UV bright red-sequence galaxies: how do UV upturn systems evolve in redshift and stellar mass?

Dantas, M. L. L.; Coelho, P.; Gonçalves, T. S.

doi:10.1093/mnras/stz3609

Cited by 12 publications

(22 citation statements)

References 122 publications

(170 reference statements)

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“…• As in previous works (e.g. Dantas et al 2020; Le Cras et al 2016b), we find that UV upturn galaxies are more massive and have redder NUV − r colours than other ETGs;…”

Section: Discussionsupporting

confidence: 88%

“…The fraction of UV upturn galaxies rises steadily towards larger values of log M , which is in agreement with several works that find the UV upturn to be more common in high-mass galaxies (e.g. Burstein et al 1988;Smith et al 2012;Le Cras et al 2016b;Dantas et al 2020).…”

Section: Sub-classes Of Etgs According To Their Uv Emissionsupporting

confidence: 92%

“…In order to test our ability to reproduce the UV upturn phenomenon, we have selected UV upturn galaxies using the criteria of Yi et al 2011:NUV − r > 5.4, FUV − NUV < 0.9 and FUV − r < 6.6. These criteria have been originally proposed to separate true UV upturn galaxies from early-type galaxies with residual star-formation, although Dantas et al (2020) have shown that this cut still allows for a minor contamination from red sequence galaxies with emission lines consistent with residual star formation. In any case these criteria are commonly used in the literature and are useful for comparison.…”

Section: Quality Of the Fitsmentioning

confidence: 99%

“…Overall, the population of UV upturn galaxies is brighter, redder in the optical, and more massive than other ETGs (e.g. Dantas et al 2020;Le Cras et al 2016b, and references therein). There is also evidence for an evolution of the fraction of UV upturn systems with redshift.…”

Section: Introductionmentioning

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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“…• As in previous works (e.g. Dantas et al 2020; Le Cras et al 2016b), we find that UV upturn galaxies are more massive and have redder NUV − r colours than other ETGs;…”

Section: Discussionsupporting

confidence: 88%

Section: Sub-classes Of Etgs According To Their Uv Emissionsupporting

confidence: 92%

Section: Quality Of the Fitsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

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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“…4 we show the difference between the magnitude of the NSC and its host galaxy for all the nucleated galaxies in our sample, as well as those from dB14 and the nucleated galaxies in the Virgo cluster from SJ19a. Similarly to what was found in the two latter works, the relative contribution of the NSC to the overall brightness of the host galaxy decreases with galaxy luminosity-albeit with a large scatter in (Dantas et al 2020). While the full behaviour of the nucleation fraction departs significantly from the logistic relation (SJ19a), we make use of the fact that for all studied environments f n appears to peak at masses log(M/M ) ≈ 9 (Neumayer et al 2020), and then declines gradually toward lower masses until it becomes negligible.…”

Section: Galfit Modellingsupporting

confidence: 80%

A high occurrence of nuclear star clusters in faint Coma galaxies, and the roles of mass and environment

Zanatta,

Sánchez-Janssen,

Chies-Santos

et al. 2021

Preprint

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We use deep high resolution HST/ACS imaging of two fields in the core of the Coma cluster to investigate the occurrence of nuclear star clusters (NSCs) in quiescent dwarf galaxies as faint as M I = −10 mag. We employ a hierarchical Bayesian logistic regression framework to model the faint end of the nucleation fraction ( f n ) as a function of both galaxy luminosity and environment. We find that f n is remarkably high in Coma: at M I ≈ −13 mag half of the cluster dwarfs still host prominent NSCs. Comparison with dwarf systems in nearby clusters and groups shows that, within the uncertainties, the rate at which the probability of nucleation varies with galaxy luminosity is nearly universal. On the other hand, the fraction of nucleated galaxies at fixed luminosity does exhibit an environmental dependence. More massive environments feature higher nucleation fractions and fainter values of the half-nucleation luminosity, which roughly scales with host halo virial mass as L I, f n50 ∝ M −0.2 200 . Our results reinforce the role of galaxy mass as a major driver of the efficiency of NSC formation and also indicate a clear secondary dependence on the environment, hence paving the way to more refined theoretical models.

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Investigating the UV-excess in Star Clusters with N-body Simulations: Predictions for Future CSST Observations*

Pang¹,

Shu²,

Wang³

et al. 2022

Res. Astron. Astrophys.

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We study the origin of the UV-excess in star clusters by performing N-body simulations of six clusters with N = 10 k and N = 100 k (single stars & binary systems) and metallicities of Z = 0.01, 0.001 and 0.0001, using petar. All models initially have a 50% primordial binary fraction. Using GalevNB we convert the simulated data into synthetic spectra and photometry for the China Space Station Telescope (CSST) and Hubble Space Telescope (HST). From the spectral energy distributions we identify three stellar populations that contribute to the UV-excess: (1) second asymptotic giant branch stars, which contribute to the UV flux at early times; (2) naked helium stars and (3) white dwarfs, which are long-term contributors to the FUV spectra. Binary stars consisting of a white dwarf and a main sequence star are cataclysmic variable (CV) candidates. The magnitude distribution of CV candidates is bimodal up to 2 Gyr. The bright CV population is particularly bright in FUV − NUV. The FUV − NUV color of our model clusters is 1–2 mag redder than the UV-excess globular clusters in M87 and in the Milky Way. This discrepancy may be induced by helium enrichment in observed clusters. Our simulations are based on simple stellar evolution; we do not include the effects of variations in helium and light elements or multiple stellar populations. A positive radial color gradient is present in CSST NUV − y for main sequence stars in all models with a color difference of 0.2–0.5 mag, up to 4 half-mass radii. The CSST NUV − g color correlates strongly with HST FUV − NUV for NUV − g > 1 mag, with the linear relation FUV − NUV =(1.09 ± 0.12) × (NUV − g) + (−1.01 ± 0.22). This allows for conversion of future CSST NUV − g colors into HST FUV − NUV colors, which are sensitive to UV-excess features. We find that CSST will be able to detect UV-excess in Galactic/extragalactic star clusters with ages >200 Myr.

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UV bright red-sequence galaxies: how do UV upturn systems evolve in redshift and stellar mass?

Cited by 12 publications

References 122 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

A high occurrence of nuclear star clusters in faint Coma galaxies, and the roles of mass and environment

Investigating the UV-excess in Star Clusters with N-body Simulations: Predictions for Future CSST Observations*

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