We identified the chemical species within I08005 using a radio spectrum from the GMT, finding HCN and a surprisingly high abundance of fast moving silicon-related species. In this project, I aimed to analyse the spectral data from I08005 and to computationally reproduce it to determine its properties. I08005 stood out because of its feeble 13CO transition line and specific intense emission lines not seen in the other spectra. We initially studied the GMT radio spectrum of three protoplanetary nebulae: I19374, I16342 and I08005. Understanding extreme outflows and how they form can help us to create more accurate models for how AGB stars transition to planetary nebulae. Extreme outflows are jets with ejection velocities surpassing 100 km/s and are thought to be an intrinsic feature of protoplanetary nebulae. They are composed of an envelope containing low velocity molecules (less than ~20 km/s) with higher velocity molecules found in molecular jets. In-between the last phase of an AGB star and a planetary nebula, these objects are known as protoplanetary nebulae. These stars eventually become a planetary nebula, where the outermost gaseous layers are ejected into space in pulses, leaving a small, bare carbon and oxygen core.
Late in their lives, when intermediate mass stars have exhausted the fuel supply of helium in their cores, they will expand and evolve into cool, giant AGB stars. These results were presented as a poster at the IAUS366. Gómez-Ruiz, where he modelled the chemistry in a protoplanetary nebula. He spent the Summer 2021 doing an internship at Instituto Nacional de Astrofísica, Óptica y Electrónica (INAOE, Mexico) supervised by Dr. Pau Grèbol Tomàs is a Physics and Chemistry graduate at Universitat Autònoma de Barcelona (UAB) currently taking his first year of a MSc in Astrophysics at Universidad de La Laguna (ULL, Canary Islands).