The changing face of RE J1034+396

1. The changing face of RE J1034+396 Matthew Middleton

2. A simple scaling... Spectral and timing similarities of AGN and BHB

3. A simple scaling... Index of -1.35 from analytical method (Vaughan et al. 2005) and large scale simulations (Middleton & Done 2010) Very ‘hot disc’ SED and massive soft excess

4. A simple scaling... 2 important things to do: Try and determine the BHB analogy Unify physics Try and spot the QPO again Determine duty cycle

5. 1. Determining the analogy Mass scaling with frequency >10LEdd XRBs show LFQPO sub-Edd Scaling gives 0.3-0.5LEdd AGN seen with this but not same SED

6. 1. Determining the analogy ‘3’ possibilities for soft excess spectrum: 1. Extra soft component 2. Smeared absorption 3. Smeared reflection

7. 1. Determining the analogy

8. 1. Determining the analogy Need to select same components to account for disc stability

9. 1. Determining the analogy AGN QPO 67Hz QPO

10. 2. Do we see it again?? First non-stationary AGN PSD!

11. 2. Do we see it again?? Drop in rms consistent with difference in PSD normalisations. Expect low T component to be more dominant at low energies in flux spectrum IF assumed deconvolution is a good description.

12. 2. Do we see it again?? CompTT/nthcomp = 2.6 CompTT/nthcomp = 5.1

13. Conclusions... By comparing the spectra and variability properties of REJ1034+396 we predict the likely spectral form is low T comp and high T comp 2. This appears similar to that of GRS1915+105 and bandpass correction leads to very similar power spectra 3. In the latest observation the QPO is not present 4. This gives the first non-stationary AGN PSD and shows transient nature much like the 67Hz QPO. 5. The power spectra and rms show much less variability and the spectral changes confirm our prediction of the deconvolution