@article{2023A&A...677A.114A,
 abstract = {Green Pea galaxies (GPs) present among the most intense starbursts known
in the nearby Universe. These galaxies are regarded as local
analogs of high-redshift galaxies, making them a benchmark in
the understanding of the star formation processes and the
galactic evolution in the early Universe. In this work, we
performed an integral field spectroscopic (IFS) study for a set
of 24 GPs to investigate the interplay between its ionized
interstellar medium (ISM) and the massive star formation that
these galaxies present. Observations were taken in the optical
spectral range (\ensuremathłambda4750
̊A-\ensuremathłambda9350 \Å) with the MUSE
spectrograph attached to the 8.2 m telescope VLT. Spatial
extension criteria were employed to verify which GPs are
spatially resolved in the MUSE data cubes. We created and
analyzed maps of spatially distributed emission lines (at
different stages of excitation), continuum emission, and
properties of the ionized ISM (e.g., ionization structure
indicators, physical-chemical conditions, dust extinction). We
also took advantage of our IFS data to produce integrated
spectra of selected galactic regions in order to study their
physical-chemical conditions. Maps of relevant emission lines
and emission line ratios show that higher-excitation gas is
preferentially located in the center of the galaxy, where the
starburst is present. The continuum maps, with an average
angular extent of 4″, exhibit more complex structures than the
emission line maps. However, the [O
III]\ensuremathłambda5007 \r̊ emission line maps tend
to extend beyond the continuum images (the average angular
extent is 5.5″), indicating the presence of low surface
brightness ionized gas in the outer parts of the galaxies.
H\ensuremathα/H\ensuremathβ, [S
II]/H\ensuremathα, and [O I]/H\ensuremathα
maps trace low-extinction, optically thin regions. The line
ratios [O III]/H\ensuremathβ and [N
II]/H\ensuremathα span extensive ranges, with values
varying from 0.5 dex to 0.9 dex and from \ensuremath-1.7 dex
to \ensuremath-0.8 dex, respectively. Regarding the
integrated spectra, the line ratios were fit to derive physical
properties including the electron densities n$_e$ = 30
\ensuremath- 530 cm$^\ensuremath-3$, and, in six GPs
with a measurable [O III]\ensuremathłambda4363 \r̊
line, electron temperatures of T$_e$ = 11 500 K-15 500 K, so
the direct method was applied in these objects to retrieve
metallicities 12 + log(O/H)≃8. We found the presence of the
high-ionizing nebular He II\ensuremathłambda4686 \rA
̊line in three GPs, where two of them present among the highest
sSFR values (> 8 × 10$^8$
yr$^\ensuremath-1$) in this sample. Non-Wolf-Rayet (WR)
features are detected in these galaxy spectra.},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2023A&A...677A.114A},
 archiveprefix = {arXiv},
 author = {Arroyo-Polonio, A. and Iglesias-Páramo, J. and Kehrig, C. and Vı́lchez, J.~M. and Amor\ń, R. and Breda, I. and Pérez-Montero, E. and Pérez-D\'ź, B. and Hayes, M.},
 doi = {10.1051/0004-6361/202346192},
 eid = {A114},
 eprint = {2309.09585},
 journal = {åp},
 keywords = {HII regions, galaxies: starburst, galaxies: ISM, galaxies: star formation, galaxies: evolution, ISM: abundances, Astrophysics - Astrophysics of Galaxies},
 month = {September},
 pages = {A114},
 primaryclass = {astro-ph.GA},
 title = {A MUSE/VLT spatially resolved study of the emission structure of Green Pea galaxies},
 volume = {677},
 year = {2023}
}