Characterisation of the X-ray point source variability in the eROSITA south ecliptic pole field

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Table 2

Properties of the brightest variable likely extragalactic sources.

Variable source	z	∑ C_S	N_b	$\bar{{N E V}_{b}}$ $\[\overline{\mathrm{NEV}_{\mathrm{b}}}\]$ (10⁻³)	ν_min (10⁻⁸ Hz)	α
eRASSt J061148.4-662435	0.230^(a)	45328	702	${2.66}_{- 0.56}^{+ 0.96}$ $\[2.66_{-0.56}^{+0.96}\]$	24.7	1.210 ± 0.053
eRASSt J054641.8-641524	0.323^(b)	19343	465	${4.3}_{- 1.1}^{+ 2.2}$ $\[4.3_{-1.1}^{+2.2}\]$	42.1	1.179 ± 0.056
eRASSt J055943.0-660909	0.547	13419	2766	${13.1}_{- 2.3}^{+ 6.2}$ $\[13.1_{-2.3}^{+6.2}\]$	6.2	0.912 ± 0.024
eRASSt J061504.1-661717	0.178	10490	520	$80_{- 33}^{+ 61}$ $\[80_{-33}^{+61}\]$	34.0	1.268 ± 0.059
eRASSt J055357.6-665003	0.311	10420	1628	${10.6}_{- 2.0}^{+ 5.3}$ $\[10.6_{-2.0}^{+5.3}\]$	14.8	0.963 ± 0.034
eRASSt J055033.4-663653	0.0752^(c)	9898	1070	$20_{- 5}^{+ 11}$ $\[20_{-5}^{+11}\]$	21.2	1.043 ± 0.039
eRASSt J061543.9-653153	0.227^(b)	7261	361	$41_{- 15}^{+ 28}$ $\[41_{-15}^{+28}\]$	50.7	1.142 ± 0.067
eRASSt J060420.2-670234	0.678	5401	1858	${14.2}_{- 2.8}^{+ 9.5}$ $\[14.2_{-2.8}^{+9.5}\]$	13.0	0.862 ± 0.038
eRASSt J055934.5-653833	0.297	5191	1103	${12.1}_{- 2.8}^{+ 8.1}$ $\[12.1_{-2.8}^{+8.1}\]$	20.7	0.905 ± 0.046
eRASSt J060534.6-640045		4836	296	${5.3}_{- 1.8}^{+ 4.3}$ $\[5.3_{-1.8}^{+4.3}\]$	60.4	1.190 ± 0.094
eRASSt J054913.6-642931	0.317	4514	514	${9.5}_{- 2.7}^{+ 7.5}$ $\[9.5_{-2.7}^{+7.5}\]$	37.1	0.977 ± 0.073
eRASSt J054334.4-642300		4484	447	${12.9}_{- 4.0}^{+ 9.9}$ $\[12.9_{-4.0}^{+9.9}\]$	39.7	1.166 ± 0.059
eRASSt J060139.2-655756	0.603	3612	1620	$16_{- 4}^{+ 13}$ $\[16_{-4}^{+13}\]$	7.8	0.955 ± 0.027
eRASSt J055801.4-665655	0.23	3305	2523	$22_{- 5}^{+ 20}$ $\[22_{-5}^{+20}\]$	9.4	0.774 ± 0.035
eRASSt J055745.4-664453	0.224	3230	3117	$29_{- 7}^{+ 25}$ $\[29_{-7}^{+25}\]$	6.2	0.619 ± 0.054
eRASSt J055333.8-665751	0.121	3221	1100	$20_{- 5}^{+ 39}$ $\[20_{-5}^{+39}\]$	19.0	0.934 ± 0.022
eRASSt J054750.3-672803	1.01^(d)	2895	488	${9.5}_{- 2.8}^{+ 8.5}$ $\[9.5_{-2.8}^{+8.5}\]$	40.4	0.681 ± 0.093
eRASSt J055419.9-663340	0.251	2829	2402	$26_{- 6}^{+ 73}$ $\[26_{-6}^{+73}\]$	6.4	0.853 ± 0.030
eRASSt J061932.9-645955	0.255	2396	269	$11_{- 4}^{+ 12}$ $\[11_{-4}^{+12}\]$	66.8	0.79 ± 0.11
eRASSt J053423.0-652004		2047	388	$27_{- 10}^{+ 28}$ $\[27_{-10}^{+28}\]$	45.4	1.184 ± 0.082
eRASSt J060528.6-652008	0.478	1812	548	$14_{- 4}^{+ 14}$ $\[14_{-4}^{+14}\]$	33.7	0.611 ± 0.082
eRASSt J055454.3-653829		1579	1133	$23_{- 6}^{+ 29}$ $\[23_{-6}^{+29}\]$	14.9	0.831 ± 0.043
eRASSt J055831.6-663948	0.328	1380	3118	$34_{- 8}^{+ 76}$ $\[34_{-8}^{+76}\]$	6.2	0.744 ± 0.040
eRASSt J055927.9-662926		1374	1053	$26_{- 7}^{+ 32}$ $\[26_{-7}^{+32}\]$	19.4	0.611 ± 0.068
eRASSt J054831.4-664259	0.116	1350	786	$21_{- 6}^{+ 29}$ $\[21_{-6}^{+29}\]$	28.0	0.809 ± 0.068
eRASSt J060221.4-671025	0.426	1345	1720	$26_{- 6}^{+ 33}$ $\[26_{-6}^{+33}\]$	16.3	0.576 ± 0.056
eRASSt J060119.3-662918		1258	3117	$70_{- 21}^{+ 150}$ $\[70_{-21}^{+150}\]$	6.2	0.948 ± 0.032
eRASSt J061134.3-674708	0.376	1127	721	$18_{- 5}^{+ 27}$ $\[18_{-5}^{+27}\]$	32.6	0.896 ± 0.065

Notes. This table contains the variable likely extragalactic sources with at least 10³ background-subtracted source counts observed by eROSITA in eRASS1, 2, and 3 in the SEP field. It lists the redshift, z, the total background-subtracted source counts in eRASS:3 (∑ C_S), and the number of bins with ε > 0.1 in eRASS:3. The sources are sorted by the number of total background-subtracted source counts observed. The table also lists the geometric mean NEV_b, for 20 bin segments in the light curve. The associated error includes both measurement and sampling errors. Finally, the table also describes the best fit properties of the periodograms of these sources. It lists the minimum frequency (ν_min) for which the power was determined, and the best fitting power law index, α, when fitting the periodograms with a single aliased power law model. The maximum frequency probed in all of these periodograms is 6.94 × 10⁻⁵ Hz. Most redshifts were determined from AAT spectroscopy. We also included the redshifts found from previous analyses of matched optical counterparts, for sources that were not observed by the AAT. These redshifts are denoted with letters as superscripts; ^(a)Masetti et al. (2008), ^(b)Barkhouse & Hall (2001), ^(c)Hewitt & Burbidge (1991), and ^(d)Geha et al. (2003). The redshift of eRASSt J055357.6-665003 was also measured by Kim et al. (2012), who measured it to be 0.32.

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