Transmisión por el canal de YouTube del IAR
Expositora: Dra. Amanda Reis Lopes, IALP
Resumen: The analysis of emission lines in astrophysical sources enables us to gain insight into the nature of the object, such as the density of the ionizing gas. Furthermore, the emission map associated with the HI image can provide us with a better understanding of the physical processes occurring in these sources. The filter configuration of the Southern Photometric Local Universe Survey (S-PLUS), a wide field 12 band (5 broad and 7 narrow) survey observing the Southern Sky, is ideal to detect emission by the combination of narrow and broad bands. To investigate Halpha emitters sources, we developed a code named P.E.L.E. (Pixel-to-pixel Emission Line Estimate) that combines S-PLUS images using the Three Filter Method to create emission line maps. We selected galaxies from the Fornax cluster to evaluate P.E.L.E., as the Halpha line is situated in the J0660 band at Fornax distance and there are already a few published Halpha maps from the Fornax 3D project that can be compared to our results. A second method to detect emission relies in the combination of color-color plots, which is efficient to search for Extreme Emission Line Galaxies (EELGs), which are low-metallicity star-forming galaxies that can be regarded as local analogs of galaxies in the early Universe. In this talk, we will discuss our two methodologies to identify emission, the first focus on the Fornax members and some preliminary tests on planetary nebulae in the Small Magellanic Cloud, and the second used to identify EELG at z<0.05.