Broad X-ray Absorption lines from the Wind in PDS 456

Transcription

1 Broad X-ray Absorption lines from the Wind in PDS 456 James Reeves (UMBC & Keele), Emanuele Nardini, Valentina Braito (Brera & UMBC), Francesco Tombesi (GSFC), Paul O Brien (Leicester), Jane Turner (UMBC), Stuart Sim (Queens/Belfast), Michele Costa, Gabi Matzeu (Keele), (Nardini et al. 2015, Science; Reeves et al., 2016, ApJ, in press)

2 PDS 456: the Rose/a Stone of AGN disk winds Most luminous radio- quiet AGN in the local Universe M B 27 L bol erg s 1 M BH 10 9 M Ra:o Systema:c detec:on of a deep trough above 7 kev rest- frame: evidence for a large column of highly ionised mamer ounlowing at about one third of the speed of light Reeves+03 Rest- frame energy (kev) Ideal target for studying BH winds in the Eddington- limited regime 2013/14 campaign: 5 simultaneous XMM + NuSTAR observa:ons

3 Revealing the Broad P- Cygni Iron line profile Nardini+15, Science

4 A persistent, wide- angle wind P- Cygni- like profile resolved at any epoch (aperture > 50 from FWHM) Nardini+15 Apparent response to con:nuum changes over 7-10 days

5 Constraints on the Disk Wind ProperPes All the informa:on can now be determined from the data The solid angle is obtained from the emimed/absorbed luminosity ra:o, and the launch radius from the variability :mescale The deposi:on of a few % of the total radiated energy is enough to prompt significant feedback on the host galaxy (Hopkins & Elvis 10). Over a life:me of 10 7 yr the energy released through the accre:on disk wind likely exceeds the binding energy of the bulge

6 Broad Soft X-ray Absorption Profiles in PDS 456 (Reeves et al. 2016, ApJ, in press) OBS B OBS E Signatures of fast (0.15c) BAL like profiles in soft X-rays with XMM-Newton/RGS. Velocity widths σ km/s.

7 Broad Soft X-ray Absorption Lines RGS$ OBS B ratio ABS1 MOS$ ABS2 XMM, OBS B ABS1 ABS2 OBS CD ratio ABS1 ABS2 XMM, OBS CD EMIS1 ABS1 ABS2 OBS E ratio EMIS1 ABS1 ABS2 XMM, OBS E. 5 0 ABS Rest Energy (kev) Rest Energy (kev) Soa X- ray absorbing gas the likely signature of an inhomogeneous wind, par:ally obscuring the AGN. Veloci:es of up to 0.1c. Absorp:on primarily due to highly ionized Fe (Fe XX- XXIV) as well as NeIX/X ratio ABS1 ABS2 XMM, 2001

8 Soft X-ray Wind in PDS 456 Fractional Absorption Fractional Absorption Fe XIX/ Ne IX Fe XX Ne X Ne IX Fe XX slow zone (v=0.06c) Ne X Fe XXII Fe XXIII Fe XXIV (a) Zone 1 (b) Zone 2 Mg XII fast zone (v=0.17c) Flux (kev cm 2 s 1 kev 1 ) emis zone 1 emis zone 1 abs zone 1 emis zone 2 XMM, OBS E abs zone Rest Energy (kev) Rest Energy (kev) 2 zones of ionized absorp:on required to explain soa X- ray spectra:- (i) slow zone - with v=0.06c and (ii) fast zone with v=0.17c. Absorp:on profiles due to Fe XX- XXIV and Ne IX- X. Emission also required (P Cygni like profiles). Covering factor 40%. Profiles rapidly variable - :mescales of weeks to months.

9 Relative F Flux Tracking the Wind Variability XMM (A, Aug 2014) XMM (E, Feb 2014) Suzaku (Mar 2013) Rest Energy (kev) >10x flux increase at 1 kev from Mar 2013 to Aug Column decreases by ΔN H > cm - 2 Factor x3 decrease in flux from Sept 2013 to Feb Soa X- ray absorp:on profiles emerge as flux drops Dras:c (x10) absorp:on variability over months :mescales. Increase in absorp:on opacity likely linked to emergence of soa X- ray broad absorp:on profiles par:al covering in clumpy wind? (see Waters & Proga 2016 for accelera:on of clouds in response to con:nuum).

10 Flux density (erg s 1 cm 2 Å 1 ) The UV connection 10-13! Lyα / N V HST/STIS 2000 Lyα HST/COS 2014 absn! C IV! Observed wavelength (Å) Very broad UV emission profiles, e.g. Lyα / C IV km/s. Highly blueshiaed, CIV=5000 km/s. Shallow absorp:on troughs, but highly blue- shiaed km/s

11 The Wind Structure R (cm) R (R g ) Innermost highly ionized wind launched from within 100 Rg of black hole ultra fast iron K absorp:on (0.3c). Inhomogeneous soa X- ray absorber R cm, n e cm - 3, with thickness ΔR cm. Filling factor f UV BLR emission (absorp:on) profiles R cm

12 An extreme disk wind in the NLS1, 1H ? Flux (kev cm 2 s 1 ) H , NuSTAR Thick DiskWind Model Energy (kev) Relative F Flux Thin Wind, R max =1.5R min, M dot =0.33 Wind model Thick Wind, R max =3R min, M dot = Energy (kev) Extension of disk- wind model (Sim et al. 2008, 2010) to the extreme NLS1,1H Can account for strong (tau>1) drop at iron K with a fast, Eddington limited wind profile. No need for highly rela:vis:c iron K reflec:on. Solar abundances of Fe only.

13 An extreme disk wind in the NLS1, 1H ? Extension of disk- wind model (Sim et al. 2008, 2010) to the extreme NLS1,1H Can account for strong (tau>1) drop at iron K with a fast, Eddington limited wind profile. No need for highly rela:vis:c iron K reflec:on. Solar abundances of Fe only.

14 Summary PDS 456 is an excep:onally luminous QSO in the local Universe, yet representa:ve of an accre:ng SMBH during the peak of the quasar era. The new XMM + NuSTAR campaign revealed a broad P Cygni profile at iron K and allowed a direct measure of the mass- loss rate and energe:cs of an accre:on disk wind, whose mechanical power is largely consistent with the requirements of feedback models. A fast component of the soa X- ray absorber has now been discovered, with BAL like absorp:on profiles emerging in the RGS data, with typical veloci:es of c The data point to a clumpy, inhomogeneous ounlow, with the soa X- ray absorber represen:ng filaments which form further out along the wind, on scale that are consistent with the inner BLR. Is PDS 456 an X- ray equivalent of a BAL quasar?

15 Revealing the Broad P- Cygni Iron line profile (Nardini et al. 2015) P- Cygni- like profile resolved at any epoch E D C B A Apparent response to con:nuum changes over 7-10 days