The AE Aqr Multi-wavelength Campaigns

1. The AE Aqr Multi-wavelength Campaigns Zach Ioannou (SQU) BELISSIMA Conference 18-21 September 2012

2. The AE Aqr Multi-wavelength Campaigns Belgrade, 20th September 2012

3. The AE Aqr Multi-wavelength Campaigns Belgrade, 20th September 2012

4. The AE Aqr Multi-wavelength Campaigns E&H (1996), WHG (1998), Meintjes et al. (2000): Magnetic propeller Patterson (1979): Oblique Rotator WKH (1997): Diamagnetic Blobs Terada et al. (2008): Cosmic Ray Accelerator Belgrade, 20th September 2012

5. The AE Aqr Multi-wavelength Campaigns The 2005 Campaign ★: CBA & AAVSO Belgrade, 20th September 2012

6. The AE Aqr Multi-wavelength Campaigns The 2012 Campaign Vidojevica ★: CBA & AAVSO KVA Belgrade, 20th September 2012

7. The AE Aqr Multi-wavelength Campaigns Belgrade, 20th September 2012

8. The AE Aqr Multi-wavelength Campaigns The 2005 Campaign Aug 30 Sep 1 2005 Aug 29 Aug 31 Sep 2 UT Chandra GALEX SWIFT VLA HESS MAGIC SALT Skinakas WHT Laguna Belgrade, 20th September 2012

9. The AE Aqr Multi-wavelength Campaigns The 2012 Campaign Observations consist of just a 30 min window per day Belgrade, 20th September 2012

10. The AE Aqr Multi-wavelength Campaigns Correlated flaresand the 33 s white dwarf spin pulseare observed in theoptical through X-ray wavebands C. W. Mauche 1530 Å C. W. Mauche J. D. Neill 2270 Å Z. Ioannou W. F. Welsh M. J. Dulude The radio light curveis uncorrelated withthe other wavebands, implying that the radio flux is due to indepen-dent processes CBA AAVSO A. Price M. Abada-Simon J.-F. Desmurs Belgrade, 20th September 2012

11. The AE Aqr Multi-wavelength Campaigns Phase offset relative to the de Jager et al.spin ephemeris of 0.237 ± 0.010 cycles  White dwarf is spinning down at a rate thatis slightly less than that predicted by thede Jager et al. (1994) quadratic ephemeris Spin phase offset variations correspond toa pulse time delay of a sini = 2.17±0.48 s*  X-ray source follows the motion of the whitedwarf around the binary center of mass *de Jager (1995) derived a sini = 2.04±0.13 s Belgrade, 20th September 2012

12. The AE Aqr Multi-wavelength Campaigns Mauche (2009, ApJ, 706, 130) Spectrum is reasonably well fit by a Gaussian emission measure distribution with a peak at log T(K) = 7.16, a width σ = 0.48, Fe/Fe = 0.44, other metals Z/Z = 0.76, EM = 8x1053 cm-3, and Lx = 1x1031 (d/100 pc)2 erg s-1 Belgrade, 20th September 2012

13. The AE Aqr Multi-wavelength Campaigns Radial velocities don’t appear to vary on thewhite dwarf orbit phase! (a) composite line profile technique  This is an unexpected result, but differs from the predicted radial velocity of the white dwarf (gray shading) by only 2.3σ Radial velocities vary on the white dwarf 33 sspin phase, with two oscillations per cycle (b) composite line profile technique (c) cross-correlation technique (d) boot-strapped cross-correlation technique  X-ray plasma is trapped on, and rotates with, the white dwarf’s dipolar magnetic field Belgrade, 20th September 2012

14. The AE Aqr Multi-wavelength Campaigns • AE Aqr was observed with the 17 m MAGIC telescope on 4 consecutive nights in 2005 August 29−September 1, and for 24 nights in 2012 at zenith angles of 300−500, for a total of >30 hr. • Analysis of each of the nights: no steady excess emission. • Analysis of the sum of the nights: no steady excess emission. • Periodic analysis of each night, using (a) the Rayleigh test on frequencies around the pulse frequency ν0 and 2ν0 and (b) phase-folding on frequencies near ν0 and 2ν0: no excess emission. Belgrade, 20th September 2012

15. The AE Aqr Multi-wavelength Campaigns No detections on the sum of the 4 nights from 2005: Whipple* F(E>E0) [10-11 cm-2s-1] * Suggesting the possibility that, contrary to previous claimsand common belief, AE Aqr is not a TeV gamma-ray source *Lang et al. (1998, Astroparticle Physics, 9, #3, 203) Belgrade, 20th September 2012

16. The AE Aqr Multi-wavelength Campaigns • The (pulsating component of the) source of X-rays in AE Aqr follows the motion of the white dwarf around the binary center of mass. • Contrary to the conclusions of Itoh et al. (2006), the majority of the plasmain AE Aqr has a density ne>1011 cm-3, hence its spatial extent is orders of magnitude less than their estimate of 5x1010 cm. • The radial velocity of the X-ray emission lines varies on the white dwarf 33 s spin phase, with two oscillations cycle and an amplitude K ≈ 160 km s-1, broadly consistent with plasma tapped, and rotating with, the white dwarf’s dipolar magnetic field. • These results are inconsistent with recent models* of an extended, low-density source of X-rays in AE Aqr, but instead support earlier models in which the dominant source of X-rays is of high density and/or in close proximity to the white dwarf. • AE Aqr is not a TeV gamma-ray source. *Meintjes (2000); Itoh et al. (2006); Ikshanov (2006); Venter & Meintjes (2007) Belgrade, 20th September 2012

17. The AE Aqr Multi-wavelength Campaigns • 2005 Campaign: • (18) Optical Telescopes • (2) γ-ray • (1) Radio • (3) Satellites • 2012 Campaign: • (7) Optical Telescopes • (1) γ-ray • (1) Satellite ★: CBA & AAVSO ★: CBA & AAVSO Belgrade, 20th September 2012

18. The AE Aqr Multi-wavelength Campaigns • We can vastly improve: • Telescope time allocation • Faster data analysis • Focus on science (not data collection) • Dynamic (re)scheduling • Reduction Pipelines • Intelligent Systems • Minimize human input Robotic Telescope Networks Belgrade, 20th September 2012