Ethylene glycol in comet C/1995 O1 (Hale-Bopp)

Crovisier, J.; Bockelée‐Morvan, Dominique; Biver, Nicolás; Colom, P.; Despois, D.; Lis, D. C.

doi:10.1051/0004-6361:20040116

Cited by 121 publications

(97 citation statements)

References 18 publications

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“…It is important to decipher the role of grain-surface chemistry and radiation processing versus gas-phase chemistry (Walsh et al 2014). As discussed by Crovisier et al (2004a) and Walsh et al (2014), an important issue is the now confirmed high abundance of ethylene glycol in comets, which is at least 5-6 times higher than that of the chemically related species CH 2 OHCHO (glycolaldehyde) ( Table 3). By contrast, both molecules are observed in similar abundances in the hot core Sgr B2(N) (Hollis et al 2002), and tentatively in the Class 0 solar-type binary protostar IRAS 16293-2422, where ethylene glycol relative to glycolaldehyde is 0.3-0.5 (Jørgensen et al 2012).…”

Section: Discussionmentioning

confidence: 99%

“…We report here the detection of ethylene glycol (CH 2 OH) 2 and formamide (NH 2 CHO) in comets C/2012 F6 (Lemmon) (hereafter referred to as Lemmon) and C/2013 R1 (Lovejoy) (hereafter Lovejoy), for the first time since their discovery in comet C/1995 O1 (Hale-Bopp) (Crovisier et al 2004a;Bockelée-Morvan et al 2000). We also present the detection of Based on observations carried out with the IRAM 30 m telescope.…”

Section: Introductionmentioning

confidence: 89%

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Complex organic molecules in comets C/2012 F6 (Lemmon) and C/2013 R1 (Lovejoy): detection of ethylene glycol and formamide

Biver

Bockelée‐Morvan

Debout

et al. 2014

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A spectral survey in the 1 mm wavelength range was undertaken in the long-period comets C/2012 F6 (Lemmon) and C/2013 R1 (Lovejoy) using the 30 m telescope of the Ins titut de radioastronomie millimétrique (IRAM) in April and November−December 2013. We report the detection of ethylene glycol (CH 2 OH) 2 (aGg' conformer) and formamide (NH 2 CHO) in the two comets. The abundances relative to water of ethylene glycol and formamide are 0.2-0.3% and 0.02% in the two comets, similar to the values measured in comet C/1995 O1 (Hale-Bopp). We also report the detection of HCOOH and CH 3 CHO in comet C/2013 R1 (Lovejoy), and a search for other complex species (methyl formate, glycolaldehyde).

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 89%

Complex organic molecules in comets C/2012 F6 (Lemmon) and C/2013 R1 (Lovejoy): detection of ethylene glycol and formamide

Biver

Bockelée‐Morvan

Debout

et al. 2014

A&A

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121

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“…Very recently, it was also detected in the hot corinos associated with the class 0 protostars NGC 1333-IRAS2A (Maury et al 2014) and, tentatively, IRAS 16293-2422B (Jørgensen et al 2012). Finally, ethanediol was also found to be abundant in the outflows of comet Hale-Bopp (Crovisier 2004).…”

Section: Introductionmentioning

confidence: 91%

Laboratory spectroscopy of 1, 2-propanediol at millimeter and submillimeter wavelengths

Bossa

Ordu

Müller

et al. 2014

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Context. Ethanediol is one of the largest complex organic molecules detected in space thus far. It has been found in different types of molecular clouds. The two propanediol isomers are the next larger diols. Hence, they are viable candidates to be searched for in space. Aims. We wish to provide sufficiently large and accurate sets of spectroscopic parameters of 1, 2-propanediol to facilitate searches for this molecule at millimeter and longer submillimeter wavelengths. Methods. We recorded rotational spectra of 1, 2-propanediol in three wide frequency windows between 38 and 400 GHz. Results. We made extensive assignments for the three lowest energy conformers to yield spectroscopic parameters up to eighth order of angular momentum. Conclusions. Our present data will be helpful for identifying 1, 2-propanediol at moderate submillimeter or longer wavelengths with radio telescope arrays such as ALMA, NOEMA, or EVLA. In particular, its detection with ALMA in sources, in which ethanediol was detected, appears to be promising.

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“…To date, more than 20 parent molecules have been observed in cometary comae including the relatively complex species, H 2 CO, CH 3 OH, HCOOH, CH 3 CHO, HC 3 N, CH 3 CN, NH 2 CHO, HCOOCH 3 , and ethylene glycol ((HOCH 2 ) 2 ), which are relevant to this work. Of these species, CH 3 CHO, NH 2 CHO, HCOOCH 3 , and (HOCH 2 ) 2 have been observed in only a single object, comet Hale-Bopp, with percentage abundances of 0.02%, 0.015%, 0.08%, and 0.25% (relative to H 2 O), respectively (see, e.g., Bockelée-Morvan et al 2004;Crovisier et al 2004aCrovisier et al ,b, 2006Mumma & Charnley 2011).…”

Section: Complex Molecules In Cometsmentioning

confidence: 99%

Complex organic molecules in protoplanetary disks

Walsh

Millar

Nomura

et al. 2014

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Context. Protoplanetary disks are vital objects in star and planet formation, possessing all the material, gas and dust, which may form a planetary system orbiting the new star. Small, simple molecules have traditionally been detected in protoplanetary disks; however, in the ALMA era, we expect the molecular inventory of protoplanetary disks to significantly increase. Aims. We investigate the synthesis of complex organic molecules (COMs) in protoplanetary disks to put constraints on the achievable chemical complexity and to predict species and transitions which may be observable with ALMA. Methods. We have coupled a 2D steady-state physical model of a protoplanetary disk around a typical T Tauri star with a large gas-grain chemical network including COMs. We compare the resulting column densities with those derived from observations and perform ray-tracing calculations to predict line spectra. We compare the synthesised line intensities with current observations and determine those COMs which may be observable in nearby objects. We also compare the predicted grain-surface abundances with those derived from cometary comae observations. Results. We find COMs are efficiently formed in the disk midplane via grain-surface chemical reactions, reaching peak grain-surface fractional abundances ∼10 −6 -10 −4 that of the H nuclei number density. COMs formed on grain surfaces are returned to the gas phase via non-thermal desorption; however, gas-phase species reach lower fractional abundances than their grain-surface equivalents, ∼10 −12 -10 −7 . Including the irradiation of grain mantle material helps build further complexity in the ice through the replenishment of grain-surface radicals which take part in further grain-surface reactions. There is reasonable agreement with several line transitions of H 2 CO observed towards T Tauri star-disk systems. There is poor agreement with HC 3 N lines observed towards LkCa 15 and GO Tau and we discuss possible explanations for these discrepancies. The synthesised line intensities for CH 3 OH are consistent with upper limits determined towards all sources. Our models suggest CH 3 OH should be readily observable in nearby protoplanetary disks with ALMA; however, detection of more complex species may prove challenging, even with ALMA "Full Science" capabilities. Our grain-surface abundances are consistent with those derived from cometary comae observations providing additional evidence for the hypothesis that comets (and other planetesimals) formed via the coagulation of icy grains in the Sun's natal disk.

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Ethylene glycol in comet C/1995 O1 (Hale-Bopp)

Cited by 121 publications

References 18 publications

Complex organic molecules in comets C/2012 F6 (Lemmon) and C/2013 R1 (Lovejoy): detection of ethylene glycol and formamide

Complex organic molecules in comets C/2012 F6 (Lemmon) and C/2013 R1 (Lovejoy): detection of ethylene glycol and formamide

Laboratory spectroscopy of 1, 2-propanediol at millimeter and submillimeter wavelengths

Complex organic molecules in protoplanetary disks

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