The impact of the FMR and starburst galaxies on the (low metallicity) cosmic star formation history

Chruślińska, Martyna; Nelemans, G.; Boco, Lumen; Lapi, A.

doi:10.1093/mnras/stab2690

Cited by 20 publications

(53 citation statements)

References 69 publications

(193 reference statements)

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“…In contrast the more recent models discussed in Chruślińska et al (2021) are broadly consistent with cosmological simulations. In these models Chruślińska et al (2021) use the redshift-invariant fundamental metallicity relation (e.g. Ellison et al 2008;Mannucci et al 2010) to characterise the metallicity of galaxies, which leads to a much more gradual metallicity evolution at redshift 2 than what is inferred from the extrapolated evolution of the mass-metallicity relation used in Chruslinska & Nelemans (2019).…”

Section: How Does the Cosmic Star Formation History Depend On Metalli...supporting

confidence: 73%

“…The cosmological simulations have a much smaller mass fraction of low metallicity Z < 0.1 Z stars, and a higher fraction of stars with a metallicity larger than Z than the analytical models of Chruslinska & Nelemans (2019). In contrast the more recent models discussed in Chruślińska et al (2021) are broadly consistent with cosmological simulations. In these models Chruślińska et al (2021) use the redshift-invariant fundamental metallicity relation (e.g.…”

Section: How Does the Cosmic Star Formation History Depend On Metalli...supporting

confidence: 61%

“…We compare the amount of low and high metallicity stars formed in TNG50 to other state-of-the-art cosmological galaxy simulations (Vogelsberger et al 2014b;Schaye et al 2015;Davé et al 2019) and observation-based models using empirical scaling relations (Chruslinska & Nelemans 2019;Chruślińska et al 2021) in Fig. 2.…”

Section: How Does the Cosmic Star Formation History Depend On Metalli...mentioning

confidence: 99%

“…There is a long history of using dark matter only simulations either in combination with analytical or semi-analytical models to constrain the low metallicity end of stars in the Milky Way and similar galaxies, often with a focus on the first generation of stars (Pop III) (White & Springel 2000;Hernandez & Ferrara 2001;Diemand et al 2005;Scannapieco et al 2006;Brook et al 2007;Cooper et al 2010;Hartwig et al 2015).…”

Section: Introductionmentioning

confidence: 99%

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Formation and fate of low metallicity stars in IllustrisTNG50

Pakmor,

Simpson,

van de Voort

et al. 2022

Preprint

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Low metallicity stars give rise to unique spectacular transients and are of immense interest for understanding stellar evolution. Their importance has only grown further with the recent detections of mergers of stellar mass black holes that likely originate mainly from low metallicity progenitor systems. Moreover, the formation of low metallicity stars is intricately linked to galaxy evolution, in particular to early enrichment and to later accretion and mixing of lower metallicity gas. Because low metallicity stars are difficult to observe directly, cosmological simulations are crucial for understanding their formation. Here we quantify the rates and locations of low metallicity star formation using the high-resolution TNG50 magnetohydrodynamical cosmological simulation, and we examine where low metallicity stars end up at 𝑧 = 0. We find that 20% of stars with 𝑍 * < 0.1 Z form after 𝑧 = 2, and that such stars are still forming in galaxies of all masses at 𝑧 = 0 today. Moreover, most low-metallicity stars at 𝑧 = 0 reside in massive galaxies. We analyse the radial distribution of low metallicity star formation, and discuss the curious case of seven galaxies in TNG50 that form stars from primordial gas even at 𝑧 = 0.

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Section: How Does the Cosmic Star Formation History Depend On Metalli...supporting

confidence: 73%

Section: How Does the Cosmic Star Formation History Depend On Metalli...supporting

confidence: 61%

Section: How Does the Cosmic Star Formation History Depend On Metalli...mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Formation and fate of low metallicity stars in IllustrisTNG50

Pakmor,

Simpson,

van de Voort

et al. 2022

Preprint

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“…Moreover, the connection between the direct observable and the SFR history is model dependent on multiple layers (see e.g. Chruślińska et al 2021). GW provide a unique new probe which suffer less from the above mentioned limitations.…”

Section: Introductionmentioning

confidence: 99%

The GW-Universe Toolbox II: constraining the binary black hole population with second and third generation detectors

Yi,

Stoppa,

Nelemans

et al. 2022

Preprint

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Context:The GW-Universe Toolbox is a software package that simulates observations of the Gravitational Wave (GW) Universe with different types of GW detectors, including Earth-based/Space-borne laser interferometers and Pulsar timing arrays. It is accessible as a website, and can also be imported as a Python module and run locally. Methods: We employ the GW-Universe Toolbox to generate synthetic catalogues of detections of stellar mass binary black hole (BBH) mergers. As an example of its scientific application, we study how GW observations of BBHs can be used to constrain the merger rate as function of redshift and masses. We study advanced LIGO (aLIGO) and Einstein Telescope (ET) as two representatives for the 2nd and 3rd generation GW observatories. We also simulate the observations from a detector that is half as sensitive as the ET in design which represents an early phase of ET. Two methods are used to obtain the constraints on the source population properties from the catalogues: the first assumes a parametric differential merger rate model and applies a Bayesian inference; The other is non-parametric and uses weighted Kernel density estimators. Results: The results show the overwhelming advantages of the 3rd generation detector over the 2nd generation for the study of BBH population properties, especially at a redshifts higher than ∼ 2, where the merger rate is believed to peak. With the LIGO catalogue, the parametric Bayesian method can still give some constraints on the merger rate density and mass function beyond its detecting horizon, while the non-parametric method lose the constraining ability completely there. The difference is due to the extra information placed by assuming a specific parameterisation of the population model in the Bayesian method; While in the non-parametric method, no assumption of the general shape of merger rate density and mass function are placed, not even the assumption of its smoothness. These two methods represent the two extreme situations of general population reconstruction. We also find that, despite the numbers of detection of the half-ET can be easily compatible with full ET after a longer observation duration, the catalogue from the full ET can still give much better constraints on the population properties, due to its smaller uncertainties on the physical parameters of the GW events.

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Chemical Evolution of the Universe and its Consequences for Gravitational‐Wave Astrophysics

Chruślińska

2022

Annalen der Physik

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We are now routinely detecting gravitational waves (GW) emitted by merging black holes and neutron stars. Those are the afterlives of massive stars that formed all across the Universe -at different cosmic times and with different metallicities (abundances of elements heavier than helium). Birth metallicity plays an important role in the evolution of massive stars. Consequently, the population properties of mergers are sensitive to the metallicity dependent cosmic star formation history (fSFR(Z,z)). In particular, within the isolated formation scenarios (the focus of this paper), a strong low metallicity preference of the formation of mergers involving black holes was found. The origin of this dependence and its consequences are discussed. Most importantly, uncertainty in the fSFR(Z,z) (substantial even at low redshifts, especially at low metallicity) cannot be ignored in the models. This poses a significant challenge for the interpretation of the observed GW source population properties. Possible paths for improvements and the role of future GW detectors are considered. Recent efforts to determine fSFR(Z,z) and the factors that dominate its uncertainty are summarized. Many of those factors are related to the properties of galaxies that are faint and distant and therefore difficult to observe. The fact that they leave imprint on the properties of mergers as a function of cosmic time makes future GW observations a promising (and complementary to electromagnetic observations) tool to study chemical evolution of galaxies.

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The impact of the FMR and starburst galaxies on the (low metallicity) cosmic star formation history

Cited by 20 publications

References 69 publications

Formation and fate of low metallicity stars in IllustrisTNG50

Formation and fate of low metallicity stars in IllustrisTNG50

The GW-Universe Toolbox II: constraining the binary black hole population with second and third generation detectors

Chemical Evolution of the Universe and its Consequences for Gravitational‐Wave Astrophysics

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