Speaker
Description
Leo P is a poorly studied near-primordial isolated dwarf irregular galaxy at a distance of ∼ 1.6 Mpc, with an extremely low mass of ∼ 105M⊙.
From Hubble Space Telescope and Arecibo Legacy Fast observations, its characteristics show the same behaviour as expected in a low-luminosity dSph Milky Way satellite. It was defined as the “quintessential system to test theories of how the smallest structures in our universe survive and grow.”
Observations suggest an ongoing star formation in its prominent H II region. This feature also gives estimations of the oxygen abundance which is around 3% of solar. It makes it one of the most metal-poor galaxies known in the local Universe.
In this work, we present the first estimated spectroscopic metallicities of evolved cool stars in Leo P. We use MUSE data to extract and analyse the spectra of 16 red giant branch stars. In order to derive the metallicity of Leo P we apply literature calibrations for our equivalent widths measurements of the Ca II triplet lines.
We will also present tentative luminosity- and stellar mass-metallicity relations compared to other low-metallicity galaxies (e.g. I Zw 18, DDO 68, and SBS 0335-052W) to check the previously detected offset of these other galaxies, with respect to Leo P, in these relations.
| Do you plan to attend the symposium in-person or virtually? | in-person |
|---|
