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

Calcutt Hannah, Serena Vita, Claudio Codella, Maria T. Beltran, Francesco Fontani, Paul M. Woods

Research output: Contribution to journalArticle

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Abstract

We present the results of a line identification analysis using data from the IRAM Plateau de Bure Plateau de Bure Interferometer, 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 (HCOOCH3) for the first time in these objects as well as transitions of other complex molecules, including ethyl cyanide (C2H5CN), and isocyanic acid (HNCO). We also postulate a detection of one transition of glycolaldehyde (CH2(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 Trot 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.
Original languageEnglish
Pages (from-to)3157-3173
Number of pages17
JournalMonthly Notices of the Royal Astronomical Society
Volume443
Issue number4
Early online date07 Aug 2014
DOIs
Publication statusPublished - 01 Oct 2014

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formates
cyanide
cyanides
high resolution
plateau
acetonitrile
molecules
plateaus
interferometer
hot working
axioms
diagram
massive stars
dust
interferometers
acid
diagrams
stars
acids

Cite this

Hannah, C., Vita, S., Codella, C., Beltran, M. T., Fontani, F., & Woods, P. M. (2014). A high-resolution study of complex organic molecules in hot cores. Monthly Notices of the Royal Astronomical Society, 443(4), 3157-3173. https://doi.org/10.1093/mnras/stu1363
Hannah, Calcutt ; Vita, Serena ; Codella, Claudio ; Beltran, Maria T. ; Fontani, Francesco ; Woods, Paul M. / A high-resolution study of complex organic molecules in hot cores. In: Monthly Notices of the Royal Astronomical Society. 2014 ; Vol. 443, No. 4. pp. 3157-3173.
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Hannah, C, Vita, S, Codella, C, Beltran, MT, Fontani, F & Woods, PM 2014, 'A high-resolution study of complex organic molecules in hot cores', Monthly Notices of the Royal Astronomical Society, vol. 443, no. 4, pp. 3157-3173. https://doi.org/10.1093/mnras/stu1363

A high-resolution study of complex organic molecules in hot cores. / Hannah, Calcutt; Vita, Serena ; Codella, Claudio; Beltran, Maria T.; Fontani, Francesco; Woods, Paul M.

In: Monthly Notices of the Royal Astronomical Society, Vol. 443, No. 4, 01.10.2014, p. 3157-3173.

Research output: Contribution to journalArticle

TY - JOUR

T1 - A high-resolution study of complex organic molecules in hot cores

AU - Hannah, Calcutt

AU - Vita, Serena

AU - Codella, Claudio

AU - Beltran, Maria T.

AU - Fontani, Francesco

AU - Woods, Paul M.

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N2 - We present the results of a line identification analysis using data from the IRAM Plateau de Bure Plateau de Bure Interferometer, 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 (HCOOCH3) for the first time in these objects as well as transitions of other complex molecules, including ethyl cyanide (C2H5CN), and isocyanic acid (HNCO). We also postulate a detection of one transition of glycolaldehyde (CH2(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 Trot 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.

AB - We present the results of a line identification analysis using data from the IRAM Plateau de Bure Plateau de Bure Interferometer, 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 (HCOOCH3) for the first time in these objects as well as transitions of other complex molecules, including ethyl cyanide (C2H5CN), and isocyanic acid (HNCO). We also postulate a detection of one transition of glycolaldehyde (CH2(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 Trot 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.

U2 - 10.1093/mnras/stu1363

DO - 10.1093/mnras/stu1363

M3 - Article

VL - 443

SP - 3157

EP - 3173

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

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