Scott Sommerfeldt Elected ASA President

We present Atacama Large Millimeter/submillimeter Array (ALMA) Cycle 7 12CO(2−1) observations of the circumnuclear disk in NGC 315 at an angular resolution of , improving on past measurements and resolving the sphere of influence (SOI) of the supermassive black hole (SMBH), whose mass has been estimated previously as MBH  M⊙. The high spatial resolution and sensitivity enable robust full-cube forward modeling of the molecular gas kinematics and a direct comparison of multiple independent gas-based dynamical modeling techniques. We apply standard Bayesian codes using both Markov chain Monte Carlo (MCMC) and nested sampling approaches, as well as a frequentist code to the same data set, exploring systematic uncertainties associated with the stellar mass distribution, gas surface-brightness parameterization, and disk geometry. All methods yield consistent black hole masses, indicating that the inferred MBH is not strongly method-dependent. Combining the ensemble of independent molecular-gas-based models, we derive an ensemble median black hole mass of (stat)(sys), where the comparable contributions to the full error budget arise from modeling systematics rather than formal fitting uncertainties. Our MBH is consistent with the empirical MBH–σ⋆ and MBH–Lbulge scaling relations, and lies 32% below an independent stellar-dynamical measurement—a discrepancy we discuss in the context of systematic differences between gas- and stellar-based methods. NGC 315 serves as a benchmark for quantifying molecular gas-dynamical MBH systematic uncertainties and for future cross-comparisons of gaseous and stellar dynamical approaches.

We investigate how local magnetic correlations evolve when the classical pyrochlore spin ice Ho₂Ti₂O₇ is transformed into the partially disordered stuffed compound Ho₂TiO₅. Neutron scattering measurements were analyzed using real space magnetic pair distribution function, reciprocal space reverse Monte Carlo, and half-polarized neutron powder diffraction methods to connect the average crystal structure with local magnetic correlations. Both compounds retain long-range 𝐹𝑑3𝑚 symmetry, but in Ho₂TiO₅ the average structure does not fully capture the local Ho–O, Ti–O, and O–O bond-length disorder associated with partial Ho/Ti occupancy. Despite this disorder, half-polarized neutron powder diffraction shows that the Ho moments retain local ⟨111⟩ Ising anisotropy and form spin-in/spin-out configurations on the tetrahedral network. In Ho₂Ti₂O₇, real- and reciprocal-space analyses show a nearly ideal 2-in/2-out spin ice state at 0.3 K, with ∼95% of tetrahedra satisfying the ice rule, followed by progressive thermal disordering on warming. In Ho₂TiO₅, most tetrahedra are magnetically incomplete because some tetrahedral vertices are occupied by nonmagnetic Ti rather than Ho; nevertheless, the dominant incomplete configurations are 2-in/1-out and 1-in/2-out, which are locally compatible with the ice rule if the missing Ho spin is restored. Ho₂TiO₅ is therefore a vacancy-disrupted spin ice in which the local ⟨111⟩ Ising character and short-range spin-in/spin-out correlations persist on a topologically incomplete magnetic network, while collective ice-rule correlations are strongly disrupted.

Raman spectroscopy is a promising label-free approach for noninvasive glucose sensing, but quantitative system design requires accurate knowledge of how strongly individual glucose bands scatter light. We report experimentally measured relative Raman scattering cross sections for several aqueous glucose bands in the fingerprint region (300 − 1500 cm⁻¹). Measurements were performed using a Raman microscope under fixed optical conditions, with neat liquid cyclohexane as a reference standard. A custom dual-reservoir sample holder enabled alternating reference and sample measurements to improve repeatability. Relative cross sections were measured using both 532 nm and 785 nm excitation. The excitation-wavelength dependence of the cross sections was then modeled using these measurements combined with literature values at 514.5 nm. For the four bands considered in this work (444 cm⁻¹, 516 cm⁻¹, 1066 cm⁻¹, 1124 cm⁻¹), our cross section values range from 0.62×10−30 to 0.76×10−30 cm²molecule⁻¹sr⁻¹ for 785 nm excitation, and 4.1×10⁻³⁰ to 4.6×10⁻³⁰ cm²molecule⁻¹sr⁻¹ for 532 nm excitation. These values match well with the existing literature and expected wavelength dependence, and the resulting wavelength-dependence models can provide quantitative inputs for designing compact Raman glucose sensing systems.

Two essential points of consideration for spherical directivity measurements are the measurement radius and the sound source's location relative to the evaluation surface. When spatial constraints, such as anechoic chamber size, limit the measurement radius, both points may lead to measured near-field directivity patterns deviating from the desired far-field radiation characteristics. To clarify the impact of source placement on near-field and far-field radiation patterns, this work develops far-field magnitude and phase relations between untranslated and translated sources. The resulting theory shows that far-field propagation via acoustical holography is sufficient to correct for source-positioning uncertainties, provided that the measurements incorporate sufficient sampling positions to avoid spatial aliasing. The magnitude equivalence of translated and untranslated far-field directivity patterns also enables an acoustic centering procedure that overcomes previous low-frequency limitations.

The Falcon 9 Block 5 is the world's most frequently launched orbital rocket, with 165 launches in 2025 alone. This cadence enables robust characterization of launch noise from repeated field measurements. This study analyzes 548 acoustic measurements from 76 Falcon 9 launches at Vandenberg Space Force Base (VSFB), spanning pad-to-station distances from approximately 230 m to 30 km. Mixed-effects models are developed to describe maximum sound level (⁠ 

⁠) and sound exposure level (SEL), including A- and C-weighted metrics, as functions of distance. Variability is modeled using a power-law variance structure, revealing increasing heteroskedasticity with distance. Prediction intervals derived from this structure quantify the range of expected individual measurements. Comparisons with Starship Super Heavy Flight 6 and launches from Florida suggest the model form is broadly applicable, though coefficients vary by vehicle. Additional analyses examine seasonal, diurnal, and terrain effects. Seasonal and diurnal effects are small for the present dataset, whereas terrain shielding can produce systematic reductions in level. Overall, this work provides a statistically grounded description of Falcon 9 launch noise and its variability and establishes a measured reference dataset for evaluation and future development of launch-noise prediction models.

When rockets ascend, accelerate, and pitch over toward orbit, they can generate sonic booms audible on the ground over 100 km from the launch site, as observed with recent launches from Vandenberg Space Force Base. The locations where these booms arrive vary seasonally, with some areas experiencing them only at certain times of year. In this paper, the seasonal variation is explored and modeled using pcboom 7.5.0, with simulations run using measured and modeled weather profiles from 2020 to 2025. pcboom peak overpressure footprints were interpolated to four locations where sonic booms have been reported and measured: Carpinteria, Ojai, Ventura, and Oxnard. The probability of a sonic boom occurring at each location was higher in the winter and lower in the summer (all seasons defined in the northern hemisphere). Changes in the footprint location were linked to seasonal changes in weather. Specifically, the changes in upper-level winds (stratospheric and mesospheric) influenced large changes in the land area that received a sonic boom. Strategic seasonal launch scheduling for missions should be considered to enable launches along all azimuths while minimizing the occurrence of sonic booms on land.