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tokens: angles and distances of events with joint γ-ray and GW detections (red crosses) from a simulation of SJPL model with θ 0 = 0.1 and δ = 4.5. Top and bottom panels show results for an effective GW horizon distance of 107 and 220 Mpc, respectively. The median distance of future joint detection events is ≈150 Mpc and correspondingly the median GRB luminosity is 7 × 10 48 ergs −1 ≫ L GRB170817 . The fact that GRB170817 is an atypical event of the sample of expected joint prompt and GW detections is also illustrated in Fig. 4 , where we present the expected L γ − θ obs distributions of joint detections for two models of prompt emission given a detection horizon of 220Mpc. For both models, the properties of GRB170817 (blue crosses) are not representative of the sample. Only and of the simulated events (jointly detected in γ-rays and GWs) in the CL and SJPL models, respectively, is found to have 0.25 ≤ θ obs ≤ 0.45 and 5 × 10 46 ≤ L γ ≤ 4.8 × 10 47 erg s −1 . The shape of the observed two-dimensional distributions is driven by the emission model, since the emission is typically dominated by material that is radiating within its 1/Γ beaming cone from the observer. A differentiation between the underlying emission models would require a sufficiently large number of joint GW and GRB detections (see also Section 5 ). Figure 3. Distances and observation angles for mergers detected in GW alone (yellow circles) and for mergers with joint GW and γ-ray detections (red crosses). We present the distribution with a detection horizon of 107 Mpc (top), corresponding to the effective detection horizon for GW170817 or 220 Mpc (bottom), suitable for future events. The inferred values for GRB170817 are shown with a blue symbol. The maximum distance at which it could have been observed in γ-rays is depicted by the vertical dashed line. Results are shown for an SJPL model with θ 0 = 0.1 and δ = 4.5. Figure 4. Two-dimensional distributions of observation angles and γ-ray luminosities for different structure models assuming a joint prompt GRB and GW detection. The location of GRB170817 on these plots is marked with blue crosses that denote the 1σ error in luminosity (Zhang et al. 2018 ) and observation angle (Mooley et al. 2018b ). 4 THE COCOON EMISSION We estimate here the thermal energy stored in the cocoon, the fraction of it radiated in γ-rays at breakout and the cooling emission signature arising when the thermal cocoon eventually becomes optically transparent. The latter corresponds to a ∼ hours long ultraviolet (UV) signal, that may be detectable, provided sufficiently rapid localization of the NS merger. The peak thermal energy stored in the cocoon (as a function of time) is found by Duffell et al. ( 2018 ). As mentioned above, here we assume that the that the injected opening angle is equal to the opening angle after breakout. Rewriting equations (10) and (21) in Duffell et al. ( 2018 ) in a slightly different form, we obtain: where erg and E j is the beaming