Table 3: Fits to the spectra of NGC 300 X-1 from Obs. 1-4, and of IC 10 X-1. The first model is an absorbed power law plus Gaussian emission line, as favoured by Carpano et al. (2007a). For this model, we give absorption, normalised to 10²² H atom cm^-2, spectral index, line energy and width (in keV), and $\chi ^2$ /d.o.f., with good fit probability in square brackets. We only apply the Gaussian to NGC 300 X-1. We also give the 0.3-10 keV luminosity normalised to 10³⁷ erg s^-1. We next provide the best fits for a disk blackbody + power law model that is often used when describing the high state of disc-accreting BH XBs. We give the absorption, temperature of the disk blackbody, spectral index of the power law component and $\chi ^2$ . We then give 0.3-10 keV luminosity as before, and the fractional contribution of the power law model.
NGC 300 X-1 IC 10 X-1

Model Parameter Obs. 1 Obs. 2 Obs. 3 Obs. 4

PL + Line $n_{\rm H}$ 0.036 0.067(12) 0.052(9) 0.07(2) 0.75(3)

$\Gamma$ 2.46(6) 2.44(7) 2.44 2.53(8) 2.56(6)

$E_{\rm Line}$ 0.95 0.93(2) 0.95(2) 0.95(2) $\dots$

$\sigma$ 0.07 0.08(2) 0.07 0.06(3) $\dots$

$\chi ^2$ /d.o.f. 100/60 [9E-4] 149/154 [0.60] 50/60 [0.82] 117/145 [0.05] 794/652 [1E-4]

$L_{\rm0.3-10~ keV}$ 11.5(13) 28.4(12) 20(2) 34.8(16) 39(3)

BB+PL
$n_{\rm H}$ 0.11(4) 0.130(12) 0.22(5) 0.17(3) 0.92(10)

kT 1.02(14) 1.02(17) 0.92(12) 1.08(15) 0.82(3)

$\Gamma$ 3.41(6) 3.01(16) 3.8(3) 3.26(6) 3.9(5)

$\chi ^2$ /d.o.f. 52/58 [0.67] 211/155 [2E-3] 59/58[0.43] 221/148[1.0E-4] 697/650 [0.09]

$L_{\rm0.3-10~ keV}$ 16.9(17) 39(2) 49(6) 59(3) 91(19)

Frac. PL 0.80(11) 0.93(14) 0.91(18) 0.92(6) 0.93(3)

DISKBB+PL
$n_{\rm H}$ 0.12(4) 0.13(4) 0.22(9) 0.17(4) 0.84(4)

$kT_{\rm in}$ 1.8(4) 1.9(6) 1.5(4) 2.0(4) 1.19(6)

$\Gamma$ 3.6(7) 3.1(4) 4.1(7) 3.4(3) 3.9

$\chi ^2$ /d.o.f. 56/58 [0.54] 213/155 [1.3E-3] 62/58[0.33] 226/148[3.0E-5] 710/651 [0.05]

$L_{\rm0.3-10~ keV}$ 19(3) 33(25) 49(6) 53(5) 72(9)

Frac. PL 0.89(17) 0.6(7) 0.91(18) 0.93(11) 0.86(19)

**Table 3:** Fits to the spectra of NGC 300 X-1 from Obs. 1-4, and of IC 10 X-1. The first model is an absorbed power law plus Gaussian emission line, as favoured by Carpano et al. (2007a). For this model, we give absorption, normalised to 10²² H atom cm^-2, spectral index, line energy and width (in keV), and $\chi ^2$ /d.o.f., with good fit probability in square brackets. We only apply the Gaussian to NGC 300 X-1. We also give the 0.3-10 keV luminosity normalised to 10³⁷ erg s^-1. We next provide the best fits for a disk blackbody + power law model that is often used when describing the high state of disc-accreting BH XBs. We give the absorption, temperature of the disk blackbody, spectral index of the power law component and $\chi ^2$ . We then give 0.3-10 keV luminosity as before, and the fractional contribution of the power law model.
			NGC 300 X-1			IC 10 X-1
Model	Parameter	Obs. 1	Obs. 2	Obs. 3	Obs. 4
PL + Line	$n_{\rm H}$	0.036	0.067(12)	0.052(9)	0.07(2)	0.75(3)
	$\Gamma$	2.46(6)	2.44(7)	2.44	2.53(8)	2.56(6)
	$E_{\rm Line}$	0.95	0.93(2)	0.95(2)	0.95(2)	$\dots$
	$\sigma$	0.07	0.08(2)	0.07	0.06(3)	$\dots$
	$\chi ^2$ /d.o.f.	100/60 [9E-4]	149/154 [0.60]	50/60 [0.82]	117/145 [0.05]	794/652 [1E-4]
	$L_{\rm0.3-10~ keV}$	11.5(13)	28.4(12)	20(2)	34.8(16)	39(3)
BB+PL	$n_{\rm H}$	0.11(4)	0.130(12)	0.22(5)	0.17(3)	0.92(10)
	kT	1.02(14)	1.02(17)	0.92(12)	1.08(15)	0.82(3)
	$\Gamma$	3.41(6)	3.01(16)	3.8(3)	3.26(6)	3.9(5)
	$\chi ^2$ /d.o.f.	52/58 [0.67]	211/155 [2E-3]	59/58[0.43]	221/148[1.0E-4]	697/650 [0.09]
	$L_{\rm0.3-10~ keV}$	16.9(17)	39(2)	49(6)	59(3)	91(19)
	Frac. PL	0.80(11)	0.93(14)	0.91(18)	0.92(6)	0.93(3)
DISKBB+PL	$n_{\rm H}$	0.12(4)	0.13(4)	0.22(9)	0.17(4)	0.84(4)
	$kT_{\rm in}$	1.8(4)	1.9(6)	1.5(4)	2.0(4)	1.19(6)
	$\Gamma$	3.6(7)	3.1(4)	4.1(7)	3.4(3)	3.9
	$\chi ^2$ /d.o.f.	56/58 [0.54]	213/155 [1.3E-3]	62/58[0.33]	226/148[3.0E-5]	710/651 [0.05]
	$L_{\rm0.3-10~ keV}$	19(3)	33(25)	49(6)	53(5)	72(9)
	Frac. PL	0.89(17)	0.6(7)	0.91(18)	0.93(11)	0.86(19)

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