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

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Table 1.

Localization and predicted Galactic DM contributions for the magnetar sample.

Name	Gal L	Gal B	D	n_H	DM_NE2001	DM_YMW16	DM_nH	DM_radio	Ref.
	(deg)	(deg)	(kpc)	(10²² cm⁻²)	(pc cm⁻³)	(pc cm⁻³)	(pc cm⁻³)	(pc cm⁻³)
3XMM J185246.6+003317	33.5785548	−0.0450683	7.1 ± 2.1	1.32 ± 0.05	$441_{- 274}^{+ 275}$ $441^{+275}_{-274}$	$1020_{- 633}^{+ 590}$ $1020^{+590}_{-633}$	440 ± 16	No	1
SGR 1900+14	43.0034808	0.8520327	12.5 ± 1.7	2.12 ± 0.08	$609_{- 80}^{+ 55}$ $609^{+55}_{-80}$	$526_{- 105}^{+ 70}$ $526^{+70}_{-105}$	707 ± 26	No	2, 3
SGR J1935+2154	57.2467449	0.8189765	9.0 ± 2.5	1.6 ± 0.2	$293_{- 114}^{+ 100}$ $293^{+100}_{-114}$	$320_{- 119}^{+ 90}$ $320^{+90}_{-119}$	533 ± 67	332.7206 ± 0.0009	4, 5, 6
SGR 2013+34	72.3203222	−0.1010242	8.8 ± 2.4	–	$279_{- 110}^{+ 77}$ $279^{+77}_{-110}$	$302_{- 133}^{+ 70}$ $302^{+70}_{-133}$	–	No	7
1E 2259+586	109.0873535	−0.9957528	3.2 ± 0.2	1.21 ± 0.04	$99_{- 11}^{+ 11}$ $99^{+11}_{-11}$	$154_{- 18}^{+ 13}$ $154^{+13}_{-18}$	403 ± 13	No	8, 9
4U 0142+61	129.3839879	−0.4307465	3.6 ± 0.4	1.00 ± 0.01	$96_{- 11}^{+ 10}$ $96^{+10}_{-11}$	$161_{- 6}^{+ 5}$ $161^{+5}_{-6}$	333 ± 3	No	10, 11
SGR 0418+5729	147.9790422	5.1191370	2.0 ± 0.6	0.115 ± 0.006	$63_{- 25}^{+ 26}$ $63^{+26}_{-25}$	$93_{- 55}^{+ 32}$ $93^{+32}_{-55}$	38 ± 2	No	12, 13
SGR 0501+4516	161.5466873	1.9489249	2.0 ± 0.6	0.88 ± 0.01	$71_{- 28}^{+ 27}$ $71^{+27}_{-28}$	$109_{- 61}^{+ 27}$ $109^{+27}_{-61}$	293 ± 3	No	14, 15

Notes. The second and third columns list the Galactic latitude and longitude of the targets, respectively. The fourth column contains the distances adopted for the magnetars. The distances of 3XMM J185246.6+003317, SGR 2013+34, SGR 0418+5729, and SGR 0501+4516 are discussed in the literature. Therefore, we chose conservative uncertainty intervals of ±30% around the most credible values. The fifth column presents the hydrogen column density derived from high-energy observations. The sixth and seventh columns show the inferred DM contributions, assuming our values for the distances using the electron density distribution models of Cordes & Lazio (2002) and Yao et al. (2017), respectively. The eighth column contains the DM contribution obtained with the best-fit relation between n_H and DM in He et al. (2013). Finally, the last column shows the DM obtained with radio observations. This value is available only for SGR J1935+2154, as the other magnetars of our sample have never been detected at radio wavelengths. (1) Rea et al. (2014); (2) Mereghetti et al. (2006); (3) Davies et al. (2009); (4) Zhong et al. (2020); (5) Israel et al. (2016); (6) CHIME/FRB Collaboration (2020); (7) Sakamoto et al. (2011a); (8) Kothes & Foster (2012); (9) Pizzocaro et al. (2019); (10) Durant & van Kerkwijk (2006); (11) Rea et al. (2007); (12) van der Horst et al. (2010); (13) Rea et al. (2013b); (14) Lin et al. (2011); (15) Camero et al. (2014).

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