The Northern Cross Fast Radio Burst project - V. Search for transient radio emission from Galactic magnetars

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Table 2.

Inferred upper limits on the sample of magnetars.

Name	Total exposure	E_min	ℛ(E > E_min)	ℛ(E > E_J1935), γ = 1	ℛ(E > E_J1935), γ = 1.3	ℛ(E > E_J1935), γ = 1.6
	(hours)	10²⁶ (erg)	(yr⁻¹)	(yr⁻¹)	(yr⁻¹)	(yr⁻¹)
3XMM J185246.6+003317	33.46	67 − 137	< 785	< 400	< 8.78	< 0.10
SGR 1900+14	40.58	209 − 424	< 647	< 342	< 10.19	< 0.17
SGR J1935+2154	52.34	108 − 220	< 502	< 260	< 6.48	< 0.09
SGR 2013+34	63.38	104 − 210	< 414	< 214	< 5.36	< 0.07
1E 2259+586	97.03	14 − 28	< 271	< 131	< 1.91	< 0.01
4U 0142+61	116.08	17 − 35	< 226	< 110	< 1.71	< 0.01
SGR 0418+5729	92.95	5 − 11	< 283	< 133	< 1.49	< 0.01
SGR 0501+4516	70.10	5 − 11	< 375	< 176	< 1.97	< 0.01

All magnetars	565.92	5 − 424	< 46	< 2.92	< 0.05	< 4.04 × 10⁻⁴
All magnetars (NO SGR 2013+34)	502.54	5 − 424	< 52	< 3.74	< 0.06	< 4.76 × 10⁻⁴

Notes. The second column contains the amount of hours observed on each target. The third column represents the interval of the minimum detectable energy above which we defined the upper limit on the rate of events. The fourth column shows the Poissonian upper limit at a 95% confidence level on the observable burst rate. The last three columns list the inferred upper limits on the rates of events with an energy greater than the FRB-like event of the magnetar SGR J1935+2154 using Eq. (7) for three different power-law indexes (as indicated in each column).

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