Kinematic modeling of disk galaxies III . The warped “ Spindle ” NGC 2685

This is the third of a series of papers in which the structure and kinematics of disk galaxies is studied. Employing direct tilted-ring fits to the data cube as introduced in Paper I, we perform an analysis of the " Spindle " galaxy NGC 2685, previously regarded as 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 centre, 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 orientated perpendicularly with respect to the central stellar body, NGC 2685 is likely not a classical polar-ring galaxy.