Multi-method-modeling of interacting galaxies
I. A unique scenario for NGC 4449?
Institut für Theoretische Physik und Astrophysik der Universität Kiel, Olshausenstr. 40, 24098 Kiel, Germany
2 Radioastronomisches Institut der Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
3 Center for Medical Diagnostic Systems and Visualization MeVis GmbH at University of Bremen, Universitätsallee 29, 28359 Bremen, Germany e-mail: firstname.lastname@example.org
Corresponding author: Ch. Theis, email@example.com
Accepted: 3 January 2001
NGC 4449 is an active star-forming dwarf ga la xy of Magellanic type. From radio observations, van Woerden et al. ([CITE]) found an extended HI-halo around NGC 4449 which is at least a factor of 10 larger than the optical diameter kpc. Recently, Hunter et al. ([CITE]) discerned details in the HI-halo: a disc-like feature around the center of NGC 4449 and a lopsided arm structure. We combined several N-body methods in order to investigate the interaction scenario between NGC 4449 and DDO 125, a close companion in projected space. In a first step fast restricted N-body models are used to confine a region in parameter space reproducing the main observational features. In a second step a genetic algorithm is applied for a uniqueness test of our preferred parameter set. We show that our genetic algorithm reliably recovers orbital parameters, provided that the data are sufficiently accurate, i.e. all the key features are included. In the third step the results of the restricted N-body models are compared with self-consistent N-body simulations. In the case of NGC 4449, the applicability of the simple restricted N-body calculations is demonstrated. Additionally, it is shown that the HI gas can be modeled here by a purely stellar dynamical approach. In a series of simulations, we demonstrate that the observed features of the extended HI disc can be explained by a gravitational interaction between NGC 4449 and DDO 125. According to these calculations the closest approach between both galaxies happened ~4-6 108 yr ago at a minimum distance of ~25 kpc on a parabolic or slightly elliptic orbit. In the case of an encounter scenario, the dynamical mass of DDO 125 should not be smaller than 10% of NGC 4449's mass. Before the encounter, the observed HI gas was arranged in a disc with a radius of 35-40 kpc around the center of NGC 4449. It had the same orientation as the central ellipsoidal HI structure. The origin of this disc is still unclear, but it might have been caused by a previous interaction.
Key words: galaxies: interactions / galaxies: kinematics and dynamics / individual: NGC 4449, DDO 125 / methods: N-body simulations / methods: data analysis
© ESO, 2001