Are PAH molecules the origin of the near-IR emission of extragalactic H(+) regions - Observations in NGC 1566

Details Are PAH molecules the origin of the near-IR emission of extragalactic H(+) regions - Observations in NGC 1566 Are PAH molecules the origin of the near-IR emission of extragalactic H(+) regions - Observations in NGC 1566

Jul 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...162..211l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 162, no. 1-2, July 1986, p. 211-216.

Astronomy and Astrophysics

Astronomy

Cyclic Hydrocarbons, Graphite, Hydrogen Clouds, Infrared Astronomy, Intergalactic Media, Cosmic Dust, Hydrogen Ions, Near Infrared Radiation, Positive Ions, Radiation Effects

Scientific paper

Observations of the H(+) emissions of the Sbc galaxy NGC 1566 using the ESO-La Silla 3.6 m telescope fitted with an IR photometer are reported and analyzed. The region is a known UV emitter and occupies a sufficiently small angular breadth of sky to obtain integrated measurements. The observations were performed at 1.25 and 2.2 microns with J and K wideband filters and at 3.28 microns with a circularly variable filter. Strong near-IR emissions from the region were considered in terms of models for nebular emission, emissions from polycyclic aromatic hydrocarbons (PAH) and stellar emissions. PAH grains were concluded to be the most likely source of emissions in excess of those which could be expected from a gaseous nebula, with the excess emission varying with the sizes of the pre-graphitic grains and molecules.

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