C<sub>2</sub>O and C<sub>3</sub>O in low-mass star-forming regions

Urso, Riccardo Giovanni; Palumbo, M. E.; Ceccarelli, C.; Balucani, Nadia; Bottinelli, S.; Codella, C.; Fontani, F.; Leto, P.; Trigilio, C.; Vastel, C.; Bachiller, R.; Baratta, G. A.; Buemi, C. S.; Caux, E.; Al-Edhari, A. Jaber; Leflóch, B.; López-Sepulcre, A.; Umana, G.; Testi, L.

doi:10.1051/0004-6361/201834322

Cited by 10 publications

(8 citation statements)

References 108 publications

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“…The protonated form of this species, HCCCO + , has been recently detected in TMC-1 (Cernicharo et al 2020a). A study of CCO and CCCO in lowmass star-forming regions has been recently made by Urso et al (2019).…”

Section: Appendix A: Observed Line Parametersmentioning

confidence: 99%

Discovery of HCCCO and C₅O in TMC-1 with the QUIJOTE line survey

Cernicharo

Agúndez

Cabezas

et al. 2021

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We report on the detection, for the first time in space, of the radical HCCCO and of pentacarbon monoxide, C5O. The derived column densities are (1.6 ± 0.2) × 1011 cm−2 and (1.5 ± 0.2) × 1010 cm−2, respectively. We have also analysed the data for all the molecular species of the families HCnO and CnO within our QUIJOTE’s line survey. Upper limits are obtained for HC4O, HC6O, C4O, and C6O. We report a robust detection of HC5O and HC7O based on 14 and 12 rotational lines detected with a signal-to-noise ratio ≥30 and ≥5, respectively. The derived N(HC3O)/N(HC5O) abundance ratio is 0.09 ± 0.03, while N(C3O)/N(C5O) is 80 ± 2, and N(HC5O)/N(HC7O) is 2.2 ± 0.3. As opposed to the cyanopolyyne family, HC2n + 1N, which shows a continuous decrease in the abundances with increasing n, the CnO and HCnO species show a clear abundance maximum for n = 3 and 5, respectively. They also show an odd and even abundance alternation, with odd values of n being the most abundant, which is reminiscent of the behaviour of CnH radicals, where in that case species with even values of n are more abundant. We explored the formation of these species through two mechanisms previously proposed, which are based on radiative associations between CnHm+ ions with CO and reactions of Cn̄ and CnH− anions with O atoms, and we found that several species, such as C5O, HC4O, and HC6O, are significantly overestimated. Our understanding of how these species are formed is incomplete as of yet. Other routes based on neutral-neutral reactions such as those of Cn and CnH carbon chains with O, OH, or HCO, could be behind the formation of these species.

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Section: Appendix A: Observed Line Parametersmentioning

confidence: 99%

Discovery of HCCCO and C₅O in TMC-1 with the QUIJOTE line survey

Cernicharo

Agúndez

Cabezas

et al. 2021

A&A

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“…In this work, we are focusing on the preparation and characterization of the H 2 C 3 O +• radical cations, which attract considerable attention as potentially important species in astrochemistry, physical organic chemistry, and mass spectrometry. − In particular, it was suggested , that the H 2 C 3 O +• radical cations may be formed in the interstellar media (ISM) by the radiative association of C 2 H 2 +• and CO and be an important source of interstellar C 3 O. Based on the measured rate coefficients and product distributions of the H 2 C 3 O +• radical cation reactions with main interstellar constituents, Petrie et al , supposed a relatively long cloud lifetime for the H 2 C 3 O +• radical cation.…”

Section: Introductionmentioning

confidence: 99%

Formation and Evolution of H₂C₃O^+•Radical Cations: A Computational and Matrix Isolation Study

et al. 2022

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The family of isomeric H2C3O+• radical cations is of great interest for physical organic chemistry and chemistry occurring in extraterrestrial media. In this work, we have experimentally examined a unique synthetic route to the generation of H2C3O+• from the C2H2···CO intermolecular complex and also considered the relative stability and monomolecular transformations of the H2C3O+• isomers through high-level ab initio calculations. The structures, energetics, harmonic frequencies, hyperfine coupling constants, and isomerization pathways for several of the most important H2C3O+• isomers were calculated at the UCCSD(T) level of theory. The complementary FTIR and EPR studies in argon matrices at 5 K have demonstrated that the ionized C2H2···CO complex transforms into the E-HCCHCO+• isomer, and this latter species is supposed to be the key intermediate in further chemical transformations, providing a remarkable piece of evidence for kinetic control in low-temperature chemistry. Photolysis of this species at λ = 410–465 nm results in its transformation to the thermodynamically most stable H2CCCO+• isomer. Possible implications of the results and potentiality of the proposed synthetic strategy to the preparation of highly reactive organic radical cations are discussed.

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“…Such processes determine changes in the physical and chemical properties of ices (e.g. Tielens & Allamandola 1987;Greenberg et al 1995;Ehrenfreund et al 1999;Urso et al 2019). Frozen small bodies in the outer so-lar system are exposed to CR, solar wind (SW) and solar energetic particles (SEP) (e.g.…”

Section: Introductionmentioning

confidence: 99%

Irradiation dose affects the composition of organic refractory materials in space

Urso

Vuitton

Danger

et al. 2020

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Context. Near-and mid-infrared observations have revealed the presence of organic refractory materials in the Solar System, in cometary nuclei and on the surface of centaurs, Kuiper-belt and trans-neptunian objects. In these astrophysical environments, organic materials can be formed because of the interaction of frozen volatile compounds with cosmic rays and solar particles, and favoured by thermal processing. The analysis of laboratory analogues of such materials gives information on their properties, complementary to observations. Aims. We present new experiments to contribute to the understanding of the chemical composition of organic refractory materials in space. Methods. We bombard frozen water, methanol and ammonia mixtures with 40 keV H + and we warmed the by-products up to 300 K. The experiments enabled the production of organic residues that we analysed by means of infrared spectroscopy and by very high resolution mass spectrometry to study their chemical composition and their high molecular diversity, including the presence of hexamethylenetetramine and its derivatives. Results. We find that the accumulated irradiation dose plays a role in determining the composition of the residue. Conclusions. Based on the laboratory doses, we estimate the astrophysical timescales to be short enough to induce an efficient formation of organic refractory materials at the surface of icy bodies in the outer Solar System.

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C₂O and C₃O in low-mass star-forming regions

Cited by 10 publications

References 108 publications

Discovery of HCCCO and C₅O in TMC-1 with the QUIJOTE line survey

Discovery of HCCCO and C₅O in TMC-1 with the QUIJOTE line survey

Formation and Evolution of H₂C₃O^+•Radical Cations: A Computational and Matrix Isolation Study

Irradiation dose affects the composition of organic refractory materials in space

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C2O and C3O in low-mass star-forming regions

Cited by 10 publications

References 108 publications

Discovery of HCCCO and C5O in TMC-1 with the QUIJOTE line survey

Discovery of HCCCO and C5O in TMC-1 with the QUIJOTE line survey

Formation and Evolution of H2C3O+•Radical Cations: A Computational and Matrix Isolation Study

Irradiation dose affects the composition of organic refractory materials in space

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C₂O and C₃O in low-mass star-forming regions

Discovery of HCCCO and C₅O in TMC-1 with the QUIJOTE line survey

Discovery of HCCCO and C₅O in TMC-1 with the QUIJOTE line survey

Formation and Evolution of H₂C₃O^+•Radical Cations: A Computational and Matrix Isolation Study