A&A 425, 457–474 (2004) Astronomy DOI: 10.1051/0004-6361:20034285 & c ESO 2004 Astrophysics Molecular hydrogen and [Fe II] in Active Galactic Nuclei A. Rodríguez-Ardila1 ,M.G.Pastoriza2,S.Viegas3,T.A.A.Sigut4, and A. K. Pradhan5 1 Laboratório Nacional de Astrofísica, Rua dos Estados Unidos 154, Bairro das Nações, CEP 37500-000, Itajubá, MG, Brazil e-mail:
[email protected] 2 Departamento de Astronomia, Instituto de Física, UFRGS, Av. Bento Gonçalves 9500, Porto Alegre, RS, Brazil e-mail:
[email protected] 3 Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Rua do Matão 1226, CEP 05508-900, São Paulo, SP, Brazil e-mail:
[email protected] 4 Department of Physics and Astronomy, The University of Western Ontario, London, ON, N6A 3K7, Canada 5 Department of Astronomy, The Ohio State University, Columbus, OH 43210-1106, USA Received 6 September 2003 / Accepted 13 June 2004 Abstract. Near-infrared spectroscopy is used to study the kinematics and excitation mechanisms of H2 and [Fe ] lines in a sample of mostly Seyfert 1 galaxies. The spectral coverage allows simultaneous observation of the JHK bands, thus eliminating the aperture and seeing effects that have usually plagued previous works. The H2 lines are unresolved in all objects in which they were detected while the [Fe ] lines have widths implying gas velocities of up to 650 km s−1. This suggests that, very likely, the H2 and [Fe ] emission does not originate from the same parcel of gas. Molecular H2 lines were detected in 90% of the sample, including PG objects, indicating detectable amounts of molecular material even in objects with low levels of circumnuclear starburst activity.