Abstract
Planetary nebulae (PNe) represent the ejected outer layers of an evolved low-to-intermediate mass 11star, and consist of ionized, neutral, and molecular components, along with dust. In total, the nebular 12 material contains the stellar envelope that was ejected during the AGB phase or through binary 13 interactions with a companion. The PN central star is formed by the former core of the AGB or RGB 14 progenitor of the PNe, which is now contracting towards the white dwarf phase. The PN central star 15 is a post-AGB object which has evolved crossing the HR diagram, and has an effective temperature 16 of 28,000 K up to more than 250,000 K. It emits a large fraction of its light as UV photons that ionize 17 the envelope. PNe are mainly studied through imaging, photometry and low-and high-resolution 18 spectroscopy techniques which allow determination of the physical conditions and chemical 19 abundances in the nebula. Through this kind of analysis it is possible to study the physical processes 20 in ionized plasmas, the evolution and characteristics of the central star, along with the mechanisms of 21 ejection of the nebula and the evolution of the interstellar medium (ISM) -in external galaxies as 22 well as in the Milky Way -which will be enriched with elements produced in the stellar 23 nucleosynthesis and brought to the stellar surface via several dredge-up episodes. Further, an accurate 24 census of PNe provides an important constraint on a galaxy's star formation history.
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