Detection of OD towards the low-mass protostar IRAS 16293−2422

Parise, B.; Du, Fujun; Liu, F.-C.; Беллоче, А.; Wiesemeyer, H.; Güsten, R.; Menten, K. M.; Hübers, Heinz‐Wilhelm; Klein, Bernd

doi:10.1051/0004-6361/201218784

Cited by 32 publications

(31 citation statements)

References 25 publications

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“…An early search for the simplest amino acid, glycine, was unsuccessful (Ceccarelli et al 2000b). IRAS16293 has also been surveyed with the HIFI instrument on the Herschel Space Observatory in various bands between 460 GHz and 2 THz Hily-Blant et al 2010;Bacmann et al 2010;Bottinelli et al 2014) as well as the GREAT instrument on SOFIA (Parise et al 2012), revealing various (deuterated) hydrides, water lines (see below) and high-excitation lines of heavier molecules.…”

Section: Single-dish Observationsmentioning

confidence: 99%

The ALMA Protostellar Interferometric Line Survey (PILS)

Jørgensen

Wiel

Coutens

et al. 2016

A&A

374

582

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Context. The inner regions of the envelopes surrounding young protostars are characterised by a complex chemistry, with prebiotic molecules present on the scales where protoplanetary disks eventually may form. The Atacama Large Millimeter/submillimeter Array (ALMA) provides an unprecedented view of these regions zooming in on Solar System scales of nearby protostars and mapping the emission from rare species. Aims. The goal is to introduce a systematic survey, "Protostellar Interferometric Line Survey (PILS)", of the chemical complexity of one of the nearby astrochemical templates, the Class 0 protostellar binary IRAS 16293−2422, using ALMA, to understand the origin of the complex molecules formed in its vicinity. In addition to presenting the overall survey, the analysis in this paper focuses on new results for the prebiotic molecule glycolaldehyde, its isomers and rarer isotopologues and other related molecules.Methods. An unbiased spectral survey of IRAS 16293−2422 covering the full frequency range from 329 to 363 GHz (0.8 mm) has been obtained with ALMA, in addition to a few targeted observations at 3.0 and 1.3 mm. The data consist of full maps of the protostellar binary system with an angular resolution of 0.5 (60 AU diameter), a spectral resolution of 0.2 km s −1 and a sensitivity of 4-5 mJy beam −1 km s −1 -approximately two orders of magnitude better than any previous studies. Results. More than 10,000 features are detected toward one component in the protostellar binary, corresponding to an average line density of approximately one line per 3 km s −1 . Glycolaldehyde, its isomers, methyl formate and acetic acid, and its reduced alcohol, ethylene glycol, are clearly detected and their emission well-modeled with an excitation temperature of 300 K. For ethylene glycol both lowest state conformers, aGg and gGg , are detected, the latter for the first time in the ISM. The abundance of glycolaldehyde is comparable to or slightly larger than that of ethylene glycol. In comparison to the Galactic Center these two species are over-abundant relative to methanol, possibly an indication of formation of the species at low temperatures in CO-rich ices during the infall of the material toward the central protostar. Both 13 C and deuterated isotopologues of glycolaldehyde are detected, also for the first time ever in the ISM. For the deuterated species a D/H ratio of ≈5% is found with no differences between the deuteration in the different functional groups of glycolaldehyde, in contrast to previous estimates for methanol and recent suggestions of significant equilibration between water and -OH functional groups at high temperatures. Measurements of the 13 C-species lead to a 12 C: 13 C ratio of ≈30, lower than the typical ISM value. This low ratio may reflect an enhancement of 13 CO in the ice due to either ion-molecule reactions in the gas before freeze-out or differences in the temperatures where 12 CO and 13 CO ices sublimate. Conclusions. The results reinforce the importance of low temperature grain surfac...

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Section: Single-dish Observationsmentioning

confidence: 99%

The ALMA Protostellar Interferometric Line Survey (PILS)

Jørgensen

Wiel

Coutens

et al. 2016

A&A

374

582

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“…+ (Miettinen et al 2012), NHD2 ; -towards low-mass and high-mass protostars: D2CO, HDCO (Bergman et al 2011), DCOOCH3 (Demyk et al 2010;Margulès et al 2010), HDO (Coutens et al 2012, D2O , OD (Parise et al 2012); -in protoplanetary disks: DCN, DCO + (van Dishoeck et al 2003;Guilloteau et al 2006;Qi et al 2008;Öberg et al 2015), N2D…”

Section: Introductionmentioning

confidence: 99%

Chemistry of TMC-1 with multiply deuterated species and spin chemistry of H ₂ , H ₂ ⁺ , H ₃ ⁺ and their isotopologues

Majumdar

Gratier

Ruaud

et al. 2016

Mon. Not. R. Astron. Soc.

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Deuterated species are unique and powerful tools in astronomy since they can probe the physical conditions, chemistry, and ionization level of various astrophysical media. Recent observations of several deuterated species along with some of their spin isomeric forms have rekindled the interest for more accurate studies on deuterium fractionation. This paper presents the first publicly available chemical network of multiply deuterated species along with spin chemistry implemented on the latest state-of-the-art gas-grain chemical code 'NAUTILUS'. D/H ratios for all deuterated species observed at different positions of TMC-1 are compared with the results of our model, which considers multiply deuterated species along with the spin chemistry of light hydrogen bearing species H 2 , H 2 + , H 3 + and their isotopologues. We also show the differences in the modeled abundances of non-deuterated species after the inclusion of deuteration and spin chemistry in the model. Finally, we present a list of potentially observable deuterated species in TMC-1 awaiting detection.

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“…This interest is due to the strong dependence the ratio has on the temperature of an icy body's formation location (Ceccarelli et al 2014). In the interstellar medium (ISM), the water D/H ratio is measured at up to ∼9 × 10 −4 (Brown & Millar 1989), although the values are much higher in the organic matter of the interstellar hot cores (∼1 × 10 −3 ) and cold clouds (up to ∼2 × 10 −2 ) (Dartois et al 2003;Robert 2006;Parise et al 2012). When a protoplanetary disk forms around a young star, these ices are heated to more than a few hundred K. At these high temperatures, gaseous HDO reacts with nebular H 2 to form water vapor and HD, HDO + H 2 H 2 O + HD,…”

Section: Introductionmentioning

confidence: 99%

Nebular dead zone effects on the D/H ratio in chondrites and comets

Ali-Dib

Martin

Petit

et al. 2015

A&A

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Context. Comets and chondrites show non-monotonic behavior of their deuterium-to-hydrogen (D/H) ratio as a function of their formation location from the Sun. This is difficult to explain with a classical protoplanetary disk model that has a decreasing temperature structure with radius from the Sun. Aims. We want to understand if a protoplanetary disc with a dead zone, i.e., a region of zero or low turbulence, can explain the measured D/H values in comets and chondrites. Methods. We use time snapshots of a vertically layered disk model with turbulent surface layers and a dead zone at the midplane. The disc has a non-monotonic temperature structure due to increased heating from self-gravity in the outer parts of the dead zone. We couple this to a D/H ratio evolution model in order to quantify the effect of such thermal profiles on D/H enrichment in the nebula. Results. We find that the local temperature peak in the disk can explain the diversity in the D/H ratios of different chondritic families. This disk temperature profile leads to a non-monotonic D/H enrichment evolution, allowing these families to acquire their different D/H values while forming in close proximity. The formation order we infer for these families is compatible with that inferred from their water abundances. However, we find that even for very young disks, the thermal profile reversal is too close to the Sun to be relevant for comets.

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Detection of OD towards the low-mass protostar IRAS 16293−2422

Cited by 32 publications

References 25 publications

The ALMA Protostellar Interferometric Line Survey (PILS)

The ALMA Protostellar Interferometric Line Survey (PILS)

Chemistry of TMC-1 with multiply deuterated species and spin chemistry of H ₂ , H ₂ ⁺ , H ₃ ⁺ and their isotopologues

Nebular dead zone effects on the D/H ratio in chondrites and comets

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Detection of OD towards the low-mass protostar IRAS 16293−2422

Cited by 32 publications

References 25 publications

The ALMA Protostellar Interferometric Line Survey (PILS)

The ALMA Protostellar Interferometric Line Survey (PILS)

Chemistry of TMC-1 with multiply deuterated species and spin chemistry of H 2 , H 2 + , H 3 + and their isotopologues

Nebular dead zone effects on the D/H ratio in chondrites and comets

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Chemistry of TMC-1 with multiply deuterated species and spin chemistry of H ₂ , H ₂ ⁺ , H ₃ ⁺ and their isotopologues