Nir Mandelker, H.U.J.I.

Transcription

1 Compressive vs Solenoidal Turbulence and Non-Linear VDI Nir Mandelker, H.U.J.I. IAU Symposium 319, August Collaborators: Avishai Dekel, Shigeki Inoue, Daniel Ceverino, Frederic Bournaud, Joel Primack

2 However

3 Compaction, Quenching, and the Main Sequence of SFGs Avishai Dekel The Hebrew University of Jerusalem IAU Symposium 319 Hawaii August 2015 Blue Nugget Red Nugget

4 Compaction Quenching, and the Main Sequence of SFGs Nir Mandelker The Hebrew University of Jerusalem IAU Symposium 319 Hawaii August 2015 Red Nugget Blue Nugget 4

5 Outline 1. Compaction and Quenching: Blue and Red Nuggets 2. Confinement of the Main Sequence of SFGs 3. Compressive vs Solenoidal Turbulence and VDI

6 Collaborators At HUJI: Avishai Dekel, Colin DeGraf, Shigeki Inoue, Sharon Lapiner, Matteo Tomassetti Elsewhere: Guillermo Barro, Frederic Bournaud, Andi Burkert, Marcella Carollo, Daniel Ceverino, Sandy Faber, Mark Krumholz, Sandro Tachella, Dylan Tweed, Joel Primack, Adi Zolotov

7 Compaction and Quenching: From Blue Nuggets to Red Nuggets Barro (CANDELS) Dekel & Burkert 2014 Zolotov, Dekel, Mandelker, et al 2015

8 Observations: Red Nuggets Van Dokkum+ 08,10,14, Damjanov+09, Newman+10, Damjanov+11, Whitaker+12, Bruce+12, z~2 M~10 11 M R e ~1 kpc low-sfr Progenitors of the cores of today s Es?

9 Wet Compaction Dekel & Burkert 2014 Compact stellar spheroid dissipative wet inflow to a blue nugget Inflow is wet if inflow > SFR In violent disk instability (VDI): torques drive AM out and mass in t inflow t sfr t 2 V tdyn 10tdyn 2 f cold tdyn Gammie 2001, Dekel, Sari & Ceverino sfr dyn f cold = gas gas + stars + dm Wetness parameter inflow 1 2 w sfr fcold 1 SFR sfr 0.02 fcold 0.2 Expect compact nuggets: - at high z, where f gas is high - for low spin, where initial R gas is low

10 Zoom in Cosmological Simulations with ART Kravtsov+ 1997, 2003; Ceverino+ 2009, 2010, zoom-in simulations M vir ~ M at z ~ 1 Maximal AMR resolution of ~25 pc Feedback Thermal - stellar winds and SNae - no shutdown of cooling Runaway stars Radiative feedback with τ IR = 0 No AGN feedback Produces mass loading of η 2 (0.2 10)

11 Bulge Growth in the Simulations Zolotov+15 mergers Fraction of bulge stars born in different components disk in bulge bulge ~ half the bulge stars formed in the bulge wet inflow

12 Observations: Blue Nuggets Red Nuggets Barro+ 13 CANDELS z=0.5-3 Evolution: diffuse compaction quenching central density

13 Observations: Blue Nuggets Red Nuggets RN Fast track to quenching BN

14 log ssfr Simulations: Compaction and Quenching quenched -1 Zolotov+15 red nugget 0 star forming +1 blue nugget diffuse compact

15 Simulations: Compaction and Quenching stars self-gravitating M stars >M dm mergers DM gas mergers +VDI outflow inflow wet inflow > SFR SFR ~outflow ~recycling SFR

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

17 vela v2 07 stars wet compaction max density core: blue nugget green nugget red nugget + envelope

18 Blue Nugget Red Nugget gas stars gas stars blue nugget red nugget Pre-BN: compaction ouside-in quenching Dense gas core dense stellar core Post BN: gas depletion from core, gas ring may form, inside-out quenching Stellar core remains dense from BN to RN

19 Blue Nugget Red Nugget naked red nugget A stellar envelope may gradually grow by dry mergers or renewed gas accretion red nugget + envelope = elliptical

20 Post BN: Inside-Out Quenching Slower Quenching in the Outer Disk inner 1 kpc whole galaxy 1 kpc 10 kpc

21 What is the Trigger of Wet Compaction? - VDI-driven inflow (Dekel, Burkert 14) - Mergers (major, minor) (Barnes, Hernquist 91; Hopkins+ 06) - Tidal compression (Dekel+ 03; Renaud+ 14) - Counter-rotating streams (Danovich+ 14, Nir+ 15) - Triaxial halo core (Ceverino+15, Tomassetti+ 15) - Return of recycled low-am gas (Elmegreen+ 14)

22 Compaction by Merger 22

23 Compaction by Intense Accretion & VDI 23

24 Confinement of the Main Sequence of SFGs Zolotov et al 2015 Tachella et al 2015c

25 The Universal Main Sequence of SFGs star forming bathtub model: M gas M in M SF (1 ) main sequence of SFGs M SF M gas / t ff 0.3 dex ssfr steady state: M SF M in quenched time evolution of main-sequence zero point: (e.g. Dekel and Mandelker 2014) ssfr M M in -1 ) 5/ Gyr (1 z M star

26 The Universal Main Sequence of SFGs MS ridge Deviation from MS ridge ssfr MS / 2 1.5Gyr M 10 (1 z) z 3 MS log ( ssfr / ssfr MS ) 0.25 dex Same simulations as Zolotov+ Tacchella+ 2015c

27 Evolution About the Main Sequence Self Regulation star forming diffuse SFG blue nugget compact gas core ssfr /(1+z) 2.5 green nugget quenched red nugget gas depleted M star

28 Blue Nuggets: Tip of the Main Sequence compact gas core gas-poor core blue nugget Main Sequence ssfr/(1+z) 2.5 Massive galaxies 1 compaction event green nugget red nugget Less massive galaxies several compaction attempts

29 Confinement of the Main Sequence star forming diffuse SFG blue nugget ssfr /(1+z) 2.5 main sequence green nugget quenched At late times red nugget M star

30 Confinement of the Main Sequence ssfr - MS ridge (cosmic accretion) ssfr MS 1 5/ 2 1.5Gyr (1 z) z 3 - ssfr up: wet compaction to BN t compact 0.3t hubble 0.7Gyr (1 z) 3/ 2 z 3 inflow > SFR M star in simulations ~ halo crossing (mergers) ~ VDI-driven inflow - Upper bound: at BN onset of quenching inflow < SFR+outflow - Lower bound: new compaction at GN need disk replenishment and a new trigger t replenish 0.7Gyr (1 z) 5/ 2 z 3 t depletion 0. 5Gyr treplenish t depletion new compaction at z>3, preferentially for lower M (halo) z M - Quenching to RS (+bending down of MS): full quenching if t rep > t dep -> Preferentially at z<3 downsizing: earlier for massive galaxies (t rep large by M halo & t dep small)

31 Full Quenching vs Quenching Attempt Inefficient replenishment full quenching efficient replenishment oscilations about the MS Tacchella+15

32 Confinement of the Main Sequence star forming diffuse SFG blue nugget ssfr /(1+z) 2.5 main sequence green nugget quenched At late times t replenish < t deplete z > 3 M halo < M shock t replenish > t deplete z < 3 M halo > M shock red nugget M star

33 Observed Gradients Across the Main t dep =M gas /SFR Sequence Genzel, Tacconi z=0-2.5 f gs =M gas /M stars t dep ~ssfr -0.5 f gs ~ssfr +0.5 Δ MS

34 Confinement of the Main Sequence star forming diffuse SFG blue nugget short t dep high f gas ssfr /(1+z) 2.5 main sequence green nugget long t dep low f gas quenched At late times red nugget M star

35 Depletion Time BN at top of MS: minimum depletion time t dep = gas mass/sfr long t dep short t dep

36 Gradients Across the Main Sequence core gas density gas fraction depletion time

37 Confinement of the Main Sequence star forming diffuse SFG blue nugget short t dep high f gas ssfr /(1+z) 2.5 main sequence green nugget long t dep low f gas quenched At late times t replenish < t deplete z > 3 M halo < M shock t replenish > t deplete z < 3 M halo > M shock red nugget M star

38 Conclusion: A Generic Sequence of Events High-z massive galaxies fed by cosmic-web streams + mergers gas-rich, dense disks - violent disk instability (VDI) Wet compaction to Blue Nuggets: by streams + mergers + VDI (in low-spin galaxies) -> compact gas disks, high SFR, flattened stellar spheroids Quenching inside-out to Red Nuggets: SFR(+AGN) + outflows > inflow -> central gas depletion. Then SFR in gas rings & stellar envelopes (ETGs) Repeated compactions in low-mass halos at high z, when inflow resumes Long-term quenching in hot massive halo at low z, when t replenish >t depletion Quenching downsizing: massive galaxies quench earlier, efficiently, at higher densities. Low-mass galaxies oscillate till inflow shutdown (halo) Confinement of the Main Sequence and gradients across it due to the evolution through episodes of compaction and quenching

39 Compressive vs. Solenoidal Turbulence and Non-linear VDI Inoue, Dekel, Mandelker et al 2015 (in prep) Mandelker, Dekel, Inoue et al 2015 (in prep) Work in Progress!

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

41 Violent Disk Instability (VDI) at High z Compaction through torques and AM transport Mass inflow to bulge + black hole Formation of giant star forming clumps Typically associated with Toomre instability, due to High gas fractions and surface densities at high z Q 1 However In simulations, VDI deviates from linear Toomre instability Q=2-5 nonlinear instability stimulated by in-streams with minor mergers

42 Non Linear Formation of Clumps

43 Non Linear Formation of Clumps

44 Non Linear Formation of Clumps

45 Non Linear Formation of Clumps

46 Non Linear Formation of Clumps

47 VDI with Q~2 3 Toomre Q / 1 Q=2-5 Q=1-2 Q=5-10 Q=1-2 Nonlinear instability stimulated by intense inflows with minor mergers, or by the non-linear clumps themselves

48 Non-Linear Instability Tentative ideas for Q>1 instability: - Rapid decay of turbulence (Elmegreen) Q<2 - Irregular rotation counter-rotating streams (Lin) - Compressive modes of turbulence solenoidal mode Stabilizing compressive mode De-stabilizing Toomre Q 1 In equilibrium, σ s 2 2σ c 2 If compressive mode dominates, e.g. during mergers due to compressive tides (Renaud+2014), then high σ high Q, but unstable

49 Compressive vs Solenoidal Modes Work in Progress! V19 V03 V07 V01

50 Open Questions What causes compressive modes to dominate? Compressive modes Clumpy discs compressive modes? Stimulated formation of new clumps in wake of old clumps Modification to Toomre Q?