Molecular gas ou,lows. K. M. Dasyra

Transcription

1 Molecular gas ou,lows K. M. Dasyra

2 Feedback & galaxy evolu6on Why do we study ou,lows, feedback? Stellar/AGN feedback is able to regulate star forma5on and explain several rela5onships: - the mass func5on of galaxies (e.g., Croton+ 2006, Bower+ 2006) - the M BH σ rela5on (e.g., Silk & Rees 1998, Debuhr+ 2012) - color- mass diagrams: green valley galaxies (e.g., Nandra+ 2007, Schawinski+2014) - the discrepancy between cosmological & galac5c baryon frac5ons (e.g., Spergel+2007, Sofue+ 12) - the stellar- halo mass rela5on (e.g., Durcalec+2014, Mitchell+ 2015, Katz+16) NFW, no feedback Feedback modified Einasto profile Katz number of galaxies AGN feedback No feedback Croton et al. (2006) (adapted) (Rota5on curve)

3 Feedback & galaxy evolu6on Feedback regulates star forma5on via processes internal+external to a galaxy Internal: - the increase in the ISM turbulence (e.g., Nesvadba+ 2011; Alatalo+ 2014, Lanz+ 2015) Σ SFR - Σ H2 not following KennicuR- Schmidt relaton - the rarefica5on/dissipa5on of clouds - the expulsion of gas (important when outside the gravita5onal poten5al) (see, e.g., the starburst- driven wind in M82; Nakai+ 1987, Walter+2002,Veilleux+ 2009) H 2 M82 CO M82 disk wind Veilleux et al. (2009) Walter+ (2002)

4 Feedback & galaxy evolu6on Feedback regulates star forma5on via processes internal+external to a galaxy External: - prevent the depositon of new gas from the IGM into galaxies, e.g., in the case of jets. CO ou_low/buoyant uplie (10 10 M ) behind X- ray bubbles in Abell 1835 McNamara+ 2014: - 210<V<- 150 km/s 270<V<470 km/s Inflow of CO from filaments + ou_low around Perseus A. Salome+ 2006: CO radio CO(1-0) Image X- rays X- ray bubbles

5 Ou,lows: the atomic phase Observa6onal signature of feedback: ou,lows Notable characteris6cs in atomic phase [CII] 158μm - Can be compact/very extended (several kpc 2 ) (e.g., Lipari+ 2006, Rupke+ 2011, Cicone+ 2016) Can be located at SF regions, nucleus, even at radio jet Tps (e.g., MorganT+ 2005) Can reach high velocites (~0.1c at <0.1pc from accreton disk) (e.g., Tombesi+ 2010) Common at low/intermediate- z (up to 70% in LIRGs/AGN) (e.g., MarTn+ 1999, Heckman+ 2000, Rupke+2005, Dasyra+ 2011, Arribas+ 2014, Cicone+ 2014, Harrison+ 2014, Obied+2015) Detectable even at high- z (up to z=6.4) (e.g., Walter+ 2009, Genzel+2014, Maiolino+ 2012) Radio contours SDSS z=6.4 Cicone+2016

6 Ou,lows: the molecular phase Observa6onal signature of feedback: ou,lows Notable characteris6cs in molecular phase - Several tens of objects with cold gas winds; mainly in the local Universe; up to z=2.3 (Eyelash) (e.g., Veilleux+ 2013, Spoon+2013, Cicone+ 2014, George +2015) - can drive gas of the star- forming phase outside gravitatonal potentals of galaxies (V>V esc ) (e.g., Veilleux+ 2013, Cicone +2014, Calderon +2014, Sakamoto+ 2014: 1000<V deprojected <2000 km/s) - dominate the wind mass (M ou_low ~ M ) and mass flow rate (1-1000M /yr) - can contain very dense gas (>10 6 /cm 3 ; that could be forming stars) NGC CO(3-2) - can be driven by SB / AGN examples follow Radio contours Calderon Sakamoto+ 2014

7 Molecular ou,lows: driving mechanism How to disentangle the driving mechanism (AGN/SB) of molecular oudlows? SpaTal distributon, or by p, E, dm/dt, dp/dt, and de k /dt (kinetc luminosity). Velocity not as safe. Starburst NGC 253 BolaRo+2013 Wind startng points E mech from SN, radiaton pressure: dm/dt ~ SFR (e.g., Murray+2011; Hopkins+2011) NGC253: dm/dt=1~3 SFR 4 molecular expanding shells in the starburst region km/s km/s Background: Hα Contours: CO(1-0) BolaRo+2013 km/s

8 Molecular ou,lows: driving mechanism How to disentangle the driving mechanism (AGN/SB) of molecular oudlows? SpaTal distributon, or by p, E, dm/dt, dp/dt, and de k /dt (kinetc luminosity). Velocity not as safe. radio mode jets AGN accreton disk winds RadiaTon pressure QSO mode Acce5on disk: dp/dt, E atypical of radia5on pressure Tombesi+2015 OH 119 μm IRAS F Fe Kα Radia5on pressure: Cicone+ 2014

9 Molecular ou,low examples: driving mechanism Jets: NGC1068: CO(3-2) Ou_low in the directon of the jet radio emission / NLR cone (dm/dt 60 M /yr, an order of magnitude higher than SFR) Garcia- Burillo et al. (2014, 2016) CO(3-2) V- field residual + radio contours (km/s)

10 Molecular ou,low examples: IC5063 mul6ple wind star6ng points along a jet IC5063: an ellipqcal, with a S- shaped disk in it center, and a jet that passes through the disk (almost parallel to it). - [OIII] emission along the jet trail, - HI (and H 2 ) wind seen in absorpton in front of the north lobe, (MorganT+2005,2007,2013,2015; Tadhunter+ 2014) This geometry leads to the highest number of jet- driven winds in a galaxy: Ionized [FeII] & H 2 winds start in at least 4 regions near the jet Dasyra Op5cal CO(2-1)

11 Molecular ou,low examples: IC5063 mul6ple wind star6ng points along a jet IC5063: winds at two radio lobes, regions R1 and R5. Blue or red- shieed emission depending on jet/cloud/observer geometry Total warm gas winds occupy ~1 kpc2 or 1/5th of the molecular disk Dasyra A diffuse cocoon is also detected for CO within R~500 pc. MorganT (C)

12 Molecular ou,low examples: NGC A radio jet probed by an ou,low NGC1377- B band: CO(3-2) flux CO(3-2) σ Aalto et al. (2016) 20 pc NGC1377: A jet revealed by a molecular wind! (mainly H 2 spectral lines; τ 9.7 >1). No detected radio emission. Roussel+ 2006; Dale+ 2007; Imanishi CO(3-2) V ALMA data show the presence of a collimated molecular oudlow of M along the minor axis. KinemaTcs: the jet is precessing near the plane of the sky Aalto > 70 km/s < - 70 km/s

13 Molecular ou,low proper6es: mass range of detected ou,lows What is the mass range of molecular ou,lows? In low- SFR galaxies with weak AGN (LINERS) Typically within 100 pc from the center, and 1-10 M /yr NGC 1433: M ; Combes+13 NGC 6764: M ; Leon NGC 1266: M ; Alatalo Combes+13 oujlow NGC 1433 V field CO(3-2) Alatalo CO(2-1) NGC <V<- 400 km/s 400<V<600 km/s p- V diagram along M.A. M.A.

14 Molecular ou,low proper6es: mass range of detected ou,lows What is the mass range of molecular ou,lows? In low- SFR galaxies with weak AGN (LINERS) Typically within 100 pc from the center, and 1-10 M /yr NGC 1433: M ; Combes+13 NGC 6764: M ; Leon NGC 1266: M ; Alatalo In high- SFR galaxies (with AGN): Mrk 231: M, dm/dt >700 M /vr (SFR=200 M /vr), Feruglio IRAS : M, dm/dt =1200 M /vr (SFR=240 M /vr) Garcia- Burillo IRAS : M, dm/dt =1200 M /vr (SFR=20 M /vr) Cicone > large fracton of the reservoir is in the wind CO(1-0) On average, 5% of the cold gas reservoir is in the wind! Cicone

15 Molecular ou,low proper6es: chemical composi6on of winds What about the chemical composiqon of the gas in the wind? Dense clouds do exist in the wind, e.g., Arp 220: HCO+(4-3), (3-2) P- cygni profile Sakamoto HCO+ x HCN Mrk 231: HCN, HCO +, HNC (Aalto+2010) The HCO+ and HCN ou_lows do not coincide + radiatve transfer: inconsistent masses - > chemical differenqaqon in the wind Lindberg+ 2015

16 Molecular ou,low proper6es: chemical composi6on of winds What about the chemical composiqon of the gas in the wind? Dense clouds do exist in the wind, e.g., Arp 220: HCO+(4-3), (3-2) P- cygni profile Sakamoto+2009 Image:radio Contours: HCN/CO NGC5194: HCN(1-0)/CO(1-0) high near the jet (shock enhancement of HCN+IR pumping) Matsushita+ 2015

17 Molecular ou,low proper6es: gas excita6on What about the gas excitaqon in the wind? Does it differ from that in the ambient ISM? Proposed for the CO: spectral line energy distributon differs in radio galaxies from other galaxies due to jets. Arp 193 3C293 vs. Papadopoulos Cicone Mrk 231: No significant differences for CO(2-1)/(1-0) (Cicone+ 2012) NGC 6764: CO(2-1)/(1-0) rato doubles from km/s to 0 km/s (Leon+ 2007) Dragonfly (z~2): CO(6-5)/(1-0): gas in outer disc parts higher excitaton than at the center (Emonts+ 15) But in last 2 cases unclear if truly associated with wind. Wind red ambient Wind blue Mrk 231: CO(2-1)/CO1-0)

18 Molecular ou,low proper6es: gas excita6on What about the gas excitaqon in the wind? Does it differ from that in the ambient ISM? Confirmed for the H 2 /CO flux raqo: 4C12.50: Ou_low seen in H 2 + CO lines. > 25% of the warm reservoir in the wind; (Dasyra & Combes 2011) M 400K M 400K (ou_low) > 30 (ambient) M 25K M 25K Dasyra & Combes (2012); Dasyra et al. (2014) (Dasyra & Combes 2011) Spitzer data HI - scaled Dasyra & Combes (2012)

19 Molecular ou,low proper6es: gas excita6on What about the gas excitaqon in the wind? Does it differ from that in the ambient ISM? Confirmed for the H 2 : IC5063: Near the jet, H 2 (1-0) S(3)/S(1) is ~2000K in the ambient medium, but in the wind it exceeds maximum value for LTE - > non- collisional excitaqon Dasyra

20 Molecular ou,low proper6es: gas excita6on What about the gas excitaqon in the wind? Does it differ from that in the ambient ISM? Confirmed for the OH: Mrk231: Wind seen 6 OH doublets, with 2 oudlow components highly (& radia5vely) excited component at R~100pc, with momentum flux 15 L AGN /c (torus?) + low- excita5on (extended) component, seen only in the 119 and 53μm lines. Gonzalez- Alfonso+ 2014

21 Molecular ou,low proper6es: gas momentum rate What about the momentum rate of the gas in the wind? Carniani Momentum rates of the molecular gas in the winds are on average ~20 L AGN /c. - not true for the atomic gas. How is this possible for winds ini5ated by radia5on? radia6on trapping (mul5ple scarerings; τ L AGN /c term) - Ishibashi & Fabian (2015) and/or energy- driven winds - Faucher- Giguère & Quataert (2012)

22 Physics of molecular ou,lows: gas momentum rate reverse shock Contact discontnuity forward shock ISM Energy or momentum driven refers to whether the wind in the reverse shock layer has 6me to cool (from ~ K) energy- driven: inefficient cooling, e.g,. in 10,000km/s winds - > hot post- shock gas does pdv work, dp s /dt ~ (v in /v s )L AGN /c // adiaba5c, Sedov- Taylor phase in SN remnant - Faucher- Giguère & Quataert (2012 ) momentum- driven: efficient cooling via, e.g., inverse Compton - > no pdv work shocked wind layer is small, not expanding (King+2011) Energy driving much more efficient in coupling with the ISM than momentum driving (Costa+ 2014)

23 Physics of molecular ou,lows: accelera6on of dense clouds Examples of energy driving: Ultra- fast oudlows (0.1c) and jets. Their passage from a clumpy ISM leads to similar wind propertes. The result largely depends on ISM distribuqon. Wagner+ 2011; 2013 jet 0.1c wind

24 Physics of molecular ou,lows: accelera6on of dense clouds What mechanisms contribute to the acceleraqon of the molecular gas? Once an atomic wind gets going, dense clumps can be accelerated / form in the wind via: - E- driven: thermal pressure from the shocked wind layer Zubovas & King 2014 Clumpy ISM+ Rayleigh Taylor unstable contact disconqnuity: - the layers mix in the ou_low, - the ou_low cools radiatvely t cool ~ kt / nλ, e.g., in yrs to kyrs for typical 100K- 1000K gas

25 Physics of molecular ou,lows: accelera6on of dense clouds What mechanisms contribute to the acceleraqon of the molecular gas? Once an atomic wind gets going, dense clumps can be accelerated / form in the wind via: - E- driven: thermal pressure from the shocked wind layer - Ram pressure (assisted by hydro instabilites and mass loading): destructon and reformaton of clumps in the wind. n=10 3 /cm 3 RT, KH - dissipation Ram pressure - accelerati on + n=0.1/cm 3 Hopkins & Elvis 2010

26 Physics of molecular ou,lows: accelera6on of dense clouds What mechanisms contribute to the acceleraqon of the molecular gas? Once an atomic wind gets going, dense clumps can be accelerated / form in the wind via: - E- driven: thermal pressure from the shocked wind layer - Ram pressure (assisted by hydro instabilites and mass loading): destructon and reformaton of clumps in the wind. Morgan Centaurus A filaments: CO higher σ in ionized medium than in HI cloud

27 Molecular ou,low proper6es: accelera6on of dense clouds Do molecular clouds form in the wind/get accelerated? V(dense) vs. V(tenuous) Mrk 231: HCN and CO- probed clouds aiain comparable V but the CO emission extends to twice the radius Aalto+ 2012; 2014 both are slower than V terminal (neutral) from NaI D Rupke & Veilleux 2011 Feruglio et al. (2010) CO(1-0) For several other sources (using OH): Veilleux Aalto et al.(2012) HCN (1-0)

28 Conclusion: challenges in the field SQll need to evaluate: - To what extent do molecular oudlows affect galaxy evoluqon overall? Hard to evaluate on individual galaxies. DepleTon Tmescales of yrs. StaTsTcs needed, so far from OH thanks to wide- spread dust contnuum ULIRGs+QSOs: >60-70% have winds; Sturm+ 2011; Veilleux+ 2013; Spoon+2013 BAT AGN: 8% have winds; Stone Feasible with ALMA: can detect ~5*10 5 M winds locally, push PdB limit to z~ For the accelerated gas - that quits galaxies: how much and how fast returns through filaments? - that remains in the galaxy: Tme delay in SFR due to turbulence Disentangling oudlows from mergers, driving mechanisms (including weak jets).