The EVN in the context of microquasars and γ -ray binaries: future perspectives

1. The EVN in the context of microquasars and γ-ray binaries: future perspectives EVN 2015 Science Vision Josep Martí Dwingeloo, 2007 March 1

2. A decade ago, microquasars emerged as low-scaleaccessiblelaboratories for easily studying the same accretion and ejection phenomena in AGN.

3. A decade ago, microquasars emerged as low-scaleaccessible laboratories for easily studying the same accretion and ejection phenomena in AGN. • Significant progress achieved since then (e.g. quantitative scaling of X-ray / radio luminosity and black hole mass).

4. A decade ago, microquasars emerged as low-scale accessiblelaboratories for easily studying the same accretion and ejection phenomena in AGN. • Significant progress achieved since then (e.g. quantitative scaling of X-ray / radio luminosity and black hole mass). • But important problems remain yet to be understood and several of them have been revealed by previous VLBI observations (e.g. dark and radiatively inefficient flows evacuated by microquasar jets).

5. A decade ago, microquasars emerged as low-scale accessible laboratories for easily studying the same accretion and ejection phenomena in AGN. • Significant progress achieved since then (e.g. quantitative scaling of X-ray / radio luminosity and black hole mass). • But important problems remain yet to be understood and several of them have been revealed by previous VLBI observations (e.g. dark and radiatively inefficient flows evacuated by microquasar jets). • Today, microquasars and X-ray binaries in general are back again to the front line of astrophysical research in the context of high energy TeV gamma-ray sources detected by Cherenkov telescopes.

6. So far most VLBI work on microquasars has been devoted to bright sources either persistent or transient (e.g. Cygnus X-3, SS433, Cygnus X-1, GRS 1915+15, etc.).

7. Microquasar and γ-ray binary LS5039 Paredes et al. (2002) A&A 393, L99

8. Broad-band emission model of the microquasar LS5039 (Paredes et al. 2006).

9. So far most VLBI work on microquasars has been devoted to bright sources either persistent or transient (e.g. Cygnus X-3, SS433, Cygnus X-1, GRS 1915+15, etc.).

10. So far most VLBI work on microquasars has been devoted to bright sources either persistent or transient (e.g. Cygnus X-3, SS433, Cygnus X-1, GRS 1915+15, etc.). What can the future EVN do to contribute to this field?

11. What can the future EVN do to contribute to this field? • A more sensitive EVN could extend VLBI observations to most microquasars and other radio emitting X-ray binaries including fainter systems currently unexplored with milli-arcsecond resolution.

13. Each source is interesting by itself. Only 15 confirmed cases with resolved jets, but probably all REXBs are microquasars!

14. What the future EVN can do to contribute to this field? • A more sensitive EVN could extend VLBI observations to most microquasars and other radio emitting X-ray binaries including fainter systems currently unexplored with milli-arcsecond resolution.

15. What the future EVN can do to contribute to this field? • A more sensitive EVN could extend VLBI observations to most microquasars and other radio emitting X-ray binaries including fainter systems currently unexplored with milli-arcsecond resolution. • The EVN could play an important role at solving the nature of ‘gamma-ray binaries’ as revealed by Cherenkov arrays.

16. MAGIC H.E.S.S.

17. Pulsar Nebula AGN gal. unid SNR The VHE Sky – today 11 Galactic, 11 Extragalactic, GC, plus 15 unidentified not many sources ... but at least 7 source populations ! H1426 1ES 1218 Mrk421 M87 Mrk501 PSR B1259 1ES 1101 1ES1959 SNR G0.9 RXJ 1713 RXJ 0852 Crab Cas A LS 5039 TeV 2032 Vela X GC 1ES 2344 HESS J1303 Cygnus Diffuse MSH 15-52 PKS 2155 H2356 PKS 2005 gal. compact Galactic Center

18. LS5039 as a TeV source (Aharonian et al. 2005, Science).

19. Very recently, the MAGIC collaboration has reported another TeV microquasar, LS I +61 303, discovering a remarkable orbital variability (Albert et al. 2006, Science).

20. Two possible models for γ-ray X-ray binaries Figure from Mirabel (2006) Perspective in Science Microquasar model Pulsar model

21. VLBI evidence supporting the pulsar X-ray binary scenario for the γ-ray binary LSI+61303 Dhawan et al. (2006)

22. Other TeV sources where the EVN could help to identify the counterpart and understand its emission mechanism: the case of TeV J2032+4130

23. Other TeV sources where the EVN could help to identify the counterpart and understand its emission mechanism: the case of TeV J2032+4130 Paredes, Martí, et al. (2007) ApJ Letters

24. Other TeV sources where the EVN could help to identify the counterpart and understand its emission mechanism: the case of TeV J2032+4130 Paredes, Martí, et al. (2007) ApJ Letters

25. What the future EVN can do to contribute to this field? • A more sensitive EVN could extend VLBI observations to most microquasars and other radio emitting X-ray binaries including fainter systems currently unexplored with milli-arcsecond resolution. • The EVN could play an important role at solving the nature of ‘gamma-ray binaries’ as revealed by Cherenkov arrays.

26. What the future EVN can do to contribute to this field? • A more sensitive EVN could extend VLBI observations to most microquasars and other radio emitting X-ray binaries including fainter systems currently unexplored with milli-arcsecond resolution. • The EVN could play an important role at solving the nature of ‘gamma-ray binaries’ as revealed by Cherenkov arrays. • Provide the capability for a flexible VLBI observing strategy well adapted to the unpredictable flaring nature of these systems.

27. MRAO 15 GHz monitoring (Pooley 2006) + ASM First eVLBI imagesof Cygnus X-3 Tudose et al. (2006)

28. What the future EVN can do to contribute to this field? • A more sensitive EVN could extend VLBI observations to most microquasars and other radio emitting X-ray binaries including fainter systems currently unexplored with milli-arcsecond resolution. • The EVN could play an important role at solving the nature of ‘gamma-ray binaries’ as revealed by Cherenkov arrays. • Provide the capability for a flexible VLBI observing strategy well adapted to the unpredictable flaring nature of these systems.

29. Thank you!