In the current cosmological model, galaxies are formed in a hierarchical way, by merging with each other. These mergers can lead to kinematic anomalies that can be used to shed light onto the formation history of the galaxy. However, it is important to be able to distinguish whether these anomalies are an unambiguous signal of a past merger or if they can originate from different processes. One of these kinematic anomalies is prolate rotation. A galaxy shows prolate rotation if it rotates around its major axis. This kinematic characteristic is relatively frequent in massive galaxies and it becomes less abundant when we move towards lower masses. In the Local Group there are only two known examples of dwarfs that show prolate rotation (Phoenix and Andromeda II). Cosmological simulations show that in massive galaxies prolate rotation is strongly related to previous mergers. In the dwarfs regime, idealised simulations have shown that it is possible to reproduce this particular kinematic property through mergers, however, it remains to be shown whether this is possible in a cosmological context. Here we have made use of hydrodynamical cosmological simulations with the aim of identifying dwarf galaxies with prolate rotation. From the 27 dwarfs explored, only 1 galaxy shows clear rotation around its major axis, whose origin can be linked to a merger with another galaxy 9 billion years ago. This galaxy shares with Phoenix and Andromeda II not only its particular kinematics, but also the way in which the metals are distributed inside the galaxy, being the central parts much more metallic than the outskirts. This distribution is also related to the merger that caused the prolate rotation. The older and less metallic stars were expelled to the outskirts by the merger, while the residual star formation kept increasing the central metallicity, building in that way a very steep metallicity gradient. In this work we have shown for the first time how it is possible to form dwarf galaxies with prolate rotation in a cosmological context, as well as how the mergers offer a viable explanation for the formation of such peculiar systems, characterized by steep metallicity gradients and prolate rotation.
It may interest you
The international team of the “Chromospheric LAyer Spectro-Polarimeter” (CLASP) space missions, which includes three scientists of the Instituto de Astrofísica de Canarias (IAC), has just received the NASA Group Achievement Honor Award for the successful execution of the recent CLASP2.1 mission. The goal of this mission is to map the magnetic field of the Sun in an extended region of the chromosphere. The Chromospheric Layer Spectro-Polarimeter series of heliophysics sounding rocket missions were designed to measure the polarization of the ultraviolet light emitted by the Sun to study theAdvertised on
A scientific team led by the University of Alicante, with participation by the Instituto de Astrofísica de Canarias (IAC) has produced a detailed study of the most massive young star cluster in the Milky Way. This cloud of stars contains different types of giant stars in diverse phases of evolution, and can be used as an excellent laboratory for the study of the formation and evolution of massive stars. Stars tend to form in clusters, containing from just a few to several thousand stars, which share the same age and composition, although they show evolutionary differences. Among the clustersAdvertised on
It took place on May 24th and 25th in the meeting room of the Parador in Breña Baja A large group of representatives of the various institutions which take part in the International Scientific Committee met face to face on the Island of La Palma last Tuesday and Wednesday, 24th and 25tnh of May, and they were joined remotely by further participants on-line. In this meeting of the CCI (International Scientific Committee Spanish initials), they discussed, among other matters, the most recent scientific achievements at the Canary Observatories, as well as the status of new projects. In additionAdvertised on