Laboratory and Observational Studies of Methyl Ethyl Ketone

Astronomy and Astrophysics – Astrophysics

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Scientific paper

A large fraction of the detected interstellar molecules are complex organic molecules (COMs) containing five or more atoms. Despite the prominence of these species in many types of astrophysical environments, the formation processes for these molecules are not well-understood. We have therefore undertaken a combined laboratory, modeling, and observational program in an attempt to more fully understand the effects that physical environment have on the chemical composition of astronomical sources. As part of this effort, we have conducted deep submillimeter spectral line surveys of multiple interstellar sources with varying physical conditions including hot cores, shocked regions, low-mass star forming regions, and stellar outflows. These surveys were conducted using a broadband receiver at the Caltech Submillimeter Observatory (CSO), and are forerunner observations to our upcoming Herschel OT1 program to continue these surveys at higher frequencies. In order to fully analyze these spectral line surveys, we have also collected laboratory spectra of several suspected interstellar organic molecules. One such molecular target is methyl ethyl ketone (CH_3COCH_2CH_3, MEK), which is a likely candidate for interstellar detection. The spectra for MEK were collected from 8.7 to 18.3 GHz using the chirped-pulse waveguide Fourier Transform microwave (FTMW) spectrometer at New College Florida. We have also collected spectra of MEK in selected frequency ranges from 32 to 125 GHz using the direct absorption flow cell spectrometer at Emory University. We will report on the laboratory characterization of MEK and compare these results to our observational spectral line surveys.

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