Notes. GRB and Redshift are for the name of the LGRB and its redshift. When observations of the host galaxy or the optical afterglow are available, we provide the name of the spectrographs used in the columns Hosts and OA, respectively. "no" indicates that no observation is available. "F1"/"F2" is for VLT/FORS1/2 and "xsh" for VLT/X-shooter spectrograph. Lyα Host and Lyα OA inform about the detection of the Lyα line in the host or afterglow spectra, respectively. No information is provided when no spectra are available to verify the presence of the line. Flux(Lyα) corresponds to the Lyα line flux, in units of 10⁻¹⁷ erg s⁻¹ cm⁻² Å⁻¹, retrieved from the literature (see references in column Refs) or derived in this work. Samples indicates to which sample the LGRB belongs. Refs is for the references where the Lyα detection is reported. ^a GRB 060707 is part of the XHG sample but the Lyα is not detected in the X-shooter spectrum. ^b For GRB 060714 the Lyα line is only detected at 2.5σ in the host galaxy observation of Milvang-Jensen et al. (2012), but is convincingly detected in the afterglow spectrum presented by Jakobsson et al. (2006), therefore we consider it as a detection and report the flux measured in the afterglow spectrum corrected for Galactic extinction.

References: (1): Kulkarni et al. (1998); (2): Fynbo et al. (2003); (3): Ahn (2000); (4): Fynbo et al. (2002); (5): Jakobsson et al. (2005); (6): Vreeswijk et al. (2004); (7): Jakobsson et al. (2004); (8): Milvang-Jensen et al. (2012); (9): Perley et al. (2016b); (10): Fynbo et al. (2009); (11): Jakobsson et al. (2006); (12): Perley et al. (2009); (13): D’Avanzo et al. (2010); (14): Hartoog et al. (2015); (15): Krühler et al. (2015); (16): Selsing et al. (2019); (17): Tanvir et al. (2019); (18): Malesani et al. (2013); (19): Cucchiara et al. (2015); (20): this work, (21): Berger & Rauch (2008), (22): D’Elia et al. (2019), (23): Wiseman et al. (2017)