Table 6: The radio power of our sample for continuous emission and flares. The radio detections in M 82 are probably SNRs while in NGC 4736 we probably detect the nucleus of the galaxy. For all other sources we present upper limits for continuous emission over all epochs and flares. The distances are taken from Tully (1988).
Name Dist. $L_{\rm X}$ $L_{\rm R,flare}$ $L_{\rm R,cont}$

[Mpc] $[10^{39}~ {\mbox{erg}~{\rm s}^{-1}}]$ $[ 10^{33} ~{\mbox{erg}~{\rm s}^{-1}}]$ $[ 10^{33} ~{\mbox{erg}~{\rm s}^{-1}}]$

M 33 0.7 1 <0.43 <0.2

NGC 2403 4.2 2 <13 <5.4

M 82-D 5.2 3 <45 290

M 82-F 5.2 6 <45 307

NGC 4736-1 4.3 1 <21 177

NGC 4736-2 4.3 1 <21 <9.2

NGC 5204 4.8 2 <18 <7.1

NGC 5457-1 5.4 2 <23 <9.1

NGC 5457-2 5.4 1 <23 <9.1

**Table 6:** The radio power of our sample for continuous emission and flares. The radio detections in M 82 are probably SNRs while in NGC 4736 we probably detect the nucleus of the galaxy. For all other sources we present upper limits for continuous emission over all epochs and flares. The distances are taken from Tully (1988).
Name	Dist.	$L_{\rm X}$	$L_{\rm R,flare}$	$L_{\rm R,cont}$
	[Mpc]	$[10^{39}~ {\mbox{erg}~{\rm s}^{-1}}]$	$[ 10^{33} ~{\mbox{erg}~{\rm s}^{-1}}]$	$[ 10^{33} ~{\mbox{erg}~{\rm s}^{-1}}]$
M 33	0.7	1	<0.43	<0.2
NGC 2403	4.2	2	<13	<5.4
M 82-D	5.2	3	<45	290
M 82-F	5.2	6	<45	307
NGC 4736-1	4.3	1	<21	177
NGC 4736-2	4.3	1	<21	<9.2
NGC 5204	4.8	2	<18	<7.1
NGC 5457-1	5.4	2	<23	<9.1
NGC 5457-2	5.4	1	<23	<9.1

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations
	3 Observational results
	4 Theoretical interpretations
	5 Conclusions
	Appendix A: The LLAGN in NGC 4736
	References