## 1 Introduction
This is an expanding ionized circumstellar cloud that was ejected during the asymptotic giant branch (AGB) phase of its progenitor star, a star below 8 to 9 solar masses [8]. A residual remnant persists from the star in the form of a white dwarf, characterized by its elevated temperature. The UV (ultraviolet) photons emitted by this star ionize the envelope, and the recombination processes in the ionized gas cause emissions in the visible and infrared (IR) range. Additionally, the physical conditions in these ionized envelopes are such that \"forbidden\" lines of oxygen, nitrogen, sulfur (OII, OIII, NII, SII), etc., are also produced, which are characteristic of these nebulae. These nebulae, in general, form rings or bubbles, but depending on the characteristics of the surrounding material or the binary nature of the progenitor (as in the case of symbiotic stars), they can also have elliptical, bipolar, and even quadrupolar or more complex morphologies [9]. * Symbiotic stars (SS). These are stellar systems composed of two separate stars orbiting around their center of mass (MC). They consist of an evolved red giant star (spectral type K or M) that loses and transfers mass to its companion, which is typically a white dwarf with high temperature emitting an important fraction of energy as ionizing photons. Occasionally, a significant wind is detected in this component. The term \"stellar symbiosis\" is used because each star depends on and influences the evolution of the other. Understanding the processes of mass transfer and accretion in these systems is not only essential for understanding the evolution of stars in general, but also for understanding any binary interaction involving evolved giants [10]. It is also important to know the fraction of objects of this type, both to count them within binary (or multiple) objects and to verify theories of star formation and evolution. The astronomical objects, PN and SS, are difficult to distinguish from each other due to their shared characteristics and their low representation compared to other celestial objects. Spectroscopy is a powerful observational technique that provides the ability to obtain and analyze the emission of objects across all wavelengths. In the visible and IR region, it enables the analysis of ionized or neutral chemical elements, as well as the determination of the physical characteristics of the gas. In the mid to far-infrared range, it allows for the analysis of the dust present around objects [11]. PN and SS are characterized by intense emission lines in their visible spectrum, although they can be easily confused with each other. Moreover, photometrically, they can be mistaken for stars of other types, such as red giants or main sequence stars (MS). As mentioned earlier, it is important to identify and quantify these objects as they are the primary contributors to the chemical evolution of galaxies. To identify the best classification models, several machine learning techniques were analyzed, including Random Forest (RF), Support Vector Machine (SVM), Artificial Neural Networks (ANN), Gradient Boosting, and Naive Bayes Classifier. The models were trained using solely the spectral information of stars of this type, which was obtained from the Gaia DR3 Catalog. It is important to note that the spectral resolution of the Gaia dataset used in this study is relatively low compared to the spectral resolution obtained with other instruments on Earth or in orbit. A higher spectral resolution would allow for the easier differentiation and distinction of these objects. However, those instruments do not have the coverage and depth that Gaia provides, as Gaia has observed around 220 million low-resolution BP/RP spectra, reaching a magnitude of G! 17.65 [12]. The results were satisfactory, achieving high classification precision values. These models will be a valuable tool, and can support the classification of this type of peculiar stars.