Porphyrins in the interstellar medium (in grains)

Details Porphyrins in the interstellar medium (in grains) Porphyrins in the interstellar medium (in grains)

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994dib..nasa...47j&link_type=abstract

In NASA. Ames Research Center, The Diffuse Interstellar Bands: Contributed Papers p 47-52 (SEE N95-15827 03-89)

Astronomy and Astrophysics

Astronomy

1

Absorption Spectra, Chemical Composition, Fluorescence, Interstellar Matter, Nonanes, Paraffins, Phosphates, Porphyrins, Pyridines, Ultraviolet Astronomy, Ultraviolet Spectra, Absorption Spectroscopy, Crystal Field Theory, Diffuse Radiation, Interstellar Radiation, Spectroscopic Analysis, Ultraviolet Radiation, Ultraviolet Spectroscopy

Scientific paper

Spectral sensitivity of the chromophores to their immediate chemical environment establishes some of the chemical constituents of the grains in which they reside. These are: (1) Paraffins, such as, octane, nonane, decane, and others...(needed for Shpolskii matrices and producing quasi-lines); and (2) Pyridine. The presence of pyridine is required not only to produce the spectral DIB matching, but also to produce the 36 cm-1 crystal field splitting of the S1 electronic state. The presence of pyridine in the grains can be confirmed spectroscopically. Pyridine produces a transmission window at 2175 A, matching exactly the well known UV hump. On grain reflection, some of the incoming UV radiation is absorbed into the grain's outer layers. Spikes in the lab and in the astronomical data are due to vibronic transitions in pyridine. The lab spectroscopy reported here clearly establishes the presence of MgTBP, H2TPB, and pyridine in the interstellar grains. The high fluorescence efficiency of MgTBP (being optically pumped in the visible) apparently accounts for all the observed UIR emissions.

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