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Beyond X-ray timing I: Using reprocessing to map the geometry of X-ray binaries Teo Muoz-Darias INAF-OSSERVATORIO ASTRONOMICO DI BRERA (OAB) University of Southampton, Black hole variability 2010 Monday, June 7, 2010 OUTLINE 1. Why could

  1. Beyond X-ray timing I: Using reprocessing to map the geometry of X-ray binaries Teo Muñoz-Darias INAF-OSSERVATORIO ASTRONOMICO DI BRERA (OAB) University of Southampton, Black hole variability 2010 Monday, June 7, 2010

  2. OUTLINE 1. Why could you be interested in optical/infrared timing? 2. How can we do it? • OIR timing instruments 3. A science case: • Echo-tomography of Low mass X-ray binaries 2 Monday, June 7, 2010

  3. WHY? 1. Multiwavelength sources LMXBs: interacting binaries with “normal” star transfering matter at ~ 10 -9 M yr -1 onto a compact object (BH or NS) 3 Monday, June 7, 2010

  4. WHY? 1. Multiwavelength sources LMXBs: interacting binaries with “normal” star transfering matter at ~ 10 -9 M yr -1 onto a compact object (BH or NS) Credit: Rob Hynes Jet Corona Accretion disc Companion star 3 Monday, June 7, 2010

  5. WHY? 1. Multiwavelength sources Radio IR Opt. X F ν Disc companion Jets Corona ν Credit: Mickaël Coriat Fast variability observed from IR to X-rays Full accretion picture MW view 4 Monday, June 7, 2010

  6. WHY? 2. Interesting science cases Complex X-ray/optical cross correlations: Contributions from jet or the corona Kanbach et al., Nature, 2001 5 Monday, June 7, 2010

  7. WHY? 2. Interesting science cases Fast infrared variability from the jet Piergiorgio’s talk Casella et al. 2010, MNRAS Lett. 6 Monday, June 7, 2010

  8. WHY? 2. Interesting science cases Optical echoes: binary geometry and neutron star masses In few minutes... 7 Monday, June 7, 2010

  9. WHY? 2. Interesting science cases Optical echoes: binary geometry and neutron star masses In few minutes... 7 Monday, June 7, 2010

  10. WHY? 2. Interesting science cases Pulsed optical emission from Magnetars: testing models See e.g. Dhillon 2005, 2009, 2010 8 Monday, June 7, 2010

  11. WHY? 3. Maybe it is the right time Science with ULTRACAM accreting white dwarfs/cataclysmic variables 20% black-hole/neutron star X-ray binaries 16% sdB stars/asteroseismology 12% eclipsing, detached white-dwarf/red-dwarf binaries 11% 220 nights extrasolar planet transits and eclipses 9% 16 runs occultations by Titan, Pluto, Uranus, Kuiper Belt Objects 6% 50+ papers flare stars 6% 8.2m VLT pulsars 5% 4.2m WHT isolated white dwarfs 5% 3.5m NTT ultra-compact binaries 4% since 2002 isolated brown dwarfs 3% GRBs 2% Miscellaneous objects (AGN, contact binaries, etc) 1% Credit: Vik Dhillon 9 Monday, June 7, 2010

  12. How? Optical: ULTRACAM at ING and ESO High temporal resolution (>100Hz) Triple beam CCD (3x1024x1024) Cover 3 different bands simoustanealy Pipeline : data on real time! See Dhillon et al. 2007 10 Monday, June 7, 2010

  13. How? Optical: ULTRACAM at ING and ESO High temporal resolution (>100Hz) Triple beam CCD (3x1024x1024) Cover 3 different bands simoustanealy Pipeline : data on real time! See Dhillon et al. 2007 10 Monday, June 7, 2010

  14. How? IR: ISAAC at ESO VLT • ‘Burst’ and ‘fastjitter’ modes • up to 3 ms ! ...but you have to stop for reading at some point • J, K, H bands See Dhillon et al. 2007 11 Monday, June 7, 2010

  15. How? IR: ISAAC at ESO VLT ★ Other Instruments • OPTIMA small telescope but nice results! • Also fast modes in e.g. VLT and Keck instruments • ‘Burst’ and ‘fastjitter’ modes • up to 3 ms ! ...but you have to stop for reading at some point • J, K, H bands See Dhillon et al. 2007 11 Monday, June 7, 2010

  16. HOW?. New things comings EMCCDs at help... They are becoming popular • Fast optical spectroscopy with ULTRASPEC Visitor instrument at ESO telescope • Fast optical spectroscopy with ISIS/EMCCD 4.2m WHT at La Palma 12 Monday, June 7, 2010

  17. MY SCIENCE CASE: constraining fundamental parameters with Echo-tomography 13 Monday, June 7, 2010

  18. Persistent / Transient bright disc Companion not detected 14 Monday, June 7, 2010

  19. Distribution of NS and BH masses 15 Monday, June 7, 2010

  20. Distribution of NS and BH masses 15 Monday, June 7, 2010

  21. Distribution of NS and BH masses Is there a real gap in the distribution? Which is the maximum mass for a NS? 15 Monday, June 7, 2010

  22. Bowen emission from the companion Steeghs & Casares 2002 ApJ 568 273  Discovery of narrow (FWHM ≈ 50 km/s) high excitation emission lines from the irradiated companion in Sco X-1. Most intense in Bowen blend: • NIII 4634, 4641-2 • CIII 4647, 4650-1 Powered by fluorescence resonance triggered by cascade recombination of HeII Ly α photons 16 Monday, June 7, 2010

  23. Bowen emission from the companion Steeghs & Casares 2002 ApJ 568 273  Discovery of narrow (FWHM ≈ 50 km/s) high excitation emission lines from the irradiated companion in Sco X-1. Most intense in Bowen blend: • NIII 4634, 4641-2 • CIII 4647, 4650-1 Powered by fluorescence resonance triggered by cascade recombination of HeII Ly α photons 16 Monday, June 7, 2010

  24. Bowen emission from the companion Steeghs & Casares 2002 ApJ 568 273  Discovery of narrow (FWHM ≈ 50 km/s) high excitation emission lines from the irradiated companion in Sco X-1. Most intense in Bowen blend: • NIII 4634, 4641-2 • CIII 4647, 4650-1 Powered by fluorescence resonance triggered by cascade recombination of HeII Ly α photons 16 Monday, June 7, 2010

  25. Bowen emission from the companion Steeghs & Casares 2002 ApJ 568 273  Discovery of narrow (FWHM ≈ 50 km/s) high excitation emission lines from the irradiated companion in Sco X-1. Most intense in Bowen blend: • NIII 4634, 4641-2 • CIII 4647, 4650-1 Powered by fluorescence resonance triggered by cascade recombination of HeII Ly α photons 16 Monday, June 7, 2010

  26. SUMMARY of results LMXB PERIOD K em M 1 REFERENCE hours km s -1 M SUN J1808.4-3658 2.01 248±20 >0.13 Cornelisse et al. 2009 4U 1636-536 3.79 277±22 >0.62 Casares et al. 2006 3.82 310±10 1.0-2.4 EXO 0748-676 Muñoz-Darias et al. 2009 XB 1254-690 3.93 245±30 1.2-2.6 Barnes et al. 2007 J1814-338 4.2 345±19 >1 Casares et al. In prep GX 9+9 4.2 230±35 >0.23 Cornelisse et al. 2007a 4U 1735-444 4.65 226±22 >0.32 Casares et al. 2006 X1822-371 5.57 280±3 1.5-1.9 Muñoz-Darias et al. In prep LMC X-2 7.7 351±28 >1.2 Cornelisse et al. 2007c Sco X-1 18.9 87±1 >0.24 Steeghs & Casares 2002 Aql X-1 18.97 247±8 >1.6 Cornelisse et al. 2007b GX 339-4 42.14 317±10 >6 (BH) Hynes et al. 2003; Muñoz- Darias et al. 2008 17 Monday, June 7, 2010

  27. What is echo-tomography? Time delays between X-ray and optical variability to map reprocessing regions in a binary (O’Brien et al. 2001) T(t- τ ) depends on orbital phase and geometry: • inclination i • binary separation O(t) = X(t) * T(t- τ ) • mass ratio q=M 2 /M 1 18 Monday, June 7, 2010

  28. What is echo-tomography? Time delays between X-ray and optical variability to map reprocessing regions in a binary (O’Brien et al. 2001) T(t- τ ) depends on orbital phase and geometry: • inclination i We propose to apply echo-tomography using a narrow filter centered at the Bowen Blend. • binary separation O(t) = X(t) * T(t- τ ) • mass ratio q=M 2 /M 1 18 Monday, June 7, 2010

  29. ULTRACAM+Narrow filters FLUX WAVELENGTH Bowen + He II continuum subtracted lightcurves !!! 19 Monday, June 7, 2010

  30. Echo-tomography of Sco X-1 Goal: search for time delayed echoes of X-ray variability from the companion using Bowen lines. Sco X-1 is the brightest LMXB in both, X-rays and optical wavelengths (V=12.9) Observational campaign with RXTE and WHT+ULTRACAM during 3 nights: 17-19 May 2004 full covering an orbital period (P=18.9 h) 0.50 0.25 0.75 0.00 20 Monday, June 7, 2010

  31. SCO X-1 during flaring! W3 φ =0.52 W4 φ =0.42 φ =0.60 W1 W5 W2 φ =0.73 21 Monday, June 7, 2010

  32. SCO X-1 during flaring! W3 φ =0.52 W4 φ =0.42 φ =0.60 W1 W5 W2 φ =0.73 21 Monday, June 7, 2010

  33. Delay at orbital phase ~0.5 43s 22 Monday, June 7, 2010

  34. Delay at orbital phase ~0.5 Bowen+He II+Continuum~11-12 s Continuum ~9 s 43s Continuum CORRELATION LEVEL DELAY (s) 22 Monday, June 7, 2010

  35. Analysis of the delays Muñoz- Darias et al. 2007 DONOR DELAY (s) CONTINUUM Text DISK MASS RATIO 23 Monday, June 7, 2010

  36. Analysis of the delays Muñoz- Darias et al. 2007 DONOR Bowen+He II CS DELAY (s) CONTINUUM Text M 1 > 1.4 M  i > 50º DISK MASS RATIO 23 Monday, June 7, 2010

  37. Analysis of the delays Muñoz- Darias et al. 2007 DONOR Bowen+He II CS DELAY (s) CONTINUUM Text M 1 > 1.4 M  i > 50º DISK MASS RATIO However, we need phase dependent echoes 23 Monday, June 7, 2010

  38. Echo-tomography of 4U 1636-536 • Emission from the companion previously detected: (Casares et al. 2006) K em =277 ± 22 km/s K 1 =90 -113 km/s • Frequent Type I bursts GOAL: using bursts to measure delays at different orbital phases Observational campaign with RXTE and VLT+ULTRACAM during 2 consecutive nights in June 2007 24 Monday, June 7, 2010

  39. Phase-dependent echoes in 4U 1636-536 CORRELATION LEVEL FLUX TIME (s) DELAY (s) 25 Monday, June 7, 2010

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