2018
DOI: 10.3847/1538-4357/aae822
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Fast and Slow Paths to Quiescence: Ages and Sizes of 400 Quiescent Galaxies from the LEGA-C Survey

Abstract: We analyze stellar age indicators (D n 4000 and EW(Hδ)) and sizes of 467 quiescent galaxies with M * ≥ 10 10 M at z ∼ 0.7 drawn from DR2 of the LEGA-C survey. Interpreting index variations in terms of equivalent single stellar population age, we find that the median stellar population is younger for larger galaxies at fixed stellar mass. The effect is significant, yet small; the ages of the larger and the smaller subsets differ by only < 500 Myr, much less than the age variation among individual galaxies (∼ 1.… Show more

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Cited by 102 publications
(126 citation statements)
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References 161 publications
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“…The spectra of 12 galaxies in the sample cover the Hβ line. Eight of them have EW(Hβ) em > −1Å, consistent with being quiescent (Wu et al 2018a). For the remaining 4 galaxies, two galaxies have EW(Hβ) em consistent with −1Å (ID: 211263, −1.20 ± 0.23Å and ID: 230053, −1.04 ± 0.36Å), one galaxy (ID: 232099, −3.92 ± 0.45Å) has strong [Ne III] and [O II] emission, indicating an ionizing source other than star formation.…”
Section: The Sample Of Recently Quenched Galaxiesmentioning
confidence: 71%
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“…The spectra of 12 galaxies in the sample cover the Hβ line. Eight of them have EW(Hβ) em > −1Å, consistent with being quiescent (Wu et al 2018a). For the remaining 4 galaxies, two galaxies have EW(Hβ) em consistent with −1Å (ID: 211263, −1.20 ± 0.23Å and ID: 230053, −1.04 ± 0.36Å), one galaxy (ID: 232099, −3.92 ± 0.45Å) has strong [Ne III] and [O II] emission, indicating an ionizing source other than star formation.…”
Section: The Sample Of Recently Quenched Galaxiesmentioning
confidence: 71%
“…If the progenitors of recently quenched galaxies are drawn from the star-forming population, the correlation between the relative size and V − J color presents a supporting evidence that the formation of recently quenched galaxies is accompanied with 'shrinking' of R e , which is a result of centrally-concentrated starburst (Wu et al 2018a). We build toy models to illustrate how the sizes evolve when centrally-concentrated starbursts happen.…”
Section: The Size Evolution: Toy Modelsmentioning
confidence: 94%
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“…Analysis of both the morphologies and spectral energy distributions (SEDs) of high redshift quiescent galaxies has led to growing evidence for at least two quenching mechanisms that act on "fast" and "slow" timescales (e.g Pacifici et al 2016;Moutard et al 2016;Maltby et al 2018;Wu et al 2018;Rowlands et al 2018;Belli et al 2019). In the case where the shut-off in star formation is both fast and sufficiently substantial, for example following a short lived burst of star formation, stellar evolution leaves a useful identifiable imprint on the integrated continuum spectra of galaxies for up to ∼1 Gyr, with dominant A and F stars leading to a strong Balmer break and Balmer absorption lines, while the lack of O and B stars leaves little ultraviolet flux or nebular emission.…”
Section: Introductionmentioning
confidence: 99%
“…The highly compact nature of massive high redshift (z 1) post-starburst galaxies, and clear dissimilarity from the morphologies of star-forming progenitors, suggests that morphological transformation via dissipative collapse precedes the quenching of star-formation for these objects (e.g. Yano et al 2016;Almaini et al 2017;Wu et al 2018). However, the prevalence of such extreme events is likely dependant on stellar mass, environment and redshift.…”
Section: Introductionmentioning
confidence: 99%