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Table 1

General information on high-redshift GRBs and model parameters of their NIR afterglow.

Identifier z RA Dec T0 TJ TH mJ mH α(a) tbreak β(b) Ref.
(deg) (deg) (MJD-53000) (h) (h) (mag) (mag) (d)
GRB 050904A 6.39 13.7116 14.0860 617.077593 3.07 9.79 17.36 18.17 (0.9,1.9) 2.1 1.25 [1]
GRB 080913A 6.695 65.7280 –24.1295 1722.282570 0.10 0.10 19.96 19.64 1.03 1.12 [2]
GRB 090429B 9.4 210.6667 32.1706 1950.2292 2.95 3.27 22.8 21.41 (0, 0.53) 0.02 0.51 [3]
GRB 090709A 8.5 289.9277 60.7276 2021.318449 0.11 0.03 18.43 15.52 0.9 3.8 [4]
GRB 100205A <8 141.3875 31.7403 2232.179664 5.48 4.73 24.29 23.63 0.43 0.51 [5]
GRB 120521C 6.03 214.2833 42.1431 3068.973692 7.63 8.54 20.4 19.8 (–0.83, 1.38) 0.34 0.34 [6]
GRB 120923A 7.8 303.7958 6.2203 3193.219514 1.37 3.24 21.9 21.4 (0.25, 2) 1.46 0.39 [7]
GRB 140515A 6.32 186.0639 15.1046 3792.38375 15.6 14.54 20.63 20.61 0.89 0.33 [8]
GRB 210905A 6.318 309.0481 –44.4396 6462.0088 0.36 0.13 17.12 16.15 (0.69, 0.94) 0.99 0.6 [9]

Notes. The first magnitude measurements in J and H bands are given along with the time after the burst when they were carried out.(a)Temporal decay index of the GRB as measured in the frame of the observer. If two values are provided, an associated time break is given (tbreak).(b)Spectral index of the GRB as measured in the frame of the observer. Is assumed to be constant over time. [1] Haislip et al. (2006); [2] Greiner et al. (2009); [3] Cucchiara et al. (2011); [4] Cenko et al. (2010); [5] Chrimes et al. (2019); [6] Laskar et al. (2014); [7] Tanvir et al. (2018); [8] Melandri et al. (2015); [9] Rossi et al. (2022).

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