The obliquity can be measured by the Rossiter-Mclaughlin (RM) effect, which is often manifested as a pattern of anomalous radial velocities (RVs) during a planetary transit. A well-established distribution of stellar obliquity can help us to understand the formation of close-orbiting gas giants. However, there are few observations focusing on evolved systems, and thus we know nothing about whether stars can keep high obliquities after a long-term evolution. Thanks to TESS, more transiting planets around evolved stars are revealed, providing opportunities to measure the obliquities of evolved stars. We here propose to observe three TOIs around evolved stars revealed by TESS to fill the vacancy of RM effects of evolved stars. Our targets are strongly supported to be hot-Jupiters by TESS Data Validation Reports, data in the archival ExoFOP, and personal communications. Within this proposal, we will be able to provide evidence of planet migration after the star moving out of the main sequence.
This document was translated from LATEX by HEVEA.