The counterpart/s of IGR J20159+3713/SWIFT J2015.9+3715: dissecting a complex region with emission from keV to TeV

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Table 2

Log of the Swift/XRT observations and count rates of each detection.

Observation	Date	Exposure^a	Count rate^b
			CV	blazar	PWN^c
		(s)	(10^-3 counts s^-1)	(10^-3 counts s^-1)	(10^-3 counts s^-1)

#1	July 12 2006	1528	40.1 ± 5.2	11.3 ± 2.9	1.3 ± 0.9
#2	Nov. 12 2006	4490	46.7 ± 3.3	22.6 ± 2.3	1.4 ± 0.7
#3	Nov. 17 2006	7367	66.8 ± 3.0	24.7 ± 1.9	13.9 ± 1.4
#4	Nov. 24 2006	170	87.6 ± 24.5	27.8 ± 13.3	10.6 ± 8.4
#5	Aug. 5 2010	962	57.9 ± 8.0	69.3 ± 8.7	7.9 ± 3.3
#5	Aug. 6 2010	7307	43.5 ± 2.5	55.6 ± 2.8	9.1 ± 1.2
#6	Aug. 22 2010	4310	43.3 ± 3.2	73.3 ± 4.2	8.8 ± 1.5
#8	Aug. 30 2010	4146	32.4 ± 2.9	46.4 ± 3.4	6.8 ± 1.4

	Total	30 280	48.4 ± 1.3	42.6 ± 1.2	10.2 ± 0.6

Notes.

^(a)

Total on-source exposure time;

^(b)

the count rate is estimated in the 0.3−10 keV energy range;

^(c)

the PWN count rate has been extracted from a circle of 20′′ radius centred on the brightest X-ray spot.

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