J/A+A/639/A135 Glycolamide rotational transitions (Sanz-Novo+, 2020)
Interstellar glycolamide: A comprehensive rotational study and an
astronomical search in Sgr B2(N).
Sanz-Novo M., Belloche A., Alonso J.L., Kolesnikova L., Garrod R.T.,
Mata S., Mueller H.S.P., Menten K.M., Gong Y.
<Astron. Astrophys. 639, A135 (2020)>
=2020A&A...639A.135S 2020A&A...639A.135S (SIMBAD/NED BibCode)
ADC_Keywords: Atomic physics
Keywords: molecular data - line: identification - ISM: molecules -
ISM: individual objects: Sagittarius B2 - astrochemistry
Abstract:
Glycolamide is a glycine isomer and also one of the simplest
derivatives of acetamide (one hydrogen atom replaced with a hydroxyl
group), which is a known interstellar molecule.
In this context, the aim of our work is to provide direct experimental
frequencies of the ground vibrational state of glycolamide in the
centimeter-, millimeter- and submillimeter wavelength regions in order
to enable its identification in the interstellar medium.
We employed a battery of state-of-the-art rotational spectroscopic
techniques in the frequency and time domain to measure its
frequencies. We used the spectral line survey named EMoCA (Exploring
Molecular Complexity with ALMA) that was performed toward the star
forming region Sgr B2(N) with ALMA to search for glycolamide in space.
We also searched for glycolamide toward Sgr B2(N) with the Effelsberg
radio telescope. The astronomical spectra were analyzed under the
local thermodynamic equilibrium approximation.We used the gas-grain
chemical kinetics mode MAGICKAL to interpret the results of the
astronomical observations.
About 1500 transitions have been newly assigned up to 460GHz to the
most stable conformer, and a precise set of spectroscopic constants
was determined. Spectral features of glycolamide were then searched
for in the prominent hot molecular core Sgr B2(N2). We report the
non-detection of glycolamide toward this source with an abundance at
least six and five times lower than that of acetamide and
glycolaldehyde, respectively. Our astrochemical model suggests that
glycolamide may be present in this source at a level just below the
upper limit derived from the EMoCA survey. We could also not detect
the molecule in the region s extended molecular envelope probed with
the Effelsberg telescope. We find an upper limit to its column density
that is similar to the column densities obtained earlier for acetamide
and glycolaldehyde with theGreen Bank Telescope.
Description:
Observed rotational transitions of glycolamide in the ground state.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
mmwlines.dat 68 1420 Fitted rotational transitions of glycolamide
in the ground state
--------------------------------------------------------------------------------
See also:
J/ApJ/723/845 : The submillimeter spectrum of glycolaldehyde (Carroll+, 2010)
J/ApJS/158/188 : Detection of glycolaldehyde toward Sgr B2 (Widicus+, 2005)
J/A+A/540/A51 : Submm spectrum of deuterated glycolaldehydes (Bouchez+, 2012)
J/A+A/549/A96 : The mm & sub-mm spectra of 13C-glycolaldehydes (Haykal+, 2013)
Byte-by-byte Description of file: mmwlines.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- N [1/1421] Sequential number of the line
5 A1 --- --- [:/]
7- 8 I2 --- J' Upper state J quantum number
10- 11 I2 --- Ka' Upper state Ka quantum number
13- 14 I2 --- Kc' Upper state Kc quantum number
18- 19 I2 --- J" Lower state J quantum number
21- 22 I2 --- Ka" Lower state Ka quantum number
24- 25 I2 --- Kc" Lower state Kc quantum number
28- 38 F11.4 MHz ObsFreq Observed transition frequency
41- 47 F7.4 MHz O-C Observed minus calculated frequency
50- 54 F5.3 MHz e_ObsFreq Experimental uncertainty
57- 63 F7.4 MHz (O-C)b ? Observed minus calculated frequency for
blends
65- 68 F4.2 --- Wb ? Weight of the components of the blends
--------------------------------------------------------------------------------
Acknowledgements:
Miguel Sanz-Novo, miguel.sanz.novo(at)uva.es
(End) Miguel Sanz-Novo [GEM, UVa, Spain], Patricia Vannier [CDS] 29-May-2020