The origin of bulges and discs in the CALIFA survey – I. Morphological evolution
MetadataShow full item record
AuthorMéndez Abreu, J.
Oxford University Press
Galaxies: bulgesGalaxies: evolutionGalaxies: formationGalaxies: structure
J Méndez-Abreu, A de Lorenzo-Cáceres, S F Sánchez, The origin of bulges and discs in the CALIFA survey – I. Morphological evolution, Monthly Notices of the Royal Astronomical Society, Volume 504, Issue 2, June 2021, Pages 3058–3073, [https://doi.org/10.1093/mnras/stab1064]
SponsorshipSpanish Government AYA2017-83204-P; Programa Operativo FEDER Andalucia 2014-2020; Andalucian Office for Economy and Knowledge; European Commission; Consejo Nacional de Ciencia y Tecnologia (CONACyT) CB-285080; Spanish Government ICTS-2009-10; Centro Astronomico Hispano-Aleman; Programa de Apoyo a Proyectos de Investigacion e Innovacion Tecnologica (PAPIIT) IN100519; Spanish Government AYA201677237-C3-1-P RTI2018-096188-B-I00 FC-2016-01-1916
This series of papers aims at understanding the formation and evolution of non-barred disc galaxies. We use the new spectro-photometric decomposition code, C2D, to separate the spectral information of bulges and discs of a statistically representative sample of galaxies from the CALIFA survey. Then, we study their stellar population properties analysing the structure-independent datacubes with the PIPE3D algorithm. We find a correlation between the bulge-to-total (B/T) luminosity (and mass) ratio and galaxy stellar mass. The B/T mass ratio has only a mild evolution with redshift, but the bulge-to-disc (B/D) mass ratio shows a clear increase of the disc component since redshift z < 1 for massive galaxies. The mass-size relation for both bulges and discs describes an upturn at high galaxy stellar masses (log(M-star/M-circle dot) > 10.5). The relation holds for bulges but not for discs when using their individual stellar masses. We find a negligible evolution of the mass-size relation for both the most massive (log(M-star,M-b,M-d/M-circle dot) > 10) bulges and discs. For lower masses, discs show a larger variation than bulges. We also find a correlation between the Sersic index of bulges and both galaxy and bulge stellar mass, which does not hold for the disc mass. Our results support an inside-out formation of nearby non-barred galaxies, and they suggest that (i) bulges formed early-on and (ii) they have not evolved much through cosmic time. However, we find that the early properties of bulges drive the future evolution of the galaxy as a whole, and particularly the properties of the discs that eventually form around them.