Inside-out growth or inside-out quenching? Clues from colour gradients of local galaxies

Lian, Jianhui; Yan, Renbin; Blanton, Michael R.; Kong, Xu

doi:10.1093/mnras/stx2216

Cited by 10 publications

(8 citation statements)

References 34 publications

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“…Finally, the required quenching process does not act as a step function in radius, only affecting the innermost regions and gradually moving outwards, but has an effect on the entire galaxy. This finding echoes that of Lian et al (2017), who considers both the NUV − u and u − i colours, to gain insight into the timescales of inside out growth and quenching in star forming galaxies. Their work favours a model where, after an initial period of inside-out growth, inner and outer regions of the galaxy 'quench' synchronously.…”

Section: The Physics Of the Slow Quenching Modesupporting

confidence: 73%

“…Their work favours a model where, after an initial period of inside-out growth, inner and outer regions of the galaxy 'quench' synchronously. It is worth noting, however, that Lian et al (2017) define quenching as a period where the SFR is declining exponentially with a faster e-folding time than during the growth phase. In this work, however, we have limited ourselves to studying the ratio between current star formation (SFR) and its time integral (M ).…”

Section: The Physics Of the Slow Quenching Modementioning

confidence: 99%

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SDSS IV MaNGA – sSFR profiles and the slow quenching of discs in green valley galaxies

Belfiore

Maiolino

Bundy

et al. 2018

Monthly Notices of the Royal Astronomical Society

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162

149

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We study radial profiles in Hα equivalent width and specific star formation rate (sSFR) derived from spatially-resolved SDSS-IV MaNGA spectroscopy to gain insight on the physical mechanisms that suppress star formation and determine a galaxy's location in the SFR-M diagram. Even within the star-forming 'main sequence', the measured sSFR decreases with stellar mass, both in an integrated and spatially-resolved sense. Flat sSFR radial profiles are observed for log(M /M ) < 10.5, while star-forming galaxies of higher mass show a significant decrease in sSFR in the central regions, a likely consequence of both larger bulges and an inside-out growth history. Our primary focus is the green valley, constituted by galaxies lying below the star formation main sequence, but not fully passive. In the green valley we find sSFR profiles that are suppressed with respect to star-forming galaxies of the same mass at all galactocentric distances out to 2 effective radii. The responsible quenching mechanism therefore appears to affect the entire galaxy, not simply an expanding central region. The majority of green valley galaxies of log(M /M ) > 10.0 are classified spectroscopically as central low-ionisation emission-line regions (cLIERs). Despite displaying a higher central stellar mass concentration, the sSFR suppression observed in cLIER galaxies is not simply due to the larger mass of the bulge. Drawing a comparison sample of star forming galaxies with the same M and Σ 1 kpc (the mass surface density within 1 kpc), we show that a high Σ 1 kpc is not a sufficient condition for determining central quiescence.

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Section: The Physics Of the Slow Quenching Modesupporting

confidence: 73%

Section: The Physics Of the Slow Quenching Modementioning

confidence: 99%

SDSS IV MaNGA – sSFR profiles and the slow quenching of discs in green valley galaxies

Belfiore

Maiolino

Bundy

et al. 2018

Monthly Notices of the Royal Astronomical Society

Self Cite

162

149

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“…The observational study of the radial mass growth of individual galaxies is based mainly on fossil signals as the color, metallicity, and age gradients obtained from photometric, spectral energy distribution, and/or linestrength indices observations of local galaxies (for recent works, see e.g., Wang et al 2011;Pan et al 2015;Li et al 2015;Dale et al 2016;Kennedy et al 2016;Lian et al 2017). A more complete inference is provided by the fossil record method using Integral Field Spectroscopy (IFS) observations across the galaxies (Lin et al 2013;Pérez et al 2013;Ibarra-Medel et al 2016;González Delgado et al 2016;Goddard et al 2017;García-Benito et al 2017).…”

Section: Observational Inferencesmentioning

confidence: 99%

“…Both the structural inside-out growth of galaxies and the inside-out SF quenching imply that the inner stellar populations result older than the outer ones and that the stellar half-mass radius grows with time. An open question is which of these processes dominates in the evolution of galaxies and what signatures evidence the dominion of one or another of these processes (Lian et al 2017).…”

Section: Introductionmentioning

confidence: 99%

The Global and Radial Stellar Mass Assembly of Milky Way-sized Galaxies

Avila-Reese

González-Samaniego

Colín

et al. 2018

ApJ

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We study the global and radial stellar mass assembly of eight zoomed-in MW-sized galaxies produced in Hydrodynamics cosmological simulations. The disk-dominated galaxies (4) show a fast initial stellar mass growth in the innermost parts, driven mostly by in-situ SF, but since z ∼ 2 − 1 the SF enters in a long-term quenching phase. The outer regions follow this trend but more gentle as more external they are. As the result, the radial stellar mass growth is highly inside-out due to both the inside-out structural growth and inside-out SF quenching. The half-mass radius evolves fast; for instance, R 0.5 (z = 1)< 0.5R 0.5 (z = 0). Two other runs resemble lenticular galaxies. One shows also a pronounced inside-out growth and the other one presents a nearly uniform radial mass assembly. The other two galaxies suffered late major mergers. Their normalized radial mass growth histories (MGHs) are nearly close among them but with periods of outside-in assembly during or after the mergers. For all the simulations, the archaeological radial MGHs calculated from the z = 0 stellar-particles age distribution are similar to the current MGHs, which evidences that the mass assembly by ex-situ stars and the radial mass transport do not change significantly their radial mass distributions. Our results agree qualitatively with observational inferences from the fossil record method applied to a survey of local galaxies and from look-back observations of progenitors of MW-sized galaxies. However, the inside-out growth mode is more pronounced and the R 0.5 growth is faster in simulations than in observational inferences.

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“…The stellar metallicity accounts for the chemical enrichment throughout the star-forming history of the galaxy. Although HII regions have a memory of the past SFH , gas-phase metallicity is susceptible to outflows and inflows, among others process (Lian et al 2017;Wu et al 2017), that can alter the metallicity radial profiles. For this reason, in this paper we have focused on stellar metallicity.…”

Section: Introductionmentioning

confidence: 99%

Effects of environment on stellar metallicity profiles of late-type galaxies in the CALIFA survey

Coenda,

Mast,

Muriel

et al. 2020

Preprint

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Aims. We explore the effects of environment in the evolution of late-type galaxies by studying the radial profiles of light-and massweighted metallicities of galaxies in two discrete environments: field and groups. Methods. To study the dependence of metallicity on environment. We use a sample of 167 late-type galaxies, with stellar masses 9 ≤ log(M /M ) ≤ 12, drawn from the CALIFA survey. Firstly, we obtain light-and mass-weighted stellar metallicty profiles, and stellar mass density profiles of these galaxies, using publicly available data. Then we classify them according to their environment into field and group galaxies. Finally, we make a study of the metallicity of galaxies in these two environments which includes the comparison of the metallicity as a function of the radius, at a characteristic scale, and as a function of a the stellar mass surface density. Since metallicity depends on galaxy mass, we take special care throughout the paper in order to compare, in all cases, subsamples of galaxies in groups and in the field that have similar masses. Results. We find significant differences between group and field late-type galaxies in terms of their metallicity, in the sense that group galaxies are systematically more metallic than their field counterparts. We find that field galaxies have, in general, metallicity profiles that show a negative gradient in their inner regions, and a shallower profile at larger radii. This contrasts with the metallicity profiles of galaxies in groups, which tend to be flat in the inner regions, and to have a negative gradient in the outer parts. Regarding the metallicity at the characteristic radius of the luminosity profiles, we consistently find that it is higher for group galaxies irrespective of galaxy mass. At fixed local stellar surface mass density, group galaxies are again more metallic, also the dependence of metallicity on surface density is less important for group galaxies. Conclusions. The evidence of a clear difference on the metallicity of group and field galaxies, as a function of mass, spatial scale, and local stellar mass density, are indicative of the different evolutionary paths that galaxies in groups and in the field have followed. We discuss possible implications of the observed differences.

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Inside-out growth or inside-out quenching? Clues from colour gradients of local galaxies

Cited by 10 publications

References 34 publications

SDSS IV MaNGA – sSFR profiles and the slow quenching of discs in green valley galaxies

SDSS IV MaNGA – sSFR profiles and the slow quenching of discs in green valley galaxies

The Global and Radial Stellar Mass Assembly of Milky Way-sized Galaxies

Effects of environment on stellar metallicity profiles of late-type galaxies in the CALIFA survey

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