Abstrakt
Context. The lenticular galaxy NGC 474 hosts a rich system of tidal shells and streams, some of which are exceptionally bright.
Two teams recently presented spectroscopic observations of the brightest shells. These were the first shell spectra ever observed in integrated starlight.
The authors studied the stellar populations of the shell, of the center of the galaxy, and of its globular clusters. The precise formation scenario for the tidal features of this prominent galaxy still remained unclear, however.
Aims. Here, we add further clues on their formation from the radii of the shells, and we present a scenario for the formation of the tidal features that seems to be unique and can explain all available data.
Methods. Shell radii were analyzed with the shell identification method, and we ran self-consistent simulations of the formation of the tidal features.
We considered Newtonian as well as MOND gravity. Results.
Observations suggest that the tidal features originate from the accretion of a spiral galaxy. According to the shell identification method, the merging galaxies first collided 1.3 Gyr ago and then again 0.9 Gyr ago, thereby forming the shells in two generations.
This would also explain the young ages of stellar populations in the center of the galaxy and the young age of the globular clusters. The analytic models of shell propagation that underlie the shell identification method are verified by a simulation.
The simulations reproduce the observed morphology of the tidal features well. The accreted spiral likely reached NGC 474 on the plane of the sky nearly radially from the south, its rotation axis pointing toward us.
It probably had a stellar mass of about one-sixth of NGC 474, that is, 10(9.8)& x2006;M-circle dot. Apparently, all tidal features in the galaxy originate from one merger.