Kinematic modeling of disk galaxies

Free access article

Issue		A&A Volume 494, Number 2, February I 2009


Page(s)		489 - 508
Section		Extragalactic astronomy
DOI		http://dx.doi.org/10.1051/0004-6361:200809372
Published online		22 December 2008

A&A 494, 489-508 (2009)
DOI: 10.1051/0004-6361:200809372

III. The warped “Spindle” NGC 2685

G. I. G. Józsa¹, T. A. Oosterloo^{1, 2}, R. Morganti^{1, 2}, U. Klein³, and T. Erben³

¹ Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2, 7990 AA Dwingeloo, The Netherlands
e-mail: [jozsa;oosterloo;morganti]@astron.nl
² Kapteyn Astronomical Institute, Univ. Groningen, Postbus 800, 9700 AV Groningen, The Netherlands
³ Argelander-Institut für Astronomie (AIfA), Univ. Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
e-mail: [uklein;erben]@astro.uni-bonn.de

Received 9 January 2008 / Accepted 10 October 2008

Abstract
This is the third of a series of papers in which the structure and kinematics of disk galaxies is studied. By employing direct tilted-ring fits to the data cube as introduced in Paper I, we analyzed the “Spindle” galaxy NGC 2685, previously regarded as a two-ringed polar ring galaxy. Deep H I and optical (i'-band) observations are presented. The H I observations strongly suggest that the gaseous structure of NGC 2685 does not consist of two separate mutually inclined regions, but forms a coherent, extremely warped disk, the appearance of two rings being due to projection effects. By comparing the H I total-intensity maps with the optical image, we demonstrate that at large radii a faint stellar disk is well aligned with the outer H I disk. The shape of the dust lanes obscuring the NE part of the inner stellar body indicates that, also at smaller radii, NGC 2685 possesses a disk containing gas, dust, and stars in which the various constituents are aligned. At smaller radii, this disk is kinematically decoupled from the central stellar body; hence, in the region of the bright, central stellar body, NGC 2685 appears to consist of two disks that share a common center, but have different orientation: a bright stellar lenticular body apparently devoid of dust and gas, and a heavily warped low-surface brightness disk containing stars, gas, and dust. The low-surface-brightness disk changes its orientation gradually and at large radii assumes the orientation of the central stellar S0 disk. Since, according to our analysis, the intrinsic orientation of the low-surface-brightness disk changes through 70°, the gaseous disk is coherent, and is at no radius oriented perpendicularly with respect to the central stellar body, NGC 2685 is not likely to be a classical polar-ring galaxy.

Key words: galaxies: kinematics and dynamics -- galaxies: structure -- galaxies: ISM -- galaxies: peculiar -- galaxies: individual: NGC 2685

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