SOFIA observations provide the first experimental magnetic-dipole hyperfine constants for [13C II] and refined centroid frequency using astronomical data.
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- background 2023; Contreras et al. 2023a; Ortega- Martinez et al. 2024). Each emulator can vary the SHAMe-SF parameters, cosmological parameters (σ8,Ω m,Ω b,n s,handM ν), redshift, and number density simultaneously within the follow- ing ranges for the SHAMe-SF parameters: β∈[0,20] γ∈[−10,25] ∆γ∈[−10,10] V1 ∈[10 1.2,10 3.5] (km/s) ∆V1 ∈[10 0.2,10 1.9] (km/s) σ∈[0,1.7] fk,(cen+sat)/2 ∈[−1,1] fk,(cen−sat)/2 ∈[−1,1] α0 ∈[0,8] αexp ∈[−8,8] (4) Mcrit ∈[9,14.5] (log(h −1M⊙)), for the cosmological parameters: σ8 ∈
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astro-ph.GA 83 astro-ph.HE 38 astro-ph.CO 17 astro-ph.EP 15 astro-ph.SR 12 astro-ph.IM 7 gr-qc 2 cs.LG 1 physics.plasm-ph 1 stat.ML 1roles
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TopoFisher optimizes trainable filtrations, vectorizations, and compressors in persistent homology to maximize Fisher information, yielding higher information than fixed cosmological summaries and approaching neural baselines with far fewer parameters while generalizing better under simulator shifts
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Dust grain size distributions evolve from large-grain dominated at high redshift to MRN-like at low redshift, driven primarily by shattering and ISM accretion after stars supply initial large grains, reproducing z=0 dust masses and Milky Way extinction properties.
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MELTYQ couples magma-atmosphere equilibrium models with spectral retrievals to constrain sub-Neptune magma oxidation states and volatile inventories from transmission spectra.
Spectroscopic members of the M92 stream yield a Milky Way bar pattern speed of 29.1 +0.7/-0.4 km s^{-1} kpc^{-1}.
New publicly available X-ray table models RXToPo and RXagn1 with realistic AGN geometries (torus, polar cone, disk, BLR) generated via RefleX and tested on NGC 424.
Lumen modeling of IllustrisTNG50 shows that high ionization parameters from massive star clusters plus enhanced nitrogen abundances are needed to reproduce the extreme [OIII]/Hβ, [OIII]/[OII], and [NII]/Hα ratios seen in z>3 galaxies.
Direct [OIII]4364-based metallicities show that galaxies with stellar masses 10^6.7-9 solar masses at z~6-8 are 0.3-0.5 dex more metal-poor than local galaxies of the same mass, with slope 0.25 and 0.2 dex scatter.
A new fitting methodology applied to UV absorption data recovers radial trends in galactic wind velocities and mass-loading factors by constraining initial hot and cool phase parameters in a multiphase model.
Cosmic ray transport in molecular cloud simulations boosts star formation efficiency by up to 43% and yields a top-heavier IMF with a high-mass slope shallower by ~20%.
First implementation of the complete Braginskii magnetized viscosity tensor in FLASH shows it damps vortices, converts kinetic energy to heat, reduces Rayleigh-Taylor growth, and preserves yield in MagLIF-relevant runs.
Massive black hole binary mergers produce orphaned low-frequency signals in PTA pulsar terms that can be stacked for archival multiband gravitational-wave detection.
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The double-white-dwarf model for sources like CHIME/ILT J1634+44 predicts a beat-period drift of |P_b dot| ~ 10^{-10} s s^{-1}, producing tens of seconds of O-C timing drift in one year and enabling a minimal falsifiable test via joint period and derivative measurements.
First obliquity measurement in an M dwarf binary shows alignment, with tentative evidence that aligned orbits around cool stars and wide separations also hold for brown dwarfs and binaries.
Simulations indicate the Balmer decrement can serve as a diagnostic to identify inflowing gas in front of face-on galaxies, showing a mean front-back offset of approximately -0.14 despite scatter from clumpy dust.
Filament dark matter density profiles become nearly universal when scaled by terminal halo virial radii, with the inner cusp produced by embedded halos and the smooth component showing a flat core that evolves from smooth to clumpy accretion.
Bar pattern speeds anti-correlate with stellar and total dynamical mass in 30 galaxies, placing the slowest bars in the most massive systems and supporting angular momentum transfer to dark matter.
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JWST Nebular Spectroscopy of SN 2023qov: Circumstellar Dust Emission in a Normal Type Ia Supernova
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Dust and Grain Size Evolution in Galaxy Simulations: What Matters and What Does Not
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Coupling magma-ocean and atmospheres in spectral retrievals of sub-Neptunes
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Constraining the Galactic bar using the M92 stellar stream
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The study of the circumnuclear environment of accreting supermassive black holes with realistic X-ray spectral models
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Origins of Extreme Emission-Line Ratios in z > 3 Galaxies: Insights from the Lumen Model
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A Glimpse of the Low-Mass End of the Direct Mass-Metallicity Relation at $z\sim6-8$
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Gauging the Impact of Cosmic Ray Feedback on the Stellar Initial Mass Function
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Development of Anisotropic Magnetized Viscosity for Magnetized Liner Inertial Fusion Simulations in FLASH
First implementation of the complete Braginskii magnetized viscosity tensor in FLASH shows it damps vortices, converts kinetic energy to heat, reduces Rayleigh-Taylor growth, and preserves yield in MagLIF-relevant runs.
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Archival Multiband Gravitational-Wave Signals from Massive Black Hole Binary Mergers
Massive black hole binary mergers produce orphaned low-frequency signals in PTA pulsar terms that can be stacked for archival multiband gravitational-wave detection.
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Photometric Identification of Unresolved Binary Stars in Nearby Open Star Clusters
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A Census of Na D-traced neutral ISM and outflows at $0.6<z<4$
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A Falsifiable Timing Test for the Double-White-Dwarf Model of Long-Period Transients
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An Aligned Very-Low-Mass Star Orbiting an M dwarf and Obliquity Patterns Across Giant Planets, Brown Dwarfs, and Binary Stars
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The Role of Baryonic and Dark Matter in Bar Kinematics
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Strong Progenitor Age Bias in Supernova Cosmology. III. Progenitor Age as the Physical Origin of the Type Ia Supernova Magnitude Steps with Host Properties
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Tracing the kinematic perturbations of the Milky Way spiral arms with APOGEE DR17 and Gaia DR3
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$V/\sigma$ Trends with Mass for Dwarf Galaxies from the Marvelous Massive Dwarfs Suite
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Binary Evolution Can Mimic the Pair-Instability Mass Gap in Black Hole Mergers
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