1. Isolating the jet in broadband spectra of XBs Dave Russell niversity of Amsterdam In collaboration with: Fraser Lewis, Dipankar Maitra, Robert Dunn, Sera Markoff, James Miller-Jones, Kieran O’Brien, Piergiorgio Casella, Peter Jonker, Jeroen Homan, Manuel Linares, Rob Fender, Elena Gallo, Valeriu Tudose 12 th October 2010

2. Radio emission:  is synchrotron in nature  unambiguously originates in collimated outflows (2 types of jet) RadioX-ray? The spectrum of a steady, hard state jet (to zeroth order): Turnover  log Optically thickOptically thin X-ray Binary Jets The jets are radiatively inefficient, and the power carried in the jets is uncertain and highly dependent on the position of the turnover/break(s) Does the turnover change with luminosity; how does the jet spectrum evolve during transitions? Black hole XB: GRO J1655-40 Tingay et al. 1995 Neutron star XB: Sco X-1 Fomalont et al. 2001 The turnover also helps constrain the synchrotron contribution to X-ray

3.  Optical outburst light curves and spectra similar to dwarf novae  disc Can we see the jet at higher energies?  Actually, the X-ray heated disc tends to dominate over the viscous disc (reprocessing) Kuulkers 1998 Hynes et al. 2002 (XTE J1859+226) Courtesy of Kieran O'Brien Well…

4. In the last decade evidence shows that:  the jet is sometimes visible in optical and NIR But wait… Mirabel et al. (1998) showed NIR flares from GRS 1915+105 (found by Fender et al. 1997) originate in the jets

5. In the last decade evidence shows that:  the jet is sometimes visible in optical and NIR  the turnover in the jet spectrum probably lies somewhere in the IR But wait… Homan et al. (2005) showed NIR emission from GX 339-4 has negative spectral index in the hard state, and is quenched in the soft state Corbel & Fender 2002 Data from Homan et al. 2005, Jain et al. 2001, Buxton & Bailyn 2004 > 90%  of flux is from the jet in the brightest hard state

6. Multi-wavelength monitoring of GX 339-4 F. Lewis et al. in prep, F. Lewis PhD thesis

7. Time resolution typically ~100 sec Multi-wavelength monitoring of GX 339-4 High amplitude variability on short timescales: monitoring the flickering See also P. Casella’s talk, next! Infrared SEDs from the VLT: We can infer the average SED by taking lots of data over long timescales “its like taking a simultaneous 2-month long exposure”

8. So where is the jet break? Not clear in GX 339-4 SEDs Hynes et al. 2006 had simultaneous NIR J,H,K observations of XTE J1118+480 They found the NIR to be consistent with optically thin synchrotron

9. So where is the jet break? Not clear in GX 339-4 SEDs Hynes et al. 2006 had simultaneous NIR J,H,K observations of XTE J1118+480 They found the NIR to be consistent with optically thin synchrotron Jet break must reside in the mid-IR Very few mid-IR data of LMXBs in outburst exist in the literature See also Migliari et al. 2006, 2007, 2010: Spitzer 4 – 24 micron detections of the BH GRO J1655-40 and the NS 4U 0614+091 Our team have approved time on the VLT with VISIR – the first data came in this summer 8 – 12 micron imaging 10-micron detections van Paradijs et al. 1994  50 mJy! Probably jet?

10. The jet is not there  Russell et al. in prep. Data of GX 339-4 during a state transition, type B QPO seen (P. Casella) – soft intermediate state Some of the first mid-IR data of outbursting LMXBs

11. VLT VISIR Data of XTE J1752-223 during the hard state decline of its 2009 – 2010 outburst (EVLA radio data courtesy of J. Miller-Jones, P. Jonker, ATel #2278, NIR also from ATel #2268) Some of the first mid-IR data of outbursting LMXBs

12. What about neutron stars? Migliari et al. 2010 identify the jet break in 4U 0614+091: In the mid-IR: between 8 and 24 microns

13. What about neutron stars? Optical, NIR, UV and X-ray monitoring of the 2008 double-peaked outburst of IGR J00291+5934 Lewis, Russell, Jonker, Linares, et al. 2010, A&A, 517, A72

14. What about neutron stars? Optical, NIR, UV and X-ray monitoring of the 2008 double-peaked outburst of IGR J00291+5934 Lewis, Russell, Jonker, Linares, et al. 2010, A&A, 517, A72 Jet break around the H-band? (1.6 microns)

15. Optical & infrared data published in Jain et al. 2001; radio in Corbel et al. 2001 X-ray analysis as in Dunn et al. 2010 Introducing the 2000 outburst of XTE J1550-564 Well monitored in X-ray, optical and near-infrared (NIR) We can separate disc and jet emission Assumes continuation of the exponential decay of disc flux Jet has optically thin spectrum

16. Russell, Maccarone, Körding & Homan 2007 Could it be a synchrotron jet dominating X-ray? NIR jet flux is proportional to X-ray flux Variability info: Kalemci et al. 2001, Kalemci’s talk at IAU Symposium, Buenos Aires 2010 Russell, Maitra, Dunn & Markoff 2010, MNRAS, 405, 1759 α (NIR  optical) ~ -0.7 α (optical  X-ray) = -0.7 α (X-ray power law) = -0.7 (photon index = 1.7) α (X-ray power law before) = -0.6 A single power law decreasing in flux by a factor of ten Markoff, Falcke & Fender 2001 XTE J1118+480

17. Fender, Gallo & Jonker 2003: Energetics are jet dominated at low luminosities in the hard state A possible revised picture for BH outbursts Jet could dominate X-ray flux in the hard state between Dunn et al. 2010: 60% of BH outbursts show this softening on the hard state decay Is the jet the reason for the softening?

19. Multi-wavelength monitoring of GX 339-4 Extinction plays a massive role in optical-UV SEDs F. Lewis et al. in prep, F. Lewis PhD thesis