The impact of radiation feedback on the assembly of star clusters in a galactic context

Guillard, Nicolas; Emsellem, Éric

doi:10.1093/mnras/sty849

Cited by 4 publications

(3 citation statements)

References 79 publications

(95 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The formation of HII regions also reduces clustering and cluster growth (e.g. Guillard et al 2018;Smith et al 2021;Rathjen et al 2021). We note however that beyond the initial starburst, the SFE2noPI simulation has a lower star formation rate.…”

Section: Star Formation and Outflow Ratesmentioning

confidence: 78%

The challenge of simulating the star cluster population of dwarf galaxies with resolved interstellar medium

Hislop

Naab

Steinwandel

et al. 2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present results on the star cluster properties from a series of high resolution smoothed particles hydrodynamics (SPH) simulations of isolated dwarf galaxies as part of the griffin project. The simulations at sub-parsec spatial resolution and a minimum particle mass of 4 M⊙ incorporate non-equilibrium heating, cooling, and chemistry processes, and realize individual massive stars. The simulations follow feedback channels of massive stars that include the interstellar-radiation field variable in space and time, the radiation input by photo-ionization and supernova explosions. Varying the star formation efficiency per free-fall time in the range ϵff = 0.2–50${{\ \rm per\ cent}}$ neither changes the star formation rates nor the outflow rates. While the environmental densities at star formation change significantly with ϵff, the ambient densities of supernovae are independent of ϵff indicating a decoupling of the two processes. At low ϵff, gas is allowed to collapse more before star formation, resulting in more massive, and increasingly more bound star clusters are formed, which are typically not destroyed. With increasing ϵff, there is a trend for shallower cluster mass functions and the cluster formation efficiency Γ for young bound clusters decreases from $50 {{\ \rm per\ cent}}$ to $\sim 1 {{\ \rm per\ cent}}$ showing evidence for cluster disruption. However, none of our simulations form low mass (<103 M⊙) clusters with structural properties in perfect agreement with observations. Traditional star formation models used in galaxy formation simulations based on local free-fall times might therefore be unable to capture star cluster properties without significant fine tuning.

show abstract

Section: Star Formation and Outflow Ratesmentioning

confidence: 78%

The challenge of simulating the star cluster population of dwarf galaxies with resolved interstellar medium

Hislop

Naab

Steinwandel

et al. 2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…This leads to a smoother density field and therefore less clustered star formation. Recently, Guillard et al (2018) confirmed this result by following the formation and destruction of individual star clusters in an isolated galaxy. They also find a significantly reduced number of star clusters compared to a simulation with identical initial conditions but only SN feedback.…”

Section: Introductionmentioning

confidence: 70%

Does radiative feedback make faint z > 6 galaxies look small?

Ploeckinger

Schaye

Hacar

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Recent observations of lensed sources have shown that the faintest (M UV ≈ −15 mag) galaxies observed at z = 6 − 8 appear to be extremely compact. Some of them have inferred sizes of less than 40 pc for stellar masses between 10 6 and 10 7 M , comparable to individual super star clusters or star cluster complexes at low redshift. High-redshift, low-mass galaxies are expected to show a clumpy, irregular morphology and if star clusters form in each of these well-separated clumps, the observed galaxy size would be much larger than the size of an individual star forming region. As supernova explosions impact the galaxy with a minimum delay time that exceeds the time required to form a massive star cluster, other processes are required to explain the absence of additional massive star forming regions. In this work we investigate whether the radiation of a young massive star cluster can suppress the formation of other detectable clusters within the same galaxy already before supernova feedback can affect the galaxy. We find that in low-mass (M 200 10 10 M ) haloes, the radiation from a compact star forming region with an initial mass of 10 7 M can keep gas clumps with Jeans masses larger than ≈ 10 7 M warm and ionized throughout the galaxy. In this picture, the small intrinsic sizes measured in the faintest z = 6 − 8 galaxies are a natural consequence of the strong radiation field that stabilises massive gas clumps. A prediction of this mechanism is that the escape fraction for ionizing radiation is high for the extremely compact, high-z sources.

show abstract

“…The impact of stellar feedback on high-density gas regions (e.g. for molecular clouds in merging galaxies) has been found to be less efficient at clearing the gas, thus high-density gas clouds could have multiple episodes of star formation (Rahner et al 2017;Guillard et al 2018). To test this idea, we examined the evolution of the gas morphology of the galaxy hosting the two SO candidates, before and after the expulsion of gas from the candidates.…”

Section: Impact Of Stellar Feedback and Gas Expulsionmentioning

confidence: 99%

Linking the internal properties of infant globular clusters to their formation environments

Phipps

Khochfar

Varri

et al. 2022

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We investigate the formation of infant globular cluster (GC) candidates in high-resolution cosmological simulations from the First Billion Years (FiBY) project. By analysing the evolution of the systems in the energy and angular momentum plane, we identify the redshift at which the infant GCs first became gravitationally bound, and we find evidence of radial infall of their gaseous and stellar components. The collapse appears to be driven by internal self-gravity, however, the initial trigger is sourced from the external environment. The phase space behaviour of the infant GCs also allows us to identify some characteristic groupings of objects. Such a classification based on internal properties appears to be reflected in the formation environment: GC candidates that belong to the same class are found in host galaxies of similar morphology, with the majority of the infant GCs located in clumpy, irregular proto-galaxies. Finally, through the inspection of two GC candidates that contain only stars by z = 6, we find that supernova feedback is the main physical mechanism behind their dearth of gas and that the systems subsequently respond with an approximately adiabatic expansion. Such infant GC candidates already resemble the GCs we currently observe in the local Universe.

show abstract

The impact of radiation feedback on the assembly of star clusters in a galactic context

Cited by 4 publications

References 79 publications

The challenge of simulating the star cluster population of dwarf galaxies with resolved interstellar medium

The challenge of simulating the star cluster population of dwarf galaxies with resolved interstellar medium

Does radiative feedback make faint z > 6 galaxies look small?

Linking the internal properties of infant globular clusters to their formation environments

Contact Info

Product

Resources

About