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	Figure 1: Image of the binary 61 Cyg in Nov. 2002 obtained with MOS1. 61 Cyg A ( upper right) is near its coronal maximum in this exposure.
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In the text

	Figure 2: Examples of light curves (PN) that are used for data screening; upper row: onset ( left) and decay ( right) of activity during an observation, bottom: flares. Quasi-quiescent time intervals are marked by arrows. 61 Cyg B exhibits more frequent and stronger variability than 61 Cyg A during our observations.
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In the text

	Figure 3: X-ray light curves of 61 Cyg A and B from the ROSAT and XMM-Newton observation program.
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In the text

	Figure 4: 61 Cyg A: Mt. Wilson CaII H+K emission core measures (open circles) in combination with observations from Lowell Observatory(filled circles). The observations are transformed to the Mt. WilsonS index.
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In the text

	Figure 5: 61 Cyg B: for more details see Fig. 4.
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In the text

	Figure 6: 61 Cyg B: Fourier spectrum of the Ca H+K time-series depicted in Fig. 5.
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In the text

	Figure 7: Fourier spectra of 61 Cyg A. Top: CaHK between 1993 and 2005. Middle: CaHK data with a similar sampling as for the X-ray data. Bottom: X-ray data of ROSAT and XMM-Newton.
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In the text

	Figure 8: 61 Cyg A: comparison between chromospheric (open circles) and coronal activity (full dots). The continuous curves are least squares sine fits.
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In the text

	Figure 9: Fourier spectra of 61 Cyg B. Top: CaHK between 1993 and 2005. Middle: CaHK data with a similar sampling as for the X-ray data. Bottom: X-ray data of ROSAT and XMM-Newton.
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In the text

	Figure 10: 61 Cyg B: comparison between chromospheric (open circles) and coronal activity (full dots). The continuous curves are least squares second-order Fourier fits basing of the long-term chromospheric cycle of 11.2 yr.
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In the text