90 likes | 250 Views
The Powerful Black Hole Wind in the Luminous Quasar PDS 456. James Reeves Astrophysics Group, Keele University & UMBC. in collaboration with: E. Nardini ( Keele ), J. Gofford ( Keele /UMBC) - M. Costa,
E N D
The Powerful Black Hole Wind in the Luminous Quasar PDS456 James Reeves Astrophysics Group, KeeleUniversity & UMBC in collaboration with: E. Nardini(Keele), J. Gofford(Keele/UMBC) - M. Costa, G. Matzeu(Keele) - V. Braito(Brera/ASI) - F. Harrison, D Walton (Caltech) - G. Risaliti(Arcetri/CfA), P.T. O’Brien (Leicester), E. Behar (Technion), G. Matt (Roma) T.J. Turner (UMBC), M. Ward (Durham) and NuSTAR team NuSTAR Special Session, High Energy Astrophysics Division Meeting, Chicago, August 17-21, 2014
Black hole/host galaxy coevolution Jahnke & Macciò 2011 Kormendy & Ho 2013 AGN feedback is widely accepted as the underlying mechanism but… Hierarchical assembly through galaxy mergers might be equally relevant
Powerful disc winds are naturally expected at high accretion rates: Maiolino+ 2012 King 2010 Tombesi+ 2010
How powerful are disc winds actually? The mass-loss rate depends on the physical, dynamical and geometrical properties of the wind. The detection of narrow, blueshifted X-ray absorption lines does not provide on its own any solid constraint on its total energetics. • Solid angle:frequency of disc wind signatures among local AGN • Column density:modelling of absorption by photo-ionised gas • Outflow velocity: observed line’s energy following identification • Launch radius: ionisation state of the gas and escape velocity The geometrical structure has to be assumed rather than directly measured: it is therefore still unclear whether disc winds have sufficient mechanical energy to power feedback on galactic scales
The new campaign: 5 simultaneous XMM + NuSTAR observations The possible Rosetta Stone: PDS456 PDS456 is the most luminous radio-quiet AGN in the local Universe (z < 0.3) Background: systematic detection of a deep trough above 7 keV rest-frame, occasionally resolved into a pair of individual absorption lines: evidence for a large column density of highly ionised matter outflowing gas at about one third of the speed of light. Ratio Reeves+ 2003 PDS456 is the ideal target for studying AGN winds in the Eddington-limited regime. Rest-frame energy (keV)
A persistent wide-angle wind The P-Cygni-like profile is resolved independently at any epoch (aperture > 50º from FWHM) The line apparently responds to continuum changes over ~7-10 days (see also Gofford+ 2014)
Some (interesting) numbers All the critical information can now be determined from the data: 1. absorbed versus re-emitted luminosity 2. self-consistent photo-ionisation modelling 3. line energy and width 4. variability timescale A few per cent of the Eddington limit is already enough to prompt significant feedback on the host galaxy (e.g. Hopkins & Elvis 2010) For a wind lifetime of 107 yr the energy released through the accretion disc wind likely exceeds the binding energy of the bulge:
Summary • PDS 456 is an exceptionally luminous AGN in the local Universe, yet • representative of an accreting SMBH during its quasar phase and thus • offering a unique view of the possible mechanism that links the growth • of the central black holes to the evolution of their host galaxies over • cosmic time. • The new campaign XMM + NuSTAR campaign allowed the first direct • measure of the mass-loss rate and total energetics of a disc outflow, • whose mechanical power is largely consistent with the requirements of • feedback models. • At the peak of the quasar epoch, such powerful winds would have • provided the energy and momentum to self-regulate the SMBH growth • and control the star formation in stellar bulges. • The present-day scaling relations are left as a record of this process. • Nardini+ (submitted)