The influence of streaming velocities and Lyman–Werner radiation on the formation of the first stars

Schauer, Anna T. P.; Glover, Simon C. O.; Klessen, Ralf S.; Clark, Paul

doi:10.1093/mnras/stab1953

Cited by 56 publications

(72 citation statements)

References 78 publications

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“…Thus, more prevalent Pop III star formation results in stronger constraints on the WDM mass. Recent simulations of feedback effects on the first halos (Kulkarni et al 2021;Schauer et al 2021) suggest a shallower relationship between the LW background intensity and minimum mass than was found in early work (e.g., Machacek et al 2001). This implies that for a given LW background intensity, the overall impact of feedback will be weaker (see also Skinner & Wise 2020), giving rise to the possibility of more Pop III star formation (as M min,iii rises more slowly).…”

Section: Likelihood Input Covariancesmentioning

confidence: 86%

Constraining Warm Dark Matter and Pop III stars with the Global 21-cm Signal

Hibbard,

Mirocha,

Rapetti

et al. 2022

Preprint

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Upcoming ground and space-based experiments may have sufficient accuracy to place significant constraints upon high-redshift star formation, Reionization, and dark matter (DM) using the global 21-cm signal of the IGM. In the early universe, when the relative abundance of low-mass DM halos is important, measuring the global signal would place constraints on the damping of structure formation caused by DM having a higher relic velocity (warm dark matter, or WDM) than in cold dark matter (CDM). Such damping, however, can be mimicked by altering the star formation efficiency (SFE) and difficult to detect because of the presence of Pop III stars with unknown properties. We study these various cases and their degeneracies with the WDM mass parameter m X using a Fisher matrix analysis. We study the m X = 7 keV case and a star-formation model that parametrizes the SFE as a strong function of halo mass and include several variations of this model along with three different input noise levels for the likelihood. We find that when the likelihood includes only Pop II stars, m X is constrained to ∼ 0.4 keV for all models and noise levels at 68% CI. When the likelihood includes weak Pop III stars, m X ∼ 0.3 keV, and if Pop III star formation is relatively efficient, m X ∼ 0.1 keV, with tight Pop III star-formation parameter constraints. Our results show that the global 21-cm signal is a promising test-bed for WDM models, even in the presence of strong degeneracies with astrophysical parameters.

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Section: Likelihood Input Covariancesmentioning

confidence: 86%

Constraining Warm Dark Matter and Pop III stars with the Global 21-cm Signal

Hibbard,

Mirocha,

Rapetti

et al. 2022

Preprint

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“…In a-sloth, Pop III stars form instantly in a single star burst in a mini-halo (haloes below the atomic cooling threshold (Tvir = 10000 K) as soon as its virial mass exceeds Mcrit. By default, we follow the prescriptions given in Schauer et al (2021, their Eqs. 9 and 10) and Hummel et al (2012, their Eq.…”

Section: Population III (Pop Iii) Starsmentioning

confidence: 99%

“…1) to determine Mcrit. Schauer et al (2021) showed that the critical mass is dependent on the LW background and the large-scale streaming velocity of the baryons relative to the dark matter: log10Mcrit,S21 = 6.0174 (1.0 + 0.166…”

Section: Population III (Pop Iii) Starsmentioning

confidence: 99%

“…which is based on the work in Greif & Bromm (2006). We take vBC = 0.8σrms as the fiducial baryonic streaming velocity, since this is the most likely value to be present at a randomly selected point in the Universe (Schauer et al 2021). The impact of varying our treatment of both of these effects is explored in Section 4.2.…”

Section: Population III (Pop Iii) Starsmentioning

confidence: 99%

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Tracing stars in Milky Way satellites with A-SLOTH

Chen,

Magg,

Hartwig

et al. 2022

Preprint

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We study the stellar mass-to-halo mass relation at z = 0 in 30 Milky Way-like systems down to the ultra-faint (M * < 10 5 M ) regime using the semi-analytic model a-sloth.A new model allows us to follow star formation and the stochastic stellar feedback from individually sampled Pop II stars. Our fiducial model produces consistent results with the stellar mass-to-halo mass relation derived from abundance matching and the observed cumulative stellar mass function above the observational completeness. We find a plateau in the stellar mass-to-halo mass relation in the ultra-faint regime. The stellar mass of this plateau tells us how many stars formed before supernovae occur and regulate further star formation, which is determined by the Pop II star formation efficiency. We also find that the number of luminous satellites increases rapidly as M * decreases until M * ≈ 10 4 M . Finally, we find that the relative streaming velocity between baryons and dark matter at high redshift is important in determining the number of ultra-faint dwarf galaxies at z = 0. The new model in a-sloth provides a framework to study the stellar properties and the formation history of metal-poor stars in Milky Way and its satellites.

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“…In contrast to previous models, when using a-sloth we do not explicitly account for the effect of Lyman-Werner (LW) radiation (Machacek et al 2001;Schauer et al 2021) or supersonic baryon streaming (a residual velocity difference between dark matter and baryonic matter resulting from recombination, Tseliakhovich & Hirata 2010) which are expected to affect Tcrit in a nonuniform manner (e.g. Fialkov et al 2012;Schauer et al 2019a).…”

Section: Basic Semi-analytical Modelmentioning

confidence: 99%

Effect of the cosmological transition to metal-enriched star-formation on the hydrogen 21-cm signal

Magg,

Reis,

Fialkov

et al. 2021

Preprint

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Mapping Cosmic Dawn with 21-cm tomography offers an exciting new window into the era of primordial star formation. However, self-consistent implementation of both the process of star formation and the related 21-cm signal is challenging, due to the multi-scale nature of the problem. In this study, we develop a flexible semi-analytical model to follow the formation of the first stars and the process of gradual transition from primordial to metal-enriched star formation. For this transition we use different in scenarios with varying time-delays (or recovery times) between the first supernovae and the formation of the second generation of stars. We use recovery times between 10 and 100 Myr and find that these delays have a strong impact on the redshift at which the transition to metal-enriched star formation occurs. We then explore the effect of this transition on the 21-cm signal and find that the recovery time has a distinctive imprint in the signal. Together with an improved understanding of how this time-delay relates to the properties of Population III stars, future 21-cm observations can give independent constraints on the earliest epoch of star formation.

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The influence of streaming velocities and Lyman–Werner radiation on the formation of the first stars

Cited by 56 publications

References 78 publications

Constraining Warm Dark Matter and Pop III stars with the Global 21-cm Signal

Constraining Warm Dark Matter and Pop III stars with the Global 21-cm Signal

Tracing stars in Milky Way satellites with A-SLOTH

Effect of the cosmological transition to metal-enriched star-formation on the hydrogen 21-cm signal

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