4 research outputs found
Using radio astronomical receivers for molecular spectroscopic characterization in astrochemical laboratory simulations: A proof of concept
We present a proof of concept on the coupling of radio astronomical receivers
and spectrometers with chemical reactorsand the performances of the resulting
setup for spectroscopy and chemical simulations in laboratory astrophysics.
Several experiments including cold plasma generation and UV photochemistry were
performed in a 40\,cm long gas cell placed in the beam path of the Aries 40\,m
radio telescope receivers operating in the 41-49 GHz frequency range interfaced
with fast Fourier transform spectrometers providing 2 GHz bandwidth and 38 kHz
resolution.
The impedance matching of the cell windows has been studied using different
materials. The choice of the material and its thickness was critical to obtain
a sensitivity identical to that of standard radio astronomical observations.
Spectroscopic signals arising from very low partial pressures of CH3OH,
CH3CH2OH, HCOOH, OCS,CS, SO2 (<1E-03 mbar) were detected in a few seconds. Fast
data acquisition was achieved allowing for kinetic measurements in
fragmentation experiments using electron impact or UV irradiation. Time
evolution of chemical reactions involving OCS, O2 and CS2 was also observed
demonstrating that reactive species, such as CS, can be maintained with high
abundance in the gas phase during these experiments.Comment: Accepted for publication in Astronomy and Astrophysics in September
21, 2017. 16 pages, 18 figure
Using radio astronomical receivers for molecular spectroscopic characterization in astrochemical laboratory simulations: A proof of concept
I. Tanarro et al. -- 16 pags., 18 figs., app.We present a proof of concept on the coupling of radio astronomical receivers and spectrometers with chemical reactors and the performances
of the resulting setup for spectroscopy and chemical simulations in laboratory astrophysics. Several experiments including
cold plasma generation and UV photochemistry were performed in a 40 cm long gas cell placed in the beam path of the Aries 40 m
radio telescope receivers operating in the 41â49 GHz frequency range interfaced with fast Fourier transform spectrometers providing
2 GHz bandwidth and 38 kHz resolution. The impedance matching of the cell windows has been studied using di erent materials. The
choice of the material and its thickness was critical to obtain a sensitivity identical to that of standard radio astronomical observations.
Spectroscopic signals arising from very low partial pressures of CH3OH, CH3CH2OH, HCOOH, OCS, CS, SO2 (<103 mbar) were
detected in a few seconds. Fast data acquisition was achieved allowing for kinetic measurements in fragmentation experiments using
electron impact or UV irradiation. Time evolution of chemical reactions involving OCS, O2 and CS2 was also observed demonstrating
that reactive species, such as CS, can be maintained with high abundance in the gas phase during these experimentsThe research leading to these results has received funding
from the European Research Council under the European Unionâs Seventh
Framework Programme (FP/2007-2013)/ERC-SyG-2013 Grant Agreement
No. 610256 NANOCOSMOS and from spanish MINECO CSD2009-00038
(ASTROMOL) under the Consolider-Ingenio Program. We also thank spanish
MINECO for funding under grants AYA2012-32032, AYA2016-75066-C2-1-P,
FIS2013-48087-C2-1-P, FIS2016-77726-C3-1-P, FIS2016-77578-R, MAT2014-
54231-C4-1-P.Peer reviewe
Using radio astronomical receivers for molecular spectroscopic characterization in astrochemical laboratory simulations: A proof of concept
International audienceWe present a proof of concept on the coupling of radio astronomical receivers and spectrometers with chemical reactors and the performances of the resulting setup for spectroscopy and chemical simulations in laboratory astrophysics. Several experiments including cold plasma generation and UV photochemistry were performed in a 40 cm long gas cell placed in the beam path of the Aries 40 m radio telescope receivers operating in the 41-49 GHz frequency range interfaced with fast Fourier transform spectrometers providing 2 GHz bandwidth and 38 kHz resolution. The impedance matching of the cell windows has been studied using different materials. The choice of the material and its thickness was critical to obtain a sensitivity identical to that of standard radio astronomical observations. Spectroscopic signals arising from very low partial pressures of CH 3 OH, CH 3 CH 2 OH, HCOOH, OCS, CS, SO 2 (<10 â3 mbar) were detected in a few seconds. Fast data acquisition was achieved allowing for kinetic measurements in fragmentation experiments using electron impact or UV irradiation. Time evolution of chemical reactions involving OCS, O 2 and CS 2 was also observed demonstrating that reactive species, such as CS, can be maintained with high abundance in the gas phase during these experiments