## 2. The orientation of the warps of the Milky Way, M 31 and M 33To characterize the position of a warp in space, we have two possibilities. One of them is the direction of the line of nodes itself. The other one is the "orientation" vector. Let us precisely define the "orientation" vector of a warp. Suppose an untwisted line of nodes. Let be a unitary vector contained in the line of nodes. Its direction is conventionally assigned as pointing to a region from which the warps are seen as N-shaped (not S-shaped), i.e. from which, due to the observed bending, the galaxy appears to have a clockwise gyration. Let be a unitary vector with the direction of a rotation axis. We define the orientation direction as that containing either defined as or . From an observational point of view and are undistinguishable. From a theoretical point of view, whatever the interpretation is assumed, the distinction between and is probably meaningless.
In the figure, we show the direction ,
in a galaxy observed as edge-on. We define
, , in this way, because
under the interpretation of warps made in the magnetic model by
Battaner The information given by both, the direction of the line of nodes and the orientation vector, are not equivalent. For instance, if the galaxy is gyrated about the line of nodes, its direction would not be modified, but the orientation vector could change. Therefore we have made the calculation about the coherence for both vectors. Let us calculate for M 31, M 33 and the Milky Way, using the same coordinate system. The orientation vector defined in the system centred in the plane of the considered galaxy must be subject to the following transformations: a) From referred to the plane of the galaxy, we obtain referred to the plane of the sky, defined by the vectors ( in the line of the sight direction; and in the tangent plane, northwards and eastwards) b) From referred to the plane of the sky, we obtain referred to the plane of the equator where are the inclination, position angle and equatorial coordinates, respectively.The same transformations must be taken into account to obtain the direction of the line of nodes. © European Southern Observatory (ESO) 1997 Online publication: June 30, 1998 |