Table 9: Parameters for representative models in agreement with the IQ (IQ1-IQ4) and flare states (F1 and F2) observed towards Sgr A*. These models are plotted in Figs. 16 and 17. The NIR flux density contributions from the synchrotron and SSC part of the spectrum as well as the SSC X-ray flux density are listed (Cols. 2 to 4). In the following columns we list the magnetic field strength B, observed cutoff frequency $\nu _{\rm m, obs}$ and flux density $S_{\rm m, obs}$ of the synchrotron spectrum, size $\theta$ of the source component and the spectral index $\alpha$ of the synchrotron component. All models except IQ2 provide synchrotron emission for frequencies up to $\nu _2 \sim 200$ THz. We assume that the cutoff in the energy spectrum of the relativistic electrons can be represented via an exponential cutoff in the observed synchrotron spectrum proportional to $\exp[-(\nu/\nu_0)^{0.5}]$ with the effective cutoff frequency $\nu _0$ . In the first column the NIR flux densities are given without (in brackets) and with modulation by the exponential cutoff.
model $S_{\rm NIR}$ $S_{\rm NIR}$ $S_{\rm X-ray}$ B $\nu$ $_{\rm max,obs}$ $S_{\rm max,obs}$ size $\alpha$ $_{\rm NIR/X-ray}$ $c/\nu$ ₀

ID synchr. SSC

(mJy) (mJy) (nJy) (G) (GHz) (Jy) ( $\mu$ as) ( $\mu$ m)

IQ1 0.8 2.0 <18 17 820 3.9 7.9 1.3 -

IQ2 - 3.0 <27 5 820 7.7 8.1 1.3 -

IQ3 (25)1 0.1 <17 80 1000 16.0 17.5 1.0 15

IQ4 2.0 0.02 <15 38 1500 0.33 1.5 0.8 -

F1 (18) 6 1.13 65 68 1640 11.5 8.5 1.1 5

F2 (300) 6 0.1 230 100 1640 5.7 8.5 0.4 90

**Table 9:** Parameters for representative models in agreement with the IQ (IQ1-IQ4) and flare states (F1 and F2) observed towards Sgr A*. These models are plotted in Figs. 16 and 17. The NIR flux density contributions from the synchrotron and SSC part of the spectrum as well as the SSC X-ray flux density are listed (Cols. 2 to 4). In the following columns we list the magnetic field strength B, observed cutoff frequency $\nu _{\rm m, obs}$ and flux density $S_{\rm m, obs}$ of the synchrotron spectrum, size $\theta$ of the source component and the spectral index $\alpha$ of the synchrotron component. All models except IQ2 provide synchrotron emission for frequencies up to $\nu _2 \sim 200$ THz. We assume that the cutoff in the energy spectrum of the relativistic electrons can be represented via an exponential cutoff in the observed synchrotron spectrum proportional to $\exp[-(\nu/\nu_0)^{0.5}]$ with the effective cutoff frequency $\nu _0$ . In the first column the NIR flux densities are given without (in brackets) and with modulation by the exponential cutoff.
model	$S_{\rm NIR}$	$S_{\rm NIR}$	$S_{\rm X-ray}$	B	$\nu$ $_{\rm max,obs}$	$S_{\rm max,obs}$	size	$\alpha$ $_{\rm NIR/X-ray}$	$c/\nu$ ₀
ID	synchr.	SSC
	(mJy)	(mJy)	(nJy)	(G)	(GHz)	(Jy)	( $\mu$ as)		( $\mu$ m)
IQ1	0.8	2.0	<18	17	820	3.9	7.9	1.3	-
IQ2	-	3.0	<27	5	820	7.7	8.1	1.3	-
IQ3	(25)1	0.1	<17	80	1000	16.0	17.5	1.0	15
IQ4	2.0	0.02	<15	38	1500	0.33	1.5	0.8	-
F1	(18) 6	1.13	65	68	1640	11.5	8.5	1.1	5
F2	(300) 6	0.1	230	100	1640	5.7	8.5	0.4	90

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