SDSS-IV MaNGA: The MaNGA Dwarf Galaxy Sample Presentation

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dc.contributor.authorCano-Diaz, M.
dc.contributor.authorHernandez-Toledo, H. M.
dc.contributor.authorRodriguez-Puebla, A.
dc.contributor.authorIbarra-Medel, H. J.
dc.contributor.authorAvila-Reese, V
dc.contributor.authorValenzuela, O.
dc.contributor.authorMedellin-Hurtado, A. E.
dc.contributor.authorVazquez-Mata, J. A.
dc.contributor.authorWeijmans, A.
dc.contributor.authorGonzalez, J. J.
dc.contributor.authorAquino-Ortiz, E.
dc.contributor.authorMartinez-Vazquez, L. A.
dc.contributor.authorLane, Richard R.
dc.date.accessioned2025-01-20T21:02:43Z
dc.date.available2025-01-20T21:02:43Z
dc.date.issued2022
dc.description.abstractWe present the MaNGA Dwarf galaxy (MaNDala) Value Added Catalog (VAC), from the final release of the Sloan Digital Sky Survey-IV program. MaNDala consists of 136 randomly selected bright dwarf galaxies with M (*) < 10(9.1) M (circle dot) and M ( g ) > -18.5, making it the largest integral field spectroscopy homogeneous sample of dwarf galaxies. We release a photometric analysis of the g, r, and z broadband imaging based on the DESI Legacy Imaging Surveys, as well as a spectroscopic analysis based on the Pipe3D SDSS-IV VAC. Our release includes the surface brightness (SB), geometric parameters, and color profiles, Sersic fits as well as stellar population properties (such as stellar ages, metallicities, and star formation histories), and emission lines' fluxes within the FOV and the effective radii of the galaxies. We find that the majority of the MaNDala galaxies are star-forming late-type galaxies with n (Sersic,r) similar to 1.6 that are centrals (central/satellite dichotomy). MaNDala covers a large range of SB values (we find 11 candidate ultra-diffuse galaxies and three compact ones), filling the gap between classical dwarfs and low-mass galaxies in the Kormendy Diagram and in the size-mass/luminosity relation, which seems to flatten at 10(8) < M (*)/M (circle dot) < 10(9) with R ( e,r ) similar to 2.7 kpc. A large fraction of MaNDala galaxies formed from an early low-metallicity burst of SF, but also from late SF events from more metal-enriched gas: half of the MaNDala galaxies assembled 50% of their mass at z > 2, while the last 20% was at z < 0.3. Finally, a bending of the sSFR-M (*) relation at M (*) similar to 10(9) M (circle dot) for the main-sequence galaxies seems to be supported by MaNDala.
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-3881/ac8549
dc.identifier.eissn1538-3881
dc.identifier.issn0004-6256
dc.identifier.urihttps://doi.org/10.3847/1538-3881/ac8549
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/93077
dc.identifier.wosidWOS:000850682000001
dc.issue.numero4
dc.language.isoen
dc.revistaAstronomical journal
dc.rightsacceso restringido
dc.titleSDSS-IV MaNGA: The MaNGA Dwarf Galaxy Sample Presentation
dc.typeartículo
dc.volumen164
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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