Stellar and ionized gas kinematics of the interacting Seyfert 1.9 galaxy NGC 2992

¹ Isaac Newton Group of Telescopes, Apdo de Correos 321, 38700 S/C de La Palma, Canary Islands, Spain
² Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA Affiliated with the Astrophysics Division, Space Science Department of ESA e-mail: arribas@stsci.edu
³ On leave from the Instituto de Astrofísica de Canarias-Consejo Superior de Investigaciones Científicas, Spain
⁴ Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Canary Islands, Spain e-mail: emg@ll.iac.es

Corresponding author: B. García-Lorenzo, bgarcia@ing.iac.es

Received: 13 March 2001
Accepted: 30 August 2001

Abstract

Integral field spectroscopy in the central (2.4 kpc 1.8 kpc, if H₀ = 75 km s^-1 Mpc^-1) of the Seyfert 1.9 galaxy NGC 2992 has been obtained using the fibre system INTEGRAL. The data are mainly used to study the stellar and ionized gas kinematics. In spite of the photometric disruptions in the outer parts ( 6 kpc) produced by the interaction with its close companion (NGC 2993), the present stellar velocity field shows regular rotation. The ionized gas presents several kinematically distinct components. Apart from the outflowing component already reported by other authors, we found an additional (high ionization) kinematic component which seems to be associated with the boundaries of the figure-of-eight-shaped emission detected in the 6 cm radio map. We locate the hidden nucleus in the apex of the biconical structure defined by the [O iii] emission, coincident with the outflow origin and with the center of the dust lane. We do not find any clear evidence of direct influence of the interaction in the kinematics of the stars or the ionized gas in the circumnuclear region of NGC 2992.