Constraining the PopIII IMF with high-<i>z</i>GRBs

Ma, Qing-Bo; Maio, Umberto; Ciardi, B.; Salvaterra, R.

doi:10.1093/mnras/stw3159

Cited by 51 publications

(30 citation statements)

References 60 publications

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“…Similarly, stellar structure models and physical processes in the stellar cores different from those adopted here, e.g. explosion mechanisms, magnetic fields, rotation and nuclear reaction rates, might affect the theoretical metal yields from supernova explosions and thus the predicted metal abundance ratios for DLAs (see more discussion in Ma et al 2017), nevertheless the cosmic gas evolution would not be changed significantly. The PopIII SFR, and thus the corresponding metal contribution, may be slightly changed by the adopted criteria for the transition from a PopIII to a PopII/I star formation mode, but the PopII/I SFR is hardly affected (Maio et al 2010).…”

Section: Discussionmentioning

confidence: 84%

“…Following the procedure of Ma et al (2017) to describe the level of metal enrichment from first stars, we define the fraction of metals in a galaxy which is produced by PopIII stars as:…”

Section: Simulationsmentioning

confidence: 99%

“…Due to the different stellar lifetimes, metal spreading from first PopIII SNe is delayed in the RSN model with respect to the VMSN and MSN models. Therefore, the PopIII SFR reaches higher levels and more prolonged duration (Ma et al 2017), delaying the transition from intermediate to PopII-dominated galaxies (i.e. more galaxies retain fIII > 20%).…”

Section: Dla Definitionmentioning

confidence: 99%

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Metal enrichment signatures of the first stars on high-z DLAs

Maio

Ciardi

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We use numerical N-body hydrodynamical simulations with varying PopIII stellar models to investigate the possibility of detecting first star signatures with observations of high-redshift damped Lyα absorbers (DLAs). The simulations include atomic and molecular cooling, star formation, energy feedback and metal spreading due to the evolution of stars with a range of masses and metallicities. Different initial mass functions (IMFs) and corresponding metaldependent yields and lifetimes are adopted to model primordial stellar populations. The DLAs in the simulations are selected according to either the local gas temperature (temperature selected) or the host mass (mass selected). We find that 3% (40%) of mass (temperature) selected high-z (z 5.5) DLAs retain signatures of pollution from PopIII stars, independently from the first star model. Such DLAs have low halo mass (< 10 9.6 M ⊙ ), metallicity (< 10 −3 Z ⊙ ) and star formation rate (< 10 −1.5 M ⊙ yr −1 ). Metal abundance ratios of DLAs imprinted in the spectra of QSO can be useful tools to infer the properties of the polluting stellar generation and to constrain the first star mass ranges. Comparing the abundance ratios derived from our simulations to those observed in DLAs at z 5, we find that most of these DLAs are consistent within errors with PopII stars dominated enrichment and strongly disfavor the pollution pattern of very massive first stars (i.e. 100 M ⊙ -500 M ⊙ ). However, some of them could still result from the pollution of first stars in the mass range [0.1, 100] M ⊙ . In particular, we find that the abundance ratios from SDSS J1202+3235 are consistent with those expected from PopIII enrichment dominated by massive (but not extreme) first stars.

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Section: Discussionmentioning

confidence: 84%

“…Following the procedure of Ma et al (2017) to describe the level of metal enrichment from first stars, we define the fraction of metals in a galaxy which is produced by PopIII stars as:…”

Section: Simulationsmentioning

confidence: 99%

Section: Dla Definitionmentioning

confidence: 99%

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Metal enrichment signatures of the first stars on high-z DLAs

Maio

Ciardi

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…This facilitates several large ground-based surveys (e.g., CALIFA, MaNGA, SAMI) to constrain the radial profile of metallicity in hundreds of galaxies, successfully capturing the dynamic signatures of the baryon cycle (see, e.g., Sanchez et al 2014;Belfiore et al 2017;Poetrodjojo et al 2018). Meanwhile, numerical simulations are now capable of making useful predictions for metallicity radial gradients and their evolution with redshift (e.g., Ma et al 2017;Tissera et al 2019). The main challenge for observations is that sub-kpc spatial resolution is required for accurate results and meaningful comparison with theoretical predictions.…”

Section: Introductionmentioning

confidence: 95%

A Census of Sub-kiloparsec Resolution Metallicity Gradients in Star-forming Galaxies at Cosmic Noon from HST Slitless Spectroscopy

Wang

Jones

Treu

et al. 2020

ApJ

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We present the hitherto largest sample of gas-phase metallicity radial gradients measured at sub-kpc resolution in star-forming galaxies in the redshift range of zä[1.2, 2.3]. These measurements are enabled by the synergy of slitless spectroscopy from the Hubble Space Telescope near-infrared channels and the lensing magnification from foreground galaxy clusters. Our sample consists of 76 galaxies with stellar mass ranging from 10 7 to 10 10  M , an instantaneous star formation rate in the range of [1, 100]  M yr −1 , and global metallicity [ ] , 2 1 12 * , with the intrinsic scatter being σ=0.060±0.006 over 4 orders of magnitude in stellar mass. Our result is consistent with strong feedback, not secular processes, being the primary governor of the chemostructural evolution of star-forming galaxies during the disk mass assembly at cosmic noon. We also find that the intrinsic scatter of metallicity gradients increases with decreasing stellar mass and increasing specific star formation rate. This increase in the intrinsic scatter is likely caused by the combined effect of cold-mode gas accretion and merger-induced starbursts, with the latter more predominant in the dwarf mass regime of   M M 10 9 * .

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“…The first generation of metal-free stars (the so-called Pop III stars) and the second generation of massive, metal-poor stars (the so-called Pop II stars) can result in powerful GRBs (see, e.g., Mészáros & Rees, 2010) that thus offer a direct route to identify such elusive objects (even JWST will not be able to detect them directly) and study the galaxies in which they are hosted. Even indirectly, the role of Pop III stars in enriching the first galaxies with metals can be studied by looking at the absorption features of Pop II GRBs blowing out in a medium enriched by the first Pop III supernovae (Ma et al, 2017). Moreover, both Pop III and massive Pop II stars may have contributed to the reionization of the Universe due to their intensive ionizing radiation (Yoon et al, 2012;Szécsi et al, 2015), thus detecting their final explosion will help us better understand our cosmic history.…”

Section: Introductionmentioning

confidence: 99%

The THESEUS space mission concept: science case, design and expected performances

Amati

O’Brien

Götz

et al. 2018

Advances in Space Research

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182

137

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THESEUS is a space mission concept aimed at exploiting Gamma-Ray Bursts for investigating the early Universe and at providing a substantial advancement of multi-messenger and time-domain astrophysics. These goals will be achieved through a unique combination of instruments allowing GRB and X-ray transient detection over a broad field of view (more than 1sr) with 0.5-1 arcmin localization, an energy band extending from several MeV down to 0.3 keV and high sensitivity to transient sources in the soft X-ray domain, as well as on-board prompt (few minutes) followup with a 0.7 m class IR telescope with both imaging and spectroscopic capabilities. THESEUS will be perfectly suited for addressing the main open issues in cosmology such as, e.g., star formation rate and metallicity evolution of the inter-stellar and intra-galactic medium up to redshift ∼10, signatures of Pop III stars, sources and physics of reionization, and the faint end of the galaxy luminosity function. In addition, it will provide unprecedented capability to monitor the X-ray variable sky, thus detecting, localizing, and identifying the electromagnetic counterparts to sources of gravitational radiation, which may be routinely detected in the late '20s / early '30s by next generation facilities like aLIGO/ aVirgo, eLISA, KAGRA, and Einstein Telescope. THESEUS will also provide powerful synergies with the next generation of multi-wavelength observatories (e.g., LSST, ELT, SKA, CTA, ATHENA).

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Constraining the PopIII IMF with high-zGRBs

Cited by 51 publications

References 60 publications

Metal enrichment signatures of the first stars on high-z DLAs

Metal enrichment signatures of the first stars on high-z DLAs

A Census of Sub-kiloparsec Resolution Metallicity Gradients in Star-forming Galaxies at Cosmic Noon from HST Slitless Spectroscopy

The THESEUS space mission concept: science case, design and expected performances

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