Massive molecular outflows from ULIRGs - Dynamics and Energetics - E. Sturm for the SHINING and QUEST Team

Massive molecular outflows from ULIRGs - Dynamics and Energetics - E. Sturm for the SHINING and QUEST Team

NGC253 AGN- ULIRGs SB- ULIRGs Sturm+ 2011 Massive molecular outflows detected in ULIRGs v (OH) promising tool to distinguish AGN from starburst driven outflows Mass loss rates up to ~ 1000 M /yr Mass Loading factor ~ 5 10 x SFR Gas depletion times: 10 6-10 8 yrs, halting the star-formation activity on the same timescale.

I Extension of the sample - 23 RBGS ULIRGs (OH65, 79, and 119) containing 3 warm quasar dominated objects (Mrk231, F05189, F08572) - 15 additional warm, late stage mergers (ULIRGS/QSOs) (OH119) - 5 IR-faint PG QSOs (OH119) Sylvain s presentation Are the strong outflows driven by the AGN rather than by the star formation in these objects? Veilleux+ 2013

II) In-depth Studies (Dynamics / Energetics) Mrk231 Arp220 NGC4418

IIa) Mkn 231 z = 0.042 L IR = 3.2 10 12 L (70% AGN) Type 1 LoBAL AGN HST, Evans et al 2008

González-Alfonso + 2013 (submitted) 65, 79, and 119 m: SHINING (PI. E. Sturm) 163 m: OT1 (PI: R. Meijerink) All other lines: OT2 observations (PI: J. Fischer)

González-Alfonso + 2013 (submitted)

CO(1-0) red wing map Roberto s presentation Chiara s presentation Cicone+ 2012

González-Alfonso + 2013 (submitted) excited, quiescent component which is warm (lack of 119 abs) and compact (close to exciting source).

- P-Cygni outflow - high velocities, but different v_max --> more than one outflowing component - excited lines have blue peak at v=0, OH119 and 79 ground transitions don t excited, quiescent component which is warm and compact - OH119 emission weaker than absorption 4π spherical symmetry not necessarily the best approximation, and extinction plays some role - radiative pumping is important (OH163 in emission) - redshifted emission components in ground transitions comparable in velocity to mm CO redshifted emission, plausibly same component

Radiative transfer code (González-Alfonso & Cernicharo 1999) Free parameters (for each component): - inner and outer radii (R int, R out ) - T dust, τ 100 - the velocity field of each velocity component (v int, v out ), - the OH density at the inner radius (N OH ), - the covering factor of the continuum FIR source, and - the solid angle of the outflow / p f and f

Given: - Line profiles and fluxes (all 9 transistions simultaneously) - OH abundance (5 10 6 ) - Mass conservation: the gas expands radially with a velocity field v(r) and H 2 density n(r), such that n OH r 2 v is constant (i.e. the mass outflow rate is constant)

The line ratios essentially depend on T dust, N OH, and R out / R int, while the absolute fluxes also depend on R int and f. The mass outflow rate per unit of solid angle is and the total mass outflow rate is with g(p f ) a geometry factor (anisotropy factor) accounting for non-spherical symmetry (g < 1 for p f < R out )

González-Alfonso + 2013 (submitted) OH35 Spitzer IRS Long-High (LH) spectrum around the OH35 doublet. H. Spoon, priv. comm. (IRS calibration programme)

The high velocity component (HVC)

The high velocity component (HVC) For full coverage of the far-ir source (f=1) the size of the far-ir source required to reproduce the absolute fluxes is R int 65 80 pc, and the outflow size (diameter) is ~200 pc R out / R int 1.1 1.3 1.5 2.0

The low velocity component (LVC) LVC more extended (needed to produce the re-emission in OH119, 79, 163 etc.) Modeled as separate component

Decelerating molecular outflow! Cp. Cicone+2012 Roberto s presentation Susanne s presentation

The quiescent component (QC) Not seen at 79 and 119 m ground transitions a highly excited component, representing an outflow-free circumnuclear component with T dust 110 K, R 65 pc, and a column of N H 2 10 24 cm 2.

Summary of components QC: a highly excited component where the OH peaks at central velocities, representing an outflow-free circumnuclear component with T dust 110 K, R 65 pc, and a column of N H 2 10 24 cm 2. HVC: high-velocity absorption by excited OH arises from a somewhat larger (R int 75 pc, R out 100 pc), radiatively excited component also associated with high far-ir radiation densities (T dust 100 K), which is likely surrounding the QC. LVC: low-velocity (200 300 kms 1 ) outflowing gas, more extended than HVC Low Ionization Component (LEC): additional low excitation gas at low and high velocities, very extended, needed to fit the 119 and 79 transitions, and plausibly tracing the same region as the mm CO and HNC lines.

Summary of components Increasing excitation with increasing velocity shift decelerating velocity field strong velocity gradient (from 1700 to 100 km/s over <~ 40 pc) high clumpiness and turbulence within the flow?

Masses, energetics and the role of the AGN in Mrk231 mass outflow rate per solid angle in the direction of the observer In spherical symmetry this correpsonds to several 10 2 M yr 1, and possibly 10 3 M yr 1, locally in the circumnuclear region of Mrk231 in the HVC

Momentum flux: Ṁv 13 L AGN /c (with L AGN = 2.8 x 10 12 L ) Mechanical luminosity: 0.5 Ṁv 2 = 6 x 10 10 L (2% of L AGN )

The flow Scenario 1: The HVC is emanating from a strong far-ir radiation field likely generated in and around a compact circumnuclear component. The LVC is more extended, could just be the extension of the HVC, but also a separate component (SB driven?) Why is the QC quiescent, and why is the OH not destroyed? If the QC is the reservoir of the OH gas that feeds the outflow then either a relatively smooth acceleration process is needed (e.g. successive low-velocity, non-dissociative C-shocks) which allows the OH to survive, or if the OH is destroyed in fast (J-) shocks, it must reform in the post-shock gas. According to outflow models driven by radiation pressure (e.g. Roth et al., 2012), the low or zero outward velocity of the QC or torus gas can be a result of high inertia, the drop of the radiation pressure with decreasing T dust, and gravitation.

Scenario 2: the observed OH outflow could probe an interclump medium of the torus itself that is flowing between and past the dense clumps (possibly probed by the QC), permeating the whole structure. Interaction with the high-density clumps, and shadowing effects (Roth et al., 2012), would decelerate the outflowing gas with increasing radial distance. Scenario 3: The highest velocity gas could also be tracing a conical transition region between the torus and the polar directions. In our model for the HVC, the densities for velocities of 500 1500 kms 1 are n H 1000 500 cm 3, respectively, also in rough agreement with the wind-driven outflow models by Faucher-Giguère & Quataert (2012).

Who is driving the outflow(s) of Mrk231? DeBuhr, Quataert & Ma 2012: - 3D SPH simulations of the interaction between a high-speed outflow produced by an AGN and interstellar gas in the AGN's host galaxy - AGN Wind feedback plus radiation pressure feedback - Momentum flux: ṗ ~ τ L/c, with τ~10 needed to explain the M BH - σ relation ram pressure: τ <1 energy trapping - Depletion time (M gas /Ṁ) : ~10Myr Radiation pressure or AGN winds? Faucher-Giguère & Quataert 2012 DeBuhr, Quataert & Ma 2012 Roth, Kasen, Hopkins & Quataert 2012

IIb) NGC4418 and IIc) Arp220 2MASS HST

Both galaxies have compact and warm (T dust > 100 K) nuclear continuum components, together with a more extended and colder component

Arp220 dm/dt = 140 M /yr Outflowing gas mass = 1.1x10 8 M Cp. Sakamoto et al. 2009: 100 M /yr, 5x10 7 M González-Alfonso+2012

NGC418 dm/dt <= 12 M /yr Infalll NH3 OI H2O González-Alfonso+2012

III) What next?

What next: CO / other (sub-)mm moleucles Ongoing programmes with IRAM/PdBI and ALMA Cicone, Maiolino, Sturm+ 2013

What next: CO / other (sub-)mm moleucles Cicone, Maiolino, Sturm+ 2013 Ongoing programmes with IRAM/PdBI and ALMA

What next: CO / other (sub-)mm moleucles Cicone+2012

What next: Extension to higher L AGN, SFR, z Javier Graciá Carpio + in prep SHINING QUEST + other OT SHINING+ (L IR > 4 x10 12 L ) Extending the outflow trends to higher SFR and L AGN Extending the outflow trends to higher z (e.g. molecular gas fraction of massive galaxies 1.5-2 larger at z ~ 0.2 to ~ 0.3 than at z ~ 0) ALMA : OH119 at z > 2.5 for the most luminous and extreme at those redshifts. Local counterparts needed to identify any strong variation with redshift of the molecular outflow properties.

What next: Extension to higher L AGN, SFR, z IRAS 10091+4704 IRAS 13352+6402 Liner HII IRAS 18216+6419 IRAS 20036-1547 QSO Sy1

What next: [C II] as a measure of molecular outflows (substitute for OH / CO)?

What next: [C II] as a measure of molecular outflows (substitute for OH / CO)? SDSS J1148+5152, z=6.4189 Maiolino + 2012 IRAM [CII]158 m FWHM=2030 km/s

What next: [C II] as a measure of molecular outflows (substitute for OH / CO)? IRAS10565 CII FWHM=856km/s CII FWHM ~ Half Width @ 2%(Max) ~ v_max

What next: [C II] as a measure of molecular outflows (substitute for OH / CO)? Mrk231 CII FWHM=1378km/s

What next: [C II] as a measure of molecular outflows (substitute for OH / CO)??

Summary Mrk 231: Several outflow components (plus a quiescent component), decelerating Mass loss rate up to ~ 1000 M /yr ~ 5 10 x SFR Momentum flux: Ṁv 13 L AGN /c Mechanical luminosity: 0.5 Ṁv 2 = 6 x 10 10 L (2% of L AGN ) Depletion time (M gas /Ṁ) : ~10Myr

Ringberg 2011 Mrk 231 Mrk 231 P-Cygni profile with blue-shifted absorption and red-shifted emission v ~ 1,170 km/s Fischer + 2010

Ringberg 2011 Molecular outflows detected in 6 SHINING ULIRGs (RBGS) Sturm+ 2011

Ringberg 2011 Sturm+ 2011 v (OH) promising tool to distinguish AGN from starburst driven outflows: - SNe driven outflows: v < ~500 km/s - v > ~500km/s not observed in pure starburst objects Mrk231: energy outflow rate ~1% of L AGN - Outflow velocities correlate with AGN-luminosity high velocity outflows may be AGN-driven

Ringberg 2011 AGN- ULIRGs NGC253 SB-ULIRGs Mass loss rates up to ~ 1000 M /yr ~ 5 10 x SFR These ULIRG winds will totally expel the cold gas reservoir in the nuclei in about 10 6-10 8 yrs, therefore halting the star-formation activity on the same timescale. Sturm+ 2011

ULIRG/QSO Sample expanded to - 23 RBGS ULIRGs (OH65, 79, and 119) containing 3 warm quasar dominated objects (Mrk231, F05189, F08572) - 15 additional warm, late stage mergers (ULIRGS/QSOs) (OH119) - 5 IR-faint PG QSOs (OH119) - 4 most luminous ULIRGs (highest SFR and AGN luminosities, 0.2 < z < 0.3, OH119) Added nearby templates (OH119 an 163 in addition to OH79) - 4 SBs + NGC4038/4039 (2 nuclei + overlap) - 5 AGN (NGC1068, Circinus, CenA, NGC4945, NGC3079) + 42 BAT AGN (OH119) In-depth studies (many OH transitions, plus H 2 O et al.) of few key objects - Mrk231, Arp220, NGC4418, NGC6240 CII as substitute for OH? Since 2011 Ground-based (IRAM / ALMA) mm-co follow-up studies Continued neutral/ionized gas outflow studies (HST, Chandra, GEMINI, KPNO)

ULIRG/QSO Sample expanded to Since 2011-23 RBGS ULIRGs (OH65, 79, and 119) containing 3 warm quasar dominated objects (Mrk231, F05189, F08572) S. Veilleux s presentation - 15 additional warm, late stage mergers (ULIRGS/QSOs) (OH119) - 5 IR-faint PG QSOs (OH119) - 4 most luminous ULIRGs (highest SFR and AGN luminosities, 0.2 < z < 0.3, OH119) Added nearby templates (OH119 an 163 in addition to OH79) - 4 SBs + NGC4038/4039 (2 nuclei + overlap) - 5 AGN (NGC1068, Circinus, CenA, NGC4945, NGC3079) + 42 BAT AGN (OH119) In-depth studies (many OH transitions, plus H 2 O et al.) of few key objects - Mrk231, Arp220, NGC4418, NGC6240 CII as substitute for OH? R. Maiolino s presentation S. Veilleux s & D. Rupke s presentations Ground-based (IRAM / ALMA) mm-co follow-up studies Continued neutral/ionized gas outflow studies (HST, Chandra, GEMINI, KPNO)

I Extension of the sample

Who is who in the outflow of Mrk231?

Velocity field The quiescent component (QC) Size (diameter) ~130 pc 1.6 MHz maser emission Klöckner, Baan & Garret 2003 Radio continuum

The quiescent component (QC) Size (diameter) ~130 pc Davies+ 2004, 2007: (using stellar absorption features) luminosity profile of the active star forming region close to the AGN is well represented by an exponential function with a disk scale length 0.18 0.24 (150 200 pc), and implying that the stars exist in a disk rather than a spheroid. Davies+ 2007

The quiescent component (QC) Size (diameter) ~130 pc Mass estimate consistent with virial mass (~10 8 M ) T dust ~ 110K Compare: (L AGN /4πR 2 σ) 1/4 ~ 130K with L AGN = 2.8 x 10 12 L QC = circumnuclear OH-megamaser torus / thick disk / oblate spheroid? inner region of the star formation region????