Discovery of crested quasi-periodic eruptions following the most luminous SRG/eROSITA tidal disruption event

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Table C.2.

Results of the double-blackbody time-resolved spectral modeling of the XMM-Newton dataset.

	Comp.	Δt	kT₁	L_bol, 1	R_BB, 1	kT₂	L_bol, 2	R_BB, 2
		[s]	[eV]	[10⁴³ erg/s]	[10¹¹ cm]	[eV]	[10⁴³ erg/s]	[10¹¹ cm]
E-1	a	414				92 ± 92	$0 . 03_{- 0.03}^{+ 1}$ $0.03^{+1}_{-0.03}$	0.2 ± 0.2
	b	378	$44_{- 9}^{+ 12}$ $44^{+12}_{-9}$	$2 . 56_{- 1.57}^{+ 3.31}$ $2.56^{+3.31}_{-1.57}$	7.4 ± 5
	c	540				$60_{- 28}^{+ 12}$ $60^{+12}_{-28}$	$3 . 66_{- 2.42}^{+ 8.04}$ $3.66^{+8.04}_{-2.42}$	4.7 ± 4.5
	d	648	57 ± 4	$2 . 61_{- 0.51}^{+ 0.62}$ $2.61^{+0.62}_{-0.51}$	4.3 ± 0.8
	e	1080	$44_{- 5}^{+ 6}$ $44^{+6}_{-5}$	$1 . 86_{- 0.68}^{+ 1}$ $1.86^{+1}_{-0.68}$	6.1 ± 2.1

F-1	a	693	$68_{- 10}^{+ 11}$ $68^{+11}_{-10}$	$0 . 61_{- 0.18}^{+ 0.25}$ $0.61^{+0.25}_{-0.18}$	1.5 ± 0.5

F-2	b	747	$58_{- 6}^{+ 7}$ $58^{+7}_{-6}$	$1 . 45_{- 0.36}^{+ 0.47}$ $1.45^{+0.47}_{-0.36}$	3.2 ± 0.8

E-2	a	189				$208_{- 23}^{+ 25}$ $208^{+25}_{-23}$	$1 . 19_{- 0.2}^{+ 0.24}$ $1.19^{+0.24}_{-0.2}$	0.2 ± 0.1
	b	237	$80_{- 17}^{+ 23}$ $80^{+23}_{-17}$	$0 . 55_{- 0.21}^{+ 0.32}$ $0.55^{+0.32}_{-0.21}$	1 ± 0.6
	c	329				$110_{- 7}^{+ 8}$ $110^{+8}_{-7}$	$2 . 21_{- 0.29}^{+ 0.35}$ $2.21^{+0.35}_{-0.29}$	1.1 ± 0.2
	d	306	71 ± 7	$2 . 39_{- 0.47}^{+ 0.54}$ $2.39^{+0.54}_{-0.47}$	2.7 ± 0.6
	e	252				$98_{- 11}^{+ 13}$ $98^{+13}_{-11}$	$1 . 41_{- 0.35}^{+ 0.45}$ $1.41^{+0.45}_{-0.35}$	1.1 ± 0.3
	f	738	64 ± 4	$1 . 31_{- 0.21}^{+ 0.23}$ $1.31^{+0.23}_{-0.21}$	2.5 ± 0.4
	g	739	$56_{- 6}^{+ 7}$ $56^{+7}_{-6}$	$1 . 01_{- 0.3}^{+ 0.44}$ $1.01^{+0.44}_{-0.3}$	2.8 ± 0.8

E-3	a	110				$381_{- 223}^{+ 688}$ $381^{+688}_{-223}$	$0 . 2_{- 0.1}^{+ 0.3}$ $0.2^{+0.3}_{-0.1}$	< 0.1
	b	356	$105_{- 10}^{+ 12}$ $105^{+12}_{-10}$	0.99 ± 0.13	0.8 ± 0.2

Notes. The second blackbody is used to model the narrow flares. In coincidence with the narrow flares, the blackbody accounting for the broad flare is constrained to vary between the minima and maxima parameter values derived for the bare broad flares. It can be seen by the large uncertainties that certain epochs reject the addition of the second blackbody component (e.g., E-1 a)

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