Near-infrared line and continuum imaging of the nuclear starburst region of NGC 1808.

Details Near-infrared line and continuum imaging of the nuclear starburst region of NGC 1808. Near-infrared line and continuum imaging of the nuclear starburst region of NGC 1808.

Sep 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...313..771k&link_type=abstract

Astronomy and Astrophysics, v.313, p.771-782

Astronomy and Astrophysics

Astrophysics

24

Galaxies: Active, Galaxies: Individual (Ngc 1808), Galaxies: Nuclei, Galaxies: Starburst, Infrared: Galaxies, Radio Continuum: Galaxies

Scientific paper

We present high spatial resolution (~1.0") imaging of Brγ, H_2_ 1-0 S(1) 2.121μm and [Fe II] 1.64μm line emission and broad-band J, H and K continuum emission of the nuclear (20"=1.6kpc diameter) region of the starburst galaxy NGC 1808. These data, combined with a 3.6cm radio continuum map, are used to study the morphology and extinction of the starburst region, the nature of the stellar population and star formation, and the possibility of hidden Seyfert activity in NGC 1808. The broad-band continuum emission is smoothly distributed throughout the circumnuclear region and peaks strongly on the nucleus. There is no strong morphological change with wavelength. Most of the continuum emission is probably produced by the evolved bulge stellar population, and not by hot dust, red giants or red supergiants, as in most other starburst galaxies. The line emission is dominated by the nucleus, but is extended along the major axis of the galaxy by ~18" (~1.4kpc) for all emission lines. The circumnuclear emission arises from several distinct regions, forming a ring-like structure. Both Brγ and [Fe II] are well correlated with the radio emission. There are, however, differences in the detailed morphology, that differentiate between hot spots dominated by supernova remnants and HII regions. The H_2_ emission is slightly better spatially correlated with Brγ than with [Fe II] emission but no firm conclusion about the excitation mechanism of the H_2_ is warranted. The Brγ emission effectively isolates the star forming activity, whereas radio and [Fe II] emission is affected by individual supernova explosions, and the optical Hα emission peaks are only seen in directions of low extinction. From comparison of Brγ and Hα fluxes we derive extinctions between A_V_ of 3 and 5 towards the hot spots. From analysis of the extinction-corrected line and continuum emission luminosities using an evolutionary starburst model, we derive for each hot spot star forming rate 0.1-0.6Msun_/yr, and supernova rate 0.4-11x10^-3^yr^-1^. We estimate the age of the current burst to be between 8 and 17Myr in the circumnuclear region, and ~40Myr in the nucleus. The circumnuclear starburst hot spots lie in the area of HII regions and starburst galaxies in the [Fe II]/Brγ vs. H_2_/Brγ diagram, whereas the nucleus has line ratios similar to Seyfert nuclei. The multiwavelength evidence for and against hidden Seyfert activity in NGC 1808, and implications for the evolution of starburst galaxies are discussed.

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