![Left. Two-dimensional UMAP representation of the TMC-1 inventory using the original ChemBERTa input vectors. Right. Same representation but using the last hidden layer of the neural netwok model. The red rectangle highlights the region of the UMAP representation where highly abundant molecules are located. The different dot sizes represent the observed column density of each molecule. -- [astro-ph.GA]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/10/A-neural.png?resize=1200%2C725&ssl=1)
[astro-ph.GA] The detection of new interstellar molecules is central to astrochemistry, and arguably the most transformative development in the field in past decade has been the increase in both number […]
astro-ph.GA
Posted inUncategorized
Complex Organic Molecules in Protostars with ALMA Spectral Surveys (COMPASS): I. Overview of the ALMA Large Program
[astro-ph.GA] It remains a fundamental research question in astrochemistry to characterize the inventory of complex organic molecules formed during the early stages of star formation, which may affect the eventual […]
![A comparison of the dominant heating and cooling mechanism for different times and at the time of the maximum temperature. Each model is started at 𝑇 = 10 K. -- [astro-ph.GA]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/10/UCLCHEM.png?resize=1200%2C716&ssl=1)
Posted inAstrochemistry
UCLCHEM 4.0: An Open Source Gas-grain Astrochemistry Simulation Framework
[astro-ph.GA] Astrochemical modeling is a key tool for the understanding of the formation and destruction of molecules in the dense gas of the interstellar medium, as observed by modern day […]
![Illustration of the spatial distribution and proposed origin of the molecular species discussed in this work, including the tentative FeS emission. Left: H2O v2 = 1 and NaCl emission maps toward Orion SrcI reported by A. Ginsburg et al. (2018). Right: schematic view of the proposed distinction between species associated with the outflow and those tracing the disk midplane, based on the results presented here (Table 1) and those of A. Ginsburg et al. (2018, 2019). -- [astro-ph.GA]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/10/Tentative-Detection.png?resize=1200%2C719&ssl=1)
Posted inAstrochemistry
Tentative Detection of FeS toward Orion SrcI
[astro-ph.GA] Iron sulfide (FeS) is a key refractory compound in astrophysical environments. It is commonly found in meteorites and evidence of FeS has only been reported in solid form in […]
Posted inAstrochemistry
Chemical Abundance Patterns at z=1-7: Carbon, Nitrogen, Neon, Sulphur, and Argon Abundances From JWST Spectroscopy
[astro-ph.GA] The relative abundances of chemical elements in the interstellar medium (ISM) trace the history of star formation and chemical enrichment in galaxies.
Posted inAstrochemistry
Resolving The Extended Interstellar Medium Of Infrared Galaxies I. Polycyclic Aromatic Hydrocarbon Emission
[astro-ph.GA] We investigate spatial variations in polycyclic aromatic hydrocarbon (PAH) properties and photoelectric heating efficiency in 67 nearby luminous infrared galaxies from the Great Observatories All-sky LIRG Survey (GOALS).
![Overview of the ML-DH framework. Top: Training stage, using DFT energies, forces, and dipoles to train the NNFF and EPNN. Bottom: Prediction stage, yielding IR spectra via NNFF optimization, normal mode analysis, and EPNN dipole derivatives.-- [astro-ph.GA]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/10/A-machine.png?resize=1200%2C719&ssl=1)
Posted inAstrochemistry
A Machine-learning-driven Dataset Of 144,111 Polycyclic Aromatic Hydrocarbon Infrared Spectra For Interpreting Aromatic Infrared Bands
[astro-ph.GA] 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 […]
![(Left) The N2H +/HCN ratio toward the central region of M83 shown in the color scale. The black contours show 3-mm continuum intensities with 0.5 mJy beam−1 increments. The beam size is shown at the bottom left corner. (Right) The same figure as Figure 2(a), but including data points from the galactic center region. The grey dashed lines have slopes of 1, and show the lines of constant N2H +/HCN ratios. -- [astro-ph.GA]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/10/ALMA-observations.png?resize=1200%2C722&ssl=1)
Posted inAstrochemistry
ALMA Observations Towards M83 Reveal N2H+ Tracing Dense Gas
[astro-ph.GA] 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.
Posted inAstrochemistry
Complex Organic Molecules In Protostars With ALMA Spectral Surveys (COMPASS) VII. First Interstellar Detection Of Fully Deuterated Methanol
[astro-ph.GA] There have been no robust identifications of fully deuterated methanol, CD3OD, in the interstellar medium (ISM) to date.
![Moment 0 maps of the molecular lines. (d) rms = 0.005 Jy beam−1 km s−1 (3, 4, 5, 6 σ); (e) rms = 0.0077 Jy beam−1 km s−1 (5, 7, 9, 11, 13, 15 σ); (f) rms = 0.009 Jy beam−1 km s−1 (5, 7, 9, 11 σ); (g) rms = 0.0039 Jy beam−1 km s−1 (3, 4, 5 σ). Close-up images of each panel are shown below. These regions are indicated by a white dashed square in panel (a). Color scales are adjusted for the close-up ones. The black and white contours are the continuum map same as in the right panel of Figure 1. -- [astro-ph.GA]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/10/A-Cyanopolyyne.png?resize=1200%2C721&ssl=1)
Posted inAstrochemistry
A Cyanopolyyne-rich But COM-poor Massive Protostar: The First Hot Carbon Chain Chemistry Source G28.28-0.36
[astro-ph.GA] We present molecular emission line data from the massive young stellar object (MYSO) G28.28-0.36 (G28.28) obtained with the Atacama Large Millimeter/submillimeter Array Band 3. Cyanopolyynes (HC3N and HC5N) and […]