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|Title:||Metal enrichment signatures of the first stars on high-z DLAs||Authors:||Ma, Q.
|Issue Date:||2017||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||472||Issue:||3||First Page:||3532||Abstract:||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 metal-dependent 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 per cent (40 per cent) of mass (temperature)-selected high-z (z ≥ 5.5) DLAs retain signatures of pollution from PopIII stars, independent of the first star model. Such DLAs have low halo mass ( < 10<SUP>9.6</SUP> M<SUB>☉</SUB>), metallicity ( < 10<SUP>- 3</SUP> Z<SUB>☉</SUB>) and star formation rate ( < 10<SUP>- 1.5</SUP> M<SUB>☉</SUB> yr<SUP>- 1</SUP>). Metal abundance ratios of DLAs imprinted in the spectra of quasi-stellar object can be useful as 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 star dominated enrichment and strongly disfavour the pollution pattern of very massive first stars (i.e. 100-500 M<SUB>☉</SUB>). 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.||URI:||http://hdl.handle.net/20.500.12386/27349||URL:||https://academic.oup.com/mnras/article-abstract/472/3/3532/4002681?redirectedFrom=fulltext||ISSN:||0035-8711||DOI:||10.1093/mnras/stx1839||Bibcode ADS:||2017MNRAS.472.3532M||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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