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Table B.1.

29 LGRBs with a detected Lyα emission line in the host galaxy or optical afterglow spectra.

GRB Redshift Host OA Lyα Host Lyα OA Flux(Lyα) Sample Refs
971214 3.4200 Keck no yes - 0.6 ± 0.1 - (1), (2), (3), (8)
000926 2.0400 AlFOSC NOT yes no 14.9 ± 1.1 - (4), (8)
011211 2.1434 xsh F1 yes no 1.6 ± 0.2 - (2)
021004 2.3298 xsh UVES yes yes 16.9 ± 0.3 - (2)
030323 3.3720 no F2 - yes 1.2 ± 0.1 - (2), (6),(8)
030429 2.6600 no F1 - yes 0.3 (2σ) - (7)
050315 1.9500 F1 no yes - 2.3 ± 0.7 TOUGH (8)
060605 3.7730 F1 PMAS yes no 1.7 ± 0.3 TOUGH (8)
060707 3.4240 F1, xsh F1 yes no 1.7 ± 0.3 TOUGH, XHGa (8), (10)
060714 2.7108 F1 F1 no yes 1.7 TOUGHb (8), (10), (11)
060908 1.8836 F1 F1, F2 yes no 7.8 ± 1.0 TOUGH (8)
060926 3.2090 xsh F1 yes yes 5.3 ± 0.4 XHG (8), (10)
061222A 2.0880 LRIS no yes - 16.8 - (8), (12)
070110 2.3523 F1, xsh F1 yes yes 4.0 ± 0.4 TOUGH, XHG (8), (10)
070223 1.6295 LRIS no yes - - - (9)
070506 2.3090 F1 F1 yes no 1.4 ± 0.4 TOUGH (8), (10)
070721B 3.6298 F1 F2 yes yes 1.1 ± 0.2 TOUGH (8), (10)
071031 2.6918 no F2 - yes 2.4 ± 0.3 - (8), (10)
080810 3.3604 LRIS AlFOSC yes yes - - (10), (23)
081121 2.5134 xsh LDSS3 yes no 4.9 ± 0.5 - (20), (21)
081222 2.7700 xsh GMOS-S yes no 1.6 ± 0.4 - (17), (20)
090205 4.6500 no F1 - yes 2.4 ± 0.5 - (8), (13)
100316A 3.1600 no OSIRIS no yes - - (17)
100424A 2.4656 xsh no yes - 3.4 ± 0.5 XHG (15), (18)
121201A 3.3830 no xsh - yes 2.1 ± 0.4 XAFT (16), (19)
150915A 1.9680 no xsh - yes 5.0 ± 1.1 XAFT (16)
151021A 2.3300 no xsh - yes 10.5 ± 0.9 XAFT (16)
170202A 3.6450 no xsh - yes 2.7 ± 0.6 XAFT (16)
191004B 3.5055 xsh xsh yes yes 1.0 ± 0.1 - (20), (22)

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)

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