SDSS-IV MaNGA: Global and local stellar population properties of elliptical galaxies

Lacerna, Iván; Ibarra-Medel, H.; Ávila-Reese, V.; Hernández-Toledo, H. M.; Vázquez-Mata, J. A.; Sánchez, S. F.

doi:10.1051/0004-6361/202037503

Cited by 37 publications

(49 citation statements)

References 167 publications

(193 reference statements)

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“…In a previous paper, Lacerna et al (2020), we have found that the CLE galaxies accumulated 90% (50%) of their stellar masses between 5 and 7 (9 and 12) Gyr ago, with a downsizing trend in both stellar mass growth and SF quenching: the most massive CLEs tend to form stars earlier and to quench SF faster than the less massive CLE galaxies. As for radial trends, most of the CLEs have nearly flat radial mass-weighted age profiles but slightly negative when the luminosity-weighted ages are used.…”

Section: Galaxy Evolution Through the Fossil Record Methodsmentioning

confidence: 77%

“…This paper presents an update of the MaNGA CLE galaxy sample of Lacerna et al (2020). By using the fossil record method, we calculate the 2D mass and light (for different rest-frame bands) spatially-resolved maps corresponding to stellar populations up to a given look-back time.…”

Section: Galaxy Evolution Through the Fossil Record Methodsmentioning

confidence: 99%

“…In the early MaNGA morphological classification used in Lacerna et al ( 2020), many of the E galaxies with an inner disc were classified as S0s. In the morphological re-evaluation of these galaxies in Vázquez-Mata et al (2021), they were re-classified as Ellipticals (actually Elliculars), that is, the number of E galaxies increased with respect to Lacerna et al (2020). These authors studied a sample of 340 MaNGA Ellipticals from DR15, but limited to 𝑧 ≤0.08.…”

Section: Morphological Classification Of Elliptical Galaxiesmentioning

confidence: 99%

“…By "dead" we understand that the galaxy has been in a quenching regime by a long time (see Appendix B for a disscusion on definitions of SF quenching), that is, it became passive or retired. The operational criteria to define red and retired galaxies were discussed in Lacerna et al (2020). A summary is as follows.…”

Section: Spectro-photometric Selection Of Classical E Galaxiesmentioning

confidence: 99%

“…The remaining 17.9% of the MaNGA E galaxies have particular photometric and spectral line diagnostic features, which evidence them as different to the CLE galaxies, specially regarding their late evolution (for details, see Lacerna et al 2020). Briefly, the remaining E galaxies in our sample are as follows.…”

Section: Spectro-photometric Selection Of Classical E Galaxiesmentioning

confidence: 99%

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The differences between mass- and light-derived structural parameters over time for MaNGA Elliptical galaxies

Ibarra-Medel,

Avila-Reese,

Lacerna

et al. 2021

Preprint

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We apply stellar population synthesis analysis to obtain spatially-resolved archaeological inferences for a large sample of "red and dead" Elliptical galaxies (Classical Ellipticals; CLEs) from the MaNGA/SDSS-IV DR15 survey. From their 2D stellar light and mass maps, we explore the differences between the radial mass and light distributions in the rest-frame bands 𝑔, 𝑟, and 𝑖 as functions of look-back time, 𝑡 lb , or redshift, 𝑧. We characterize these differences through the ratios between the following mass-and light-derived global properties: sizes, concentrations, and effective surface densities. We find that the mass-to-light ratios of these properties change with 𝑡 lb , more the more massive the galaxies are. The CLE galaxy archaeological progenitors are, on average, less compact, concentrated, and dense in light than in mass as 𝑧 decreases. However, at later times, when also the evolution of the progenitors becomes passive at all radii, there is an upturn in these trends and the differences between mass and light in compactness/concentration decrease towards 𝑧 ∼ 0. The trends in the ratios of mass to light sizes agree qualitatively with results from direct observations in galaxy surveys at different redshifts. We discuss the caveats and interpretations of our results, and speculate that the strong structural evolution found in some previous studies for early-type galaxies could be explained partially by photometric changes rather than by intrinsic structural changes.

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Section: Galaxy Evolution Through the Fossil Record Methodsmentioning

confidence: 77%

Section: Galaxy Evolution Through the Fossil Record Methodsmentioning

confidence: 99%

Section: Morphological Classification Of Elliptical Galaxiesmentioning

confidence: 99%

Section: Spectro-photometric Selection Of Classical E Galaxiesmentioning

confidence: 99%

Section: Spectro-photometric Selection Of Classical E Galaxiesmentioning

confidence: 99%

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The differences between mass- and light-derived structural parameters over time for MaNGA Elliptical galaxies

Ibarra-Medel,

Avila-Reese,

Lacerna

et al. 2021

Preprint

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The role of AGN feedback in the structure, kinematics, and evolution of ETGs in Horizon simulations

Rosito

Pedrosa

Tissera

et al. 2021

A&A

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Context. Feedback processes play a fundamental role in the regulation of the star formation (SF) activity in galaxies and, in particular, in the quenching of early-type galaxies (ETGs) as has been inferred by observational and numerical studies of Λ-CDM models. At z = 0, ETGs exhibit well-known fundamental scaling relations, but the connection between scaling relations and the physical processes shaping ETG evolution remains unknown. Aims. This work aims to study the impact of the energetic feedback due to active galactic nuclei (AGN) on the formation and evolution of ETGs. We focus on assessing the impact of AGN feedback on the evolution of the mass–plane and the fundamental plane (FP; defined using mass surface density) as well as on morphology, kinematics, and stellar age across the FP. Methods. The Horizon-AGN and Horizon-noAGN cosmological hydrodynamical simulations were performed with identical initial conditions, including the same physical processes except for the activation of the AGN feedback in the former. We selected a sample of central ETGs from both simulations using the same criteria and exhaustively studied their SF activity, kinematics, and scaling relations for z ≤ 3. Results. We find that Horizon-AGN ETGs identified at z = 0 follow the observed fundamental scaling relations (mass–plane, FP, and mass–size relation) and qualitatively reproduce kinematic features albeit conserving a rotational inner component with a mass fraction regulated by the AGN feedback. We discover that AGN feedback seems to be required to reproduce the bimodality in the spin parameter distribution reported by observational works and the mass–size relation; more massive galaxies have older stellar populations, larger sizes, and are slower rotators. We study the evolution of the fundamental relations with redshift, finding a mild evolution of the mass–plane of Horizon-AGN ETGs for z < 1, whereas a stronger change is detected for z > 1. The ETGs in Horizon-noAGN show a strong systematic redshift evolution of the mass–plane. The FP of Horizon-AGN ETGs agrees with observations at z = 0. When AGN feedback is switched off, a fraction of galaxies depart from the expected FP at all analysed redshifts owing to the presence of a few extended galaxies with an excess of stellar surface density. We find that AGN feedback regulates the SF activity as a function of stellar mass and redshift being able to reproduce the observed relations. Our results show the impact of AGN feedback on the mass-to-light ratio (M/L) and its relation with the tilt of the luminosity FP (L-FP; defined using the averaged surface brightness). Overall, AGN feedback has an impact on the regulation of the SF activity, size, stellar surface density, stellar ages, rotation, and masses of ETGs that is reflected on the fundamental relations, particularly on the FP. We detect a dependence of the FP on stellar age and galaxy morphology that evolves with redshfit. The characteristics of the galaxy distribution on the FP according to these properties change drastically by z ∼ 1 in Horizon-AGN and hence this feature could provide further insight into the action of AGN feedback.

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Downsizing revised: Star formation timescales for elliptical galaxies with an environment-dependent IMF and a number of SNIa

Yan

Jeřabková

Kroupa

2021

A&A

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Previous studies of the stellar mean metallicity and [Mg/Fe] values of massive elliptical (E) galaxies suggest that their stars were formed over a very short timescale that cannot be reconciled with estimates from stellar population synthesis (SPS) studies and with hierarchical assembly. Applying the previously developed chemical evolution code, GalIMF, which allows an environment-dependent stellar initial mass function (IMF) to be applied to the integrated galaxy initial mass function theory instead of an invariant canonical IMF, the star formation timescales (SFT) of E galaxies are re-evaluated. The code’s uniqueness lies in it allowing the galaxy-wide IMF and associated chemical enrichment to evolve as the physical conditions in the galaxy change. The calculated SFTs become consistent with the independent SPS results if the number of type Ia supernovae (SNIa) per unit stellar mass increases for more massive E galaxies. This is a natural outcome of galaxies with higher star formation rates producing more massive star clusters, spawning a larger number of SNIa progenitors per star. The calculations show E galaxies with a stellar mass ≈109.5 M⊙ to have had the longest mean SFTs of ≈2 Gyr. The bulk of more massive E galaxies were formed faster (SFT ≈ 1 Gyr) leading to domination by M dwarf stars and larger dynamical mass-to-light ratios as observed, while lower mass galaxies tend to lose their gas supply more easily due to their shallower potential and therefore also have similarly-short mean SFTs. This work achieves, for the first time, consistency of the SFTs for early-type galaxies between chemical-enrichment and SPS modelling. Equally, it leads to an improved understanding of how the star formation environment may affect the total number of SNIa per unit stellar mass formed.

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SDSS-IV MaNGA: Global and local stellar population properties of elliptical galaxies

Cited by 37 publications

References 167 publications

The differences between mass- and light-derived structural parameters over time for MaNGA Elliptical galaxies

The differences between mass- and light-derived structural parameters over time for MaNGA Elliptical galaxies

The role of AGN feedback in the structure, kinematics, and evolution of ETGs in Horizon simulations

Downsizing revised: Star formation timescales for elliptical galaxies with an environment-dependent IMF and a number of SNIa

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