1. High-resolution observations of X-ray Binaries
James Miller-Jones
(NRAO, Charlottesville)

2. X-ray binaries

3. Comparison to AGN Closer Less massive Smaller sample size
Proper motion studies
Parallactic distances
Less massive
Less angular resolution (rSch/d = 2GMBH/c2d)
Increased time resolution (t a MBH)
Smaller sample size
Study individual objects rather than large samples

4. What can you do with VLBI?
Astrometry:
Distances (via parallax)
Proper motions
Imaging:
Observe real-time jet evolution
Resolve jet morphology

5. Astrometry: LSI +61o303
Dhawan, Mioduszewski & Rupen (2006)

6. Astrometry: Parallaxes
Source
Parallax (mas)
Distance (kpc)
Reference
Sco X-1
0.36 ± 0.04
2.8 ± 0.3
Bradshaw et al. (1999)
Cyg X-1
0.73 ± 0.30
Lestrade et al. (1999)
Requires persistent, unresolved source
Model-independent distances
Distance needed for other quantities
Bradshaw et al. (1999)

7. Astrometry: kinematics
Source
Peculiar
velocity (km/s)
GRO J
420 ± 53
Sco X-1
286 ± 18
XTE J
159 ± 25
V404 Cyg
84 ± 83
GRS
53 ± 68
Cyg X-1
37 ± 28
LSI
22 ± 2
Grimm, Gilfanov & Sunyaev (2002)

8. Astrometry: kinematics (cont’d)
GRO J (HST): formed in the disk, large natal kick, now on eccentric orbit
XTE J : high velocity system in eccentric orbit, probably formed in the halo
Sco X-1: eccentric orbit similar to globular clusters
GRS : peculiar velocity due to scattering off spiral arms
Cygnus X-1: formed with no energetic SN
LSI +61o303: lost only ~1MO in SN, received asymmetric kick

9. Galactic dynamics: XTE J1118+480

10. Real-time evolution of jets: SS 433
Precessing, antiparallel jets moving at 0.26c
Inflate W50 nebula
Dubner et al. (1998)
Hjellming & Johnston (1981)

11. Real-time evolution of jets: SS 433
162.5 day precession cycle
Knots move ballistically outwards at 0.26c
Nodding motion superposed on precession

12. Equatorial emission in SS 433
Disc wind
High mass loss rate
Blundell et al. (2001)

13. Real-time evolution of jets
Mioduszewski, Rupen, Walker & Taylor (2004)

14. 2 flavours of jets Mirabel & Rodriguez (1994) Fender et al. (1999)
Dhawan et al. (2000)

15. State diagram for black holes (aka “the turtle head”)

16. Jet properties in the hard state
Non-linear Radio/X-ray correlation
LR a LX0.7
Persists up to ~0.02 Ledd
Self-absorbed flat-spectrum jets
Gallo (2007)

17. Jet properties in the hard state
GRS
LX ~ LEdd
Resolved jet
Gallo (2007)
Dhawan et al. (2000)

18. Jet properties in the hard state
Cygnus X-1
LX ~ 0.02 LEdd
Resolved jet
Gallo (2007)
Stirling et al. (2001)

19. Jet properties in the hard state
V404 Cyg
LX ~ 5x10-6 LEdd
Unresolved ?
Gallo (2007)
Miller-Jones et al. (submitted)

20. Jet properties in the hard state
Quiescent properties
Collimation?
Speeds?
Energetics?
Scaling with m
Higher sensitivity! ? .
Gallo (2007)

21. Neutron stars Intrinsically fainter than BH
Also produce resolved, highly relativistic jets
Migliari & Fender(2006)

22. Neutron stars
Fender et al. (2004)
Fomalont et al. (2001)

23. White dwarfs – RS Oph Recurrent nova
White dwarf accretes from red giant wind
Thermonuclear runaway every ~20y
RG atmosphere shapes ejected material
Radio emission from shocks
Credit: David Hardy/PPARC

24. White dwarfs – RS Oph

25. White dwarfs – RS Oph 6 cm 18 cm
Rupen, Mioduszewski & Sokoloski (2008)
O’Brien et al. (2006)

26. eVLBI: Rapid Response Science
Sources vary on timescales of days
Traditional disk-based VLBI can take weeks to correlate
Impossible to make decisions on follow-up observations
Transfer data over the internet
Correlate in real time
Enables refinement of observing strategy based on actual data

27. eVLBI: Rapid Response Science
eEVN
Phased WSRT, Cambridge, Jodrell Mk II, Medicina, Onsala, Torun
128 Mbps
Due for upgrade to 1Gbps
Southern hemisphere eVLBI
Phased ATCA, Parkes, Mopra, Hobart
1Gbps/155Mbps

28. eVLBI: Rapid Response Science
Tudose et al. (2006):
5-GHz eEVN imaging of Cygnus X-3

29. eVLBI: Rapid Response Science
Phillips et al. (2007):
1.6-GHz eVLBI imaging of Cir X-1
Rushton et al. (2007):
5-GHz eEVN imaging of GRS

30. Future developments Upgrade VLBA to 4Gbps by 2011
16Gbps within a decade?
10mJy/beam in 8h
Better than the HSA for astrometry
<10mas astrometry on a 1mJy source
Scalable software correlator
22GHz receiver system already upgraded
Further possible receiver upgrades (4-8 GHz)

31. Future developments Improved instantaneous sensitivity
Time-resolved lightcurves
Probe nature of quiescent state
Track moving components on ~1h timescales
Closer calibrators (possibly in-beam)
Observe neutron star systems
Typically a factor 30 fainter than black holes
Resolve hard/quiescent state jets
How do jet parameters vary with m?
Jet power/length/collimation .

32. Future developments High frequency observations with good sensitivity
Beat scattering
Extra resolution
How does t=1 surface move with frequency?
<10mas astrometry
Accurate parallactic distances to all Galactic XRBs
Resolve orbits of shorter-period systems
Wider bandwidth gives potential for MFS

33. Conclusions
High-resolution observations are crucial in furthering our understanding of X-ray binaries
Only way to probe jet morphologies
Astrometry crucial in tying down the fundamental parameters of these systems
Upgrades to existing instruments will make much more possible within the next few years
Take advantage of the wonderful facilities available!

34. Thank you, and goodnight…
Thanks to the organisers for a wonderful conference!
Have a safe journey home!