Study of X-ray emission from the S147 nebula with SRG/eROSITA: X-ray imaging, spectral characterization, and a multiwavelength picture

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Volume 689 (September 2024)

A&A, 689 (2024) A277

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Table 2.

Best-fit spectral parameters.

Region	A ^( † ) region	B region	C ^( * ) region

Model	vnei
kT(keV)	$0 . 41_{- 0.05}^{+ 0.09}$ $0.41_{-0.05}^{+0.09}$	$0 . 23_{- 0.04}^{+ 0.06}$ $0.23_{-0.04}^{+0.06}$	$0 . 50_{- 0.11}^{+ 0.21}$ $0.50_{-0.11}^{+0.21}$
N_H (10²² cm⁻²)	$0 . 23_{- 0.04}^{+ 0.03}$ $0.23_{-0.04}^{+0.03}$	$0 . 18_{- 0.04}^{+ 0.04}$ $0.18_{-0.04}^{+0.04}$	$0 . 32_{- 0.04}^{+ 0.04}$ $0.32_{-0.04}^{+0.04}$
O	$1 . 30_{- 0.28}^{+ 0.40}$ $1.30_{-0.28}^{+0.40}$	$1 . 96_{- 0.25}^{+ 0.32}$ $1.96_{-0.25}^{+0.32}$	$0 . 47_{- 0.13}^{+ 0.21}$ $0.47_{-0.13}^{+0.21}$
Ne	$1 . 63_{- 0.37}^{+ 0.67}$ $1.63_{-0.37}^{+0.67}$	$3 . 48_{- 0.77}^{+ 0.96}$ $3.48_{-0.77}^{+0.96}$	$1 . 70_{- 0.54}^{+ 0.66}$ $1.70_{-0.54}^{+0.66}$
Mg	$5 . 95_{- 2.07}^{+ 3.05}$ $5.95_{-2.07}^{+3.05}$	$9 . 98_{- 2.08}^{+ 4.01}$ $9.98_{-2.08}^{+4.01}$	–
Ionization time (10¹⁰s ⋅ cm⁻³)	$0 . 66_{- 0.24}^{+ 0.23}$ $0.66_{-0.24}^{+0.23}$	$4 . 59_{- 2.61}^{+ 5.74}$ $4.59_{-2.61}^{+5.74}$	$0 . 09_{- 0.02}^{+ 0.03}$ $0.09_{-0.02}^{+0.03}$

χ²/d.o.f.	1.04	1.09	1.11

Region	D region	E ^( † ) region	F region

Model	vnei

kT(keV)	$0 . 19_{- 0.05}^{+ 0.18}$ $0.19_{-0.05}^{+0.18}$	$0 . 42_{- 0.06}^{+ 0.14}$ $0.42_{-0.06}^{+0.14}$	$2 . 17_{- 0.83}^{+ 1.57}$ $2.17_{-0.83}^{+1.57}$
N_H(10²² cm⁻²)	$0 . 49_{- 0.12}^{+ 0.11}$ $0.49_{-0.12}^{+0.11}$	$0 . 28_{- 0.06}^{+ 0.05}$ $0.28_{-0.06}^{+0.05}$	$0 . 33_{- 0.04}^{+ 0.03}$ $0.33_{-0.04}^{+0.03}$
O	–	$2 . 41_{- 0.68}^{+ 0.62}$ $2.41_{-0.68}^{+0.62}$	$0 . 80_{- 0.23}^{+ 0.29}$ $0.80_{-0.23}^{+0.29}$
Ne	–	$2 . 58_{- 0.81}^{+ 1.66}$ $2.58_{-0.81}^{+1.66}$	$1 . 19_{- 0.42}^{+ 0.43}$ $1.19_{-0.42}^{+0.43}$
Mg	–	$7 . 07_{- 2.72}^{+ 4.96}$ $7.07_{-2.72}^{+4.96}$	–
Ionization time (10¹⁰s ⋅ cm⁻³)	$2 . 09_{- 1.21}^{+ 6.69}$ $2.09_{-1.21}^{+6.69}$	$0 . 64_{- 0.19}^{+ 0.29}$ $0.64_{-0.19}^{+0.29}$	$0 . 065_{- 0.02}^{+ 0.03}$ $0.065_{-0.02}^{+0.03}$

χ²/d.o.f.	1.34	0.99	1.19

Region	G region	H ^( * ) region	I region

Model	vnei

kT(keV)	$0 . 25_{- 0.04}^{+ 0.12}$ $0.25_{-0.04}^{+0.12}$	$0 . 47_{- 0.08}^{+ 0.04}$ $0.47_{-0.08}^{+0.04}$	$0 . 21_{- 0.02}^{+ 0.06}$ $0.21_{-0.02}^{+0.06}$
N_H (10²² cm⁻²)	$0 . 29_{- 0.08}^{+ 0.05}$ $0.29_{-0.08}^{+0.05}$	$0 . 33_{- 0.01}^{+ 0.02}$ $0.33_{-0.01}^{+0.02}$	$0 . 24_{- 0.09}^{+ 0.10}$ $0.24_{-0.09}^{+0.10}$
O	$2 . 08_{- 0.35}^{+ 0.43}$ $2.08_{-0.35}^{+0.43}$	$0 . 33_{- 0.04}^{+ 0.05}$ $0.33_{-0.04}^{+0.05}$	$0 . 57_{- 0.14}^{+ 0.12}$ $0.57_{-0.14}^{+0.12}$
Ne	$2 . 62_{- 0.65}^{+ 0.88}$ $2.62_{-0.65}^{+0.88}$	$0 . 95_{- 0.16}^{+ 0.18}$ $0.95_{-0.16}^{+0.18}$	$0 . 98_{- 0.34}^{+ 0.35}$ $0.98_{-0.34}^{+0.35}$
Mg	$9 . 31_{- 2.45}^{+ 3.31}$ $9.31_{-2.45}^{+3.31}$	–	$11 . 1_{- 0.43}^{+ 0.62}$ $11.1_{-0.43}^{+0.62}$
Ionization time (10¹⁰s ⋅ cm⁻³)	$2 . 32_{- 0.87}^{+ 3.06}$ $2.32_{-0.87}^{+3.06}$	$0 . 11_{- 0.01}^{+ 0.01}$ $0.11_{-0.01}^{+0.01}$	$11 . 94_{- 7.97}^{+ 11.69}$ $11.94_{-7.97}^{+11.69}$

χ²/d.o.f.	1.2	1.54	1.22

Region	J ^( * ) region	Entire remnant	XMM-Newton

Model	vnei

kT(keV)	$0 . 75_{- 0.17}^{+ 0.11}$ $0.75_{-0.17}^{+0.11}$	$0 . 22_{- 0.03}^{+ 0.02}$ $0.22_{-0.03}^{+0.02}$	Identical to region H
N_H(10²² cm⁻²)	$0 . 30_{- 0.01}^{+ 0.03}$ $0.30_{-0.01}^{+0.03}$	$0 . 30_{- 0.03}^{+ 0.04}$ $0.30_{-0.03}^{+0.04}$
O	$0 . 46_{- 0.06}^{+ 0.06}$ $0.46_{-0.06}^{+0.06}$	$2 . 34_{- 0.18}^{+ 0.20}$ $2.34_{-0.18}^{+0.20}$
Ne	$1 . 00_{- 0.16}^{+ 0.18}$ $1.00_{-0.16}^{+0.18}$	$3 . 13_{- 0.34}^{+ 0.40}$ $3.13_{-0.34}^{+0.40}$
Mg	–	$9 . 53_{- 1.31}^{+ 1.47}$ $9.53_{-1.31}^{+1.47}$
Ionization time (10¹⁰s ⋅ cm⁻³)	$0 . 09_{- 0.01}^{+ 0.01}$ $0.09_{-0.01}^{+0.01}$	$4 . 27_{- 0.99}^{+ 1.87}$ $4.27_{-0.99}^{+1.87}$

χ²/d.o.f.	1.31	1.63

Notes. The best-fit spectral parameters of the regions that have been selected to best represent the spectral variation detected across the remnant are provided with 1σ statistical errors. Where not defined, elemental abundances are set to solar values. For regions marked with an ^( * ), very small N elemental abundance values (essentially equal to zero) were found. For regions marked with a ^( † ), Si appears to be present, and the corresponding elemental abundance is highly degenerate; thus, we allowed it to vary, aiming to improve the fit quality.

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