Miracle-dz/UniFAR-FTUs huggingface dataset:
THE MASS-LOSS RETURN FROM EVOLVED STARS TO THE LARGE MAGELLANIC CLOUD. IV. CONSTRUCTION AND VALIDATION OF A GRID OF MODELS FOR OXYGEN-RICH AGB STARS, RED SUPERGIANTS, AND EXTREME AGB STARS

To measure the mass loss from dusty oxygen-rich (O-rich) evolved stars in the Large Magellanic Cloud (LMC), we have constructed a grid of models of spherically symmetric dust shells around stars with constant mass-loss rates using 2Dust. These models will constitute the O-rich model part of the “Grid of Red supergiant and Asymptotic giant branch star ModelS” (GRAMS). This model grid explores four parameters—stellar effective temperature from 2100 K to 4700 K; luminosity from 103 to 106 L☉; dust shell inner radii of 3, 7, 11, and 15 Rstar; and 10.0 μm optical depth from 10−4 to 26. From an initial grid of ∼1200 2Dust models, we create a larger grid of ∼69,000 models by scaling to cover the luminosity range required by the data. These models are available online to the public. The matching in color–magnitude diagrams and color–color diagrams to observed O-rich asymptotic giant branch (AGB) and red supergiant (RSG) candidate stars from the SAGE and SAGE-Spec LMC samples and a small sample of OH/IR stars is generally very good. The extreme AGB star candidates from SAGE are more consistent with carbon-rich (C-rich) than O-rich dust composition. Our model grid suggests lower limits to the mid-infrared colors of the dustiest AGB stars for which the chemistry could be O-rich. Finally, the fitting of GRAMS models to spectral energy distributions of sources fit by other studies provides additional verification of our grid and anticipates future, more expansive efforts.
On Goren–Oort stratification for quaternionic Shimura varieties

Let $F$ be a totally real field in which a prime $p$ is unramified. We define the Goren–Oort stratification of the characteristic- $p$ fiber of a quaternionic Shimura variety of maximal level at $p$ . We show that each stratum is a $(\mathbb{P}^{1})^{r}$ -bundle over other quaternionic Shimura varieties (for an appropriate integer $r$ ). As an application, we give a necessary condition for the ampleness of a modular line bundle on a quaternionic Shimura variety in characteristic $p$ .
About mechanics of the structured particles

The principles of creation of the mechanics of structured particles in the frame of the Newton’s laws are considered. The explanation how this mechanics leads to the account of dissipative forces is offered. It is discussed why the motions of the system determine by two type of symmetry: symmetry of the system and symmetry of space and how it leads to two types of energy and forces accordingly. It is shown how the mechanics of the structured particles leads to thermodynamics, statistical physics and kinetics.
ExoMol molecular line lists - X. The spectrum of sodium hydride

Accurate and complete rotational, rotational-vibrational and rotational-vibrational-electronic line lists are calculated for sodium hydride: both the NaH and NaD isotopologues are considered. These line lists cover all ro-vibrational states of the ground (X 1 � + ) and first excited (A 1 � + ) electronic states. The calculations use available spectroscopically-determined potential energy curves and new high-quality, ab initio dipole moment curves. Partition functions for both isotopologues are calculated and the effect of quasi-bound states is considered. The resulting line listsare suitable for temperatures up to about 7000 Kand are designed for studies of exoplanet atmospheres, brown dwarfs and cool stars. In particular, the NaH A − X band is found to show a broad absorption feature at about 385 nm which should provide a signature for the molecule. All partition functions, lines and transitions are available as supplementary information to this article and at www.exomol. com.
Some local questions for hyperbolic systems with non-regular time dependent coefficients

In this note we investigate local properties for microlocally symmetrizable hyperbolic systems with just time dependent coefficients. Thanks to Paley-Wiener theorem, we establish finite propagation speed by showing precise estimates on the evolution of the support of the solution in terms of suitable norms of the coefficients of the operator and of the symmetrizer. From this result, local existence and uniqueness follow by quite standard methods. Our argument relies on the use of Fourier transform, and it cannot be extended to operators whose coefficients depend also on the space variables. On the other hand, it works under very mild regularity assumptions on the coefficients of the operator and of the symmetrizer.
A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE. IV. THE NEUTRINO SIGNAL

Considering six general relativistic, two-dimensional (2D) supernova (SN) explosion models of progenitor stars between 8.1 and 27 M☉, we systematically analyze the properties of the neutrino emission from core collapse and bounce to the post-explosion phase. The models were computed with the Vertex-CoCoNuT code, using three-flavor, energy-dependent neutrino transport in the ray-by-ray-plus approximation. Our results confirm the close similarity of the mean energies, 〈E〉, of and heavy-lepton neutrinos and even their crossing during the accretion phase for stars with M ≳ 10 M☉ as observed in previous 1D and 2D simulations with state-of-the-art neutrino transport. We establish a roughly linear scaling of with the proto-neutron star (PNS) mass, which holds in time as well as for different progenitors. Convection inside the PNS affects the neutrino emission on the 10%–20% level, and accretion continuing beyond the onset of the explosion prevents the abrupt drop of the neutrino luminosities seen in artificially exploded 1D models. We demonstrate that a wavelet-based time-frequency analysis of SN neutrino signals in IceCube will offer sensitive diagnostics for the SN core dynamics up to at least ∼10 kpc distance. Strong, narrow-band signal modulations indicate quasi-periodic shock sloshing motions due to the standing accretion shock instability (SASI), and the frequency evolution of such “SASI neutrino chirps” reveals shock expansion or contraction. The onset of the explosion is accompanied by a shift of the modulation frequency below 40–50 Hz, and post-explosion, episodic accretion downflows will be signaled by activity intervals stretching over an extended frequency range in the wavelet spectrogram.
Non-LTE oxygen line formation in 3D hydrodynamic model stellar atmospheres

The O (Iota) 777 nm lines are among the most commonly used diagnostics for the oxygen abundances in the atmospheres of FGK-type stars. However, they form in conditions that are far from local thermodynamic equilibrium (LTE). We explore the departures from LTE of atomic oxygen, and their impact on O I lines, across the STAGGER-grid of three-dimensional hydrodynamic model atmospheres. For the O (Iota) 777 nm triplet, we find significant departures from LTE. These departures are larger in stars with larger effective temperatures, smaller surface gravities, and larger oxygen abundances. We present grids of predicted 3D non-LTE based equivalent widths for the O (Iota) 616 nm, [O (Iota)] 630 nm, [O (I)] 636 nm, and O (Iota) 777 nm lines, as well as abundance corrections to 1D LTE based results.
Next-to-leading order transverse momentum-weighted Sivers asymmetry in semi-inclusive deep inelastic scattering: The role of the three-gluon correlator

Here, we study the Sivers asymmetry in semi-inclusive hadron production in deep inelastic scattering. We concentrate on the contribution from the photon-gluon fusion channel at O(α em 2α s), where three-gluon correlation functions play a major role within the twist-3 collinear factorization formalism. We establish the correspondence between such a formalism with three-gluon correlation functions and the usual transverse momentum-dependent (TMD) factorization formalism at moderate hadron transverse momenta. We derive the coefficient functions used in the usual TMD evolution formalism related to the quark Sivers function expansion in terms of the three-gluon correlation functions. We further perform the next-to-leading order calculation for the transverse momentum-weighted spin-dependent differential cross section and identify the off-diagonal contribution from the three-gluon correlation functions to the QCD collinear evolution of the twist-3 Qiu-Sterman function.
Closed strings as single-valued open strings: a genus-zero derivation

Based on general mathematical assumptions we give an independent, elementary derivation of a theorem by Brown and Dupont (2018 Talk given by F Brown in ‘String Math’ (Sendai, June 2018)) which states that tree-level amplitudes of closed and open strings are related through the single-valued map ‘sv’. This relation can be traced back to the underlying moduli-space integrals over punctured Riemann surfaces of genus zero. The sphere integrals in closed-string amplitudes and the disk integrals in open-string amplitudes are shown to obey .
SPECTRAL CLASSIFICATION AND REDSHIFT MEASUREMENT FOR THE SDSS-III BARYON OSCILLATION SPECTROSCOPIC SURVEY

We describe the automated spectral classification, redshift determination, and parameter measurement pipeline in use for the Baryon Oscillation Spectroscopic Survey (BOSS) of the Sloan Digital Sky Survey III (SDSS-III) as of the survey's ninth data release (DR9), encompassing 831,000 moderate-resolution optical spectra. We give a review of the algorithms employed, and describe the changes to the pipeline that have been implemented for BOSS relative to previous SDSS-I/II versions, including new sets of stellar, galaxy, and quasar redshift templates. For the color-selected “CMASS” sample of massive galaxies at redshift 0.4 ≲ z ≲ 0.8 targeted by BOSS for the purposes of large-scale cosmological measurements, the pipeline achieves an automated classification success rate of 98.7% and confirms 95.4% of unique CMASS targets as galaxies (with the balance being mostly M stars). Based on visual inspections of a subset of BOSS galaxies, we find that approximately 0.2% of confidently reported CMASS sample classifications and redshifts are incorrect, and about 0.4% of all CMASS spectra are objects unclassified by the current algorithm which are potentially recoverable. The BOSS pipeline confirms that ∼51.5% of the quasar targets have quasar spectra, with the balance mainly consisting of stars and low signal-to-noise spectra. Statistical (as opposed to systematic) redshift errors propagated from photon noise are typically a few tens of km s−1 for both galaxies and quasars, with a significant tail to a few hundreds of km s−1 for quasars. We test the accuracy of these statistical redshift error estimates using repeat observations, finding them underestimated by a factor of 1.19–1.34 for galaxies and by a factor of two for quasars. We assess the impact of sky-subtraction quality, signal-to-noise ratio, and other factors on galaxy redshift success. Finally, we document known issues with the BOSS DR9 spectroscopic data set and describe directions of ongoing development.
THE POWER OF SIMULTANEOUS MULTIFREQUENCY OBSERVATIONS FOR mm-VLBI: ASTROMETRY UP TO 130 GHz WITH THE KVN

Simultaneous observations at multiple frequency bands have the potential to overcome the fundamental limitation imposed by the atmospheric propagation in (sub)millimeter very long baseline interferometry (mm-VLBI) observations. The propagation effects place a severe limit on the sensitivity achievable in mm-VLBI, reducing the time over which the signals can be coherently combined, and preventing the use of phase referencing and astrometric measurements. We carried out simultaneous observations at 22, 43, 87, and 130 GHz of a group of five active galactic nuclei, the weakest of which is ∼200 mJy at 130 GHz, with angular separations ranging from 3. °6 to 11°, using the Korean VLBI Network. We analyzed these data using the frequency phase transfer (FPT) and the source frequency phase referencing (SFPR) techniques, which use the observations at a lower frequency to correct those at a higher frequency. The results of the analysis provide an empirical demonstration of the increase in the coherence times at 130 GHz from a few tens of seconds to about 20 minutes, with FPT, and up to many hours with SFPR. Moreover, the astrometric analysis provides high-precision relative position measurements between two frequencies, including, for the first time, astrometry at 130 GHz. Finally, we demonstrate a method for the generalized decomposition of the relative position measurements into absolute position shifts for bona fide astrometric registration of the maps of the individual sources at multiple frequencies, up to 130 GHz.
YSO jets in the Galactic plane from UWISH2 - II. Outflow luminosity and length distributions in Serpens and Aquila

Jets and outflows accompany the mass accretion process in protostars and young stellar objects. Using a large and unbiased sample, they can be used to study statistically the local feedback they provide and the typical mass accretion history. Here we analyse such a sample of molecular hydrogen emission-line objects in the Serpens and Aquila part of the Galactic plane. Distances are measured by foreground star counts with an accuracy of 25per cent. The resulting spacial distribution and outflow luminosities indicate that our objects sample the formation of intermediate-mass objects. The outflows are unable to provide a sizeable fraction of energy and momentum to support, even locally, the turbulence levels in their surrounding molecular clouds. The fraction of parsec scale flows is one quarter and the typical dynamical jet age of the order of 10 4yr. Groups of emission knots are ejected every 10 3yr. This might indicate that low-level accretion rate fluctuations and not FU-Ori-type events are responsible for the episodic ejection of material. Better observational estimates of the FU-Ori duty cycle are needed. Â© 2012 The Authors Monthly Notices of the Royal Astronomical Society Â© 2012 RAS.
THE INITIAL MASS FUNCTION AND DISK FREQUENCY OF THE ρ OPHIUCHI CLOUD: AN EXTINCTION-LIMITED SAMPLE

We have completed an optical spectroscopic survey of an unbiased, extinction-limited sample of candidate young stars covering 1.3 deg2 of the ρ Ophiuchi star-forming region. While infrared, X-ray, and optical surveys of the cloud have identified many young stellar objects (YSOs), these surveys are biased toward particular stages of stellar evolution and are not optimal for studies of the disk frequency and initial mass function. We have obtained over 300 optical spectra to help identify 135 association members based on the presence of Hα in emission, lithium absorption, X-ray emission, a mid-infrared excess, a common proper motion, reflection nebulosity, and/or extinction considerations. Spectral types along with R- and I-band photometry were used to derive effective temperatures and bolometric luminosities for association members to compare with theoretical tracks and isochrones for pre-main-sequence stars. An average age of 3.1 Myr is derived for this population which is intermediate between that of objects embedded in the cloud core of ρ Ophiuchi and low-mass stars in the Upper Scorpius subgroup. Consistent with this age we find a circumstellar disk frequency of 27% ± 5%. We also constructed an initial mass function for an extinction-limited sample of 123 YSOs (Av ⩽ 8 mag), which is consistent with the field star initial mass function for YSOs with masses >0.2 M☉. There may be a deficit of brown dwarfs but this result relies on completeness corrections and requires confirmation.
How to detect the signatures of self-gravitating circumstellar discs with the Atacama Large Millimeter/sub-millimeter Array

In this paper we present simulated Atacama Large Millimetre/sub-millimetre Array (ALMA) observations of self-gravitating circumstellar discs with different properties in size, mass and inclination, located in four of the most extensively studied and surveyed star-forming regions. Starting from a Smoothed Particle Hydrodynamics (SPH) simulation and representative dust opacities, we have initially constructed maps of the expected emission at sub-mm wavelengths of a large sample of discs with different properties. We have then simulated realistic observations of discs as they may appear with ALMA using the Common Astronomy Software Application ALMA simulator. We find that, with a proper combination of antenna configuration and integration time, the spiral structure characteristic of self-gravitating discs is readily detectable by ALMA over a wide range of wavelengths at distances comparable to TW Hydrae ($\sim 50 \,$pc), Taurus - Auriga and Ophiucus ($\sim 140 \,$pc) star-forming regions. However, for discs located in Orion complex ($\sim 400 \,$pc) only the largest discs in our sample (outer radius of 100 au) show a spatially resolved structure while the smaller ones (outer radius of 25 au) are characterized by a spiral structure that is not conclusively detectable with ALMA.
UNDERSTANDING THE UNIQUE ASSEMBLY HISTORY OF CENTRAL GROUP GALAXIES

Central galaxies (CGs) in massive halos live in unique environments with formation histories closely linked to that of the host halo. In local clusters, they have larger sizes (Re) and lower velocity dispersions (σ) at fixed stellar mass M*, and much larger Re at a fixed σ than field and satellite galaxies (non-CGs). Using spectroscopic observations of group galaxies selected from the COSMOS survey, we compare the dynamical scaling relations of early-type CGs and non-CGs at z ∼ 0.6 to distinguish possible mechanisms that produce the required evolution. CGs are systematically offset toward larger Re at fixed σ compared to non-CGs with similar M*. The CG Re–M* relation also shows differences, primarily driven by a subpopulation (∼15%) of galaxies with large Re, while the M*–σ relations are indistinguishable. These results are accentuated when double Sérsic profiles, which better fit light in the outer regions of galaxies, are adopted. They suggest that even group-scale CGs can develop extended components by these redshifts that can increase total Re and M* estimates by factors of ∼2. To probe the evolutionary link between our sample and cluster CGs, we also analyze two cluster samples at z ∼ 0.6 and z ∼ 0. We find similar results for the more massive halos at comparable z, but much more distinct CG scaling relations at low-z. Thus, the rapid, late-time accretion of outer components, perhaps via the stripping and accretion of satellites, would appear to be a key feature that distinguishes the evolutionary history of CGs.
Effect of the Addition of Edible Insect Flour from Yellow Mealworm (Tenebrio molitor) on the Sensory Acceptance, and the Physicochemical and Textural Properties of Sponge Cake

The aim of this study was to evaluate the possibility of using insect flour for sponge cake supplementation. Consumer acceptance, chemical com - position, textural properties, and microbiological characteristics were determined. The addition of mealworm flour significantly increased the content of nutrients, especially protein, ash, lipid, and dietary fiber. Mealworm flour influenced the color parameters as well as textural properties. The fatty acid profile was dominated by monounsaturated fatty acids, ranging from 9.72 g/100 g for wheat flour sponge cake to 41.82 g/100 g for sponge cake with 20% addition of mealworm flour. The amino acid profile of mealworm flour was characterized by a significantly higher content of essential amino acids compared to wheat flour and sponge cakes. Sponge cake supplementation resulted in a good nutritional value of protein except for lysine which was the limiting amino acid in all samples. However, the limiting amino acid index was 63.04-63.10% compared to 30.38% for the mealworm and wheat sponge cake, respectively. The presence of insect flour reduced the organoleptic properties of the obtained sponge cakes, regardless of its quantity. The addition of mealworm flour contributed to a significant reduction in the hardness and fracturability of the sponge cakes on the baking day and dur - ing the 30-day storage. Insect flour addition did not reduce the microbiological safety of the final product. The study results indicate the possibility of using mealworm flour in the production of confectionery products.
EXAMINATION OF THE ASTROPHYSICAL S-FACTORS OF THE RADIATIVE PROTON CAPTURE ON 2H, 6Li, 7 Li, 12C AND 13C

Astrophysical S-factors of radiative capture reactions on light nuclei have been calculated in a two-cluster potential model, taking into account the separation of orbital states by the use of Young schemes. The local two-body potentials describing the interaction of the clusters were determined by fitting scattering data and properties of bound states. The many-body character of the problem is approximatively accounted for by Pauli forbidden states. An important feature of the approach is the consideration of the dependence of the interaction potential between the clusters on the orbital Young schemes, which determine the permutation symmetry of the nucleon system. Proton capture on 2H, 6Li, 7Li, 12C and 13C was analyzed in this approach. Experimental data at low energies were described reasonably well when the phase shifts for cluster–cluster scattering, extracted from precise data, were used. This shows that decreasing the experimental error on differential elastic scattering cross-sections of light nuclei at astrophysical energies is very important also to allow a more accurate phase shift analysis. A future increase in precision will allow more definite conclusions regarding the reaction mechanisms and astrophysical conditions of thermonuclear reactions.
Quasiperiodic and mixed commutator factorizations in free products of groups

It is well known that a nontrivial commutator in a free group is never a proper power. We prove a theorem that generalizes this fact and has several worthwhile corollaries. For example, an equation [x1,y1]…[xk,yk]=zn , where n⩾2k , in the free product F of groups without nontrivial elements of order ⩽n implies that z is conjugate to an element of a free factor of F . If a nontrivial commutator in a free group factors into a product of elements which are conjugate to each other then all these elements are distinct.