Isolating the jet in broadband spectra of XBs

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 12th October 2010

2. X-ray Binary Jets Black hole XB: GRO J1655-40 Tingay et al. 1995 Neutron star XB: Sco X-1 Fomalont et al. 2001 Radio emission:  is synchrotron in nature  unambiguously originates in collimated outflows (2 types of jet) The spectrum of a steady, hard state jet (to zeroth order): Optically thick Optically thin Turnover  log log Radio X-ray? • 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? • The turnover also helps constrain the synchrotron contribution to X-ray

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

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

5. But wait… 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 > 90%  of flux is from the jet in the brightest hard state 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

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

7. 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” Time resolution typically ~100 sec

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. Some of the first mid-IR data of outbursting LMXBs 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

11. Some of the first mid-IR data of outbursting LMXBs 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)

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? Jet break around the H-band? (1.6 microns) 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

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

16. Could it be a synchrotron jet dominating X-ray? Russell, Maitra, Dunn & Markoff 2010, MNRAS, 405, 1759 NIR jet flux is proportional to X-ray flux Markoff, Falcke & Fender 2001 XTE J1118+480 Variability info: Kalemci et al. 2001, Kalemci’s talk at IAU Symposium, Buenos Aires 2010 Russell, Maccarone, Körding & Homan 2007 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

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

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