Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005mnras.364.1041r&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 364, Issue 3, pp. 1041-1053.
Astronomy and Astrophysics
Astronomy
23
Line: Formation, Molecular Processes, Galaxies: Seyfert, Infrared: Galaxies
Scientific paper
Near-infrared spectroscopy is used to study the kinematics and excitation mechanisms of H2 and [FeII] lines in a sample dominated by Seyfert 2 galaxies. The spectra simultaneously cover the JHK bands, allowing us to compare line fluxes emitted in the interval 0.8-2.4 μm and avoiding aperture and seeing effects. The H2 lines are systematically narrower than the narrow-line region lines, suggesting that, very likely, the H2 does not originate from the same parcel of gas that forms the narrow-line region. Emission-line ratios between H2 lines favour thermal excitation mechanisms for the molecular gas in active galactic nuclei. It was found that non-thermal excitation contributes, at most, 30 per cent of the observed H2. Thermal excitation is also confirmed by the rather similar vibrational and rotational temperatures in the objects (~2000 K). The mass of hot H2 ranges from 102 to 103Msolar, with nearly half of objects showing values of <500 Msolar. It shows that the fraction of molecular mass present in the nuclear region and emitting in the near-infrared is a very small fraction of the warm molecular mass present in the centre. A diagnostic diagram composed of the line ratios H2/Brγ and [FeII]/Paβ proves to be a useful tool in the near-infrared for separating emission-line objects by their degree of nuclear activity. We found that active galactic nuclei are characterized by H2 2.121 μm/Brγ and [FeII] 1.257 μm/Paβ flux ratios between 0.6 and 2. Starburst/HII galaxies display line ratios <0.6 while low-ionization nuclear emission-line regions are characterized by values larger than 2 in either ratio.
Pastoriza Miriani Griselda
Riffel Rogério
Rodriguez-Ardila Alberto
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