudinal modes at relatively low rotation rates. The mode-splitting pattern for the differentially rotating stars we model is different than that for uniformly rotating stars, making the mode splitting a possible discriminant of the internal angular momentum distribution if one assumes that the formidable challenge of mode identification can be overcome.
CLUSTER MORPHOLOGIES AND MODEL-INDEPENDENT YSZ ESTIMATES FROM BOLOCAM SUNYAEV–ZEL'DOVICH IMAGES

We present initial results from our ongoing program to image the Sunyaev–Zel'dovich (SZ) effect in galaxy clusters at 143 GHz using Bolocam; five clusters and one blank field are described in this manuscript. The images have a resolution of 58 arcsec and a radius of ≃6–7 arcmin, which is approximately r500–2r500 for these clusters. We effectively high-pass filter our data in order to subtract noise sourced by atmospheric fluctuations, but we are able to obtain unbiased images of the clusters by deconvolving the effects of this filter. The beam-smoothed rms is ≃10 μKCMB in these images; with this sensitivity, we are able to detect the SZ signal to beyond r500 in binned radial profiles. We have fit our images to beta and Nagai models, fixing spherical symmetry or allowing for ellipticity in the plane of the sky, and we find that the best-fit parameter values are in general consistent with those obtained from other X-ray and SZ data. Our data show no clear preference for the Nagai model or the beta model due to the limited spatial dynamic range of our images. However, our data show a definitive preference for elliptical models over spherical models, quantified by an F ratio of ≃20 for the two models. The weighted mean ellipticity of the five clusters is ϵ = 0.27 ± 0.03, consistent with results from X-ray data. Additionally, we obtain model-independent estimates of Y500, the integrated SZ y-parameter over the cluster face to a radius of r500, with systematics-dominated uncertainties of ≃10%. Our Y500 values, which are free from the biases associated with model-derived Y500 values, scale with cluster mass in a way that is consistent with both self-similar predictions and expectations of a ≃10% intrinsic scatter.
Propagating edge states in strained honeycomb lattices

We investigate the helically-propagating edge states associated with pseudo-Landau levels in strained honeycomb lattices. We exploit chiral symmetry to derive a general criterion for the existence of these propagating edge states in the presence of only nearest-neighbour hoppings and we verify our criterion using numerical simulations of both uni-axially and trigonally strained honeycomb lattices. We show that the propagation of the helical edge state can be controlled by engineering the shape of the edges. Sensitivity to chiral-symmetry-breaking next-nearest-neighbour hoppings is assessed. Our result opens up an avenue toward the precise control of edge modes through manipulation of the edge shape.
Safety of an aqueous ethanolic extract of Labisia pumila as a novel food pursuant to Regulation (EU) 2015/2283

Abstract Following a request from the European Commission, the EFSA Panel on Nutrition, Novel Foods and Food Allergens (NDA) was asked to deliver an opinion on aqueous extract of Labisia pumila as a novel food (NF) pursuant to Regulation (EU) 2015/2283. The NF is a standardised hydroalcoholic extract from a dried whole plant (including roots) of L. pumila, mixed with maltodextrin (as a drying aid), and proposed by the applicant to be used as a food supplement in amounts up to 750 mg/day. The target population is the general adult population, except pregnant and lactating women. The major constituents of this NF are carbohydrates (up to 85.5%), with a smaller amount of proteins (up to 6.5%), gallic acid (up to 3.7%) and fats (up to 1.6%). The Panel considers that taking into account the composition of the NF and the proposed conditions of use, consumption of the NF is not nutritionally disadvantageous. The provided genotoxicity studies do not raise concerns about the genotoxicity of the NF. Based on the available toxicological data, the Panel considers an intake of up to 5 mg/kg body weight per day as safe. For the target population, this level corresponds to 350 mg/day, which is lower than the use level proposed by the applicant. The Panel concludes that the NF is safe for the target population up to 350 mg/day.
Disparities in mobile phone use among adults with type 2 diabetes participating in clinical trials 2017–2021

Abstract Despite smartphone ownership becoming ubiquitous, it is unclear whether and where disparities persist in experience using health apps. In 2 diverse samples of adults with type 2 diabetes collected 2017–2018 and 2020–2021, we examined adjusted disparities in smartphone ownership and health app use by age, gender, race, education, annual household income, health insurance status, health literacy, and hemoglobin A1c. In the earlier sample (N = 422), 87% owned a smartphone and 49% of those had ever used a health app. Participants with lower income or limited health literacy had ≥50% lower odds of owning a smartphone. Comparatively, in the later sample (N = 330), almost all participants (98%) owned a smartphone and 70% of those had ever used a health app; however, disparities in health app use closely mirrored disparities in smartphone ownership from 2017 to 2018. Our findings suggest device ownership is necessary but insufficient for assuming people will use apps to support their health.