1. V. Tudose (UvA, AIRA), R. Fender (Soton, UvA), M. Garrett (JIVE), J. Miller-Jones (UvA), Z. Paragi (JIVE), R. Spencer (Jodrell), G. Pooley (Cambridge), M. van der Klis (UvA), A. Szomoru (JIVE) e-VLBI observations of a microquasar in outburst : Cygnus X-3 Special acknowledgements : R. Campbell (JIVE) and C. Reynolds (JIVE)

2. Real-time VLBI: e-VLBI Data transferred in real-time over optical fibers

3. e-VLBI : the real thing ! e-VLBI : the real thing ! enables very rapid access to the data provides the ability to make informed decisions wrt the subsequent observations improves the decision making process wrt potential follow-ups avoids embarrassing situations…..

4. 5 km of tape (~1000 $) on Onsala control room floor due to incorrectly mounting on drive Credit: A. Roy Oooops…

5. Marti et al. 2001 Cygnus X-3 1997 Feb 61997 Feb 81997 Feb 11 Mioduszewski et al. 2001 Miller-Jones et al. 2004 15 GHz 5 GHz d ~ 9 kpc P = 4.8 h compact object: unknown companion : WN Wolf-Rayet

6. First open call European e-VLBI observations* 2006 March 16 (dark Epoch) 2006 April 20 (Epoch I) 2006 May 18 (Epoch II) Cygnus X-3 V X V 6 antennae : Onsala (SW), Torun (PL), Jodrell Bank (UK), Cambridge (UK), Medicina (IT) and Westerbork (NL) frequency : 5 GHz (6 cm) transfer rate : 128 Mbit/s 7 h 12 h *For the results of the e-VLBI observations of GRS 1915+105 see the poster by Rushton et al.

7. Mar 16Apr 20May 18 Epoch IEpoch II dark Epoch

8. Tudose et al., submitted peak flux : 3.4 mJy/beam rms noise : 0.03 mJy/beam contour levels: (-15,15,25,35,45,55,65,75,85,95) x rms Cygnus X-3 peak flux : 18.2 mJy/beam rms noise : 0.2 mJy/beam contour levels: (-15,15,25,35,45,55,65,75,85,95) x rms

9. Tudose et al., submitted Cygnus X-3 Distribution of the electric vector PAs Fractional linear polarization

10. 2006 April 20 Epoch 101 ± 3 748 ± 17 150 ± 2 60 ± 6 87 ± 9 17.5 ± 0.3 X 8.8 ± 0.5 Flux density (mJy) PA (degree) Size (mas 2 ) 2006 May 18 Component single A B C RA (J2000) DEC (J2000) 20h32m25.771437s 20h32m25.771628s 20h32m25.771051s 20h32m25.771525s +40°57'27''.92800 +40°57'27''.96566 +40°57'27''.95621 +40°57'27''.93000 23.2 ± 0.7 X 10.6 ± 2.5 38.4 ± 2.1 X 30.7 ± 8.1 19.4 ± 1.1 X 12.2 ± 2.3 69 ± 13 82 ± 22 55 ± 7 Data fitting uv-plane fitting Cygnus X-3

11. Gallo et al. 2003 during Epoch I the core of Cyg X-3 was quenched Cygnus X-3

12. Conclusions on Epoch I the core of Cyg X-3 was in deep quenching; 3  upper limit to the flux density is 0.4 mJy on Epoch II almost 40 % of the radio emission of Cyg X-3 at large scale is missing at e-VLBI scale evidence in Cyg X-3 for interaction of the jet with the surrounding medium e-VLBI will ultimately improve our knowledge of transient sources