[astro-ph.GA] There have been no robust identifications of fully deuterated methanol, CD3OD, in the interstellar medium (ISM) to date.
astro-ph.GA
![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 […]
Posted inAstrochemistry
The JWST Proto-PAH Project: Aromatic Backbones With Extensive Aliphatic Substitution Account For Both The Aromatic And Aliphatic mission
[astro-ph.GA] We find that the aromatic and aliphatic emission bands in four carbon-rich post-asymptotic giant branch stars with class D emission arise from a single carrier population: extensive aliphatic decoration […]
![Schematic representation of the evolution of sulfur in light of our experiments. The diagram provides a conceptual overview of sulfur depletion driven by visual extinction.-- [astro-ph.GA]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/10/Thermally.png?resize=1200%2C719&ssl=1)
Posted inAstrochemistry
Thermally Irreversible Sulfur Chemisorption On Silicate Grains As A Major Sulfur Reservoir In Molecular Clouds
[astro-ph.GA] Sulfur (S) chemistry in the interstellar medium remains poorly constrained due to the longstanding “missing sulfur” problem, where a significant fraction of cosmic sulfur in molecular clouds remains unidentified.
![The per-tile processing chain, applied to the Detector-4 tile of Fig. 1. (a) After flag masking and zodiacal-light subtraction, the input to the stellar subtraction. (b) After fitting and subtracting the empirical PSF at every catalogued source above the magnitude limit, with the saturated cores of the brightest stars masked. (c) After the median filter and the Gaussian smoothing to 2.6 ′ , which is what is coadded into the HEALPix maps. All three panels share a single histogram-equalised colour scale. -- [astro-ph.GA]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/10/A-Full-Sky.png?resize=1200%2C637&ssl=1)
Posted inAstrochemistry
A Full-Sky SPHEREx Map of Integrated 3.3 And 3.4 μm PAH Emission
[astro-ph.GA] Polycyclic aromatic hydrocarbons (PAHs) are ubiquitous in the interstellar medium and are among its smallest carbonaceous grains.
![Infrared spectra of pure H2S (blue) and H2O:H2S (10:1) (red) ice mixtures after UV irradiation followed by warm-up to room temperature, measured at 300 K. The residue from the H2S ice does not show any IR absorption band. Functional groups assigned to bands in the H2O:H2S (10:1) residue are indicated at the top; vibrational bands and assignments are also listed in Table 1, along with possible carrier species or chemical families producing those features. -- [astro-ph.GA]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/10/Water-.png?resize=1200%2C720&ssl=1)
Posted inAstrochemistry
Water Enhances The Formation Of Refractory Sulfur In Interstellar Ices
[astro-ph.GA] Sulfur is the tenth most abundant element in space, yet it is strongly depleted in the gas phase of dense interstellar regions, suggesting sequestration in dust grain components that […]
![Rest-frame equivalent widths of C iii] 𝜆𝜆1907, 1909 (left) and C iv 𝜆𝜆1548, 1550 (right) against the direct 𝑇e-based ([O III]𝜆4363) metallicity. Curves are the star-forming photoionisation grids of Nakajima et al. (2018) at a burst age of 1 Myr and log(𝑛H/cm−3 ) = 3. Solid curves represent the POPSTAR single-star models (Mollá et al. 2009), and dashed curves indicate the BPASS binary models (Eldridge et al. 2017), coloured by ionisation parameter as shown in the colour-bar. -- [astro-ph.GA]](https://i0.wp.com/astrobiology.com/wp-content/uploads/2026/10/Precise.png?resize=1200%2C720&ssl=1)
Posted inAstrochemistry
Precise C-N-O Abundances of Individual Galaxies In The First Billion Years From Ultra-Deep, Rest-UV-to-Optical JWST Spectroscopy
[astro-ph.GA] We present ultra-deep JWST/NIRSpec 𝑅 ∼ 1000 spectroscopy of nine star-forming galaxies at 𝑧 = 6.0 − 8.3 in the GOODSN field, drawn from the Origins of Metal Enrichment […]
Posted inAstrochemistry
The Abundance And Emission Of PAHs From The Local To Early Universe
[astro-ph.GA] We present the first large-volume cosmological simulation of galaxy evolution with a model for the abundance and luminous emission of Polycyclic Aromatic Hydrocarbons (PAHs) across a wide range of […]
Posted inAstrochemistry
Thioacetaldehyde (CH3CHS) On Interstellar Ices: A Key Molecule To Unravel Two Chemical Dichotomies In The ISM
[astro-ph.GA] Thioacetaldehyde (CH3CHS), recently detected in TMC-1, has an abundance approximately 36 times lower than its oxygen analog, acetaldehyde (CH3CHO). This makes the CH3CHS/CH3CHO pair the one with the largest […]
Posted inAstrochemistry
Interstellar Disparity: N- vs O-bearing Molecules: A Multidisciplinary Perspective across Interstellar Environments
[astro-ph.GA] Observations of O- and N-bearing molecules reveal systematic chemical differentiation across a wide range of interstellar environments.