Deep observation of the NGC 1275 region with MAGIC: search of diffuse γ-ray emission from cosmic rays in the Perseus cluster

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Volume 589 (May 2016)

A&A, 589 (2016) A33

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Table 2

Integral flux upper limits between E_th and 10 TeV assuming observed power-law spectrum with an index Γ = 2.33.

E _th	Model	N _ON ^a	N _OFF ^a	σ _LiMa ^b	^c	^c


	point-like	332	304.1	1.4	12.2	12.2
630 GeV	isobaric	1327	1256	1.4	24.8	65.5
	semi-analytic	749	681	1.8	26.8	49.0
	extended	1327	1256	1.4	25.6	124.

	point-like	159	157.5	0.1	3.84	3.84
1.0 TeV	isobaric	675	652	0.6	10.7	28.3
	semi-analytic	369	352	0.6	9.77	17.9
	extended	675	652	0.6	11.1	54.0

	point-like	77	75.9	0.1	2.34	2.34
1.6 TeV	isobaric	321	317	0.2	5.09	13.5
	semi-analytic	169	167	0.1	4.61	8.43
	extended	321	317	0.2	5.26	25.6

	point-like	38	37.4	0.1	1.57	1.57
2.5 TeV	isobaric	143	153	-0.6	2.18	5.75
	semi-analytic	77	81	-0.3	2.30	4.21
	extended	143	153	-0.6	2.25	11.0

2.5 TeV	isobaric	–	–	–	3.10	8.15
for zero	semi-analytic	–	–	–	2.81	5.15
excess^d	extended	–	–	–	3.21	15.5

Notes.

^(a)

Number of events in the signal (N_ON) and background (N_OFF) regions.

^(b)

Significance of the measured excess in standard deviations.

^(c)

95%-c.l. flux upper limits in units of 10^-14 cm^-2 s^-1 within a radius of 0.15° and 1.4° from the cluster centre.

^(d)

For negative measured excess, we provide conservative upper limits assuming zero excess.

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