White dwarf-neutron star binaries: A plausible pathway for long-duration gamma-ray bursts from compact object mergers

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Table 2.

Summary of host galaxy and GRB offset parameters.

	GRB211211A	GRB230307A
z	0.076 ^(a)	0.065 ^(b)
M_B	−17.38 ^(c)	−18.77
log₁₀(M_⋆/M_⊙)	8.84 $_{- 0.05}^{+ 0.10}$ $^{+0.10}_{-0.05}$ ^(a)	9.28 ± 0.01 ^(b)
t_m/Gyr	2.53 $_{- 0.50}^{+ 1.24}$ $^{+1.24}_{-0.50}$ ^(d)	1.00 $_{- 0.01}^{+ 0.02}$ $^{+0.02}_{-0.01}$ ^(d)
r₅₀/kpc	1.6 ^(e)	0.03/2.04 ^(b)
Sérsic n	1.0 ^(a)	0.5/1.1 ^(b)
Z/Z_⊙	0.20 $_{- 0.08}^{+ 0.05}$ $^{+0.05}_{-0.08}$ ^(a)	0.57 $_{- 0.01}^{+ 0.03}$ $^{+0.03}_{-0.01}$ ^(b)
r_grb/kpc	7.92 ± 0.03 ^(a)	38.9 ^(b)

Notes. References are listed below. If the value is not referenced, it was calculated for this work. The host of GRB 230307A is modelled with two Sérsic components (see text). For star formation histories we used the non-parametric fits of Nugent et al. (2025, see Figure 3).

^(a)

Rastinejad et al. (2022)

^(b)

Levan et al. (2024)

^(c)

Gaspari et al. (2025)

^(d)

Nugent et al. (2025)

^(e)

Troja et al. (2022).

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