Spin Acquisition, Violent Disks, Compaction and Quenching

Transcription

1 Spin Acquisition, Violent Disks, Compaction and Quenching Avishai Dekel The Hebrew University of Jerusalem July 2014 stars 5 kpc

2 Three Provocative Questions concerning high-z massive galaxy formation 1. How do galaxies acquire AM? Gas ~ DM? 2. Do we understand violent disk instability? 3. How do galaxies compactify and quench? Hydro simulations cosmological - 25pc, isolated 1pc resolution - ART (Klypin, Kravtsov, Ceverino) - RAMSES (Teyssier, Bournaud+) Combined with toy modeling

3 1. Angular Momentum: from the cosmic web to disks & spheroids Pichon, Devriendt Pichon, Devriendt Stewart, Bullock+ 2011, 2013 Danovich, Dekel+ 2012, 2014

4 Massive halos at high-sigma nodes are fed by relatively thin dense filaments cold streams Typical halos reside in relatively thick filaments, fed from all directions the millenium cosmological simulation

5 Gas streams along the cosmic web AMR RAMSES Teyssier, AD box 300 kpc res 50 pc z = 5 to 2.5

6 Streams Feeding a Hi-z Galaxy Tweed, Dekel, Teyssier RAMSES Res. 50 pc

7 Co-planar ~3 Streams (in a pancake) influx M yr -1 rad R vir Danovich, Dekel, Teyssier, Hahn 12

8 Narrow dense gas streams at high z versus spherical infall at low z high z low z M=10 12 M ʘ >>M PS M=10 12 M ʘ ~M PS Ocvirk, Pichon, Teyssier 08

9 Cold Streams Penetrate through Hot Halos M v > M 100 kpc Agertz et al 09

10 AM Buildup by Cold Gas in 4 Phases III. inner halo extended tilted ring non-linear torques, dissipation AM loss λ cold 0.04 & alignment Danovich, Dekel, Hahn+ 14 II. outer halo AM transport, j~const. λ cold ~3λ dm ~0.1 DM mix V v I. cosmic web linear tidal torques impact parameter λ cold ~1.7λ dm ~ R v 2R v IV. inner disc (+ bulge) disk instability, outflows λ baryons ~0.03 spin parameter λ ~ J / M 2R V V V

11 TTT outside the halo: λ cold ~1.7λ DM due to quadrupole moment of inertia J tε i ijk T jl I lk R v ~100 kpc cold gas dark matter TTT is applied at max-expansion along the streams, after pre-collapse of gas to the filaments cords

12 AM of Cold Gas R v AM is represented by impact parameters <0.3R v Some counter-rotating In outer halo AM transport by straight streams Most of the AM is in one stream (determines the AM plane at R v ) Deep penetration of the streams

13 How do the streams join the disk? Ceverino, Dekel, Bournaud 2010 ART 35-70pc resolution streams disk 30 kpc interface region A messy interface region: breakup due to shocks, hydro and thermal instabilities, collisions between streams and clumps, heating

14 An Extended Tilted Ring about the Disk gas density 30 kpc stream lines expressway entrance

15 A tilted AM transport rotating ring the in outer the inner halo halo radial inflow AM loss circular orbits AM conserved spiral in alignment with disk color indicates mass in each cell impact parameter ~ const. AM not aligned with disk

16 AM Exchange in the Ring: Torques by Disk torques by an idealized disk Torques in the simulated galaxies

17 Extended Ring: HI Column Density Random lines of sight through ( )R v 30% DLAS HI 60% no HI n > 0.01 H cm -3

18 Detection of an Extended Ring? Bouche z=2.3 Low-Z gas 26 kpc from center V=180 km/s Crighton z=2.4, 54 kpc Steidel+ 2002, Kacprzak+ 2010

19 Outflows do not halt the Inflows DeGraf+ 14 Gas density Temperature Velocity dilute hot z=2.6 M v =7x Dense, cold, metal-poor inflows penetrate into the galaxy - Hot, metal-rich, fast outflows fly through the dilute CGM -300 M yr -1 rad -2 - outflows remove low-angular-momentum gas outflows help quenching SFR +50

20 AM Evolution in Disks Gas-rich -> violent disk instability (VDI) (Noguchi 99; Dekel+ 09) -> torques -> AM outflow and mass inflow (Gammie 01) -> massive spheroids (+BHs) with low AM (Genzel+ 08; Bournaud+11; Dekel+ 13) Stellar and AGN feedback -> outflows remove low-am gas from galaxy centers (Maller & Dekel 02; Governato+ 10; Guedes+ 11) λ gal < λ disk ~ 0.03 λ disk is only slightly smaller than λ DM -> naïve model is ~valid despite the different AM evolution

21 2. Violent Disk Instability Clumpy disk galaxies: Elmegreen+ UDF Genzel, Tacconi, Forster-Schreiber+ SINS Guo, Giavallisco+ 12, 14 CANDELS

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

23 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+ 04a,b Bournaud, Elmegreen+ 06, 08 Hopkins+ 12 Bournaud+ 13 In cosmology: Dekel, Sari, Ceverino 09 Agertz et al. 09 Ceverino, AD, Bournaud 10 Ceverino+ 11 Cacciato, AD, Genel 12a,b Genel+ 12 Forbes et al. 12, 13, 14 Self-regulated at Q~1 by torques and inflow high σ/v~1/5 Inflow in disk compact bulge and BH Steady state: disk draining and replenishment, bulge ~ disk

24 Violent Disk Instability (VDI) at High z Ceverino+ ART-AMR cosmological simulations at 25pc resolution highly perturbed, clumpy rotating disk: H/R ~ σ/v ~ f cold ~ 0.2

25 Violent Disk Instability (VDI) at High z Ceverino+ ART-AMR cosmological simulations at 25pc resolution H/R ~ σ/v ~ f cold ~ 0.2

26 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). In some galaxies from z>7 to z<1. 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. 14

27 Elmegreen et al Observations vs. Simulations

28 A typical star-forming galaxy at z=2: clumpy, rotating, extended disk & a bulge Hα star-forming regions color-code velocity field Genzel et al 08

29 BzK 6004 (2.4) BzK (2.4) BX 610 (2.2) BX482 (2.2) ZC (2.2) merger merger -160 BX389 (2.2) D3a 6397 (1.51) +50 K20-7 (2.2) BX663 (2.4) MD 41 (2.2) K20-9 (2.0) HDF 242 (2.49) ZC (1.41) BX528 (2.3) (8 kpc) -70 K20-8 (2.2) -170 K20-6 (2.2) K20-5 (2.2) GK2471 (2.43) D3a 4751 (2.27) SA (1.51) 150 HDF 169 (1.2) BX 405 (2.03) GK2252 (2.41) BX 599 (2.33) 100 BzK 4165 (1.7) SMMJ09431 (3.35) H7 H6 HDF 76 (2.20) SA (2.3) BX 502 (2.16) N (2.45) BM 1163 (1.41) GK 167 (2.58) SA (2.2) BX 404 (2.03) (Förster SMMJ Schreiber (3.41) et al. 2006, 2008) SMMJ (1.21) N (2.38) +200 GK 2113 (1.61) (8 kpc) The SINS survey of galaxy kinematics at z~

30 High-z Disks with Giant Clumps Guo et al. 12 CANDELS

31 Simulated hi-z galaxy through Dust SUNRISE low dust RGB colors MW3 z=2.33 Moody+ medium high

32 In-situ (VDI) and Ex-situ (merger) Clumps gas Poster by Nir Mandelker: clump properties, young survival stars under feedback, observable gradients of age/color 10 kpc dark matter stars

33 Clumps in VDI Disks - most hi-z galaxies go through a VDI phase - perturbed by intense inflows including minor mergers - bulge ~ disk in cosmological steady state - giant clumps M~ M R<0.5kpc - in-situ (gaseous, SFR) and ex-situ (stellar, mergers) - half the SFR in clumps - migration to center in ~300 Myr gas+ young stars - clumps >10 8 M survive outflows with mass~constant η~1-2 winds, gas accretion, tidal stripping - less massive clumps disrupt - VDI feed gas & stars to the bulge and BH Expect a weak gradient of clump mass in disks Certain gradient in age/color for in-situ clumps

34 Violent Instability with Q~2-3 Toomre Q Ωσ / Σ 1 Q=1-2 Q=2-5 Q=1-2 Q=5-10 Nonlinear instability - driven by intense inflows with minor mergers, or by the non-linear clumps themselves Compression modes of turbulence r r r σ = σ + σ = r φ + r irrotation solenoid A r

35 Compression Modes of Turbulence: Merger r r r σ = σ + σ = r φ+ r irrotational solenoidal A r Renaud+ 14

36 3. Compaction to Blue Nuggets Quenching to Red Nuggets Cheung+ 12; Fang+13; Barro+ 13,14a,b; Bruce+ 12,14; Williams+ 14; Nelson, van Dokkum+ 14 Dekel & Burkert 2014; Zolotov et al. 2014

37 Inflow in unstable disks Clump migration in ~300 Myr Massive clumps survive feedback Elmegreen, Bournaud+ 07, 08; Genzel+ 06, 08; Dekel, Sari, Ceverino 09; Bournaud+ 14; Dekel+ 14 Inflow in disk, evaluated by torques, dynamical friction, clump encounters, self-regulated instability t 2 inflow f cold t dyn 2 ( V σ) tdyn 10tdyn Gammie 01; Dekel, Sari, Ceverino 09 Wet compaction if 2 tinflow / tsfr εsfr fcold< 1 valid when gas fraction is high (high z) and spin is relatively low Dekel, Burkert 14 Bournaud, Dekel+ 13

38 Red Nuggets and Blue Nuggets Dekel & Burkert 2013; Zolotov et al Compact stellar spheroid dissipative wet inflow to a blue nugget by mergers and/or VDI Inflow is wet if t inflow << t sfr Self-regulated instability Q ~ 1 Wetness parameter M M cold M tot σ δ V tsfr 1 2 w ε sfrδ > 1 ε sfr 0.02 δ 0. 2 t inflow Expect VDI-driven nuggets: - at high z, where f gas is high - for low spin λ, where R gas is low

39 Wet Origin of Bulge: Stellar Birthplace Zolotov, Dekel, Mandelker, Tweed, Ceverino, Primack 2013 Fraction of bulge stars born in different components in bulge 60-30% of the bulge stars form in the bulge wet inflow Driven by wet VDI or wet mergers

40 Compaction and quenching Zolotov ART cosmological simulations, res. 25pc, with radiative fdbk SFR ~outflow ~recycling VDI + merger self-gravitating M stars >M dm wet inflow > SFR

41 Compaction and quenching stars self-gravitating M stars >M dm mergers DM merger gas no mergers VDI outflow inflow wet inflow > SFR SFR ~outflow ~recycling SFR

42 gas + young stars wet compaction max density: blue nugget vdi disk a hole and a ring vela v2 07

43 stars wet compaction max density: blue nugget green nugget red nugget vela v2 07

44 Stellar Component at z=2.3, edge-on Ceverino Overall Sersic n=2-4 Classical bulge n=3-5

45 Blue and Red Nuggets blue nugget Zolotov, AD+ 14 ssfr quenching SFR stars wet compaction z=3.7 central density SFR stars Observed at z~2-3: - compact passive ellipticals - their progenitors: compact star-forming galaxies z=1.2 red nugget

46 Observations: Blue Nuggets > Red Nuggets Barro+ 13 CANDELS z=1-3 Evolution: diffuse compaction quenching

47 Similar Structure for Blue & Red Nuggets Z=2 M * =10 11 M R e =1 kpc σ=300 km s -1 SFR=90 M yr -1 Nelson, vandokkum+ 2014

48 line width evolution in simulated galaxies quenching blue nugget red nugget extended disk compaction Inoue, Zolotov+ Barro+ 14

49 Blue Nuggets by Wet Inflow: Spin and ssfr Simulations confirm model predictions Dekel, Burkert 14; Zolotov+ 14 low-spin disk -> high Σ max 0.7 ssfr 0.5 high-ssfr disk -> high Σ max 0.3 Σ max

50 Two Modes of Evolution: Fast and Slow Barro, Fang, Yesuf, Woo, Faber, Koo, AD 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

51 critical halo mass ~10 12 M ʘ Virial Shock Heating Dekel & Birnboim t cool < t compress Kravtsov+ in hi-z massive hot halos cold streams penetrate slow cooling -> shock fast cooling > no shock

52 Cold Streams in Big Galaxies at High z M vir [M ʘ ] all hot cold filaments in hot medium M shock ~M * M shock >>M * M shock all cold M * redshift z Dekel & Birnboim 06

53 Two Quenching Mechanisms: Bulge & Halo Compact gaseous bulge -> gas removal by high SFR, outflow, AGN, Q-quenching quenched In halos > M -> long-term shutdown of gas supply by virial shock heating Woo, Dekel, Faber, Koo+ 14 star forming Need both bulge and halo quenching

54 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

55 Conclusions High-z massive galaxies at cosmic-web nodes Fed by ~3 co-planar streams penetrating hot CGM Angular-momentum: - effective tidal torques on gas streams, AM transport to inner halo - spiral-in through an extended rotating tilted ring (DLAS?) - disk spin halo spin Typical SFGs have perturbed rotating disks at violent instability (VDI) - Massive clumps (>10 8 M ) survive feedback - off-center in-situ young clumps <300 Myr, showing age/gas gradient - older ex-situ clumps Nonlinear instability driven by inflow+mergers. Compressive turbulence? A characteristic sequence of events: - wet compaction by mergers and VDI into compact SFGs (blue nuggets) - high SFR+AGN, outflows, massive self-gravitating bulge fast quenching to compact ellipticals (red nuggets) +gas rings (?) - long-term quenching by hot massive halo