First Detection of Glycolaldehyde Outside the Galactic Center

Beltrán, M. T.; Codella, C.; Viti, S.; Neri, R.; Cesaroni, R.

doi:10.1088/0004-637x/690/2/l93

Cited by 132 publications

(107 citation statements)

References 17 publications

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“…This important organic molecule was first tentatively detected at 1.4 mm with the PdBI outside the Galactic centre, where it was observed in Sgr B2(N) (Hollis et al 2000) towards three massive hotcores (G31, G24A1, and G24A2) by Beltrán et al (2005). Later on, Beltrán et al (2009) confirmed the detection by observing two additional Glycolaldehyde transitions towards G31 at 2.1 and 2.9 mm with the PdBI. Recently, Jørgensen et al (2012) have detected 13 transitions towards the Class 0 IRAS 16293-2422 object at 0.4 and 1.4 mm, using the ALMA array towards the hot-corino surrounding the Solar-type protostar.…”

Section: Glycolaldehyde (Ch2(oh)cho)mentioning

confidence: 68%

A high-resolution study of complex organic molecules in hot cores

Calcutt

Viti

Codella

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present the results of a line identification analysis using data from the IRAM Plateau de Bure Inferferometer, focusing on six massive star-forming hot cores: G31.41+0.31, G29.96-0.02, G19.61-0.23, G10.62-0.38, G24.78+0.08A1 and G24.78+0.08A2. We identify several transitions of vibrationally excited methyl formate (HCOOCH 3 ) for the first time in these objects as well as transitions of other complex molecules, including ethyl cyanide (C 2 H 5 CN), and isocyanic acid (HNCO). We also postulate a detection of one transition of glycolaldehyde (CH 2 (OH)CHO) in two new hot cores. We find G29.96-0.02, G19.61-0.23, G24.78+0.08A1 and G24.78+0.08A2 to be chemically very similar. G31.41+0.31, however, is chemically different: it manifests a larger chemical inventory and has significantly larger column densities. We suggest that it may represent a different evolutionary stage to the other hot cores in the sample, or it may surround a star with a higher mass. We derive column densities for methyl formate in G31.41+0.31, using the rotation diagram method, of 4×10 17 cm −2 and a T rot of ∼170 K. For G29.96-0.02, G24.78+0.08A1 and G24.78+0.08A2, glycolaldehyde, methyl formate and methyl cyanide all seem to trace the same material and peak at roughly the same position towards the dust emission peak. For G31.41+0.31, however, glycolaldehyde shows a different distribution to methyl formate and methyl cyanide and seems to trace the densest, most compact inner part of hot cores.

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Section: Glycolaldehyde (Ch2(oh)cho)mentioning

confidence: 68%

A high-resolution study of complex organic molecules in hot cores

Calcutt

Viti

Codella

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…Line profiles look like a rotating toroid with infall motion. Several complex hot-core molecules have been observed in G31, including glycolaldehyde CH 2 OHCHO (Beltrán et al 2009), but again no abundance ratios have been presented.…”

Section: Iras 18089-1732mentioning

confidence: 99%

Chemistry of massive young stellar objects with a disk-like structure

Isokoski

Bottinelli

Dishoeck

2013

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Aims. Our goal is to take an inventory of complex molecules in three well-known high-mass protostars for which disks or toroids have been claimed and to study the similarities and differences with a sample of massive young stellar objects (YSOs) without evidence of such flattened disk-like structures. With a disk-like geometry, UV radiation can escape more readily and potentially affect the ice and gas chemistry on hot-core scales. Methods. A partial submillimeter line survey, targeting CH 3 OH, H 2 CO, C 2 H 5 OH, HCOOCH 3 , CH 3 OCH 3 , CH 3 CN, HNCO, NH 2 CHO, C 2 H 5 CN, CH 2 CO, HCOOH, CH 3 CHO, and CH 3 CCH, was made toward three massive YSOs with disk-like structures, IRAS 20126+4104, IRAS 18089-1732, and G31.41+0.31. Rotation temperatures and column densities were determined by the rotation diagram method, as well as by independent spectral modeling. The molecular abundances were compared with previous observations of massive YSOs without evidence of any disk structure, targeting the same molecules with the same settings and using the same analysis method. Results. Consistent with previous studies, different complex organic species have different characteristic rotation temperatures and can be classified either as warm (>100 K) or cold (<100 K). The excitation temperatures and abundance ratios are similar from source to source and no significant difference can be established between the two source types. Acetone, CH 3 COCH 3 , is detected for the first time in G31.41+0.31 and IRAS 18089-1732. Temperatures and abundances derived from the two analysis methods generally agree within factors of a few. Conclusions. The lack of chemical differentiation between massive YSOs with and without observed disks suggest either that the chemical complexity is already fully established in the ices in the cold prestellar phase or that the material experiences similar physical conditions and UV exposure through outflow cavities during the short embedded lifetime.

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“…It has been detected in the SFR Sgr B2(N) by Hollis et al (2000) from 2 and 3 mm single-dish surveys, with an estimated rotational temperature (T rot ) of 35 K from 34 lines detected. Beltrán et al (2009) reported identification of three lines towards the hot core G31.41 +0.31 using the Plateau de Bure Interferometer. Their analysis indicated that emission comes from the hottest (≥300 K) and the densest (≥2 × 10 8 cm −3 ) region closest to the protostar.…”

Section: Introductionmentioning

confidence: 99%

The submillimeter spectrum of deuterated glycolaldehydes

Bouchez

Margulès

Motiyenko

et al. 2012

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Context. Glycolaldehyde, a sugar-related interstellar prebiotic molecule, has recently been detected in two star-forming regions, Sgr B2(N) and G31.41+0.31. The detection of this new species increased the list of complex organic molecules detected in the interstellar medium (ISM) and adds another level to the chemical complexity present in space. Besides, this kind of organic molecule is important because it is directly linked to the origin of life. For many years, astronomers have been struggling to understand the origin of this high chemical complexity in the ISM. The study of deuteration may provide crucial hints. Aims. In this context, we have measured the spectra of deuterated isotopologues of glycolaldehyde in the laboratory: the three monodeuterated ones (CH 2 OD-CHO, CHDOH-CHO and CH 2 OH-CDO) and one dideuterated derivative (CHDOH-CDO) in the ground vibrational state. Methods. Previous laboratory work on the D-isotopologues of glycolaldehyde was restricted to less than 26 GHz. We used a solidstate submillimeter-wave spectrometer in Lille with an accuracy for isolated lines better than 30 kHz to acquire new spectroscopic data between 150 and 630 GHz and employed the ASFIT and SPCAT programs for analysis. Results. We measured around 900 new lines for each isotopologue and determined spectroscopic parameters. This allows an accurate prediction in the ALMA range up to 850 GHz. Conclusions. This treatment meets the needs for a first astrophysical research, for which we provide an appropriate set of predictions.

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First Detection of Glycolaldehyde Outside the Galactic Center

Cited by 132 publications

References 17 publications

A high-resolution study of complex organic molecules in hot cores

A high-resolution study of complex organic molecules in hot cores

Chemistry of massive young stellar objects with a disk-like structure

The submillimeter spectrum of deuterated glycolaldehydes

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