On the Synthesis of Chocolate Flavonoids (Propanols, Butanals) in the Interstellar Medium

Abplanalp, Matthew J.; Góbi, Sándor; Bergantini, Alexandre; Turner, Andrew M.; Kaiser, Ralf I.

doi:10.1002/cphc.201701350

Cited by 13 publications

(12 citation statements)

References 22 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…[69] Most important, since the fundamentals of functional groups such as of carbonyls in COMs potentially synthesized during the radiation processing of acetaldehyde often fall in the same range, infrared spectroscopy rarely allows an identification of individual COMs. [63,70] Therefore, an alternative analytical technique is critical to probe discrete organics in the irradiated ices. Figure 3.…”

Section: Resultsmentioning

confidence: 99%

On the Formation of the Popcorn Flavorant 2,3‐Butanedione (CH₃COCOCH₃) in Acetaldehyde‐Containing Interstellar Ices

et al. 2020

Self Cite

View full text Add to dashboard Cite

show abstract

Section: Resultsmentioning

confidence: 99%

On the Formation of the Popcorn Flavorant 2,3‐Butanedione (CH₃COCOCH₃) in Acetaldehyde‐Containing Interstellar Ices

et al. 2020

Self Cite

View full text Add to dashboard Cite

show abstract

“…Further increasing the interest of n-and i-butanal (also known as n-and i-butyraldehyde and hereafter n-PrCHO and i-PrCHO, respectively) as astronomical candidates, Abplanalp et al (2018) revealed that both isomers -together with distinct C 3 H 8 O species, such as propanol and methyl ethyl ether (the latter was already detected in the ISM toward Orion KL by Tercero et al 2018and toward IRAS 16293-2422A by Manigand et al 2020) -could be generated by exposing interstellar analog ices to ionizing radiation. Therefore, they should be detectable in the gas phase after desorption from the icy grains in regions of star formation (Abplanalp & Kaiser 2019).…”

Section: Introductionmentioning

confidence: 99%

Toward the limits of complexity of interstellar chemistry: Rotational spectroscopy and astronomical search for n- and i-butanal

Sanz-Novo

Беллоче

Rivilla

et al. 2022

A&A

View full text Add to dashboard Cite

Context. In recent times, large organic molecules of exceptional complexity have been found in diverse regions of the interstellar medium. Aims. In this context, we aim to provide accurate frequencies of the ground vibrational state of two key aliphatic aldehydes, n-butanal and its branched-chain isomer, i-butanal, to enable their eventual detection in the interstellar medium. We also want to test the level of complexity that interstellar chemistry can reach in regions of star formation. Methods. We employ a frequency modulation millimeter-wave absorption spectrometer to measure the rotational features of n-and i-butanal. We analyze the assigned rotational transitions of each rotamer separately using the A-reduced semirigid-rotor Hamiltonian. We use the spectral line survey ReMoCA performed with the Atacama Large Millimeter/submillimeter Array to search for n-and i-butanal toward the star-forming region Sgr B2(N). We also search for both aldehydes toward the molecular cloud G+0.693-0.027 with IRAM 30 m and Yebes 40 m observations. The observational results are compared with computational results from a recent gas-grain astrochemical model. Results. Several thousand rotational transitions belonging to the lowest-energy conformers of two distinct linear and branched isomers have been assigned in the laboratory spectra up to 325 GHz. A precise set of the relevant rotational spectroscopic constants has been determined for each structure as a first step toward identifying both molecules in the interstellar medium. We report non-detections of n-and i-butanal toward both sources, Sgr B2(N1S) and G+0.693-0.027. We find that n-and i-butanal are at least 2-6 and 6-18 times less abundant than acetaldehyde toward Sgr B2(N1S), respectively, and that n-butanal is at least 63 times less abundant than acetaldehyde toward G+0.693-0.027. While propanal is not detected toward Sgr B2(N1S) either, with an abundance at least 5-11 lower than that of acetaldehyde, propanal is found to be 7 times less abundant than acetaldehyde in G+0.693-0.027. Comparison with astrochemical models indicates good agreement between observed and simulated abundances (where available). Grain-surface chemistry appears sufficient to reproduce aldehyde ratios in G+0.693-0.027; gas-phase production may play a more active role in Sgr B2(N1S). Model estimates for the larger aldehydes indicate that the observed upper limits may be close to the underlying values. Conclusions. Our astronomical results indicate that the family of interstellar aldehydes in the Galactic center region is characterized by a drop of one order of magnitude in abundance at each incrementation in the level of molecular complexity.

show abstract

“…Hudson et al (2017) were able to form propanal by proton irradiation of a CO 2 :C 3 H 6 ice mixture at 10 K. H 2 O: 13 CH 3 OH:NH 3 78 K ice exposed to UV photons and heated to room temperature also yielded propanal (de Marcellus et al 2015). Propanol was reported to be formed by electron irradiation of a 13 CO: 13 CD 4 ice mixture at 5 K in experiments that did not allow to discriminate between 1and 2-propanol (Abplanalp et al 2018a).…”

Section: Introductionmentioning

confidence: 99%

Formation of interstellar propanal and 1-propanol ice: a pathway involving solid-state CO hydrogenation

Qasim

Fedoseev

Chuang

et al. 2019

A&A

View full text Add to dashboard Cite

Context. 1-propanol (CH 3 CH 2 CH 2 OH) is a three carbon-bearing representative of the primary linear alcohols that may have its origin in the cold dark cores in interstellar space. To test this, we investigated in the laboratory whether 1-propanol ice can be formed along pathways possibly relevant to the prestellar core phase. Aims. We aim to show in a two-step approach that 1-propanol can be formed through reaction steps that are expected to take place during the heavy CO freeze-out stage by adding C 2 H 2 into the CO + H hydrogenation network via the formation of propanal (CH 3 CH 2 CHO) as an intermediate and its subsequent hydrogenation. Methods. Temperature programmed desorption-quadrupole mass spectrometry (TPD-QMS) was used to identify the newly formed propanal and 1-propanol. Reflection absorption infrared spectroscopy (RAIRS) was used as a complementary diagnostic tool. The mechanisms that can contribute to the formation of solid-state propanal and 1-propanol, as well as other organic compounds, during the heavy CO freeze-out stage are constrained by both laboratory experiments and theoretical calculations. Results. Here it is shown that recombination of HCO radicals formed upon CO hydrogenation with radicals formed via C 2 H 2 processing -H 2 CCH and H 3 CCH 2 -offers possible reaction pathways to solid-state propanal and 1-propanol formation. This extends the already important role of the CO hydrogenation chain to the formation of larger complex organic molecules (COMs). The results are compared with ALMA observations. The resulting 1-propanol:propanal ratio concludes an upper limit of < 0.35 − 0.55, which is complemented by computationally derived activation barriers in addition to the experimental results.

show abstract

On the Synthesis of Chocolate Flavonoids (Propanols, Butanals) in the Interstellar Medium

Cited by 13 publications

References 22 publications

On the Formation of the Popcorn Flavorant 2,3‐Butanedione (CH₃COCOCH₃) in Acetaldehyde‐Containing Interstellar Ices

On the Formation of the Popcorn Flavorant 2,3‐Butanedione (CH₃COCOCH₃) in Acetaldehyde‐Containing Interstellar Ices

Toward the limits of complexity of interstellar chemistry: Rotational spectroscopy and astronomical search for n- and i-butanal

Formation of interstellar propanal and 1-propanol ice: a pathway involving solid-state CO hydrogenation

Contact Info

Product

Resources

About

On the Synthesis of Chocolate Flavonoids (Propanols, Butanals) in the Interstellar Medium

Cited by 13 publications

References 22 publications

On the Formation of the Popcorn Flavorant 2,3‐Butanedione (CH3COCOCH3) in Acetaldehyde‐Containing Interstellar Ices

On the Formation of the Popcorn Flavorant 2,3‐Butanedione (CH3COCOCH3) in Acetaldehyde‐Containing Interstellar Ices

Toward the limits of complexity of interstellar chemistry: Rotational spectroscopy and astronomical search for n- and i-butanal

Formation of interstellar propanal and 1-propanol ice: a pathway involving solid-state CO hydrogenation

Contact Info

Product

Resources

About

On the Formation of the Popcorn Flavorant 2,3‐Butanedione (CH₃COCOCH₃) in Acetaldehyde‐Containing Interstellar Ices

On the Formation of the Popcorn Flavorant 2,3‐Butanedione (CH₃COCOCH₃) in Acetaldehyde‐Containing Interstellar Ices