@ARTICLE{2026A&A...706A.289P,
       author = {{P{\'e}rez-D{\'\i}az}, Borja and {V{\'\i}lchez}, Jos{\'e} M. and {P{\'e}rez-Montero}, Enrique and {Zinchenko}, Igor A. and {Tapia-Contreras}, Brian and {Tissera}, Patricia B.},
        title = "{Chemical enrichment in LINERs from MaNGA: II. Characterizing the shape of the radial metallicity gradients}",
      journal = {\aap},
     keywords = {galaxies: abundances, galaxies: active, galaxies: ISM, galaxies: nuclei, Astrophysics of Galaxies},
         year = 2026,
        month = feb,
       volume = {706},
          eid = {A289},
        pages = {A289},
     abstract = "{Context. Chemical abundance radial gradients provide key information on
        how the processes that affect chemical enrichment of the gas-
        phase interstellar medium (ISM) act at different galaxy scales.
        In the past decades, though there has been an increase in the
        number of galaxies studied with integral field spectroscopy,
        there is still not a clear picture on a subsequent
        characterization of the chemical abundance radial gradients in
        galaxies hosting active galactic nuclei (AGNs). This lack of
        studies is even more accentuated in the case of low-ionization
        nuclear emission-line regions (LINERs). Aims. For the first
        time, we analyze the chemical abundance radial gradients in a
        sample of LINER-like galaxies, whose nuclear emission has been
        previously discussed (Paper I). Methods. We used a sample of 97
        galaxies from the Mapping Nearby Galaxies at Apache Point
        Observatory (MaNGA), whose nuclear regions show LINER-like
        emission. We used the open-source code HII-CHI-MISTRY to
        estimate the chemical abundance ratios 12+log(O/H) and log(N/O)
        in the HII regions across the disks in our sample as well as in
        the nuclear parts where the LINER-like activity dominates. To
        fit the radial profiles, we used a piecewise methodology that
        uses a non-fixed number of breaks to find the best fit for the
        data. Results. We find that a majority of our sample of galaxies
        exhibit departures from the single linear gradient both in
        12+log(O/H) and log(N/O), as expected from the inside-out
        scenario. We investigated whether these departures are driven by
        galaxy properties (stellar mass, neutral gas mass, stellar
        velocity dispersion) but found no correlation at all. We also
        report that in most cases, there is no correlation between the
        shape of the 12+log(O/H) and log(N/O) radial profiles. We
        propose a model in which AGN feed(back), acting at different
        scales depending on the galaxy and its evolutionary stage, might
        be responsible for these departures.}",
          doi = {10.1051/0004-6361/202555821},
archivePrefix = {arXiv},
       eprint = {2512.10769},
 primaryClass = {astro-ph.GA},
       adsurl = {https://ui.adsabs.harvard.edu/abs/2026A&A...706A.289P},
      adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}