0518 - Meta-analysis of human gut metagenomes reveals taxonomic and metabolic signatures of the presence of the methanogen M. smithii

Ruaud, Albane; Ley, Ruth E.

doi:10.26226/morressier.5b5199bfb1b87b000ecee301

Cited by 1 publication

(3 citation statements)

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“…To simulate the abundance of various COMs in hot cores, the NAUTILUS gas-grain chemical model (Ruaud et al 2016) was used with the fast warm-up model presented in Garrod (2013). This chemical model computes the time evolution of species in three-phases, gas-phase, grain surface, and grain mantle.…”

Section: The Chemical Modelmentioning

confidence: 99%

“…This chemical model computes the time evolution of species in three-phases, gas-phase, grain surface, and grain mantle. All the physico-chemical processes included in the model can be found with their corresponding equations in Ruaud et al (2016). The gas-phase chemistry is described by the public network kida.uva.2014 (Wakelam et al 2015).…”

Section: The Chemical Modelmentioning

confidence: 99%

“…For the initial composition, we used the initial abundances from Ruaud et al (2016) assuming that the chemical evolution started from atomic form except for H 2 . Elements with an ionization potential below 13.6 eV, corresponding to that of hydrogen, C, S, Si, Fe, Na, Mg, Cl, and P were initially singly ionized.…”

Section: The Chemical Modelmentioning

confidence: 99%

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The Difference in Abundance between N-bearing and O-bearing Species in High-mass Star-forming Regions

Suzuki

Ohishi

Saito

et al. 2018

ApJS

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The different spatial distributions of N-bearing and O-bearing species, as is well known towards Orion KL, is one of the long-lasting mysteries. We conducted a survey observation and chemical modeling study to investigate if the different distributions of O-and N-bearing species are widely recognized in general star-forming regions. First, we report our observational results of complex organic molecules (COMs) with the 45 m radio telescope at the Nobeyama Radio Observatory towards eight star-forming regions. Through our spectral survey ranging from 80 to 108 GHz, we detected CH 3 OH, HCOOCH 3 , CH 3 OCH 3 , (CH 3 ) 2 CO, CH 3 CHO, CH 3 CH 2 CN, CH 2 CHCN, and NH 2 CHO. Their molecular abundances were derived via the rotation diagram and the least squares methods. We found that N-bearing molecules, tend to show stronger correlations with other N-bearing molecules rather than O-bearing molecules. While G10.47+0.03 showed high fractional abundances of N-bearing species, those in NGC6334F were not so rich, being less than 0.01 compared to CH 3 OH. Then, the molecular abundances towards these sources were evaluated by chemical modeling with NAUTILUS three-phase gas-grain chemical code. Through the simulations of time evolutions for the abundances of COMs, we suggest that observed correlations of fractional abundances between COMs can be explained by the combination of the different temperature structures inside the hot cores and the different evolutionary phase. Since our modeling could not fully explain the observed excitation temperatures, it is important to investigate the efficiency of grain surface reactions and their activation barriers, and the binding energy of COMs to further promote our understanding.

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Section: The Chemical Modelmentioning

confidence: 99%

Section: The Chemical Modelmentioning

confidence: 99%