A new understanding of the Gemini-Monoceros X-ray enhancement from discoveries with eROSITA

Open Access

Table 3

Spectral fit results for the Monoceros SNRs.

Region	N_H	kT₁	τ	Norm₁	kT₂	Norm₂	Cstat/d.o.f.
	[10²² cm⁻²]	[keV]	[s cm⁻³]	[cm⁻⁵ arcmin⁻²]	[keV]	[cm⁻⁵ arcmin⁻²]
MC⁽¹⁾	0.282^+0.067	${0.968}_{- 0.102}^{+ 0.165}$ $\[0.968_{-0.102}^{+0.165}\]$	( ${0.94}_{- 0.29}^{+ 0.41}$ $\[0.94_{-0.29}^{+0.41}\]$ ) × 10¹¹	( ${0.23}_{- 0.04}^{+ 0.04}$ $\[0.23_{-0.04}^{+0.04}\]$ ) × 10⁻⁶	${0.133}_{- 0.004}^{+ 0.005}$ $\[0.133_{-0.004}^{+0.005}\]$	( ${1.50}_{- 0.11}^{+ 0.07}$ $\[1.50_{-0.11}^{+0.07}\]$ ) × 10⁻⁶	1.11
MC HS⁽²⁾	${1.040}_{- 0.208}^{+ 0.156}$ $\[1.040_{-0.208}^{+0.156}\]$	${0.467}_{- 0.107}^{+ 0.138}$ $\[0.467_{-0.107}^{+0.138}\]$	>1.00 × 10¹¹	( ${5.83}_{- 2.43}^{+ 4.62}$ $\[5.83_{-2.43}^{+4.62}\]$ ) × 10⁻⁶	${0.194}_{- 0.014}^{+ 0.012}$ $\[0.194_{-0.014}^{+0.012}\]$	( ${1.27}_{- 0.10}^{+ 0.10}$ $\[1.27_{-0.10}^{+0.10}\]$ ) × 10⁻⁶	1.07
PKS⁽³⁾	0.245	${0.773}_{- 0.134}^{+ 0.279}$ $\[0.773_{-0.134}^{+0.279}\]$	( ${0.66}_{- 0.40}^{+ 0.40}$ $\[0.66_{-0.40}^{+0.40}\]$ ) × 10¹¹	( ${0.74}_{- 0.21}^{+ 0.17}$ $\[0.74_{-0.21}^{+0.17}\]$ ) × 10⁻⁶	${0.147}_{- 0.015}^{+ 0.016}$ $\[0.147_{-0.015}^{+0.016}\]$	( ${2.35}_{- 0.24}^{+ 0.34}$ $\[2.35_{-0.24}^{+0.34}\]$ ) × 10⁻⁶	1.06

Notes. The source model is TBABS × VNEI₁ +APEC₂, where the absorbed VNEI component represents the hotter diffuse emission in the back, and the APEC the unabsorbed Monogem Ring emission. No significant elemental abundances different from solar were found for the regions. ⁽¹⁾Monoceros Loop. ⁽²⁾Monoceros Loop Hot Spot. ⁽³⁾PKS 0646+06.

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