The evolution of the UV luminosity function of globular clusters in the E-MOSAICS simulations

Abstract

We present the evolution of the rest-frame ultraviolet (UV) properties of the globular cluster (GC) populations and their host galaxies formed in the E-MOSAICS suite of cosmological hydrodynamical simulations. We compute the luminosities of all clusters associated with 25 simulated Milky Way-mass galaxies, discussed in previous works, in the rest-frame UV and optical bands by combining instantaneous cluster properties (age, mass, metallicity) with simple stellar population models, from redshifts $z=0$ to 10. Due to the rapid fading of young stellar populations in the UV, most of the simulated galaxies do not host GCs bright enough to be individually identified in deep Hubble Space Telescope (HST) observations, even in highly magnified systems. The median age of the most UV-luminous GCs is $<10$ Myr (assuming no extinction), increasing to $\gtrsim 100$ Myr for red optical filters. We estimate that these GCs typically only contribute a few per cent of the total UV luminosity of their host galaxies at any epoch. We predict that the number density of UV-bright proto-GCs (or cluster clumps) will peak between redshifts $z=1-3$. In the main progenitors of Milky Way-mass galaxies, $10$-$20$ per cent of the galaxies at redshifts $1\lesssim z\lesssim 3$ have clusters brighter than $M_{\mathrm{UV}}<-15$, and less than $10$ per cent at other epochs. The brightest cluster in the galaxy sample at $z>2$ is typically $M_{\mathrm{UV}}\sim -16$, consistent with the luminosities of observed compact, high-redshift sources.

15 pages, 9 figures, accepted for publication in MNRAS (4 June 2019)

References in corpus (39)

• Cosmic Star Formation History
• The EAGLE project: Simulating the evolution and assembly of galaxies and their environments
• The propagation of uncertainties in stellar population synthesis modeling I: The relevance of uncertain aspects of stellar evolution and the IMF to the derived physical properties of galaxies
• The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations
• The effect of photo-ionization on the cooling rates of enriched, astrophysical plasmas
• Chemical enrichment in cosmological, smoothed particle hydrodynamics simulations
• Formation and Dynamical Evolution of Multiple Stellar Generations in Globular Clusters
• Model-independent evidence in favor of an end to reionization by z~6
• Evidence of patchy hydrogen reionization from an extreme Ly$\alpha$ trough below redshift six
• Evolution of asymptotic giant branch stars I. Updated synthetic TP-AGB models and their basic calibration
• Fast and inefficient star formation due to short-lived molecular clouds and rapid feedback
• Clumpy Galaxies in CANDELS. I. The Definition of UV Clumps and the Fraction of Clumpy Galaxies at 0.5<z<3
• On the Star Formation Rate - Brightest Cluster Relation: Estimating the peak SFR in post-merger galaxies
• A chronicle of galaxy mass assembly in the EAGLE simulation
• Paving the way for the JWST: witnessing globular cluster formation at z>3
• Probing the role of the galactic environment in the formation of stellar clusters; using M83 as a test bench
• Resolved spectroscopy of gravitationally lensed galaxies: global dynamics and star-forming clumps on ~100pc scales
• Star cluster formation in cosmological simulations. I. Properties of young clusters
• Studying the YMC population of M83: how long clusters remain embedded, their interaction with the ISM and implications for GC formation theories
• The E-MOSAICS project: tracing galaxy formation and assembly with the age-metallicity distribution of globular clusters
• Modeling the Formation of Globular Cluster Systems in the Virgo Cluster
• The nature of giant clumps in distant galaxies probed by the anatomy of the Cosmic Snake
• The sizes of $z\sim 6-8$ lensed galaxies from the Hubble Frontier Fields Abell 2744 data
• Chemical composition and constraints on mass loss for globular clusters in dwarf galaxies: WLM and IKN
• Using H-alpha Morphology and Surface Brightness Fluctuations to Age-Date Star Clusters in M83
• Star Formation at z=2.481 in the Lensed Galaxy SDSS J1110+6459: Star Formation down to 30 parsec scales
• A Common Origin for Globular Clusters and Ultra-faint Dwarfs in Simulations of the First Galaxies
• Formation histories of stars, clusters and globular clusters in the E-MOSAICS simulations
• On the stellar masses of giant clumps in distant star-forming galaxies
• The origin of globular cluster systems from cosmological simulations
• Constraining Globular Cluster Formation Through Studies of Young Massive Clusters - IV. Testing the Fast Rotating Massive Star Scenario
• Clues on the Missing Sources of Reionization from Self-consistent Modeling of Milky Way and Dwarf Galaxy Globular Clusters
• Hierarchical Star Formation in Turbulent Media: Evidence from Young Star Clusters
• The minimum metallicity of globular clusters and its physical origin -- implications for the galaxy mass-metallicity relation and observations of proto-globular clusters at high redshift
• The vertical structure of gaseous galaxy discs in cold dark matter halos
• Star Formation at z=2.481 in the Lensed Galaxy SDSS J1110+6459, I: Lens Modeling and Source Reconstruction
• Star Formation at z=2.481 in the Lensed Galaxy SDSS J1110+6459, II: What is missed at the normal resolution of the Hubble Space Telescope?
• Little Blue Dots in the Hubble Space Telescope Frontier Fields: Precursors to Globular Clusters?
• SHARDS Frontier Fields: Physical properties of a low mass Lyman-alpha emitter at z=5.75

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