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arXiv · 1806.07732

Nature and chemical abundances of a sample of Lyman-$\alpha$ emitter objects at high redshift

O. L. Dors·B. Agarwal·G. F. Hagele·M. V. Cardaci·C. -E. Rydberg·R. A. Riffel·A. S. Oliveira·A. C. Krabbe
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Abstract

We built a grid of photoionization models and compiled already available observational emission line intensities ($\rm 1000 \: < \: \lambda(\AA) \: < \: 2000$) of confirmed star formation regions and Active Galactic Nucleus (AGNs) in order to classify five Ly$\alpha$ emitter (LAE) objects at high redshift $(5.7 \: < \: z \: < \:7.2)$. We selected objects for which at least one metal emission-line was measured. The resulting sample is composed by the objects RXCJ2248.7-4431-ID3, HSCJ233408+004403, COSY, A1703-zd6, and CR7 (clump C). The photoionization models were built assuming a Power Law (associated with the presence of an AGN), a Direct Collapse Black Hole (DCBH), and Population II stars for the ionizing source. The resulting models were then compared with observational emission-line ratios in six diagnostic diagrams to produce a spectral classification of the sample. We found that CR7 (clump C), HSCJ233408+004403 and COSY probably have a non thermal ionizing source (AGN or DCBH) while the RXC J2248.7-4431-ID3 and A1703-zd6 seem to host a stellar cluster. Detailed photoionization models were constructed to reproduce observational emission line ratios of the sample of LAEs, and to derive chemical abundances and number of ionizing photons $Q(\rm H)$ of these objects. From these models, we found metallicities in the range $(Z/Z_{\odot})=0.1-0.5$ and $\log Q(\rm H) \: > \: 53$. Values for C/O abundance ratio derived for the LAEs seem to be consistent with those derived for local star forming objects with similar metallicities, while an overabundance of N/O was found for most of the LAEs.

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O. L. Dors, B. Agarwal, G. F. Hagele, M. V. Cardaci, C. -E. Rydberg, R. A. Riffel, A. S. Oliveira, A. C. Krabbe. 2018-06-20. Nature and chemical abundances of a sample of Lyman-$\alpha$ emitter objects at high redshift. https://doi.org/10.1093/mnras%2Fsty1658

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