Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Quasar Rain Chandra and the Inner Structure of AGNs Quasar Rain Chandra and the Inner Structure of AGNs Warm Absorbers, X-ray Eclipses and Broad Line Region Inflows, a unification Martin Elvis Harvard-Smithsonian Center for Astrophysics

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Chandra taught us about AGN structure 2 >100 absorption features - 6 parameter model Chandra HETGS 850ksec spectrum of NGC 3783 AGN km s -1 : 2-3 phase gas in pressure equilibrium to 5% Krongold, Nicastro, Brickhouse, Elvis, Liedahl & Mathur, 2003 ApJ 597, X-ray Warm Absorber Outflows

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Chandra taught us about AGN structure 3 Compton Thin  Thick  Thin in 4 days  N H >~10 24 cm -2 in 2 days –> n e >10 9 cm -3 –> R(N H ) < few 1000 R s –> NOT the “torus” 2 days Chandra monitoring Risaliti et al., 2007, ApJL, 659, L Rapid eclipses by thick, cool gas clouds

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz I thought I knew AGN structure Broad Absorption Lines Reflection features Thin Vertical wind Narrow absorption lines X-ray `warm’ absorbers Broad High ionization Emission Lines hollow cone Accretion disk Supermassive black hole X-ray/UV ionizing continuum Accelerating bi-conical disk wind no absorption lines Failed Disk wind Broad Low ionization Emission Lines Bi-conical Extended Narrow Line Region Elvis 2000 Disk Winds solve everything – it’s all outflows and rotation

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz But… A Theory of Everything must explain Every. Single. Thing. Do Broad Line Region Inflows spoil it all?

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Reverberation Mapping  -function flash from quasar Produces  -function response in an emission line from a gas cloud at distance R after “lag” time t=R/c flux Emission Line Response R/c flux Central Continuum Source Flash time

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Isodelay Surfaces Parabolas of equal delay time: Zero delay ONLY possible on our line-of-sight to continuum 7  = r/c Brad Peterson, OSU

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz ARP 151  RedshiftsBlueshifts  Lag time Broad Line Region Inflows Velocity Resolved Reverberation Mapping (VRRM) – Bentz et al Redshifts at zero lag  Infall ! Redshifts at zero lag 0 Isodelay Surfaces Peterson 2003 Infalling gas MUST be here

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz More blueshifts at zero lag Broad Line Region Inflows Inflows seem to be common – Grier et al. 2013

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Inflow leads to disks UMBC Can’t fall far without angular momentum creating a disk Broad Line Region is not a disk: – covers ~10% of 4  – Accretion disk covers ~0.1% of 4 .

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Broad Line Region Inflow ?

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz the outflow is the inflow

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Can outflows solve Broad Line Region Inflows? Use the Chandra results: 1. X-ray Warm Absorbers, Low Ionization Phase Krongold et al Log Temperature Log Ionization parameter 2. X-ray Eclipsing Clouds Schwartzchild radii Density (cm -3 ) X-ray Eclipsers Elvis et al BLR

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Can outflows solve Broad Line Region Inflows? Broad Emission Line Region Warm Absorber (LIP)* X-ray eclipsing clouds Temperature T(K) (1-2) X 10(4)Few X 10(4)<10(5) log[Density n e (cm -3 )] log[Ionization parameter, U] -1.5 – < 100 Same physical conditions Same gas? But WA is an OUTFLOW Outflow * LIP = Low Ionization Phase, Krongold et al. 2003

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Cool Phases in the Warm Absorber Outflow Found often (always?): NCG 3783 (Krongold et al. 2003; Netzer et al ), NCG 985 (Krongold et al. 2005b, 2009 ), NGC 4051 (Krongold et al ), Mrk 279 (Fields et al ), NGC5548 (Andráde-Velasquez et al. 2010) Thermal equilibrium Log(1/Pressure) Log(Temperature) Form naturally in gas illuminated by quasar spectrum – Krolik, McKee & Tarter 1981; Chakravorty+08,09 High metallicity helps -- Chakravorty et al. 2012

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Cool Phase is dense 100 x denser than Warm Absorber: n e ~ 10 8 cm -2 Column Density, N H ~ 30 x N H (WA) ≤ cm -2 Size, d ~ cm ≈ 300 M 8 R g ≈ 60 R X-ray (M 8 ) Hard to accelerate High Mass/cross-section ratio – Mushotzky, Solomon & Strittmatter 1972 – Risaliti & Elvis 2010 Stops accelerating while warm phase continues up to escape velocity Stops accelerating while warm phase continues up to escape velocity?

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Dense condensed phase, below v escape Falls back after ~1 dynamical time ~ 1 year = Quasar Rain

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Quasar Rain: How quickly does it form? Cooling time:  cool = 1.8x10 10  0 (T)/  (T) T 6 1/2 n e8 -1 sec. –  (T) ~60  0 (T) Tucker 1975, Gehrels & Williams 1993 ≈ 3 days  cool = 3 T 6 1/2 n e8 -1 days ≈ 3 days Collapse time: Collapse time: ≈ 23 days  sound = c s /R = 300 km s -1 / cm ≈ 23 days

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz How quickly does wind reach v escape ? Acceleration time to v escape :  acc ~ 4M 8 days (Risaliti & Elvis 2010 model)  cool <  acc <  sound Similar ballpark – competitive processes Some condensations escape, some fall back Some condensations escape, some fall back

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Fate of the infalling rain? Feels ram pressure of warm outflowing gas Mach ~20 Strips away gas into a tail “raindrops” destroyed On elliptical orbits  Non-radial tails

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Fate of the infalling rain? Feels ram pressure of warm outflowing gas Mach ~20 Strips away gas into a tail “raindrops” destroyed Timescale: – Ram Pressure needs ~10x cloud mass to sweep by (Nulsen, 1982) : – 3 v 1000 n e (cloud) /n e (wind) years ~ 300 years! – But: pancakes on few sound crossing times (e.g. Hopkins & Elvis 2010) ~ xxx On elliptical orbits  Non-radial tails

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz We see these ablating “raindrops” NGC1365 X-ray eclipsing clouds N H rises fast at low covering factor, f c Then N H drops as f c increases “Cometary” tail – non-radial Lifetime ~60 days Cannot reach high infall velocity Maiolino et al Covering factor NHNH 1 day

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Quasar Rain Explains: – Infalling Broad Line Region Gas – at moderate infall velocities Unifies: – Broad Line Region clouds – Low Ionization X-ray Warm Absorber – X-ray eclipsing clouds – Cometary tails on X-ray eclipsing clouds Forms naturally Appealing: Disk winds still solve everything

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz The Way Forward Vikhlinin et al ×100 Chandra gratings Chandra HRC-LETGS >250 X Chandra Calorimeter A(0.5)~10,000cm X Chandra NGC3783 in 1ksec dE ~< 5 eV 0.5keV Similar to Athena Calorimeter A(0.5)~10,000cm X Chandra NGC3783 in 1ksec dE ~< 5 eV 0.5keV Similar to Athena R ~ 5000 >10 X Chandra NGC3783 spectrum in 3 ksec Variability -> density, radius Large Surveys: M , L/L Edd, … High z 60 km s -1 Resolves thermal line widths Turbulence, T thermal vs T ion Curve of growth n(ion) Diagnostic line ratios Resolves UV-like components Nearer term: “ARCUS” – see Randall Smith poster 8.11

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Quasar Rain does not reach “ground” Rain that does not reach the ground is “Virga”

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Quasar Virga Thank you KWWL.com

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Quasar Rain/Virga Explains: – Infalling Broad Line Region Gas – at moderate infall velocities Unifies Chandra and reverberation results: – Broad Line Region clouds – Low Ionization X-ray Warm Absorber – X-ray eclipsing clouds – Cometary tails on X-ray eclipsing clouds Forms naturally Appealing: Disk winds still solve everything KWWL.com

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Distribution of gas clouds Response is a convolution “Response Function” Zero Delay Mea n Delay “lag” Central Continuum Source Emission Line Response time 1 month Cross- correlat e Cross- correlat e Brad Peterson, OSU

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz Do Broad Line Region Inflows spoil it all? Velocity Resolved Reverberation Mapping (VRRM) – Bentz et al Isodelay Surfaces: Quasar flash followed by emission line flash

Martin Elvis, Martin Elvis, 15 Years of Chandra, Boston, November 2014 © Harry Morosz BLR was Supposed to Rotate, Outflow Rotation – Wills & Browne 1986 – Young et al – Peterson & Wandel 1999 Outflow – Gaskell 1982 – Leighly & Moore 2004 Radio Core/Lobe ratio H  FWHM face-on edge-on blueshift