Abstract
Aims.We present the updated census and statistics of Lyman-αemitting long gamma-ray burst host galaxies (LAE-LGRBs). We investigate the properties of a subsample of LAE-LGRBs and test the shell model that is commonly used to fit Lyman-α(Lyα) emission line spectra.Methods.We considered all LGRB host galaxies with relevant publicly available information. We defined a golden sample of four LAE-LGRBs (GRBs 011211, 021004, 060926, and 070110) with afterglow and host galaxy observations allowing us to constrain the shell modeling of the Lyαline.Results.The census results in 29 detected LAE-LGRBs. We present 5 new Lyαemission detections in host-galaxy spectra and the corresponding unpublished VLT/X-shooter data (GRBs 060926, 070110, 081121, 081222, and 100424A). From the comparison of the statistics and properties of LAE-LGRBs to those of LAE samples in the literature, we find evidence of Lyαsuppression in dusty systems. The fraction of LAE-LGRBs in the overall LGRB hosts is lower than that found for Lyman-break galaxy (LBG) samples at similar redshift range. This result can arise because the selection criteria of the parent samples are different and the spectral observations of LGRB samples are shallower than those of LBG. However, we find that LAE-LGRBs are representative of Lyαemission from the bulk of UV-selected galaxies atz ∼ 2. We find that the golden sample of LAE-LGRBs we studied consists of complex systems characterized by multiple emission blobs and by signs of possible galaxy interactions. The fitting procedure recovers the HIcolumn densities (NHI) measured from the afterglow spectra and the other properties described by the shell-model parameters in the two low-NHIcases, but it fails to do this in the other two cases with highNHI. The afterglows of most LGRBs and LAE-LGRBs show log(NHI/cm−2) > 20.3, implying that statistically, the bulk of Lyαphotons that is expected to be produced by massive stars in the star-forming region hosting the GRB will be surrounded by these opaque lines of sight. We therefore interpret our results in the context of more sophisticated models and of different dominant Lyα-emitting regions. We also compare LAE-LGRBs to LAE Lyman continuum (LyC) leakers in the literature in terms of the properties that are identified as possible indirect indicators of LyC leakage. We find that only one LGRB (GRB 021004) would likely be a strong LyC leaker and discuss the validity of these indicators at high redshift. While our work shows that LGRBs are useful tools for probing LAEs and radiative transfer models, larger statistics are required to strengthen our findings.
Highlights
Because of its brightness and rest-frame wavelength, the Lymanα (Lyα) emission line is one of the most frequently used features for detecting high-redshift galaxies (e.g., Ouchi et al 2009; Sobral et al 2015; Zitrin et al 2015; Bagley et al 2017)
While the unconstrained shell model succeeds in reproducing the observed profiles, the comparison between the best shell parameters returned by the fitting (Table 5) and the corresponding values determined from the observations (Table 6) reveals important discrepancies for GRBs 060926 and 070110
These statistics are lower than those found for Lyman-break galaxy (LBG) samples at similar redshift range, but they become comparable when only LAEs with rest-frame
Summary
Because of its brightness and rest-frame wavelength, the Lymanα (Lyα) emission line is one of the most frequently used features for detecting high-redshift galaxies (e.g., Ouchi et al 2009; Sobral et al 2015; Zitrin et al 2015; Bagley et al 2017). Similar discrepancies for the FWHMi(Lyα) were found by Hashimoto et al (2015) for double-peak Lyα profiles of galaxies at z ∼ 2.2 These studies emphasize that the shell model must be used with caution to interpret the Lyα line and retrieve physical properties, such as the HI column density (NHI), to avoid misinterpretation. We select a golden sample of four LAE-LGRBs at 2 < z < 3.2 with information on the emission properties of the host galaxies and on the ISM probed by the afterglow We use this combined information to investigate the properties of these systems and test the Lyα radiative transfer modeling.
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Free) 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
