E-VLBI observations of a microquasar in outburst : Cygnus X-3
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e-VLBI observations of a microquasar in outburst : Cygnus X-3. 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).

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e-VLBI observations of a microquasar in outburst : Cygnus X-3

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)

Special acknowledgements : R. Campbell (JIVE) and C. Reynolds (JIVE)


Real-time VLBI: e-VLBI X-3

Data transferred in real-time over optical fibers


e-VLBI : the real thing ! X-3

enables very rapid access to the data

improves the decision making process wrt potential follow-ups

provides the ability to make informed decisions wrt the subsequent observations

avoids embarrassing situations…..


Oooops… X-3

Credit: A. Roy

5 km of tape (~1000 $) on Onsala control room floor due to incorrectly mounting on drive


5 GHz X-3

Cygnus X-3

d ~ 9 kpc

P = 4.8 h

compact object: unknown

companion : WN Wolf-Rayet

Marti et al. 2001

15 GHz

Miller-Jones et al. 2004

1997 Feb 6

1997 Feb 8

1997 Feb 11

Mioduszewski et al. 2001


First open call European e-VLBI observations* X-3

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

Cygnus X-3

X

2006 March 16 (dark Epoch)

V

2006 April 20 (Epoch I)

7 h

V

2006 May 18 (Epoch II)

12 h

*For the results of the e-VLBI observations of GRS 1915+105 see the poster by Rushton et al.


Mar 16 X-3

Apr 20

May 18

Epoch I

Epoch II

dark Epoch


Cygnus X-3 X-3

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

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


Cygnus X-3 X-3

Fractional linear polarization

Distribution of the electric vector PAs

Tudose et al., submitted


DEC (J2000) X-3

Size

(mas2)

PA

(degree)

Flux density

(mJy)

Epoch

RA (J2000)

Component

single

150 ± 2

17.5 ± 0.3 X 8.8 ± 0.5

87 ± 9

2006 April 20

20h32m25.771437s

+40°57'27''.92800

A

69 ± 13

23.2 ± 0.7 X 10.6 ± 2.5

20h32m25.771628s

+40°57'27''.96566

60 ± 6

2006 May 18

B

82 ± 22

38.4 ± 2.1 X 30.7 ± 8.1

748 ± 17

20h32m25.771051s

+40°57'27''.95621

101 ± 3

C

55 ± 7

19.4 ± 1.1 X 12.2 ± 2.3

20h32m25.771525s

+40°57'27''.93000

Data fitting

uv-plane fitting

Cygnus X-3


during Epoch I the core of X-3Cyg X-3 was quenched

Cygnus X-3

Gallo et al. 2003


Conclusions X-3

on Epoch I the core of Cyg X-3 was in deep quenching; 3s 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


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