Probing sulphur chemistry in oxygen-rich asymptotic giant branch stars with ALMA

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A90106%2F25%3A00646437" target="_blank" >RIV/67985815:90106/25:00646437 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1051/0004-6361/202555994" target="_blank" >https://doi.org/10.1051/0004-6361/202555994</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202555994" target="_blank" >10.1051/0004-6361/202555994</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Probing sulphur chemistry in oxygen-rich asymptotic giant branch stars with ALMA

Popis výsledku v původním jazyce

Sulphur and its isotopic ratios play a crucial role in our understanding of the physical properties of astrophysical environments, in particular, providing key insights into nucleosynthesis, interstellar medium processes, star formation, planetary system evolution, and galactic chemical evolution. Aims. We aim to investigate the distribution of sulphur species SO2, (SO2)-S-34, SO, and (SO)-S-34 towards a sample of five oxygen-rich asymptotic giant branch (AGB) stars, along with measurements of excitation temperature, column density, and isotopic ratios. Methods. We used ALMA Band 6, 7, and 8 data of o Ceti, R Dor, W Hya, R Leo, and EP Aqr. SO2,(SO2)-S-34, SO, and (SO)-S-34 were detected towards AGB stars using the CASSIS software. To estimate the gas temperature and column density of these species, we applied the rotational diagram method (when applicable) and the Markov chain Monte Carlo method, assuming local thermodynamic equilibrium (LTE). Finally, line imaging of different transitions was performed to infer the distributions of the detected sulphur-bearing species in our sample. Results. The measured excitation temperatures of SO2 for our sample sources range from similar to 200 to 600 K, with estimated column densities in the range of 1-7 x 10(16) cm(-2). The excitation temperatures estimated using (SO2)-S-34 are comparable or slightly lower, while the column densities are about an order of magnitude lower than those of SO2. Our measured S-32/S-34 ratios for R Dor and W Hya are close to the solar value, however, the measured value for o Ceti is slightly higher, and the measured values for EP Aqr and R Leo are lower. Finally, spatial analysis shows that most detected lines appear as centralized emissions. Moreover, the high excitation transitions of SO2 show compact emission and probe hot gas of the inner region circumstellar envelopes (CSEs), whereas low-excitation transitions trace slightly extended structures. However, we find some differences in the emission of detected species across our sample. Conclusions. The excitation temperature of the observed regions of the CSE can be probed using the SO2 molecule. The morphological correlation between SO and SO2 emissions suggests that they are chemically linked. Differences in the emission distributions of the detected species across our sample of low mass-loss rate AGB stars such as (i) centralized emission towards o Ceti with irregular emission shapes, (ii) centralized emission with ordered circular features towards R Leo and W Hya, (iii) clumpy emission features in R Dor, and (iv) unresolved emission in Ep Aqr may arise from several factors, i.e. the physical conditions of the sources (e.g. density and temperature structures of the CSEs), source multiplicity, outflows, rotation, or other associated physical processes such as thermal and nonthermal desorption, the effects of UV photons and cosmic rays, and finally the resolution of our observations. Nonetheless, the predominantly centralized distributions of SO and SO2 in our sample support previous findings for low mass-loss rate AGB stars.

Název v anglickém jazyce

Probing sulphur chemistry in oxygen-rich asymptotic giant branch stars with ALMA

Popis výsledku anglicky

Sulphur and its isotopic ratios play a crucial role in our understanding of the physical properties of astrophysical environments, in particular, providing key insights into nucleosynthesis, interstellar medium processes, star formation, planetary system evolution, and galactic chemical evolution. Aims. We aim to investigate the distribution of sulphur species SO2, (SO2)-S-34, SO, and (SO)-S-34 towards a sample of five oxygen-rich asymptotic giant branch (AGB) stars, along with measurements of excitation temperature, column density, and isotopic ratios. Methods. We used ALMA Band 6, 7, and 8 data of o Ceti, R Dor, W Hya, R Leo, and EP Aqr. SO2,(SO2)-S-34, SO, and (SO)-S-34 were detected towards AGB stars using the CASSIS software. To estimate the gas temperature and column density of these species, we applied the rotational diagram method (when applicable) and the Markov chain Monte Carlo method, assuming local thermodynamic equilibrium (LTE). Finally, line imaging of different transitions was performed to infer the distributions of the detected sulphur-bearing species in our sample. Results. The measured excitation temperatures of SO2 for our sample sources range from similar to 200 to 600 K, with estimated column densities in the range of 1-7 x 10(16) cm(-2). The excitation temperatures estimated using (SO2)-S-34 are comparable or slightly lower, while the column densities are about an order of magnitude lower than those of SO2. Our measured S-32/S-34 ratios for R Dor and W Hya are close to the solar value, however, the measured value for o Ceti is slightly higher, and the measured values for EP Aqr and R Leo are lower. Finally, spatial analysis shows that most detected lines appear as centralized emissions. Moreover, the high excitation transitions of SO2 show compact emission and probe hot gas of the inner region circumstellar envelopes (CSEs), whereas low-excitation transitions trace slightly extended structures. However, we find some differences in the emission of detected species across our sample. Conclusions. The excitation temperature of the observed regions of the CSE can be probed using the SO2 molecule. The morphological correlation between SO and SO2 emissions suggests that they are chemically linked. Differences in the emission distributions of the detected species across our sample of low mass-loss rate AGB stars such as (i) centralized emission towards o Ceti with irregular emission shapes, (ii) centralized emission with ordered circular features towards R Leo and W Hya, (iii) clumpy emission features in R Dor, and (iv) unresolved emission in Ep Aqr may arise from several factors, i.e. the physical conditions of the sources (e.g. density and temperature structures of the CSEs), source multiplicity, outflows, rotation, or other associated physical processes such as thermal and nonthermal desorption, the effects of UV photons and cosmic rays, and finally the resolution of our observations. Nonetheless, the predominantly centralized distributions of SO and SO2 in our sample support previous findings for low mass-loss rate AGB stars.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

—

Rok uplatnění

2025

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astronomy & Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Svazek periodika

704

Číslo periodika v rámci svazku

Dec.

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

21

Strana od-do

A31

Kód UT WoS článku

001627823900006

EID výsledku v databázi Scopus

2-s2.0-105023554165