The origin of the X-ray luminosity of the green pea galaxies: X-ray binaries or active galactic nuclei?

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Table 2.

Measured physical properties of GPs with X-ray detections.

Source	X-ray	F_X(0.5 − 8 keV)⁽¹⁾	log(L_X(0.5 − 8 keV)) ⁽¹⁾	log(L_X(2 − 10 keV))⁽¹⁾	log(SFR)	SFR	12 + log(O/H)	Metal	log(M_⋆) ⁽²⁾	Age⁽²⁾	BPT
	survey	10⁻¹⁴ erg s⁻¹ cm⁻²	(erg s⁻¹)	(erg s⁻¹)	M_⊙ yr⁻¹	source		method	log(M_⊙)	(Gyr)
J1330-0043	XMM-Newton	0.18 ± 0.06	$41 . 94_{- 0.16}^{+ 0.12}$ $41.94^{+0.12}_{-0.16}$	$42 . 33_{- 0.16}^{+ 0.12}$ $42.33^{+0.12}_{-0.16}$	$0 . 27_{- 0.05}^{+ 0.04}$ $0.27^{+0.04}_{-0.05}$	SED	8.63±0.22	O3N2	9.91 ± 0.02	1.5	SF
J0035+0431	XMM-Newton	1.04 ± 0.26	$42 . 26_{- 0.12}^{+ 0.10}$ $42.26^{+0.10}_{-0.12}$	$42 . 65_{- 0.12}^{+ 0.10}$ $42.65^{+0.10}_{-0.12}$	$0 . 34_{- 0.03}^{+ 0.02}$ $0.34^{+0.02}_{-0.03}$	SED	7.88±0.30	R23	10.22 ± 0.02	1.0	–
J0205+1504	Swift	16.83 ± 6.73	$43 . 51_{- 0.22}^{+ 0.15}$ $43.51^{+0.15}_{-0.22}$	$43 . 90_{- 0.22}^{+ 0.15}$ $43.90^{+0.15}_{-0.22}$	0.62 ± 0.02	SED	8.51 ± 0.35	O3N2	9.49 ± 0.02	0.8	SF
J0227+2355	Swift	$1 . 21_{- 0.31}^{+ 0.36}$ $1.21^{+0.36}_{-0.31}$	$42 . 40_{- 0.13}^{+ 0.11}$ $42.40^{+0.11}_{-0.13}$	$42 . 80_{- 0.13}^{+ 0.11}$ $42.80^{+0.11}_{-0.13}$	0.42 ± 0.02	SED	8.91 ± 0.15	SB98⁽³⁾	10.05 ± 0.02	4.0	AGN
J1605+4405	Chandra	$3 . 03_{- 0.89}^{+ 0.84}$ $3.03^{+0.84}_{-0.89}$	$43 . 02_{- 0.15}^{+ 0.11}$ $43.02^{+0.11}_{-0.15}$	$43 . 41_{- 0.15}^{+ 0.10}$ $43.41^{+0.10}_{-0.15}$	1.05 ± 0.02	SED	8.63 ± 0.04	SB98⁽³⁾	10.51 ± 0.02	1.8	AGN
J0906+0242	eROSITA	5.52 ± 2.18	$43 . 10_{- 0.22}^{+ 0.14}$ $43.10^{+0.14}_{-0.22}$	$43 . 49_{- 0.22}^{+ 0.14}$ $43.49^{+0.14}_{-0.22}$	0.21 ± 0.02	SED	8.42±0.08	O3N2	9.59 ± 0.02	1.0	SF

J0749+3337	XMM-Newton	0.5±0.15	$42 . 08_{- 0.18}^{+ 0.12}$ $42.08^{+0.12}_{-0.18}$	< 41.42	1.77	NUV+W4	8.3	O3N2	9.8	–	SF
J0822+2241	XMM-Newton	$0 . 8_{- 0.15}^{+ 0.18}$ $0.8 ^{+0.18}_{-0.15}$	$42 . 08_{- 0.12}^{+ 0.07}$ $42.08^{+0.07}_{-0.12}$	$41 . 79_{- 0.30}^{+ 0.25}$ $41.79^{+0.25}_{-0.30}$	1.57	NUV+W4	8.1	O3N2	9.6	–	SF
J1339+1516	XMM-Newton	–	< 41.11	–	1.27	NUV+W4	8.1	O3N2	9.3	–	SF

Notes. ⁽¹⁾The X-ray flux and the luminosity in 0.5–8 keV band, as well as the X-ray luminosity in 2–10 keV band, are measured in the rest frame, assuming Γ = 2.0.

⁽²⁾The stellar mass and age are obtained based on the CIGALE fitting result.

⁽³⁾ The metallicities for the sources that are classified as AGNs from the BPT diagram (see Fig. 4) were determined using the method from Storchi-Bergmann et al. (1998).

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