Rejuvenation in z ∼ 0.8 Quiescent Galaxies in LEGA-C

Chauké, Priscilla; Wel, Arjen van der; Pacifici, Camilla; Bezanson, Rachel; Wu, Po-Feng; Gallazzi, Anna; Straatman, Caroline; Franx, Marijn; Barišić, Ivana; Bell, Eric F.; Houdt, Josha van; Maseda, Michael V.; Muzzin, Adam; Sobral, David; Spilker, Justin

doi:10.3847/1538-4357/ab164d

Cited by 55 publications

(50 citation statements)

References 54 publications

(63 reference statements)

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“…Recently, Pawlik et al (2018) found that 40 per cent of massive post-starburst galaxies in the local universe are the result of red sequence galaxies undergoing 'rejuvenation events' and moving towards the massive end of the red sequence through minor mergers. Such rejuvenation of ETGs has also been observed at z ∼ 0.8 by Chauke et al (2019). Works by the SAURON collaboration have found that ETGs can be divided in fast and slow rotators (Emsellem et al 2007) according to the prominence of their rotational component, a classification that has been linked to different formation processes (Cappellari et al 2011;Penoyre et al 2017;Smethurst et al 2018).…”

Section: Introductionmentioning

confidence: 70%

“…Therefore, at large masses, it is likely that the young components are the result of rejuvenation (e.g. Pawlik et al 2018;Chauke et al 2019) events triggered by minor mergers or cold gas accretion in previously quiescent systems. A merger-driven scenario is consistent with results by Kaviraj et al (2011), who find that ETGs at z ∼ 0.6 showing signs of recent starformation are more likely to exhibit disturbed morphologies reminiscent of recent minor mergers.…”

Section: Where Do Young Components Come From?mentioning

confidence: 99%

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Clues on the history of early-type galaxies from SDSS spectra and GALEX photometry

Werle

Fernandes

Asari

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Stellar population studies of early-type galaxies (ETGs) based on their optical stellar continuum suggest that these are quiescent systems. However, emission lines and ultraviolet photometry reveal a diverse population. We use a new version of the starlight spectral synthesis code and state-of-the-art stellar population models to simultaneously fit SDSS spectra and GALEX photometry for a sample of 3453 galaxies at z < 0.1 with NUV − r > 5 that are classified as elliptical by Galaxy Zoo. We reproduce FUV magnitudes for 80 per cent of UV upturn galaxies selected using criteria from the literature, suggesting that additional stellar population ingredients such as binaries and extreme horizontal branch stars may have a limited contribution to the UV upturn. The addition of ultraviolet data leads to a broadening of the distributions of mean stellar ages, metallicities and attenuation. Stellar populations younger than 1 Gyr are required to reproduce the ultraviolet emission in 17 per cent of our sample. These systems represent 43 per cent of the sample at 5 < NUV − r < 5.5 and span the same stellar mass range as other ETGs in our sample. ETGs with young stellar components have larger Hα equivalent widths (WHα) and larger dust attenuation. Emission line ratios and WHα indicate that the ionising source in these systems is a mixture of young and old stellar populations. Their young stellar populations are metal-poor, especially for high-mass galaxies, indicating recent star formation associated with rejuvenation events triggered by external processes, such as minor mergers.

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Section: Introductionmentioning

confidence: 70%

Section: Where Do Young Components Come From?mentioning

confidence: 99%

Clues on the history of early-type galaxies from SDSS spectra and GALEX photometry

Werle

Fernandes

Asari

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…3). Finally, even rejuvenated QGs are typically identified as sub-MS (Chauke et al 2019;Mancini et al 2019). Model predictions might therefore substantially deviate from observations for galaxy populations where these processes play a significant role.…”

Section: Resultsmentioning

confidence: 95%

The evolution of the gas fraction of quiescent galaxies modeled as a consequence of their creation rate

Gobat

Magdis

D’Eugenio

et al. 2020

A&A

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We discuss the evolution of the interstellar medium of quiescent galaxies, currently emerging from recent analyses, with the help of a simple model based on well-established empirical relations such as the stellar mass functions and the main sequence of star formation. This model is meant to describe observed quantities without making specific assumptions on the nature of quenching processes, but relying on their observable consequences. We find that the high gas fractions seen or suggested at high redshift in quiescent galaxies, and their apparent mild evolution at early times, can be mostly attributed to a progenitor effect where recently quenched galaxies with ∼10% gas fractions dominate the quiescent galaxy population until z ∼ 1. In the same context, the much lower gas and dust fractions measured in local early-type galaxies are interpreted as the product of the steady depletion of their interstellar medium on a ∼ 2 Gyr timescale, coupled with a higher fraction of more gas-exhaustive events.

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“…Due to requiring sensitivity to low-levels of star-formation from the UV emission, we limit our analysis in this section to galaxies at < 0.1. Note that this is a shorter-timescale rejuvenation selection than previous studies (see, e.g., Thomas et al 2010;Chauke et al 2019, for low-and high-redshift analyses respectively) which used spectral features to Figure 11. Histograms of stellar mass binned transient and star-forming galaxies with respect to / 180 .…”

Section: Rejuvenating Galaxiesmentioning

confidence: 98%

The environmental dependence of rapidly quenching and rejuvenating galaxies

Cressida

McGee

2020

Monthly Notices of the Royal Astronomical Society

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By combining Hα flux measurements from the Sloan Digital Sky Survey (SDSS) with UV flux observations from the Galaxy Evolution Explorer (GALEX), we examine the environmental dependence (through central/satellite distinction) of the rapid quenching and rejuvenation of galaxies. Hα emissions trace the most massive stars, thereby indicating star-formation on timescales of ∼ 10 Myr, while UV emission traces star-formation on timescales of ∼ 100 Myr. These varying timescales are exploited to probe the most recent star-formation histories of galaxies. In this work, we define a class of transient galaxies which have UV emission typical of star-formation but negligible Hα emission. We find that the occurrence of these transients has a strong stellar mass dependence in both the satellite and central population. However, while at stellar masses greater than M* ∼ 1010 M⊙ they occur with equal frequency regardless of environmental class, at lower stellar masses they are more common in satellites only, with an excess of about 1 percentage point across all low stellar mass galaxies. These satellite transients also have a strong halo mass and group-centric radial dependence suggesting they are driven by an environmental process. Finally, we select a sample of galaxies with Hα emission but not UV emission which could contain short-timescale rejuvenating galaxies. These rejuvenating candidates are few in number and do not have a strong difference in their occurrence rate in centrals or satellites. These unique probes point to an environmental quenching mechanism which occurs on short timescales after the satellite has been in the group environment for a significant time – consistent with ‘delayed-then-rapid’ quenching.

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Rejuvenation in z ∼ 0.8 Quiescent Galaxies in LEGA-C

Cited by 55 publications

References 54 publications

Clues on the history of early-type galaxies from SDSS spectra and GALEX photometry

Clues on the history of early-type galaxies from SDSS spectra and GALEX photometry

The evolution of the gas fraction of quiescent galaxies modeled as a consequence of their creation rate

The environmental dependence of rapidly quenching and rejuvenating galaxies

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