Violent Disk Instability Inflow to Spheroid and Black Hole

Transcription

1 Violent Disk Instability Inflow to Spheroid and Black Hole Avishai Dekel The Hebrew University of Jerusalem Jerusalem Winter School 101/13 Lecture stars 5 kpc

2 Outline 1. Violent Disk Instability (VDI): cosmological steady state. Giant clumps: in-situ versus mergers 3. Clump evolution and migration 4. DVI-driven wet inflow: compact spheroids 5. Two-zone rotation in ellipticals: VDI and mergers 6. Black Holes and AGN

3 AMR Cosmological Simulations Cosmological box, RAMSES (Teyssier), resolution 1 kpc Zoom-in individual galaxies, ART (Kravtsov, Klypin), RAMSES Ceverino, Tweed, Dekel, Primack: - 50 pc res. (30 galaxies) - 5 pc res., lower SFR, stronger feedback Isolated galaxies, resolution 1-10 pc, RAMSES, Bournaud et al. Collaborators: Bournaud, Teyssier, Krumholz, HUJI: Ceverino, Goerdt, Mandelker, Tweed, Zolotov, UCSC: Fumagalli, Moody, Mozena,

4 1. Violent Disk Instability (VDI): Clumpy Disks at High Redshift

5 Clumpy Disk Ceverino, Dekel et al. 10 kpc z=4-.1

6 Clumpy Disk Ceverino, Dekel et al. 10 kpc z=.4-.1

7 Toomre Disk Instability Gravitational instability Q σ k = π G Σ <1 k = r dω dr + 4Ω k = Ω Ω Ω kepler flat solid Jeans instability λ> λ J = σ GΣ GΣ GM r 1 σ = P ρ r Rotation instability λ< λ rot = 4π GΣ k GΣ GM r Ω r For any unstable scale must have λ J < λ rot Q = σ k <1 π G Σ Scale of maximum instability Q 1 π GΣ λc = λj 0. 5λ k R R clump disk σ V h R disk rot

8 Violent Disk Instability (VDI) at High z High gas density disk unstable Q σω G Σ 1 Giant clumps and transient features GΣ R rapid evolution on dynamical time clump Ω Toomre 64; Isolated galaxies: Noguchi 99; Immeli et al. 04; Bournaud, Elmegreen, Elmegreen 06, 08 5 kpc In cosmology: Dekel, Sari, Ceverino 09 Agertz et al. 09 Ceverino, AD, Bournaud 10 Ceverino et al. 11 Cacciato, AD, Genel 1 Krumholz, Forbes et al 1 Self-regulated at Q~1 by torques and inflow high σ/v~1/4 Inflow compact bulge and BH Steady state: disk draining and replenishment, bulge ~ disk Star formation and feedback in clumps

9 z=4 Clumpy Disk in a cosmological steady state VDI is robust at z>1 because of high gas density (cosmological density and intense accretion) z=3 VDI in some galaxies from z>7 to z<1 z= z=1.5 z=1 Σ gas [M pc - ] Dekel, Sari, Ceverino 09; Ceverino, Dekel, Bournaud 10 Mandelker et al. 1

10 Clumpy Disk in a cosmological steady state z=4 z=3 z= z=1.5 z=1 Σ gas [M pc - ] Dekel, Sari, Ceverino 09; Ceverino, Dekel, Bournaud 10 Mandelker et al. 1

11 Elmegreen et al Observations vs. Simulations

12 Simulated hi-z galaxy through Dust SUNRISE low dust RGB colors MW3 z=.33 medium Ceverino, Moody, Mozena, Dekel, Primack high

13 Simulated hi-z galaxy through Dust SUNRISE low dust RGB colors SFG1 z=1.56 medium Ceverino, Moody, Mozena, Dekel, Primack high

14 A typical star-forming galaxy at z=: clumpy, rotating, extended disk & a bulge Hα star-form regions color-code velocity field Genzel et al 08

15 BzK 6004 (.4) BzK (.4) BX 610 (.) BX48 (.) ZC78941 (.) merger merger -160 BX389 (.) D3a 6397 (1.51) +50 K0-7 (.) BX663 (.4) MD 41 (.) K0-9 (.0) HDF 4 (.49) ZC (1.41) BX58 (.3) (8 kpc) -70 K0-8 (.) -170 K0-6 (.) K0-5 (.) GK471 (.43) D3a 4751 (.7) SA1 619 (1.51) 150 HDF 169 (1.) BX 405 (.03) GK5 (.41) BX 599 (.33) 100 BzK 4165 (1.7) SMMJ09431 (3.35) H7 H6 HDF 76 (.0) SA (.3) BX 50 (.16) N 850. (.45) BM 1163 (1.41) GK 167 (.58) SA (.) BX 404 (.03) (Förster SMMJ13101 Schreiber (3.41) et al. 006, 008) SMMJ (1.1) N850.4 (.38) +00 GK 113 (1.61) (8 kpc) The SINS survey of galaxy kinematics at z~

16 High-z Disks with Giant Clumps Guo et al. 1 CANDELS

17 VDI at z=4-9 despite t merg /t dyn (1+z) -1 SFG z=4.9 z=5.0 SFG7 z=6.0 z=6.7 z=8.5 Oesch z=7

18 . Clump Support: Rotation+Pressure Ceverino et al. 011

19 Rotating Clumps in a Wildly Unstable Disk Naab

20 The Clumps are Spinning Jeans equation for an isotropic rotator Rotation support, induced by disk rotation and AM conservation during clump collapse, but the spin can be tilted V circ V V rot circ GM R = = Vrot Σ 0. Σ clump disk + σ 1/

21 Protoclump Spin from Disk Rotation V=r V=r 1/ V=const. V α r ω = 0.5(1+ α) Ω ω=ω ω=0.75ω ω=0.5ω

22 Clump Support against Free Fall Jeans equation for an isotropic rotator V circ GM R = = Vrot + σ Proto-clump rotation ω 0. 5Ω Clump Collapse factor, Assume AM conservation c = ( Σclump / Σdisk 1/ ) Gravitational instability Q M R, M disk σ clump i σ clump σ 1 M V R V M V tot disk disk V c, rot cvc, i 0.55cσ disk V c, circ 1. 5 c 1/ σ disk V V c, rot c, circ 0. c σ σ clump disk (1.6c 0.3c 1/ ) 1/ 1 Rotation support for c>.5 No much dispersion imprint

23 Clump Support: Rotation and Pressure Rotational Support Clump-Disk Spin Alignment V V c, rot c, circ 0. c

24 Clump Support: Rotation and Pressure Validity of Jeans Eq. Rotation support vs collapse factor V circ GM R = = Vrot + σ V V c, rot c, circ 0. c

25 Sub-structure in the disk giant clumps When clump substructure is resolved: Less dissipative contraction? Angular-momentum loss? a 0-30% effect Caution: MW molecular clouds are not spin-supported Bournaud, Teyssier AMR pc resolution

26 . Clumps: In-situ vs Mergers Ceverino et al. 010; 011 Mandelker et al. 01

27 In-situ and Ex-situ Clumps gas young stars 10 kpc dark matter stars

28 Stellar images of z~ simulated disks observed with HST bands and PSF B Mozena, Moody, Mendelker, Ceverino, et al. - CANDELS H Needed: a Morphological new morphological classification classification scheme for high-z galaxies, emphasizing the in-situ clumpy disks Hα gas

29 Clump Classification Mandelker et al. 01 Compact & round - 90% of mass In-situ clumps Ex-situ, merging clumps Number 70% 30% Mass 45% 55% SFR 75% 5% Kinematics rotating disk 50/50% disk/off disk Dark matter no yes M clump /M disk 0.0 ( ) 0.06 ( ) Stellar age 180 Myr (45-450) 1. Gyr ( ) ssfr (Gyr -1 ) 4 (0.7-30) 0.3 (0.0-3) Gas fraction Metallicity low tail no low tail Mass gradient declining declining Age gradient declining flat ssfr gradient declining rising Correlations of clump properties, Clumps vs host galaxy

30 Gradients of clump properties ex-situ in-situ - in-situ vs ex-situ - migrating vs disrupting

31 Clump Disruption by Explosive Outflows? Stellar radiative feedback: Murray et al. 10 disruption on a dynamical timescale Krumholz & Dekel 10,1 gradual mass loss during migration Genel et al. 11

32 Observational indications for clump survival? Forster Schreiber et al. 11 MD41 BX48 Guo et al 11

33 3. Clump Migration and Evolution

34 Isolated, gas-rich, turbulent disk - giant clumps - migration - bulge Noguchi 99; Immeli et al. 04; Bournaud, Elmegreen, Elmegreen 06, 08

35 Clump Formation & Migration

36 Quinn, Mayer

37 Clump Migration Dekel, Sari, Ceverino 09 Toomre instablity: Q σω π G Σ 0.67 Giant clumps: R clump 7 GΣ Ω δ Mdisk M tot ( R disk ) baryon Disk fraction: 0. 6 M M tot ( R disk ) h R R d σ δ V Q δ 1 σ V dark matter m clump M disk 0.0δ 0.3 Self-regulation by clump encounters at Q ~ 0.67 ~ dissipation of turbulence t t 1 4 enc α Q tdyn 1 dis 1. 4Q tdyn m α clump M disk 0. Migration to the center by encounters and dynamical friction t V mig α tenc Qδ tdyn σ For δ~0.3, t mig ~ 10 t dyn ~ 1- orbital time 1 t evac α tmig

38 Clump Evolution During Migration: Accretion, Stripping, Mergers M& αρ π R ac d T σ d R T = tidal (Hill) radius ~ Toomre radius of a proto-clump if Q~1 M M c d R R T d h R c 1 ac td M& ac d d σ d V d Clump mass more than doubles during migration M t α Gas dissipates and becomes bound: α ~ 1 Stars need to be bound: α ~ R c /R T ~1/3 In simulations, + mergers and stripping t ac ~ t mig ~ 8t d M α r -1, α~0.5

39 M & M& Steady Momentum-driven Outflows from Clumps ν = V V w V w = ε w ff c M = p w = w V L M * L c = V L M V L 3 & ψ ψ w & = ψ ψ ψ 1 Krumholz & Thompson 13, simulations of wind instability + proto-stellar winds + stellar winds + supernovae ej in ej & 160 ψ in, rad Dekel & Krumholz 013 km Stellar physics STARBURST90 SFR in clumps drives η~1 steady winds ψ in 4.4 while -1 c t ε migrating 0.01 inwards 1 3 and gaining mass. ff tff = G Rc M c 7Myr Vc = GM c Rc 140 km s ff They live for t mig ~ 50 Myr, 1 t & sfr = M c M = ε ff t ff and feed gas & stars to the bulge Explosive ejection 1 p& tff M gvc M g M c 0.5ε ffψ wvlvc << 1.5 s -1 ψ w Myr steady wind Mass loading SF efficiency Gas depletion η M& w M& ψ 1 * = wvlvw 1 ε* M & * ( M& * + M& w ) = (1+ η) t M M& + M& ) ε (1+ η) t dep c ( * w ff ff Myr Migration time Little mass loss t mig M δ c,mig t M d c 10td 30tff 50 Myr 1 0.4ηε ff, t mig t dep 1ε ff (1+ η) 0.4< 1 Gas rich ε *, mig 0. 4ε ff,

40 Observed Outflows from Clumps Genzel et al. 011; Newman et al. 01 Typical clumps - momentum-driven stellar fbck ok Extreme outflows energy-driven SN feedback?

41 Steady State: SFR Governed by Accretion Mass conservation M & τ, 1 acc M & gas = M& acc Kennicutt SFR If sfr vary on a timescale < τ sfr Steady state after τ sfr M& * M & = M * gas τ sfr f& = a bf M & gas 0 M& * M& acc Timescale for change of parameters from z=4 to below 1 M& 1 acc τ sfr t 4τ sfr dm& t 4τ 1 sfr -1 / dt dτ / dt acc sfr t t ff t t ff disk t t disk vir t t vir τ sfr ε t ff ff Gyr 0.003

42 Cosmological Steady State Gas mass conservation M & = M& M& M& = g g,ac sink sink M g τ τ SFR 1 = εsfrtd τ out = η εsfrtd τ inf = δ td τ = τ + τ + τ SFR out inf If the accretion rate and τ vary on a timescale longer than τ t / τ t / τ M& M& e M M& τ (1 e ) at t>>τ M & g g, ac & g g, ac g 0 M g M g,acτ M sink M g,ac Dekel, Sari, Ceverino 09, gas inflow only: δ 0.3 Cosmological steady state where bulge~disk~dm Cacciato et al. 1, gas+stars two-component instability: the disk stabilizes when it becomes stellar dominated at z~1 Bouche et al 10, SFR only: effect of minimum halo mass for SFR Krumholz, Dekel 10, SFR+outflow: effect of metallicity on SFR & &

43 4. VDI-Driven Wet Inflow: Compact Spheroid

44 Violent Disk Instability Inflow to Center Self-regulated Toomre instability Q σω Σ δ 1 σ 1 V M M cold tot σ δ V 1. Torques between perturbations drive AM out and mass in (e.g. clump migration) Gammie 01; Dekel, Sari, Ceverino 09. Inflow down the potential gradient provides the energy for driving σ to Q~1..compensating for the dissipative losses M& inf V Mσ t dyn t inf t δ dyn Krumholz, Burkert 10; Bournaud, Dekel et al. 11; Cacciato, Dekel, Genel 1 M & 5 + δ 1 3/ inflow MΘyr M cold,10.5 (1 z) 3 Inflow of gas (and stars), not limited to clump migration 0. clumpy gas disk compact stellar bulge

45 VDI-driven Inflow in Simulations Cacciato et al. M & 5 + δ 1 3/ inflow MΘyr M cold,10.5 (1 z) 3 0.

46 Torques in Simulated Disks Bournaud, Dekel et al. 011 Isolated disk at 1-pc res Inflow in an unstable disk is not limited to clump migration, and it occurs even if clumps are disrupted, and involves stars

47 DVI-driven Inflow in simulations M& M inflow cold 1 γ t dyn δ Dekel et al M & 5 + δ 1 3/ inflow MΘyr M cold,10.5 (1 z) 3 0. γ=1 M M cold tot σ δ V

48 Formation of Spheroid by VDI Bulge~Disk in Steady State gas young stars 10 kpc dark matter stars

49 Stellar Component z=.3 Edge-on Classical bulge: n=-6

50 Red Nuggets and Blue Nuggets Dekel & Burkert 013; Zolotov et al. 013 Compact stellar spheroid dissipative wet inflow to a blue nugget, by mergers or VDI VDI inflow is wet if t inflow << t sfr Self-regulated instability Q ~ 1 t inflow ε sfrδ < tsfr 1 ε sfr M M cold tot σ δ V 0.0 δ 0. δ Σ g Σ +Σ g +Σ dm Bi-modality in Σ: either compact nuggets or extended stellar disks wet inflow Σ up t inf /t sfr down wetter inflow Blue nuggets dispersion dominated: σ/v ~ δ Expect VDI-driven nuggets: - at high z, where f gas is high - for low spin λ, where R gas is low

51 Wet Origin of Bulge: Stellar Birthplace Simulations: Tweed, Zolotov, Dekel ex-situ (mergers) in disk in bulge 60-30% of the bulge stars form in the bulge wet inflow Driven by wet VDI or wet mergers

52 Blue Nuggets from Wet Inflow Ceverino et al Σ *,eff M kpc - Szomoru, Franx, van Dokkum 011

53 Observations: Blue Nuggets Red Nuggets RN BN log Σ e RN BN log M s Barro et al. z=1-3 Kauffmann et al. gas z=0 Fang et al. (z=0), Cheung et al. (z~1) Red and blue nuggets Evolution: diffuse compact quench downsizing of quenching RN BN

54 Bulge mass [10 10 M ] B/D=-4 major mergers? Bulge growth by mergers versus disk instability Tweed, Zolotov µ m = fraction of mass added in mergers of 1:m µ 3 Bulge mass [10 10 M ] minor mergers? Bulge mass [10 10 M ] disk instability? µ 10 # clumps

55 5. Two-Zone Rotation in Ellipticals: VDI and Minor Mergers Romanowsky, Dekel, Arnold, Hoffman, Ceverino, Brodie, Primack,

56 Kinematics: Outer vs Inner Rotation Binary major merger simulation, gas-rich 1:3 (Burkert et al.) Disky elliptical (NGC 3377; Romanowsky et al.) Cosmological simulation (Ceverino et al.)

57 Outer vs Inner Rotation Hoffman et al. Outer rotation Major mergers Cosmological: VDI + minor mergers Observed Es at z=0 Inner rotation

58 Origin of -zone Rotation in-situ birth Romanowsky, Dekel, Arnold et al. Inner rotator by disk instability Outer non-rotating halo by minor mergers inner rotator ex-situ birth outer non-rotator

59 6. Growth of Black Holes and AGN Bournaud et al. 011; 01

60 Bulge Black Hole - AGN Bournaud, Dekel, Teyssier, Cacciato, Daddi, Juneau, Shankar 11 Black hole growth by VDI-driven inflow in the disk % Sub-Eddington AGN, L x ~ erg s -1 Bright episodes by clump coalescence Obscured by Σ gas ~ cm - Similar to major mergers, but more abundant At z>6: VDI inflow allows Eddington accretion onto the BH By z~6 grow M BH ~10 9 M from a seed ~5x10 4 M at z~10

61 AGN associated with Clumpy Disks Bournaud, Juneau, Le Floch, Mullaney, Daddi, Dekel, Duc, Elbaz, Salmi, Dickinson 11 z=

62 Stream-Fed Galaxies at High z cold streams compact spheroid wet inflow to bulge quenching thick disk hot halo clumpy disk In parallel, mergers outflows clumpy disk VDI SFR spheroid late disk The main mode of galaxy formation hot halo

63 Conclusions Certain robust predictions for high-z galaxies in λcdm cosmology. 1. Fed from the cosmic web: ~3 co-planar streams (70%) in a pancake (0%). - Smooth + mergers. - 50% penetration into the galaxy. - Streams (mostly one) transport AM. AM exchange in inner halo. - Cold streams are observable in Lya emission (LAB) and absorption (LLS). - Outflows are in harmony with the in-streams (tentative).. Violent disk instability (VDI): by intense gas inflow and high density. - In-situ giant clumps and transient features, plus merged clumps. - In-situ clumps are 70% in number and SFR but 45% in mass, younger, higher ssfr (blue), lower Z, showing gradients due to migration. - Gradual mass loss from clumps. They grow as they migrate inward. 3. VDI-driven inflow to disk center classical bulge. - Blue Nuggets and AGN when the inflow is wet, i.e. faster than SFR. This is when Σ gas is high, i.e. at high z and in galaxies of low spin. - Dispersion-dominated galaxies. - Quenching to Red Nuggets by feedback. - Two-zone kinematics of Es: Inner rotation by VDI, Outer dispersion by minor mergers.

64 Cosmic Web, Cold Streams, Clumpy Disks & Spheroids 50 Mpc 100 kpc 100 kpc stars 5 kpc 5 kpc

65