A new insight of AGC 198691 (Leoncino) galaxy with MEGARA at the GTC
We describe the observations of the low metallicity nearby galaxy AGC 198691 (Leoncino Dwarf) obtained with the Integral Field Unit of the instrument MEGARA at the Gran Telescopio Canarias. The observations cover the wavelength ranges 4304-5198 Aand 6098-7306 Awith a resolving power R approximate to...
| Authors: | , , , , , , , , , , , |
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| Format: | article |
| Publication Date: | 2022 |
| Country: | España |
| Institution: | Universidad Complutense de Madrid (UCM) |
| Repository: | Docta Complutense |
| Language: | English |
| OAI Identifier: | oai:docta.ucm.es:20.500.14352/72136 |
| Online Access: | https://hdl.handle.net/20.500.14352/72136 |
| Access Level: | Open access |
| Keyword: | 52 Evolutionary synthesis models Extragalactic hii-regions Emission-line galaxies Metal-poor galaxies Rich dwarf galaxy Fast alpha survey Alfalfa discovery Low-mass Oxygen abundances Leo P Astrofísica |
| Summary: | We describe the observations of the low metallicity nearby galaxy AGC 198691 (Leoncino Dwarf) obtained with the Integral Field Unit of the instrument MEGARA at the Gran Telescopio Canarias. The observations cover the wavelength ranges 4304-5198 Aand 6098-7306 Awith a resolving power R approximate to 6000. We present 2D maps of the ionized gas, deriving the extension of the H II region and gas kinematics from the observed emission lines. We have not found any evidence of recent gas infall or loss of metals by means of outflows. This result is supported by the closed-box model predictions, consistent with the oxygen abundance found by other authors in this galaxy and points towards Leoncino being a genuine XMD galaxy. We present for the first time spatially resolved spectroscopy allowing the detailed study of a star-forming region. We use POPSTAR + CLOUDY models to simulate the emission-line spectrum. We find that the central emission-line spectrum can be explained by a single young ionizing cluster with an age of approximate to 3.5 +/- 0.5 Myr and a stellar mass of approximate to 2 x10(3) M-circle dot. However, the radial profiles of [O III].5007Aand the Balmer lines in emission demand photoionization by clusters of different ages between 3.5 and 6.5 Myr that might respond either to the evolution of a single cluster evolving along the cooling time of the nebula (approximate to 3 Myr at the metallicity of Leoncino, Z approximate to 0.0004) or to mass segregation of the cluster, being both scenarios consistent with the observed equivalent widths of the Balmer lines. |
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