Miracle-dz/UniFAR-FTUs huggingface dataset:
A new population of recently quenched elliptical galaxies in the SDSS

We use the Sloan Digital Sky Survey to investigate the properties of massive elliptical galaxies in the local Universe (z\leq0.08) that have unusually blue optical colors. Through careful inspection, we distinguish elliptical from non-elliptical morphologies among a large sample of similarly blue galaxies with high central light concentrations (c_r\geq2.6). These blue ellipticals comprise 3.7 per cent of all c_r\geq2.6 galaxies with stellar masses between 10^10 and 10^11 h^{-2} {\rm M}_{\sun}. Using published fiber spectra diagnostics, we identify a unique subset of 172 non-star-forming ellipticals with distinctly blue urz colors and young (< 3 Gyr) light-weighted stellar ages. These recently quenched ellipticals (RQEs) have a number density of 2.7-4.7\times 10^{-5}\,h^3\,{\rm Mpc}^{-3} and sufficient numbers above 2.5\times10^{10} h^{-2} {\rm M}_{\sun} to account for more than half of the expected quiescent growth at late cosmic time assuming this phase lasts 0.5 Gyr. RQEs have properties that are consistent with a recent merger origin (i.e., they are strong `first-generation' elliptical candidates), yet few involved a starburst strong enough to produce an E+A signature. The preferred environment of RQEs (90 per cent reside at the centers of < 3\times 10^{12}\,h^{-1}{\rm M}_{\sun} groups) agrees well with the `small group scale' predicted for maximally efficient spiral merging onto their halo center and rules out satellite-specific quenching processes. The high incidence of Seyfert and LINER activity in RQEs and their plausible descendents may heat the atmospheres of small host halos sufficiently to maintain quenching.
FORMATION HISTORY OF METAL-POOR HALO STARS WITH THE HIERARCHICAL MODEL AND THE EFFECT OF INTERSTELLAR MATTER ACCRETION ON THE MOST METAL-POOR STARS

We investigate star formation and chemical evolution in the early universe by considering the merging history of the Galaxy in the Λ cold dark matter scenario according to the extended Press–Schechter theory. We give some possible constraints from comparisons with observation of extremely metal-poor (EMP) stars, made available by the recent large-scale surveys and by the follow-up high-resolution spectroscopy. We demonstrate that (1) the hierarchical structure formation can explain the characteristics of the observed metallicity distribution function including a break around [Fe/H] = −4; (2) a high-mass initial mass function (IMF) of peak mass ∼10 M☉ with the contribution of binaries, derived from the statistics of carbon-enhanced EMP stars, predicts the frequency of low-mass survivors consistent with the number of EMP stars observed for −4 ≲ [Fe/H] ≲ −2.5; (3) the stars formed from primordial gas before the first supernova (SN) explosions in their host mini-halos are assigned to the hyper metal-poor (HMP) stars with [Fe/H] ∼ −5; and (4) there is no indication of significant changes in the IMF and the binary contribution at metallicities −4 ≳ [Fe/H] ≳ −2.5, or even larger, as far as the field stars of the Galactic halo are concerned. We further study the effects of surface pollution through the accretion of interstellar matter (ISM) along the chemical and dynamical evolution of the Galaxy for low-mass Population III and EMP survivors. Because of the shallower potential of smaller halos, the accretion of ISM in the mini-halos in which these stars were born dominates the surface metal pollution. This can account for the surface iron abundances as observed for the HMP stars if the cooling and concentration of gas in their birth mini-halos are taken into account. We also study the feedback effect from the very massive Population III stars. The metal pre-pollution by pair-instability SNe is shown to be compatible with the observed lack of their nucleosynthetic signatures when some positive feedback on gas cooling works and changes the IMF from being very massive to being high mass.
Tracing the general structure of Galactic molecular clouds using Planck data: I. The Perseus region as a test case

We present an analysis of probability distribution functions (pdfs) of column density in different zones of the star-forming region Perseus and its diffuse environment based on the map of dust opacity at 353 GHz available from the Planck archive. The pdf shape can be fitted by a combination of a lognormal function and an extended power-law tail at high densities, in zones centred at the molecular cloud Perseus. A linear combination of several lognormals fits very well the pdf in rings surrounding the cloud or in zones of its diffuse neighbourhood. The slope of the mean density scaling law hρiL ∝ L � is steep (α = −1.93) in the former case and rather shallow (α = −0.77 ± 0.11) in the rings delineated around the cloud. We interpret these findings as signatures of two distinct physical regimes: i) a gravoturbulent one which is characterized by nearly linear scaling of mass and practical lack of velocity scaling; and ii) a predominantly turbulent one which is best described by steep velocity scaling and by invariant for compressible turbulence hρiLu 3 /L, describing a scale-independent flux of the kinetic energy per unit volume through turbulent cascade. The gravoturbulent spatial domain can be identified with the molecular cloud Perseus while a relatively sharp transition to predominantly turbulent regime occurs in its vicinity.
NLTE strontium abundance in a sample of extremely metal poor stars and the Sr/Ba ratio in the early Galaxy

Context. Heavy element abundances in extremely metal-poor stars provide strong constraints on the processes of forming these elements in the first stars. Aims. We attempt to determine precise abundances of strontium in a homogeneous sample of extremely metal-poor stars. Methods. The abundance of strontium in 54 very or extremely metal-poor stars, was redetermined by abandoning the local thermodynamic equilibrium (LTE) hypothesis, and fitting non-LTE (NLTE) profiles to the observed spectral lines. The corrected Sr abundances and previously obtained NLTE Ba abundances are compared to the predictions of several hypothetical formation processes for the lighter neutron-capture elements. Results. Our NLTE abundances confirm the previously determined huge scatter of the strontium abundance in low metallicity stars. This scatter is also found (and is even larger) at very low metallicities (i.e. early in the chemical evolution). The Sr abundance in the extremely metal-poor (EMP) stars is compatible with the main r-process involved in other processes (or by variations of the r-process), as we briefly discuss.
An axiomatic approach to Maxwell’s equations

This paper suggests an axiomatic approach to Maxwell’s equations. The basis of this approach is a theorem formulated for two sets of functions localized in space and time. If each set satisfies a continuity equation then the theorem provides an integral representation for each function. A corollary of this theorem yields Maxwell’s equations with magnetic monopoles. It is pointed out that the causality principle and the conservation of electric and magnetic charges are the most fundamental physical axioms underlying these equations. Another application of the corollary yields Maxwell’s equations in material media. The theorem is also formulated in the Minkowski space-time and applied to obtain the covariant form of Maxwell’s equations with magnetic monopoles and the covariant form of Maxwell’s equations in material media. The approach makes use of the infinite-space Green function of the wave equation and is therefore suitable for an advanced course in electrodynamics.
Parametrizing the time-variation of the ‘surface term’ of stellar p-mode frequencies: application to helioseismic data

The solar-cyle variation of acoustic mode frequencies has a frequency dependence related to the inverse mode inertia. The discrepancy between model predictions and measured oscillation frequencies for solar and solar-type stellar acoustic modes includes a significant frequency-dependent term known as the surface term that is also related to the inverse mode inertia. We parametrize both the surface term and the frequency variations for low-degree solar data from Birmingham Solar-Oscillations Network (BiSON) and medium-degree data from the Global Oscillations Network Group (GONG) using the mode inertia together with cubic and inverse frequency terms. We find that for the central frequency of rotationally split multiplets the cubic term dominates both the average surface term and the temporal variation, but for the medium-degree case the inverse term improves the fit to the temporal variation. We also examine the variation of the even-order splitting coefficients for the medium-degree data and find that, as for the central frequency, the latitude-dependent frequency variation, which reflects the changing latitudinal distribution of magnetic activity over the solar cycle, can be described by the combination of a cubic and an inverse function of frequency scaled by inverse mode inertia. The results suggest that this simple parametrization could be used to assess the activity-related frequency variation in solar-like asteroseismic targets.
Progressive multifocal leukoencephalopathy outcomes in patients with multiple sclerosis treated with dimethyl fumarate

Background and objectives Dimethyl fumarate (DMF), an oral disease-modifying therapy with an established benefit and well-described safety profile, is among the most commonly used therapies for relapsing forms of multiple sclerosis. As of 31 December 2021, >560,000 patients have been treated with DMF, representing >1,190,000 person-years of exposure. Of these, 6413 patients (14,292 person-years) were from clinical trials. Methods and results Progressive multifocal leukoencephalopathy (PML) has occurred in the setting of lymphopenia (<0.91 × 109/L) in patients treated with DMF. We present detailed clinical characteristics and outcomes of the 12 confirmed PML cases occurring in MS patients on DMF as of 21 July 2021. The PML incidence in DMF-treated patients is 1.07 per 100,000 person-years of DMF exposure. Lymphopenia is the common risk for PML in DMF treatment. Discussion DMF-related PML is rare but has occurred in the setting of lymphopenia, supporting the current recommendations for absolute lymphocyte count monitoring in all patients, regardless of age and time on therapy.
(ALMOST) DARK HI SOURCES IN THE ALFALFA SURVEY: THE INTRIGUING CASE OF HI1232+20

We report the discovery and follow-up observations of a system of three objects identified by the ALFALFA extragalactic HI survey, cataloged as (almost) dark extragalactic sources, i.e., extragalactic HI detections with no discernible counterpart in publicly available, wide-field, imaging surveys. We have obtained deep optical imaging with WIYN pODI and HI synthesis maps with WSRT of the HI1232+20 system. The source with the highest HI flux has a newly discovered ultra-low surface brightness (LSB) optical counterpart associated with it, while the other two sources have no detected optical counterparts in our images. Our optical observations show that the detected LSB optical counterpart has a peak surface brightness of ∼26.4 mag arcsec−2 in g′, which is exceptionally faint. This source (AGC 229385) has the largest accurately measured HI mass-to-light ratio of an isolated object: M HI / L g ′ ? > = 46 M ⊙ / L ⊙ ? > , and has an HI mass of 7.2 × 10 8 M ⊙ ? > . The other two HI sources (with HI masses 2.0 × 108 and 1.2 × 10 8 M ⊙ ? > ) without optical counterparts have upper limit surface brightnesses of 27.9 and 27.8 mag arcsec−2 in g′, and lower limits on their gas mass-to-light ratio of M HI / L g ′ ? > > 57 and > 31 M ⊙ / L ⊙ ? > . This system lies relatively close in projection to the Virgo Cluster, but velocity flow models indicate that it is located at 25 Mpc, substantially beyond Virgo. The system appears to be quite isolated, with no known object closer than ∼500 kpc. These HI sources may represent both sides of the threshold between “dark” star-less galaxies and galaxies with stellar populations. We discuss a variety of possible formation scenarios for the HI1232+20 system.
High Excitation Molecular Gas in the Galactic Center Loops; 12CO(J =2-1 and J =3-2) Observations

We have carried out 12CO(J =2-1) and 12CO(J =3-2) observations at spatial resolutions of 1.0-3.8 pc toward the entirety of loops 1 and 2 and part of loop 3 in the Galactic center with NANTEN2 and ASTE. These new results revealed detailed distributions of the molecular gas and the line intensity ratio of the two transitions, R3-2/2-1. In the three loops, R3-2/2-1 is in a range from 0.1 to 2.5 with a peak at ~ 0.7 while that in the disk molecular gas is in a range from 0.1 to 1.2 with a peak at 0.4. This supports that the loops are more highly excited than the disk molecular gas. An LVG analysis of three transitions, 12CO J =3-2 and 2-1 and 13CO J =2-1, toward six positions in loops 1 and 2 shows density and temperature are in a range 102.2 - 104.7 cm-3 and 15-100 K or higher, respectively. Three regions extended by 50-100 pc in the loops tend to have higher excitation conditions as characterized by R3-2/2-1 greater than 1.2. The highest ratio of 2.5 is found in the most developed foot points between loops 1 and 2. This is interpreted that the foot points indicate strongly shocked conditions as inferred from their large linewidths of 50-100 km s-1, confirming the suggestion by Torii et al. (2010b). The other two regions outside the foot points suggest that the molecular gas is heated up by some additional heating mechanisms possibly including magnetic reconnection. A detailed analysis of four foot points have shown a U shape, an L shape or a mirrored-L shape in the b-v distribution. It is shown that a simple kinematical model which incorporates global rotation and expansion of the loops is able to explain these characteristic shapes.
Spin-foam models and the physical scalar product

This paper aims at clarifying the link between Loop Quantum Gravity and Spin-Foam models in four dimensions. Starting from the canonical framework, we construct an operator P acting on the space of cylindrical functions Cyl($\Gamma$), where $\Gamma$ is the 4-simplex graph, such that its ma- trix elements are, up to some normalization factors, the vertex amplitude of Spin-Foam models. The Spin-Foam models we are considering are the topological model, the Barrett-Crane model and the Engle-Pereira-Rovelli model. The operator P is usually called the "projector" into physical states and its matrix elements gives the physical scalar product. Therefore, we relate the physical scalar product of Loop Quantum Gravity to vertex amplitudes of some Spin-Foam models. We discuss the possibility to extend the action of P to any cylindrical functions on the space manifold.
RESISTIVE MAGNETOHYDRODYNAMIC SIMULATIONS OF RELATIVISTIC MAGNETIC RECONNECTION

Resistive relativistic magnetohydrodynamic (RRMHD) simulations are applied to investigate the system evolution of relativistic magnetic reconnection. A time-split Harten–Lan–van Leer method is employed. Under a localized resistivity, the system exhibits a fast reconnection jet with an Alfvénic Lorentz factor inside a narrow Petschek-type exhaust. Various shock structures are resolved in and around the plasmoid such as the post-plasmoid vertical shocks and the “diamond-chain” structure due to multiple shock reflections. Under a uniform resistivity, Sweet–Parker-type reconnection slowly evolves. Under a current-dependent resistivity, plasmoids are repeatedly formed in an elongated current sheet. It is concluded that the resistivity model is of critical importance for RRMHD modeling of relativistic magnetic reconnection.
Spatial, temporal and demographic patterns of cetacean strandings in the northcentral Gulf of Mexico

There are few published reports that summarise long‐term stranding data for cetaceans in the Gulf of Mexico (GoM). Cetacean stranding data from Alabama (AL) in the northcentral GoM have been recorded since 1978, with dedicated stranding response beginning in 1987, providing an opportunity to characterise spatial, temporal and demographic stranding patterns for this unique area, which links the eastern and western northern GoM coastline. To elucidate long‐term patterns, we analysed stranding records in AL from 1978–2018, taking into consideration the effects of periodic unusual mortality events (UMEs) on stranding demographics. During this 41‐year period, 774 stranding events were recorded involving at least 13 different cetacean species. Common bottlenose dolphins (Tursiops truncatus) were the most reported stranded cetacean (n = 692, 89.4%), followed by Stenella spp. (n = 31, 4.0%). Spatial analysis revealed three stranding hotspots for bottlenose dolphins and an additional hotspot for non‐bottlenose dolphin species that may represent a geographic influence in the northcentral GoM for strandings of offshore cetaceans. Because strandings were dominated by bottlenose dolphins, additional demographic analyses were possible for this species. Strandings occurred most often in the spring (March–May), and females and foetuses stranded more often in calving (January–April) than non‐calving season, consistent with increased mortality related to birthing or reproductive‐associated events. Subadults were found stranded more often than other size classes, indicating a potential stranding bias for this age class. These data are critical to guide future stranding response efforts, define vulnerable populations and help understand causes of mortality through time in the northcentral GoM. Our findings also highlight the importance of long‐term, consistent stranding response to enable identifying spatial and temporal trends that are necessary to support meaningful, range‐wide management and conservation.
Weak lensing analysis of SZ-selected clusters of galaxies from the SPT and Planck surveys

We present the weak lensing analysis of the Wide-Field Imager SZ Cluster of Galaxy (WISCy) sample, a set of ten clusters of galaxies selected for their Sunyaev-Zel’dovich (SZ) effect. After developing new and improved methods for background selection and determination of geometric lensing scaling factors from absolute multi-band photometry in cluster fields, we compare the weak lensing result with public X-ray and SZ data. We find consistency with published hydrostatic X-ray masses with no significant bias and an intrinsic scatter σint,log10 = 0.13 +0.11 0.13 . We independently calibrate the SPT significance-mass relation and find consistency with previous results at an intrinsic scatter of σint,log10 = 0.09 +0.15 0.09 , with indications for a slightly higher normalisation mass and steeper slope. The comparison of weak lensing mass and Planck Compton parameters, whether extracted self-consistently with a mass-observable relation (MOR) or using X-ray prior information on cluster size, shows significant discrepancies. Since the deviations from the MOR strongly correlate with cluster redshift, we hypothesise that they are related to a size or redshift dependent bias in either signal extraction in the Planck SZ catalogues or their previous X-ray based mass calibration, or in measurement related excess intrinsic scatter.
General-relativistic electromagnetic fields around a slowly rotating neutron star: stationary vacuum solutions

Pulsars are thought to be highly magnetized rotating neutron stars accelerating charged particles along magnetic field lines in their magnetosphere and visible as pulsed emission from the radio wavelength up to high energy X-rays and gamma-rays. Being highly compact objects with compactness close to $\Xi = R_s/R\approx0.5$, where $\Rs=2\,G\,M/c^2$ is the Schwarzschild radius and $\{M,R\}$ the mass and radius of the neutron star, general-relativistic effects become important close to their surface. This is especially true for the polar caps where radio emission is supposed to emanate from, leading to well defined signatures such as linear and circular polarization. In this paper, we derive a general formalism to extend to general relativity the Deutsch field solution valid in vacuum space. Thanks to a vector spherical harmonic expansion of the electromagnetic field, we are able to express the solution to any order in the spin parameter $\Omega$ of the compact object. We hope this analysis to serve as a benchmark to test numerical codes used to compute black hole and neutron star magnetospheres.
CMB internal delensing with general optimal estimator for higher-order correlations

We present a new method for delensing $B$ modes of the cosmic microwave background (CMB) using a lensing potential reconstructed from the same realization of the CMB polarization (CMB internal delensing). The $B$-mode delensing is required to improve sensitivity to primary $B$ modes generated by, e.g., the inflationary gravitational waves, axion-like particles, modified gravity, primordial magnetic fields, and topological defects such as cosmic strings. However, the CMB internal delensing suffers from substantial biases due to correlations between observed CMB maps to be delensed and that used for reconstructing a lensing potential. We construct a realization-dependent (RD) estimator for correcting these biases by deriving a general optimal estimator for higher-order correlations. The RD estimator is less sensitive to simulation uncertainties. Compared to the previous methods, we find that the RD estimator corrects the biases without substantial degradation of the delensing efficiency.
Evaluating the stability of atmospheric lines with HARPS

Context. When searching for extrasolar systems using the radial velocity technique, the need for high-precision measurements implies that a precise wavelength calibration is required. The choice of the calibrator is a particularly important open question in the infra-red domain, where precision and achievements remain inferior to those in the optical. Aims. We investigate the long-term stability of atmospheric lines as a precise wavelength reference and analyze their sensitivity to different atmospheric and observing conditions. Methods. We use HARPS archival data for three bright stars, TauCeti, μ Arae, and eEri, which span 6 years and include highcadence measurements performed over several nights. We cross-correlate this data with an O2 mask and evaluate both radial velocity and bisector variations to a photon noise level of 1m/s. Results. We find that the telluric lines in the three data-sets are stable down to 10m/s (rms) over the 6 years. We also show that the radial velocity variations can be modeled by simple atmospheric models, yielding a final precision of 1‐2m/s. Conclusions. The long-term stability of atmospheric lines was 10m/s over six years, in spite of atmospheric phenomena. Atmospheric lines can be used as awavelength reference for short timescale programs, yielding a precision of 5m/s without any correction. A higher precision, of 2m/s, can be reached if the atmospheric phenomena are corrected for using the simple atmospheric model described, making it a very competitive method even on long timescales.