The population of X-ray supernova remnants in the Large Magellanic Cloud

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Volume 585 (January 2016)

A&A, 585 (2016) A162

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Table E.1

X-ray spectral results of LMC SNRs.

	Component 1					Component 2					χ² / ν

MCSNR	N_{H LMC}	kT	τ	EM	Abundances	N_{H LMC}	kT	τ	EM	Abundances
	(10²¹ cm^-2)	(keV)	(10¹¹ s cm^-3)	(10⁵⁸ cm^-3)		(10²¹ cm^-2)	(keV)	(10¹¹ s cm^-3)	(10⁵⁸ cm^-3)
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)

J0449−6920	6.97	0.20	CIE	18.3	RD92	–					1985.3/1863 (1.07)
J0450−7050^a	1.31	0.24 ± 0.02	CIE	33.6	0.20	–					4669.4/3294 (1.42)
					0.40
					0.20 (<0.48)
J0453−6655	1.10	0.36	1.38	30.7	0.13	–					4460.9/4214 (1.06)
					0.12
					0.15
					0.29
J0453−6829^b	0.93	0.37	1.58	27.2	0.17 ±0.01	–					2156.2/1860 (1.16)
					0.25
					0.37 ± 0.05
					0.61
					0.28
J0454−6626	1.15	0.34	1.17	1.67	0.14	–					2136.8/1811 (1.18)
					0.15(<0.39)
					0.26
J0505−6802^c	1.58	0.32	3.40	107.4	0.11	1.58	1.09	2.46	6.50	–	454.4/407 (1.12)
					0.16 ± 0.02
					0.18 ± 0.03
					0.37
					0.20
J0506−6541	0.59(<1.34)	0.18 ± 0.01	CIE	2.27	1.26	–					8549.4/7232 (1.18)
J0506−7026	<0.12	0.70	1.99 (1.08)	0.61± 0.09	0.33	–					9026.4/8365 (1.08)
					0.42
					0.22
					1.49
J0508−6830^d	<1.80	0.71	CIE	1.0	0	–					1488.3/1554 (0.96)
					792.9(>1.1)
J0508−6902^e	<0.8	0.41	27.0	0.48	RD92	0	0.78 ± 0.03	CIE	< 48.8	pure O	267.1/219 (1.22)
									0.16 ±0.01	pure Fe
J0511−6759^d	<2.10	0.65	CIE	1.2	0	–					707.5/692 (1.02)
					11.4(>4.7)
J0512−6707	0.82	0.24 ±0.01	CIE	0.15	RD92	–					3059.4/2083 (1.47)
J0513−6912 ?	1.34	0.43± 0.08	10.9	1.28	0.27	–					5352.3/4996 (1.07)
					0.46
					0.75
					1.33
					0.20
J0514−6840^d	<0.09	0.30 ±0.01	2.60	0.51 ±0.03	0.28 ±0.03	–					8005.3/7957 (1.01)
					0.38
J0517−6759^d	3.5	0.1	CIE	11.2	RD92	< 1.7	0.59	CIE	0.19	RD92	2558.9/2547 (1.00)
J0518−6939 ?	<1.16	0.44	4.91	1.53	0.14	–					2292.1/2190 (1.05)
					0.23 ±0.15
					0.31
					0.96
					0.27
J0519−6926	<0.09	0.39	3.58	4.53	0.15	–					3602.5/3033 (1.19)
					0.36
					0.34 ±0.10
					1.21
					0.21 ±0.03
J0523−6753	0.75	0.62 ±0.04	22.7	0.66	1.49	–					5075.9/4532 (1.12)
					3.08
					1.57
					1.13 ±0.43
					0.48 ±0.16
J0525−6559	2.17	0.60	2.34	50.3	0.07 ±0.05	2.17	0.32 ±0.07	4.34	43.6	RD92	3981.8/2884 (1.38)
					0.27 ±0.04
					0.43 ±0.09
					0.33 ±0.07
					0.10
J0526−6605^f	2.64	0.42 ±0.02	5.26	112.3	0.30 ±0.03	2.64	1.04	>35.0	27.4	–	3509.3/2038 (1.72)
					0.42
					0.52
					1.0 ±0.11
					0.41
J0527−6714^g	2.0	0.18 ±0.01	CIE	1.31 ±0.23	RD92	–					5999.0/5237 (1.15)
J0527−6912^h ?	2.0	0.18 ±0.01	CIE	1.31 ±0.23	RD92	–					12115.5/10771(1.12)
J0527−7104	1.33	0.37	1.33	0.30	0.05	–					6801.8/5788 (1.18)
					0.86
					1.43
J0528−6727	<0.39	0.22± 0.02	CIE	1.70	0.30	–					5510.0/5265 (1.05)
					0.66
					0.66
J0529−6653ⁱ	0.48	1.51 ±0.28	0.30	0.83	0.09 ±0.02	–					1961.3/2987 (0.66)
					0.03(< 0.05)
					0.07 ±0.06
					0.21(<0.49)
					0.07
J0530−7008 ?	0.37	0.18	CIE	1.34	RD92	0.37	0.74 ±0.06	CIE	0.36 ±0.06	RD92	9284.5/7105 (1.31)
J0531−7100	<0.12	0.52	2.50	1.63	RD92	–					2864.9/2361 (1.20)
J0532−6732	0.94	0.53	0.83	2.30	0.25	–					3824.0/3562 (1.10)
					0.24
					0.17
					1.44
					0.34
J0533−7202	0.47	0.31	1.39	1.13	0.27	–					4128.0/3265 (1.26)
					0.37
					< 0.18
					0.37
J0534−6955^j ?	2.27	0.31	3.04	26.1	0.14 ±0.01	2.27	1.32	pure Si: τ = 0.05 ± 0.01; EM			3400.8/2727 (1.25)
					0.23			pure S: ; EM
					0.27			pure Fe: ; EM
					0.34
J0534−7033^k	<0.03)	0.78 ± 0.01	208(>63.1)	0.87	0.30 ±0.18	0	0.27	2.65	0.46	RD92	3496.61/2922 (1.20)
					0.08(<0.27)
					1.26
J0535−6602^l	0.68	0.52 ±0.01	7.49	251.1		2.48	1.10	10.4	99.1	0.71	1962.4/1634 (1.20)
					0.23					< 0.12
					0.57					0.85
					0.12					0.76
					< 0.13					0.48 ±0.05
					0.28 ±0.01					< 0.02
										0.14(<0.34)
J0535−6918	2.31 ±0.03	0.31	1.71	1.85	0.15	–					1999.9/1589 (1.26)
					0.34
					0.34
					1.60
					0.30
J0536−6735^m	2.26 ±0.20	0.56	7.59	2.00	1.57	–					6015.7/4816 (1.25)
					2.52
					1.35
					0.04
J0536−6913ⁿ	4.89	0.75	10.5	0.11	RD92	4.89	4.22	0.08	0.06 ±0.02	1.68	1107.4/1139 (0.97)
										0.59
										1.51
										7.9
J0536−7039^o	<0.07	0.27	3.85	0.56	RD92	0	0.73	7.26	0.50	0.12(<1.12)	3555.7/3441 (1.03)
										0.37
										0.37(<0.77)
										1.89
J0537−6628	0.56(<1.13)	0.42	10.2	0.60	0.32	–					3489.1/2983 (1.17)
					0.34
					0.07(<0.31)
					0.26
J0537−6910^p	9.11	4.92 ±0.35	0.19	0.53	RD92	–					3866.8/3452 (1.12)
J0540−6920^q	6.85	0.49 ±0.06	1.87	6.03	RD92	–					5528.0/4763 (1.16)
J0540−6944^r	11.4	0.20 ±0.02	CIE	30.64	RD92	–					1323.4/770 (1.72)
J0541−6659	< 0.07	0.40	0.36	0.38	RD92	–					6933.5/5886 (1.18)
J0543−6858	2.09	1.12	0.35	1.14	0.37 ±0.10	–					7211.4/6717 (1.07)
					0.36
					0.29
					0.36(<0.98)
					0.32
J0547−6941	4.91	1.25 ±0.18	2.38	0.83	0.26	–					3451.2/3196 (1.08)
					< 0.37
					0.39
					0.71
					2.30 ±0.70
J0547−6943^s	3.73	0.27	493(>5.32)	3.67	0.22	3.73	2.16	2.33	0.89	–	4468.2/4356 (1.03)
					0.27
					0.76
					0.58
					0.33
					0.58
J0547−7025 ?	3.04	0.31	3.12	4.72	RD92	3.04	0.80	1.18	1.65	< 0.08	2949.1/2559 (1.15)
										0.32 ±0.01
										0.07(<0.12)
										0.28 ±0.25
										1.10
										0.92

Notes. Columns are described in Sect. 5.1. ? These SNRs were observed with XMM-Newton EPIC instruments for the first time over the course of this work. Their spectra are shown in Fig. D.1.

^(a)

Only MOS data available.

^(b)

Fit includes a power-law component for the central PWN.

^(c)

Same absorption column and abundances in the two components; nitrogen abundance is also fitted to 0.07 solar.

^(d)

Results from MHK14.

^(e)

Results from BKM14. The first component is a Sedov model. The second is split into two pure-metal components (O and Fe) with the corresponding emission measures given as EM_X × (n_X/n_H).

^(f)

Same absorption column and abundances in the two components; fit includes a power-law component for SGR 0526−66 (Park et al. 2012).

^(g)

N_{H LMC} fixed to the value from the H i map of the LMC.

^(h)

Abundances from RD92 are scaled by a common factor.

⁽ⁱ⁾

Affected by strong background flare.

^(j)

The second component comprises three pure-metals NEI models with a common temperature and distinct τ and EM, for each Si, S, and Fe.

^(k)

C, N, O, and Ne abundances of the iron-rich component (Component 1) are fixed to 0.

^(l)

Abundance of Ca fixed at 0 in the second component; fit includes an Fe K (Gaussian) line, see Sect. 5.4.

^(m)

Fit includes a power-law component for the interior HMXB (Seward et al. 2012).

⁽ⁿ⁾

Elements other than O, Ne, Mg, and Si in the second component are set to 0.

^(o)

C, N, and O abundances of the iron-rich component (Component 2) are fixed to 0.

^(p)

Fit includes a power-law component for the interior PWN.

^(q)

Strongly affected by the emission from PSR 0540−69.3 (modeled by a power law).

^(r)

Dominated by the contamination from LMC X-1 (modeled by a power law).

^(s)

Same absorption column and abundances in the two components.

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