Physical and chemical properties of galactic molecular gas toward QSO J1851+0035
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A90106%2F24%3A00617497" target="_blank" >RIV/67985815:90106/24:00617497 - isvavai.cz</a>
Result on the web
<a href="https://doi.org/10.3847/1538-4357/ad3d5b" target="_blank" >https://doi.org/10.3847/1538-4357/ad3d5b</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.3847/1538-4357/ad3d5b" target="_blank" >10.3847/1538-4357/ad3d5b</a>
Alternative languages
Result language
angličtina
Original language name
Physical and chemical properties of galactic molecular gas toward QSO J1851+0035
Original language description
Atacama Large Millimeter/submillimeter Array (ALMA) data toward QSO J1851+0035 (l = 33.degrees 498, b = +0.degrees 194) were used to study absorption lines by Galactic molecular gas. We detected 17 species (CO, 13CO, C18O, HCO+, H13CO+, HCO, H2CO, C2H, c-C3H, c-C3H2, CN, HCN, HNC, CS, SO, SiO, and C) and set upper limits to 18 species as reference values for chemical models. About 20 independent velocity components at 4.7-10.9 kpc from the Galactic center were identified. Their column density and excitation temperature estimated from the absorption study, as well as the CO intensity distributions obtained from the FUGIN survey, indicate that the components with tau less than or similar to 1 correspond to diffuse clouds or cloud outer edges. Simultaneous multiple-Gaussian fitting of CO J = 1-0 and J = 2-1 absorption lines shows that these are composed of narrow- and broad-line components. The kinetic temperature empirically expected from the high HCN/HNC isomer ratio (greater than or similar to 4) reaches greater than or similar to 40 K and the corresponding thermal width accounts for the line widths of the narrow-line components. CN-bearing molecules and hydrocarbons have tight and linear correlations within the groups. The CO/HCO+ abundance ratio showed a dispersion as large as 3 orders of magnitude with a smaller ratio in a smaller N(HCO+) (or lower A V) range. Some of the velocity components are detected in single-dish CO emission and ALMA HCO+ absorption but without corresponding ALMA CO absorption. This may be explained by the mixture of clumpy CO emitters not resolved with the similar to 1 pc single-dish beam surrounded by extended components with a very low CO/HCO+ abundance ratio (i.e., CO-poor gas).
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
—
Continuities
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Others
Publication year
2024
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Astrophysical Journal
ISSN
0004-637X
e-ISSN
1538-4357
Volume of the periodical
969
Issue of the periodical within the volume
2
Country of publishing house
GB - UNITED KINGDOM
Number of pages
48
Pages from-to
102
UT code for WoS article
001261102400001
EID of the result in the Scopus database
2-s2.0-85198492563