Search arXiv⌕ Search

arXiv · 2610.21205

A machine-learning-driven dataset of 144,111 polycyclic aromatic hydrocarbon infrared spectra for interpreting aromatic infrared bands

Abstract

The interpretation of interstellar aromatic infrared bands (AIBs) relies on reference spectral libraries, but the chemical space covered by existing databases remains incomplete relative to the vast structural diversity of polycyclic aromatic hydrocarbons (PAHs) expected in the interstellar medium. We present a large-scale, high-throughput PAH infrared (IR) spectral database that complements existing reference libraries by providing significantly more continuous coverage of the PAH chemical space for small to medium-sized PAHs. We used a machine-learning double-harmonic (ML-DH) framework that integrates neural network force fields with electronic dipole models. This framework achieves quantum-chemical accuracy at a fraction of the computational cost. It has been validated against independent density functional theory calculations and benchmark spectral databases. The resulting dataset comprises 144,111 IR spectra for 48,037 closed-shell, even-carbon benzenoid PAH structures across neutral, cationic, and anionic charge states, complete with per-spectrum uncertainty estimates. The spectral library, optimized geometries, and model code are publicly available. They can be used to complement existing libraries for interpreting and modeling JWST AIB observations and those from future IR missions.

Explore related subjects

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Xinghong Mai, Zu-Jia Lu, Zhao Wang. 2026-10-15. A machine-learning-driven dataset of 144,111 polycyclic aromatic hydrocarbon infrared spectra for interpreting aromatic infrared bands. https://doi.org/10.1051/0004-6361%2F202662240

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

ALMA observations towards M83 reveal N2H+ tracing dense gas

Galactic observations have shown that N2H+ intensities preferentially trace star-forming dense molecular gas compared with HCN or HCO+, which are conventionally used as dense-gas tracers in extragalactic studies. In this study, we aim to verify this trend in the nearby star-forming galaxy M83. Using ALMA, we observed the J=1-0 transitions of N2H+ and HCN, along with the 1-mm and 3-mm continuum, and analyzed the archival CO(1-0) data. The data achieved a spatial resolution of 48 pc in the southwestern bar-end region of M83, covering an area of 2.1 kpc x 1.8 kpc. N2H+ and HCN intensities are approximately linearly correlated, indicating that HCN luminosity can still reasonably predict the amount of dense gas as well as N2H+ luminosity does. However, in regions with high column densities, N2H+ becomes a super-linear function of HCN, suggesting that the N2H+ emission is more sensitive to dense gas than HCN. We employed a radiative transfer model that predicts line intensities as a function of column density, adopting parametric column density probability distribution functions (N-PDFs) to describe the underlying column density distribution. The model demonstrates that the observed linear or superlinear trend can be explained by a log-normal distribution only or a log-normal and a power-law tail distribution in the N-PDF. Furthermore, the N2H+ intensity is significantly more sensitive to the power-law tail than the HCN intensity. In addition, our analysis incorporating archival data shows that N2H+ is a less reliable tracer of dense gas in galactic center regions, where warmer temperatures may promote N2H+ destruction.

astro-ph.GA↗

An Energetic Consistency Test for Feedback-Driven Gas Loss in Milky Way Dwarf Satellites

Dwarf spheroidal galaxies (dSphs) contain little detectable cold gas, but the relative roles of stellar feedback, reionization, and environmental effects in their gas loss remain uncertain. We apply an order-of-magnitude energy-budget test to nine Milky Way dwarf satellites using published color--magnitude-diagram star formation histories (SFHs), galaxy-level velocity dispersions, effective radii, and integrated $V$-band luminosities. For each galaxy and halo prescription, we define the energy-equivalence time $τ_{\mathrm{E}}$, when a crossing exists, as the first elapsed time at which the cumulative effective energy from core-collapse supernovae equals the adopted gas binding energy. This quantity is an energetic diagnostic rather than a direct measurement of wind launch. Under the fiducial parameters, all nine galaxies reach the nominal threshold under the kinematic--size prescription K+B16, yet star formation often continues long after threshold crossing. We compare the corresponding lookback time $t_{\mathrm{E,lb}}$ with $t_{90,\mathrm{lb}}$, the lookback time at which 90\% of the total initial stellar mass had formed. Because both times are derived from the same cumulative SFH, their temporal proximity is interpreted descriptively rather than as independent evidence of feedback-driven quenching. Whether the threshold is reached depends on the adopted halo mass, radius, retained gas fraction, and supernova--gas coupling efficiency. These results distinguish the availability of sufficient cumulative feedback energy from the processes that determine the timing of quenching.

astro-ph.GA↗

Disk tilts in Milky Way-like galaxies and their link to mergers

We investigated disk reorientation and its relationship to mergers in a sample of 93 Milky Way-mass galaxies drawn from the TNG50 simulations. From this sample, we identified 117 individual disk-tilt events with clearly defined start and end times, and we divided them into two classes based on whether the disk evolves smoothly or undergoes rapid disruption and regrowth during the tilt duration. For each tilt event, we linked the most massive merger that occurs in close temporal association with it. We focus on those tilt events occurring during phases of smooth disk evolution, which typically show tilt rates below 10 degrees per Gyr, persist for 2-9 Gyr, and are generally connected to minor mergers. Roughly 40% of these events reach tilt angles exceeding 30 degrees, most often triggered by satellites whose masses are comparable to or less massive than the galaxy's total stellar mass, merging on tangential orbits with orbital angular momentum that is retrograde or nearly perpendicular to the disk spin. The satellite consistently drives the disk tilt toward alignment with the satellite's orbital spin; satellites that came in on retrograde orbits relative to the disk spin can thus induce large tilt angles and can produce an almost orthogonal configuration between the stellar disk and the satellite's orbital plane as an intermediate phase. Owing to the comparatively slow tilt rates, the stellar disk can keep stable and continue to grow throughout the reorientation process. Consequently, galaxies that experience strong disk tilts can still maintain stellar disks that are as thin as those in systems without significant reorientation.

astro-ph.GA↗