Sazuna/UAT_keywords huggingface dataset:
Molecules with ALMA at Planet-forming Scales. XX. The Massive Disk around GM Aurigae. Gas mass remains one of the most difficult protoplanetary disk properties to constrain. With much of the protoplanetary disk too cold for the main gas constituent, H2, to emit, alternative tracers such as dust, CO, or the H2 isotopologue HD are used. However, relying on disk mass measurements from any single tracer requires assumptions about the tracer's abundance relative to H2 and the disk temperature structure. Using new Atacama Large Millimeter/submillimeter Array (ALMA) observations from the Molecules with ALMA at Planet-forming Scales (MAPS) ALMA Large Program as well as archival ALMA observations, we construct a disk physical/chemical model of the protoplanetary disk GM Aur. Our model is in good agreement with the spatially resolved CO isotopologue emission from 11 rotational transitions with spatial resolution ranging from 0"15 to 0"46 (24-73 au at 159 pc) and the spatially unresolved HD J = 1-0 detection from Herschel. Our best-fit model favors a cold protoplanetary disk with a total gas mass of approximately 0.2 M⊙, a factor of 10 reduction in CO gas inside roughly 100 au and a factor of 100 reduction outside of 100 au. Despite its large mass, the disk appears to be on the whole gravitationally stable based on the derived Toomre Q parameter. However, the region between 70 and 100 au, corresponding to one of the millimeter dust rings, is close to being unstable based on the calculated Toomre Q of &lt;1.7. This paper is part of the MAPS special issue of the Astrophysical Journal Supplement.

Keywords: Protoplanetary disks, Astrochemistry
VERTICO: The Virgo Environment Traced in CO Survey. We present the Virgo Environment Traced in CO (VERTICO) survey, a new effort to map 12CO (2-1), 13CO (2-1), and C18O (2-1) in 51 Virgo Cluster galaxies with the Atacama Compact Array, part of the Atacama Large Millimeter/submillimeter Array. The primary motivation of VERTICO is to understand the physical mechanisms that perturb molecular gas disks, and therefore star formation and galaxy evolution, in dense environments. This first paper contains an overview of VERTICO's design and sample selection, 12CO (2-1) observations, and data reduction procedures. We characterize global 12CO (2-1) fluxes and molecular gas masses for the 49 detected VERTICO galaxies, provide upper limits for the two nondetections, and produce resolved 12CO (2-1) data products (median resolution = 8″ ≍ 640 pc). Azimuthally averaged 12CO (2-1) radial intensity profiles are presented along with derived molecular gas radii. We demonstrate the scientific power of VERTICO by comparing the molecular gas size-mass scaling relation for our galaxies with a control sample of field galaxies, highlighting the strong effect that radius definition has on this correlation. We discuss the drivers of the form and scatter in the size-mass relation and highlight areas for future work. VERTICO is an ideal resource for studying the fate of molecular gas in cluster galaxies and the physics of environment-driven processes that perturb the star formation cycle. Upon public release, the survey will provide a homogeneous legacy data set for studying galaxy evolution in our closest cluster.

Keywords: Virgo Cluster, Molecular gas, Interstellar medium, Galaxies
Exploring the Stellar Rotation of Early-type Stars in the LAMOST Medium-resolution Survey. I. Catalog. We derive stellar parameters and abundances ("stellar labels") of 40,034 late-B and A-type main-sequence stars extracted from the Large Sky Area Multi-Object Fiber Spectroscopic Telescope Medium Resolution Survey (LAMOST-MRS). The primary selection of our early-type sample was obtained from LAMOST Data Release 7 based on spectral-line indices. We employed the Stellar Label Machine to derive their spectroscopic stellar parameters, drawing on Kurucz spectral synthesis models with 6000 &lt; Teff &lt; 15,000 K and -1 &lt; [M/H] &lt; 1 dex. For a signal-to-noise ratio of ~60, the cross validated scatter is ~75 K, 0.06 dex, 0.05 dex, and ~3.5 km s-1 for Teff, $\mathrm{log}g$ , [M/H], and $v\sin i$ , respectively. A comparison with objects with prior known stellar labels shows great consistency for all stellar parameters, except for $\mathrm{log}g$ . Although this is an intrinsic caveat that comes from the MRS's narrow wavelength coverage, it only has a minor effect on estimates of the stellar rotation rates because of the decent spectral resolution and the profile-fitting method employed. The masses and ages of our early-type sample stars were inferred from nonrotating stellar evolution models. This paves the way for reviewing the properties of stellar rotation distributions as a function of stellar mass and age.

Keywords: Early-type stars, Stellar properties, Astronomy data analysis, Stellar rotation, Catalogs
Multiwavelength Properties of Miras. We comprehensively study the variability of Miras in the Large Magellanic Cloud by simultaneously analyzing light curves in 14 bands in the range of 0.5-24 μm. We model over 20 yr long, high-cadence I-band light curves collected by the Optical Gravitational Lensing Experiment (OGLE) and fit them to light curves collected in the remaining optical/near-infrared/mid-infrared bands to derive both the variability amplitude ratio and phase lag as a function of wavelength. We show that the variability amplitude ratio declines with increasing wavelength for both oxygen-rich (O-rich) and carbon-rich (C-rich) Miras, while the variability phase lag increases slightly with increasing wavelength. In a significant number of Miras, mostly the C-rich ones, the spectral energy distributions (SEDs) require the presence of a cool component (dust) in order to match the mid-IR data. Based on SED fits for a golden sample of 140 Miras, we calculated synthetic period-luminosity relations (PLRs) in 42 bands for the existing and future sky surveys that include OGLE, the VISTA Near-Infrared YJKs Survey of the Magellanic Clouds System, Legacy Survey of Space and Time, Gaia, Spitzer, the Wide-field Infrared Survey Explorer, the James Webb Space Telescope, the Nancy Grace Roman Space Telescope (formerly WFIRST), and the Hubble Space Telescope. We show that the synthetic PLR slope decreases with increasing wavelength for both the O-rich and C-rich Miras in the range of 0.1-40 μm. Finally, we show the location and motions of Miras on the color-magnitude and color-color diagrams.

Keywords: Stellar distance, Pulsating variable stars, Large Magellanic Cloud, Infrared astronomy, Stellar astronomy, Asymptotic giant branch stars, Mira variable stars, Long period variable stars, Late-type giant stars, Asteroseismology, Magellanic Clouds, Near infrared astronomy
An Entropy-stable Ideal EC-GLM-MHD Model for the Simulation of the Three-dimensional Ambient Solar Wind. The main aim of the current work is to apply the Roe+Lax-Friedrichs (LF) hybrid entropy-stable scheme to the simulation of the three-dimensional ambient solar wind. The governing equations for the solar wind flow and magnetic field utilize the entropy-consistent nine-wave magnetic field divergence diminishing ideal magnetohydrodynamics (MHD) equations, which are symmetric and Galilean invariant with some nonconservative terms proportional to the divergence of magnetic field or the gradient of the Lagrange multiplier ψ. By using solenoidality-preserving and non-negativity-preserving reconstruction, the divergence error is further constrained, and the densities and pressures are reliably guaranteed. Moreover, the entropy is used as an auxiliary equation to completely avoid the appearance of negative pressure, which is independent of any numerical flux and can be retrofit into any MHD equations straightforwardly. All the properties referred to above make the newly developed scheme more handy and robust to cope with the high Mach number or low plasma β situations. After the experiments of the entropy consistency and the robustness of the proposed entropy-stable scheme through two simple tests, we carry out the simulation of the large-scale solar wind structures for Carrington Rotation 2183 (CR 2183) in a six-component grid system with the initial potential field obtained from the Helioseismic and Magnetic Imager magnetogram by retaining spherical harmonics of degree 50. The comparisons of the numerical results with the remote sensing observations and in situ data show that the new model has the capability to produce structured solar wind.

Keywords: Solar wind, Solar corona, Magnetohydrodynamical simulations
GR-Athena++: Puncture Evolutions on Vertex-centered Oct-tree Adaptive Mesh Refinement. Numerical relativity is central to the investigation of astrophysical sources in the dynamical and strong-field gravity regime, such as binary black hole and neutron star coalescences. Current challenges set by gravitational-wave and multimessenger astronomy call for highly performant and scalable codes on modern massively parallel architectures. We present GR-Athena++, a general-relativistic, high-order, vertex-centered solver that extends the oct-tree, adaptive mesh refinement capabilities of the astrophysical (radiation) magnetohydrodynamics code Athena++. To simulate dynamical spacetimes, GR-Athena++ uses the Z4c evolution scheme of numerical relativity coupled to the moving puncture gauge. We demonstrate stable and accurate binary black hole merger evolutions via extensive convergence testing, cross-code validation, and verification against state-of-the-art effective-one-body waveforms. GR-Athena++ leverages the task-based parallelism paradigm of Athena++ to achieve excellent scalability. We measure strong-scaling efficiencies above 95% for up to ~1.2 × 104 CPUs and excellent weak scaling is shown up to ~105 CPUs in a production binary black hole setup with adaptive mesh refinement. GR-Athena++ thus allows for the robust simulation of compact binary coalescences and offers a viable path toward numerical relativity at exascale.

Keywords: Astronomy software, Black holes, Compact objects
Glycolonitrile (HOCH<SUB>2</SUB>CN) Chemistry in Star-forming Regions. Glycolonitrile (HOCH2CN) is an attractive interstellar prebiotic molecule. Glycolonitrile is considered not only as a possible precursor for glycine but also as a key intermediate for adenine formation. Recently, HOCH2CN was detected toward IRAS 16293-2422 B with the Atacama Large Millimeter/submillimeter Array (ALMA). In this study we perform a comprehensive modeling study on HOCH2CN chemistry under the physical conditions of IRAS 16293-2422 B's cold envelope and hot corino evolutions using the astrochemical code NAUTILUS and the updated gas-grain chemical network. Our studies not only give the main reactions and the favorable physical conditions for the formation of HOCH2CN but also uncover that the observed glycolonitrile in the cold envelope originates from the gradual accumulation of the gas-phase molecules during the ambient cloud, freefall collapse, and warm-up phases of the cold envelope evolution, and in the hot corino it mainly comes from the accumulated ices during the hot corino evolution. Using the updated chemical network, we also conduct chemical simulations under the physical conditions of Sagittarius (Sgr) B2(N) evolution. The simulation results show that varying the cosmic-ray ionization rate is needed to best reproduce the observational upper limits of HOCH2CN and the observed abundances of CNCHO and CH2CNH toward Sgr B2(N). Moreover, we predict that HOCHCNH, OCH2CN, HOCHCN, HOCCNH, OCCNH, and OCCN have high abundances and may be detectable toward IRAS 16293-2422 B and Sgr B2(N).

Keywords: Interstellar molecules, Theoretical models, Interstellar abundances, Astrochemistry, Interstellar medium, Pre-biotic astrochemistry
Fast Scalar Quadratic Maximum Likelihood Estimators for the CMB B-mode Power Spectrum. Constructing a fast and efficient estimator for the B-mode power spectrum of the cosmic microwave background (CMB) is of critical importance for CMB science. For a general CMB survey, the Quadratic Maximum Likelihood (QML) estimator for CMB polarization has been proved to be the optimal estimator with minimal uncertainties, but it is computationally very expensive. In this article, we propose two new QML methods for B-mode power spectrum estimation. We use the Smith-Zaldarriaga approach to prepare the pure B-mode map and the E-mode recycling method to obtain a leakage free B-mode map. We then use the scalar QML estimator to analyze the scalar pure B map (QML-SZ) or B-mode map (QML-TC). The QML-SZ and QML-TC estimators have similar error bars as the standard QML estimators but their computational cost is nearly one order of magnitude smaller. The basic idea is that one can construct the pure B-mode CMB map by using the E-B separation method proposed by Smith &amp; Zaldarriaga (SZ) or the one considering the template cleaning (TC) technique, then apply the QML estimator to these scalar fields. By simulating potential observations of space-based and ground-based detectors, we test the reliability of these estimators by comparing them with the corresponding results of the traditional QML estimator and the pure B-mode pseudo-C&amp;ell; estimator.

Keywords: Cosmic microwave background radiation
An ACA Survey of [C I] <SUP>3</SUP>P<SUB>1</SUB>-<SUP>3</SUP>P<SUB>0</SUB>, CO J = 4 - 3, and Dust Continuum in Nearby U/LIRGs. We present the results of surveying [C I] 3P1-3P0, 12CO J = 4 - 3, and 630 μm dust continuum emission for 36 nearby ultra/luminous infrared galaxies (U/LIRGs) using the Band 8 receiver mounted on the Atacama Compact Array of the Atacama Large Millimeter/submillimeter Array. We describe the survey, observations, data reduction, and results; the main results are as follows. (i) We confirmed that [C I] 3P1-3P0 has a linear relationship with both the 12CO J = 4 - 3 and 630 μm continuum. (ii) In NGC 6052 and NGC 7679, 12CO J = 4 - 3 was detected but [C I] 3P1-3P0 was not detected with a [C I] 3P1-3P0/12CO J = 4 - 3 ratio of ≲0.08. Two possible scenarios of weak [C I] 3P1-3P0 emission are C0-poor/CO-rich environments and an environment with an extremely large [C I] 3P1-3P0 missing flux. (iii) There is no clear evidence showing that galaxy mergers, AGNs, and dust temperatures control the ratios of [C I] 3P1-3P0/12CO J = 4 - 3 and ${L}_{[{\rm{C}}\,{\rm\small{I}}](1-0)}^{{\prime} }/{L}_{630\mu {\rm{m}}}$ . (iv) We compare our nearby U/LIRGs with high-z galaxies, such as galaxies on the star formation main sequence (MS) at z ~ 1 and submillimeter galaxies (SMGs) at z = 2-4. We found that the mean value for the [C I] 3P1-3P0/12CO J = 4 - 3 ratio of U/LIRGs is similar to that of SMGs but smaller than that of galaxies on the MS.

Keywords: Starburst galaxies, Interstellar line emission, Galaxy collisions, Galaxy evolution, Interstellar medium, CO line emission, Extragalactic astronomy, Submillimeter astronomy, Ultraluminous infrared galaxies, Luminous infrared galaxies
Extended Calculations of Energy Levels and Transition Rates for Singly Ionized Lanthanide Elements. II. Tb-Yb. In this work, we continue large-scale ab initio computations for single ionized lanthanides. Extended atomic calculations for the set of ions from Pr II (Z = 59) to Gd II (Z = 64) have been performed in our previous work. In this study, ions from Tb II (Z = 65) to Yb II (Z = 70) are analyzed. By employing the same multiconfiguration Dirac-Hartree-Fock and relativistic configuration interaction methods that are implemented in the general-purpose relativistic atomic structure package GRASP2018, the energy levels and transition data of electric dipole (E1) transitions are computed. These computations are based on the strategies (with small variations) of Paper I. Accuracy of data is evaluated by comparing the computed energy levels with the data provided by the National Institute of Standards and Technology (NIST) database and with data from various methods. We obtain the average accuracy in the energy level compared with the NIST database: 6%, 5%, 4%, 5%, 3%, and 3% for Tb II, Dy II, Ho II, Er II, Tm II, and Yb II, respectively. We also provide extensive comparison of transition probabilities and wavelengths. Our results reach the average accuracy of transition wavelengths: 9%, 9%, 9%, 3%, 4%, and 11% for Tb II, Dy II, Ho II, Er II, Tm II, and Yb II, respectively.

Keywords: Atomic spectroscopy, Atomic physics
Characterising the Extended Morphologies of BL Lacertae Objects at 144 MHz with LOFAR. We present a morphological and spectral study of a sample of 99 BL Lac objects using the LOFAR Two-Metre Sky Survey Second Data Release (LDR2). Extended emission has been identified at gigahertz frequencies around BL Lac objects, but with LDR2 it is now possible to systematically study their morphologies at 144 MHz, where more diffuse emission is expected. LDR2 reveals the presence of extended radio structures around 66/99 of the BL Lac nuclei, with angular extents ranging up to 115″, corresponding to spatial extents of 410 kpc. The extended emission is likely to be both unbeamed diffuse emission and beamed emission associated with relativistic bulk motion in jets. The spatial extents and luminosities of the extended emission are consistent with the unification scheme for active galactic nuclei, where BL Lac objects correspond to low-excitation radio galaxies with the jet axis aligned along the line of sight. While extended emission is detected around the majority of BL Lac objects, the median 144-1400 MHz spectral index and core dominance at 144 MHz indicate that the core component contributes ~42% on average to the total low-frequency flux density. A stronger correlation was found between the 144 MHz core flux density and the γ-ray photon flux (r = 0.69) than between the 144 MHz extended flux density and the γ-ray photon flux (r = 0.42). This suggests that the radio-to-γ-ray connection weakens at low radio frequencies because the population of particles that give rise to the γ-ray flux are distinct from the electrons producing the diffuse synchrotron emission associated with spatially extended features.

Keywords: BL Lacertae objects, Radio source catalogs
The mini-JPAS: A Study of the Wavelength Dependence of the Photon Response Nonuniformity of the JPAS-Pathfinder Camera. Understanding the origins of small-scale flats of CCDs and their wavelength-dependent variations plays an important role in high-precision photometric, astrometric, and shape measurements of astronomical objects. Based on the unique flat data of 47 narrowband filters provided by JPAS-Pathfinder, we analyze the variations of small-scale flats as a function of wavelength. We find moderate variations (from about 1.0% at 390 nm to 0.3% at 890 nm) of small-scale flats among different filters, increasing toward shorter wavelengths. Small-scale flats of two filters close in central wavelengths are strongly correlated. We then use a simple physical model to reproduce the observed variations to a precision of about ±0.14% by considering the variations of charge collection efficiencies, effective areas, and thicknesses between CCD pixels. We find that the wavelength-dependent variations of the small-scale flats of the JPAS-Pathfinder camera originate from inhomogeneities of the quantum efficiency (particularly charge collection efficiency), as well as the effective area and thickness of CCD pixels. The former dominates the variations in short wavelengths, while the latter two dominate at longer wavelengths. The effects on proper flat-fielding, as well as on photometric/flux calibrations for photometric/slitless spectroscopic surveys, are discussed, particularly in blue filters/wavelengths. We also find that different model parameters are sensitive to flats of different wavelengths, depending on the relations between the electron absorption depth, photon absorption length, and CCD thickness. In order to model the wavelength-dependent variations of small-scale flats, a small number (around 10) of small-scale flats with well-selected wavelengths are sufficient to reconstruct small-scale flats in other wavelengths.

Keywords: CCD observation, CCD photometry, Astronomy data reduction, Flux calibration
A Provably Positive, Divergence-free Constrained Transport Scheme for the Simulation of Solar Wind. In this paper, we present a provably positive, divergence-free constrained transport (CT) scheme to simulate the steady-state solar wind ambient with the three-dimensional magnetohydrodynamics numerical model. The positivity can be lost in two ways: one way is in the reconstruction process, and the other is in the updating process when the variables are advanced to the next time step. We adopt a self-adjusting strategy to bring the density and pressure into the permitted range in the reconstruction process, and use modified wave speeds in the Harten-Lax-van Leer flux to ensure the positivity in the updating process. The CT method can keep the magnetic fields divergence-free if the magnetic fields are divergence-free initially. Thus, we combine the least-squares reconstruction of the magnetic fields with the divergence-free constraints to make the magnetic fields globally solenoidal initially. Furthermore, we adopt a radial basis function method to interpolate variables at boundaries that can keep the magnetic field locally divergence-free. To verify the capability of the model in producing structured solar wind, the modeled results are compared with Parker Solar Probe (PSP) in situ observations during its first two encounters, as well as Wind observations at 1 au. Additionally, a solar maximum solar wind background is simulated to show the property of the model's ability to preserve the positivity. The results show that the model can provide a relatively satisfactory comparison with PSP or Wind observations, and the divergence error is about 10-10 for all of the tests in this paper.

Keywords: Solar wind, Magnetohydrodynamical simulations
Using CME Progenitors to Assess CME Geoeffectiveness. There have been a few previous studies claiming that the effects of geomagnetic storms strongly depend on the orientation of the magnetic cloud portion of coronal mass ejections (CMEs). Aparna &amp; Martens, using halo-CME data from 2007 to 2017, showed that the magnetic field orientation of filaments at the location where CMEs originate on the Sun can be used to credibly predict the geoeffectiveness of the CMEs being studied. The purpose of this study is to extend their survey by analyzing the halo-CME data for 1996-2006. The correlation of filament axial direction on the solar surface and the corresponding Bz signatures at L1 are used to form a more extensive analysis for the results previously presented by Aparna &amp; Martens. This study utilizes Solar and Heliospheric Observatory Extreme-ultraviolet Imaging Telescope 195 Å, Michelson Doppler Imager magnetogram images, and Kanzelhöhe Solar Observatory and Big Bear Solar Observatory Hα images for each particular time period, along with ACE data for interplanetary magnetic field signatures. Utilizing all these, we have found that the trend in Aparna &amp; Martens' study of a high likelihood of correlation between the axial field direction on the solar surface and Bz orientation persists for the data between 1996 and 2006, for which we find a match percentage of 65&amp;percnt;.

Keywords: Space weather, Solar filaments, Solar coronal mass ejections