The 217.5 nm band, infrared absorption and infrared emission features in hydrogenated amorphous carbon nanoparticles

TL;DR

This study demonstrates laboratory-produced hydrogenated amorphous carbon nanoparticles that replicate the interstellar 217.5 nm absorption feature and IR emission spectra, suggesting their presence in space.

Contribution

It provides the first laboratory synthesis of carbon nanoparticles matching interstellar spectral features, linking their formation to diffuse cloud conditions.

Findings

Reproduces interstellar 217.5 nm absorption band in lab-made particles.

Matches IR emission spectra from Galactic sources using laboratory spectra.

Identifies naphthalene derivatives as key constituents of the particles.

Abstract

We report on the preparation of hydrogenated amorphous carbon nano-particles whose spectral characteristics include an absorption band at 217.5 nm with the profile and characteristics of the interstellar 217.5 nm feature. Vibrational spectra of these particles also contain the features commonly observed in absorption and emission from dust in the diffuse interstellar medium. These materials are produced under slow deposition conditions by minimizing the flux of incident carbon atoms and by reducing surface mobility. The initial chemistry leads to the formation of carbon chains, together with a limited range of small aromatic ring molecules, and eventually results in carbon nano-particles having an sp2/sp3 ratio = 0.4. Spectroscopic analysis of particle composition indicates that naphthalene and naphthalene derivatives are important constituents of this material. We suggest that carbon nano-particles with similar composition are responsible for the appearance of the interstellar 217.5 nm band and outline how these particles can form in situ under diffuse cloud conditions by deposition of carbon on the surface of silicate grains. Spectral data from carbon nano-particles formed under these conditions accurately reproduces IR emission spectra from a number of Galactic sources. We provide the first detailed fits to observational spectra of Type A and B emission sources based entirely on measured spectra of a carbonaceous material that can be produced in the laboratory.