Violent Disk Instability at z=1-4 Outflows; Clump Evolution; Compact Spheroids

Transcription

1 Violent Disk Instability at z=1-4 Outflows; Clump Evolution; Compact Spheroids Avishai Dekel The Hebrew University of Jerusalem Santa Cruz, August 2013 stars 5 kpc

2 Outline 1. Inflows and Outflows 2. Evolution of giant clumps in VDI disks 3. Formation of compact spheroids: blue & red

3 1. Inflows and Outflows

4 Cosmic-web Streams feed galaxies: mergers and a smoother component AMR RAMSES Teyssier, Dekel box 300 kpc res 30 pc z = 5.0 to 2.5

5 Streaming to the disk - a Messy Region Ceverino, Dekel, Bournaud 2010 ART 35-70pc resolution streams disk interaction region Breakup due to shocks, hydro and thermal instabilities, collisions between streams and clumps, heating.

6 Inflows & Outflows Tweed, Dekel, Teyssier RAMSES 70-pc resolution Do outflows find their way out through the dilute medium with no noticeable effect on the dense cold rapid inflows? dilute hot high Z Gas density Temperature Metallicity

7 Inflows and Outflows Gas density Temperature Velocity House, Ceverino, et al. in prep. ART cosmological simulations res 25pc Do outflows find their way out through the dilute medium? How do they affect the dense cold rapid inflows? radiative fdbk outflow η~1-7 dilute hot z=2.6 M v =7x10 11

8 Interaction of Outflows and Inflows House, Ceverino,Tweed, et al. 13 ART cosmological simulations at 25pc resolution with radiative feedback Inflow penetration M & 0.1R ) / M& ( R ) ( v v The inflows and outflows live in harmony Outflow strength

9 2. Evolution of Giant Clumps in VDI Disks

10 Clumpy Disk Ceverino, Dekel et al. 10 kpc z=4-2.1

11 Elmegreen et al Observations vs. Simulations

12 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 2 Ω 5 kpc Toomre 64; Isolated galaxies: Noguchi 99; Immeli et al. 04; Bournaud, Elmegreen, Elmegreen 06, 08; Hopkins et al. 12; Bournaud et al. 13 In cosmology: Dekel, Sari, Ceverino 09 Agertz et al. 09 Ceverino, AD, Bournaud 10 Ceverino et al. 11 Cacciato, AD, Genel 12a,b Genel et al. 12 Forbes et al. 12, 13 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

13 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=2 z=1.5 z=1 Σ gas [M pc -2 ] Dekel, Sari, Ceverino 09; Ceverino, Dekel, Bournaud 10 Mandelker et al. 13

14 Clumpy Disk in a cosmological steady state z=4 z=3 z=2 z=1.5 z=1 Σ gas [M pc -2 ] Dekel, Sari, Ceverino 09; Ceverino, Dekel, Bournaud 10 Mandelker et al. 13

15 Simulated hi-z galaxy through Dust SUNRISE low dust RGB colors MW3 z=2.33 medium Moody, Ceverino, Mozena, Dekel, Primack high

16 In-situ (VDI) and Ex-situ (merger) Clumps Nir Mandelker gas young stars 10 kpc dark matter stars

17 Clumps in Cosmological Simulations Ceverino, Dekel, Bournaud 10; Ceverino et al. 12; Mandelker et al Gas disks in 83% of the galaxies Off-center clumps in 70% of disks, compact & round, 3-4 per galaxy In-situ clumps Ex-situ, merging clumps Dark matter no yes Kinematics rotating disk 50/50% disk/off disk Number 70% 30% Mass 45% 55% SFR 75% 25% M clump /M disk Stellar age (Myr) ssfr (Gyr -1 ) Gas fraction Metallicity low tail no low tail

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

19 Observational indications for clump survival? Forster Schreiber et al. 11 BX482 Guo et al 11

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

21 Clump Migration on an Orbital Timescale Ceverino, Dekel, Bournaud 10

22 Clump Evolution during Migration Toomre instability 1 Migration to center: torques,.encounters, dyn. friction Mass gain M& ρ R acc d 2 T σ Q d δ 1 t σ V 2 mig δ t t δ dyn M disk M ( R disk ) tot 8t dyn Dekel, Sari, Ceverino 09 acc 8tdyn tmig 250Myr Dekel, Krumholz 13 Mandelker et al 13 Bournaud et al 13 dark matter Star formation t 1 sfr 3ε sfr ) tdyn 30tdyn 3 ( t mig Momentum-driven outflows; steady wind p& = ψ w w V L M& Simulations of wind instability * L c = V M & -1 L L 160 km s +proto-stellar winds + stellar winds + supernovae t ( ηε η t 1 1 out 3 sfr ) tdyn tsfr (1 2) V Dekel, Krumholz 13 STARBURST99 Krumholz, Thompson 13 mig t mig ψ w 2.5 η 1 2 Consistent with observed t acc t out t sfr

23 M & gas gas Clump Evolution during Migration = M & = t M& -1 gas acc M gas M& sfr -1 gas M& = out 1 dyn final mass at t mig /initial t t 0 M & ε t M stars 3 sfr 1 [( 8 f gas ) 3(1+η ) ε sfr ] -1 dyn max tidal stripping SFR only gas any η, mass varies by < x2 η~2-4, M clump ~ const. η<<1, M clump ~ x2 η>>1, M clump 0 for η<4, f gas ~ const. M gas exp ( t / t gas η~2-4 t mig <<t gas M gas ~ const. Confirmed in simulations Bournaud et al. 13, Mandelker et al. 13 )

24 Clump Survival RAMSES simulations of isolated gas-rich disks at 5pc resolution with radiative feedback η~2 Bournaud, AD, Elbaz et al. 13 Migration ~300 Myr Massive clumps survive with mass ~constant

25 Clump Evolution during Migration: Summary - SFR in clumps drives η~1-2 steady winds - Gas gain by accretion - Stellar loss by tidal stripping - The massive clumps keep ~constant mass - They live for t mig ~ 300 Myr - They feed gas & stars to the bulge - Less massive clumps disrupt Expect a weak gradient of clump mass in disks Certain gradient in age/color

26 3. Formation of Compact Spheroids Blue and Red

27 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 Inflow down the potential gradient provides the energy for driving σ to Q~1..compensating for the dissipative losses M& inflow V 2 2 Mσ t dyn t inflow t δ dyn Krumholz, Burkert 10; Bournaud et al. 11; Cacciato et al. 12; Forbes et al. 13; Dekel et al M & 25 + δ 1 3/ 2 inflow MΘyr M cold,10.5 (1 z) 3 Inflow of gas (and stars), not limited to clump migration clumpy gas disk compact stellar bulge

28 VDI-driven Inflow in Simulations Dekel et al. 2013; Cacciato stable M & 25 + δ 1 3/ 2 inflow MΘyr M cold,10.5 (1 z) VDI

29 VDI-driven Inflow in simulations M& M inflow cold 1 δ 2t dyn 2 Dekel et al M & 25 + δ 1 3/ 2 inflow MΘyr M cold,10.5 (1 z) M M cold tot σ δ 2 V

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

31 Stellar Component z=2.3 Edge-on Ceverino et al Classical bulge: n=3-5 overall: n=2-4

32 Red Nuggets and Blue Nuggets Dekel & Burkert 2013; Zolotov et al 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 Wetness parameter w t t ε δ sfr 1 2 sfr > inflow 1 M M ε sfr cold tot σ δ V 0.02 δ δ 0.2 Σ g Σ +Σ g +Σ dm Bi-modality in Σ: either compact nuggets or extended disks Start wet inflow Σ up w up wetter inflow Blue nuggets are 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 - for high mass, where outflows are weak, Σ hi, λ low

33 Wet Origin of Bulge: Stellar Birthplace Simulations: Tweed, Zolotov, Dekel, Ceverino, Primack 2013 ex-situ (mergers) Fraction of bulge stars born in in disk in bulge 60-30% of the bulge stars form in the bulge wet inflow Driven by wet VDI or wet mergers

34 Observations: Blue Nuggets > Red Nuggets Barro et al. CANDELS z=1-3 Evolution: diffuse compact quench

35 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

36 ART Cosmological Simulations with Fdbk Zolotov et al. 2013

37 Bimodality in Compactness: Blue Nuggets at Hi z extended BN Compactness Barro et al. 2013

38 Quenching: BN to RN Compact gaseous bulge -> 1. starburst -> gas removal by star formation & outflow 2. AGN feedback -> gas removal by outflow In halos > M long-term shutdown of gas supply by virial shock heating Need both bulge and halo quenching Woo et al. 13

39 Two Modes of Evolution: Fast and Slow Barro, Fang, Yesuf, Woo quenched ssfr star forming low z Halo quenching Slow: lower Σ gas disk secular inflow halo grows high z Bulge quenching stellar & AGN fdbk morph. quenching Fast: hi Σ gas disk wet VDI or merger inflow starburst diffuse compact Σ

40 ART Cosmological Simulations with Fdbk Zolotov et al. 2013

41 ART Cosmological Simulations with Fdbk Zolotov et al. 2013

42 Conclusions 1. Disks are fed by cosmic-web cold streams: smooth + mergers - Interphase streams-disk: to be studied - Outflows and inflows live in harmony 2. Violent disk instability (VDI): by intense gas in-streaming and high density - In-situ 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 certain gradients due to migration - Steady mass loss by momentum-driven outflows from clumps, η~1-2 - The clumps grow by accretion from the disk during migration, M~const. 3. VDI-driven inflow to disk center classical compact bulge - Blue nuggets (and AGN) when the inflow is wet, i.e. faster than SFR VDI and mergers. This is when Σ gas is high, at high z and in galaxies of low spin or high mass - The nuggets are dispersion-dominated - Fast mode: bulge quenching to red nuggets by stellar/agn feedback, maintained by halo heating. - Slow mode: dominated by halo quenching

43 The High-z Hubble Sequence Red nuggets Blue nuggets Clumpy disks Compact ellipticals Starburst in a compact bulge No bars Perturbed spiral patterns

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

45 Bulge mass [10 10 M ] B/D=2-4 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

46 Inflows and Outflows House, Tweed, Ceverino et al. outflow η~0.7 in-streaming ~1.7SFR

47 Outflow and Inflows