Observational constraints on the distribution of AGN BH spin in the - PowerPoint PPT Presentation

Observational constraints on the distribution of AGN BH spin in the 5 1 0 2 h c r a local Universe M h t 0 3 , i a h g n a h S , ” N G A n i n i p s H B Matteo Guainazzi g n i r u s a e M “ , i z z a ASTRO-H Science Operation Team n i a u G o ISAS/JAXA & ESA/ESAC e t t a M

Outline ● How to measure spin in accreting Super- Massive Black Holes (SMBH) 5 1 0 2 h ● Why measuring spin in accreting SMBH c r a M h t 0 3 , i a ● Where do we stand now? h g n a h S , ” N ● Why is it such a difficult (and controversial) G A n i n i p measurement? s H B g n i r ● How we can put these measurements on u s a e M “ , i more robust ground? z z a n i a u G o e t t a M

Outline ● How to measure spin in accreting Super- Massive Black Holes (SMBH) 5 1 0 2 h ● Why measuring spin in accreting SMBH c r a M h t 0 3 , i a ● Where do we stand now? h g n a h S , ” N ● Why is it such a difficult (and controversial) G A n i n i p measurement? s H B g n i r ● How we can put these measurements on u s a e M “ , i more robust ground? z z a n i a u G o e t t a M

Measuring spin in BHs Astrophysical black holes are characterized by three quantities: mass (measurable through gas and/or 5 1 0 stellar dynamics), charge (assumed 0), spin 2 h c r a M h t 0 Method XRB? SgrA* AGN? 3 , i a h g n a h S , ” N G Thermal emission YES a NO NO A n i from the accretion n i p s disk H B g n i r X-ray spectroscopy YES b NO YES b u s a e of the disk reflection M “ , i spectrum z z a n i a u G Measurement of GR YES c YES d NO o e frequencies in the t t a M precession model e X-ray polarimetry NO NO NO ( a McClintock et al., 2011, arXiv:1101:0811; b this talk; c Motta et al., 2013, arXiv:1309.3652; d Aschenbach, 2004, A&A, 425,1075; e Stella & Vietri, 1999, PhRvL, 82, 17)

What we really measure is the ISCO=r ms 5 1 0 2 h c r a M h t 0 3 , i a h g n a h S , ” N G A n i n i p s H B g n i r u s a e M “ , i z z a n i a u G o e t t a M (Bardeen et al., 1972, ApJ, 178, 347)

Optically thick accretion disk reflection Astrophysical scenario underlying the “disk reflection method” in AGN (ad XRB) 5 1 0 2 h c r a M h t 0 = Hard component 3 , i a h g n a h S , ” N G A n i n i p s H B g n i r u s a e M “ , i z z a n i a u G Reflection component o e t t a M (Fabian et al., 2000, PASP, 12, 1145) (Reynolds, 2013, SSRv, 81))

The disk reflection method: monochromatic case 5 1 0 2 h c r a M h t 0 3 , i a h g n a h S , ” N G A n i n i p s H B g n i r u s a e M “ , i z z a n i a u G o e t t a M (Brenneman & Reynolds, 2006, ApJ, 652, 1028) (Fabian et al., 2000, PASP, 112, 1145)

The disk reflection method: reality The whole disk reflection spectrum is blurred 5 1 0 2 “Pure” reflection spectrum h c r a Blurred with a Schwarzschild (a=0) kernel M h t 0 Blurred with a Kerr (a=0.998) kernel 3 , i a h g n a h S , ” N G A n i n i p s H B a=0 g n i r u s a e M “ , i z z a n i a u a=0.998 G o e t t a M (based on Ross & Fabian, 2007, MNRAS, 381, 1697; Brenneman & Reynolds, 2006, ApJ, 652, 1028)

Outline ● How to measure spin in accreting Super- Massive Black Holes (SMBH) 5 1 0 2 h ● Why measuring spin in accreting SMBH c r a M h t 0 3 , i a ● Where do we stand now? h g n a h S , ” N ● Why is it such a difficult (and controversial) G A n i n i p measurement? s H B g n i r ● How we can put these measurements on u s a e M “ , i more robust ground? z z a n i a u G o e t t a M

Why do we care? The distribution of super-massive BH spins in the local Universe carries the imprinting of the host galaxy history (=evolution) 5 1 0 2 h c r a M h t 0 3 , i a h g n a h S , ” N G A n i n i p s H B g n i r u s a e M “ , i z z a n i a u G o e t t a M (Courtesy Dr. Giovanni Miniutti, LAEX; based on Berti & Volonteri, 2008, ApJ, 684, 822)

BH spin as tracer of BH-galaxy evolution BZ = Blandford-Znajek BP = Blandford-Payne 5 1 0 2 h c r a M h t 0 3 , i a h g n a h S , ” N G A n i n i p s H B g n i r u s a e M “ , i z z a n i a u G o e t t a M The BH spin could drive the evolution of radio-loud galaxies into radio-quiet (Garofalo et al., 2010, MNRAS, 409, 975)

BH spin (possibly) powering jets 5 1 0 2 h Power of ballistic jets in transient XRBs c r a M h t 0 3 , i a h g n a h S , ” N G A n i n i p s H B g n i r u s a e M “ , i z z a n i a u G o e t t a M (McClintock et al., 2013, arXiv:1302.1583; see a different view in: Russell et al., 2013, MNRAS, 2013, 431, 405)

Outline ● How to measure spin in accreting Super- Massive Black Holes (SMBH) 5 1 0 2 h ● Why measuring spin in accreting SMBH c r a M h t 0 3 , i a ● Where do we stand now? h g n a h S , ” N ● Why is it such a difficult (and controversial) G A n i n i p measurement? s H B g n i r ● How we can put these measurements on u s a e M “ , i more robust ground? z z a n i a u G o e t t a M

Early results The archetypal case: MCG-6-30-15 5 1 0 2 h c r a M h t 0 3 , i a h g n a h S , ” N G A n i n i p s H B g n i r u s a e M “ , i z z a n i a u G o e t t a Confirmation:Chandra/HETG M Discovery: ASCA/SIS Grating resolution CCD resolution Most of our current measurements are still at CCD resolution (Tanaka et al, 1995, Nat, 375, 659) (Young et al., 2005, ApJ, 631, 733)

Summary of AGN BH spin measurements t h a z z i , “ M e a s u r i n g B H s p i n i n A G N ” , S h a n g h a i , 3 0 M a r c h 2 0 1 5 M a t t e o G u a i n (Reynolds, 2013, SSRv, 183, 277)

Comparison with AGN evolution models 5 1 0 2 h c r a M h t 0 3 , i a h g n a h S , ” N G A n i n i p s H B g n i r u s a e M “ , i z z a n i a u G o e t t a M Pure “coherent”/”chaotic” evolutionary models predicts distributions clustered towards too high/low BH spin values (Sesana et al., 2014, ApJ. 2014. 794, 104)

First attempt on lensed QSOs 5 1 RXJ1131-1231 (z=0.658) 0 2 h a=0.87 +0.15 c r a -0.08 M h t 0 3 , i a h g n a h S , ” N G A n i n i p s H B g n i r u s a e M “ , i z z a n i a u G o e t t a M (Reis et al., Nat, 507, 207; Reynolds et al., 2014, ApJ, 792, L41; Walton et al., 2015, arXiv:1503.05255)

Outline ● How to measure spin in accreting Super- Massive Black Holes (SMBH) 5 1 0 2 h ● Why measuring spin in accreting SMBH c r a M h t 0 3 , i a ● Where do we stand now? h g n a h S , ” N ● Why is it such a difficult (and controversial) G A n i n i p measurement? s H B g n i r ● How we can put these measurements on u s a e M “ , i more robust ground? z z a n i a u G o e t t a M

Systematics due to the disk physics 5 1 0 2 h c r a M h t 0 3 , i a h g n a h S , ” N G A n i n i p s H B g n i r u s a e M “ , i z z a n i a u G o e t t a M (Reynolds & Fabian, 2008, ApJ, 675, 1048)

Systematics due to the disk structure Test case: MCG-6-30-15 Physics: lamppost over a disk with radially stratified ionisation 5 1 Model: single-ionisation reflection 0 2 h c r a M h t 0 3 , i a h g n a h S , ” N G A n i n i p s H B g n i r u s a e M “ , i z z a n i a u G o e t t a M [ε(r) ~ r -q ] (Svoboda et al., 2012, A&A, 545, 106)

Systematics due to parameter degeneracies free abundance 5 Solar abundance 1 0 2 free (disk)/Solar (torus) abundance h c Probability for the BH spin in NGC3783 r a M h t 0 3 , i a h g n a ( Suzaku observation) h S , ” N G A n i n i p s H B g n i r u s a e M “ , i z z a n i a u G o e t t a M (Reynolds et al., 2012, ApJ, 755, 88)

Systematics due to data modeling t h a z z i , “ M e a s u r i n g B H s p i n i n A G N ” , S h a n g h a i , 3 0 M a r c h 2 0 1 5 M a t t e o G u a i n Fairall 9 – Suzaku data

Systematics due to data modeling Fairall 9 – Suzaku data Model “B”: a≈0.96, i ≈36º, Z/Z solar >0.75 Model “A”: a≈0.52, i ≈48º, Z/Z solar >8.3 5 1 0 2 h c r a M h t 0 3 , i a h g n a h S , ” N G A n i n i p s H B g n i r u s a e M “ , i z z a n i a u G o e t t a M Same data, same analysers, different models (Lohfink et al., 2012, ApJ, 758, 67)