http://arxiv.org/abs/2305.09343
We examine the Galactic warp in a sample of all classical Cepheids with Gaia DR3 radial velocity. In each radial bin, we determine (1) the inclined plane normal to the mean orbital angular momentum of the stars and (2) that best fitting their positions. We find no warping inside $R\approx 11$ kpc; for larger $R$ the disc is increasingly inclined, reaching $i\sim 3^{\circ}$ at $R \ge 14$ kpc. With larger $R$ the azimuth of the warp’s ascending node shifts from $\varphi_{\mathrm{lon}}\approx-15^\circ$ at 11 kpc by about $14^{\circ}$/kpc in the direction of Galactic rotation, implying a leading spiral of nodes, the general behaviour of warped galaxies. From the method of fitting planes to the positions we also obtain $\dot{\varphi}{\mathrm{lon}}$ and find prograde precession of $\dot{\varphi}{\mathrm{lon}} \sim 12$ km/s/kpc at 12 kpc decreasing to $\sim 6$ km/s/kpc at 14 kpc and beyond. This would unwind the leading spiral of nodes in $\sim 100$ Myr, suggesting that our instantaneous measurements of $\dot{\varphi}{\mathrm{lon}}$ reflect transient behaviour. This is consistent with existing simulations, which show oscillations in $\dot{\varphi}{\mathrm{lon}}$ overlaying a long-term retrograde differential precession which generates the leading spiral of nodes.
W. Dehnen, M. Semczuk and R. Schönrich
Wed, 17 May 23
60/67
Comments: 9 pages, accepted for publication in MNRAS
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