The Formation of Population III Binaries

Saigo, Kazuya; Matsumoto, Toshiro; Umemura, Masayuki

doi:10.1086/426389

Cited by 42 publications

(39 citation statements)

References 31 publications

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“…Simulations following direct cosmological initial conditions by Abel et al (2002) find a single star with no further fragmentation; however, different simulations with somewhat more artificial initial conditions (a rotating cylinder) find efficient binary formation (Saigo et al 2004). It is conceivable that at high redshifts, a WDM universe could mimic the GRB rates of a CDM universe by compensating for a loss of small-scale power with higher efficiencies of GRB production (e.g., a higher K value at high redshifts) and visa versa.…”

Section: Uncertainties In Grb Redshift Evolutionmentioning

confidence: 99%

Constraints on the Small‐Scale Power Spectrum of Density Fluctuations from High‐Redshift Gamma‐Ray Bursts

Mesinger

Perna

Haiman

2005

ApJ

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Cosmological models that include suppression of the power spectrum of density fluctuations on small scales exhibit an exponential reduction of high-redshift, nonlinear structures, including a reduction in the rate of gammaray bursts (GRBs). Here we quantify the constraints that the detection of distant GRBs would place on structure formation models with reduced small-scale power. We compute the number of GRBs that could be detectable by the Swift satellite at high redshifts (z k 6), assuming that the GRBs trace the cosmic star formation history, which itself traces the formation of nonlinear structures. We calibrate simple models of the intrinsic luminosity function of the bursts to the number and flux distribution of GRBs observed by the Burst and Transient Source Experiment. We find that a discovery of high-z GRBs would imply strong constraints on models with reduced small-scale power. For example, a single GRB at z k10 or 10 GRBs at z k 5 discovered by Swift during its scheduled 2 year mission would rule out an exponential suppression of the power spectrum on scales below R c ¼ 0:09 Mpc (exemplified by warm dark matter models with a particle mass of m x ¼ 2 keV). Models with a less sharp suppression of small-scale power, such as those with a red tilt or a running scalar index, n s , are more difficult to constrain, because they are more degenerate with an increase in the power-spectrum normalization, 8 , and with models in which star formation is allowed in low-mass minihalos. We find that a tilt of n s % 0:1 is difficult to detect; however, an observed rate of one GRB yr À1 at z k12 would yield an upper limit on the running of the spectral index, dn s /d ln k > À0:05.

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Section: Uncertainties In Grb Redshift Evolutionmentioning

confidence: 99%

Constraints on the Small‐Scale Power Spectrum of Density Fluctuations from High‐Redshift Gamma‐Ray Bursts

Mesinger

Perna

Haiman

2005

ApJ

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“…Uniform reheating of the filaments and voids is a characteristic of reionization and reheating from X-rays produced by remnants of the first stars accreting from the ISM at higher redshift (Venkatesan et al 2001;Ricotti & Ostriker 2004;Ripamonti et al 2008;Shull & Venkatesan 2008). X-rays could also be produced by primordial black hole binaries (Mirabel et al 2011;Saigo et al 2004). When compared to reheating by UV radiation, X-ray reheating produces noticeably darker voids.…”

Section: Approximating Cosmic Variancementioning

confidence: 99%

Where Are the Fossils of the First Galaxies? I. Local Volume Maps and Properties of the Undetected Dwarfs

Bovill

Ricotti

2011

ApJ

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We present a new method for generating initial conditions for ΛCDM N-body simulations which provides the dynamical range necessary to follow the evolution and distribution of the fossils of the first galaxies on Local Volume, 5-10 Mpc, scales. The initial distribution of particles represents the position, velocity, and mass distribution of the dark and luminous halos extracted from pre-reionization simulations. We confirm previous results that ultra-faint dwarfs have properties compatible with being well-preserved fossils of the first galaxies. However, because the brightest pre-reionization dwarfs form preferentially in biased regions, they most likely merge into non-fossil halos with circular velocities > 20-30 km s −1 . Hence, we find that the maximum luminosity of true fossils in the Milky Way is L V < 10 6 L , casting doubts on the interpretation that some classical dSphs are true fossils. In addition, we argue that most ultra-faints at small galactocentric distance, R < 50 kpc, had their stellar properties modified by tides, while a large population of fossils is still undetected due to their extremely low surface brightness log(Σ V ) < −1.4. We estimate that the region outside R 50 (∼400 kpc) up to 1 Mpc from the Milky Way contains about a hundred true fossils of the first galaxies with V-band luminosity 10 3 -10 5 L and half-light radii, r hl ∼ 100-1000 pc.

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“…The high-redshift population of mergers of compact objects originates in populations of stars with various A&A 574, A58 (2015) metallicities, including very low ones. Previous studies of Saigo et al (2004), Machida et al (2008), Stacy & Bromm (2013), and many others have shown that in the very early Universe, where the environment was nearly metal free, binaries might have been created. A investigation of the GW background must therefore take the effects of metallicity into account.…”

Section: Introductionmentioning

confidence: 99%

Effect of metallicity on the gravitational-wave signal from the cosmological population of compact binary coalescences

Kowalska-Leszczynska

Regimbau

Bulik

et al. 2015

A&A

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Context. Recent studies on stellar evolution have shown that the properties of compact objects strongly depend on the metallicity of the environment in which they were formed. Aims. Using some very simple assumptions on the metallicity of the stellar populations, we explore how this property affects the unresolved gravitational-wave background from extragalactic compact binaries. Methods. We obtained a suit of models using population synthesis code, estimated the gravitational-wave background they produce, and discuss its detectability with second-(advanced LIGO, advanced Virgo) and third-(Einstein Telescope) generation detectors. Results. Our results show that the background is dominated by binary black holes for all considered models in the frequency range of terrestrial detectors, and that it could be detected in most cases by advanced LIGO/Virgo, and with Einstein Telescope with a very high signal-to-noise ratio. The observed peak in a gravitational-wave spectrum depends on the metallicity of the stellar population.

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The Formation of Population III Binaries

Cited by 42 publications

References 31 publications

Constraints on the Small‐Scale Power Spectrum of Density Fluctuations from High‐Redshift Gamma‐Ray Bursts

Constraints on the Small‐Scale Power Spectrum of Density Fluctuations from High‐Redshift Gamma‐Ray Bursts

Where Are the Fossils of the First Galaxies? I. Local Volume Maps and Properties of the Undetected Dwarfs

Effect of metallicity on the gravitational-wave signal from the cosmological population of compact binary coalescences

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