the self-regulated agn feedback loop: chaotic cold accretion

Transcription

1 the self-regulated agn feedback loop: chaotic cold accretion Massimo Gaspari Max Planck Institute for Astrophysics

2 the self-regulated agn feedback loop: raining onto black holes Massimo Gaspari Max Planck Institute for Astrophysics

3 self-regulated agn feedback AMR zoom-in 3D simulations (FLASH) FEEDING cold versus hot mode linking host scale to sub-pc scale beyond classic Bondi and thin disc turbulence, cooling, heating, rotation: chaotic cold accretion [CCA] MG sims FEEDBACK amount of energy released deposition of energy mechanical versus thermal bubbles, shocks, metal uplift, turbulence, L x -T x <---> observations MG sims SELF-REGULATED LOOP P out = ɛ ṀBHc 2

4 feeding: smbh accretion FLASH4 simulations MG concentric AMR zooming: box = 50 kpc dx ~ 20 R S pc ~10 million range 600 r B and 200 t B 3D eulerian gas dynamics: unsplit PPM (3rd order) + varying physics massive group dark matter halo: Mvir = 4x10 13 M ʘ central elliptical galaxy (NGC 5044): Mstar = 3.4x10 11 M ʘ SMBH: Mbh = 3x10 9 M ʘ relativistic PW: φ PW = GM bh /(r R S ) observed gas T(r) [cool-core] n(r) via hydrostatic equilibrium

5 turbulence in hot halos AGN feedback, SNe, mergers, galaxy motions,... subsonic (~100 km s -1 ) ICM turbulence MG+2014 Gaspari & Churazov D velocity Density v cut δρ/ρ Mach 1D

6 hot accretion MG+2013 MG+2015 rotation < turbulence BHAR rotation > turbulence Ta t v rot /σ v < 1 Ta t v rot /σ v > 1 σ v 100 km s 1 v rot,gas 100 km s 1 pure Bondi Ta t < 1 Ta t > 1 Ṁ Bondi =4π(GM BH ) 2 ρ /c 3 s,

7 Werner et al. (2014) Perseus Fabian et al.

8 pure cold accretion MG+2013 MG+2015 no rotation rotation cold thin disc adiabatic (rotation)

9 Global thermal equilibrium AGN outflow feedback: net heating deposition erg/s/cm 3 internal energy increase (averaged over 1 Gyr) MG+2012 H L

10 chaotic cold accretion [CCA] MG COOLING + TURBULENCE + AGN HEATING σ v 100 km s 1 H L

11 chaotic cold accretion [CCA] MG+15 Ṁ BH 100 ṀBondi Ṁcool Ta t < 1 CCA dominates cold phase Ṁ cool Ta t 0.75 Ta t 1.5 pure Bondi Ta t 3 Ta t > 1 disc dominates

12 cold vs hot accretion t cool/t ff < 10 => condensation & TI chaotic cold accretion Ṁ BH 100 ṀBondi X-ray temperature t cool/t ff >> 10 => overheated phase stifled Bondi/hot accretion Ṁ BH 1/3 ṀBondi X-ray temperature ~ flat T X profile cuspy T X profile e.g. NGC 3115 (Wong et al. 2014) NGC 4261, 4472 (Humphrey et al. 2009) M87 (Russell et al. 2015) e.g. NGC 4649 (Humphrey et al. 2008) NGC 1332 (Humphrey et al. 2009)

13 Halpha SIMS MG+15 full CCA disc mode SOAR DATA Werner+14

14 Raining on to black holes DENS MG+13 Highly clumpy & turbulent torus (key for AGN unification theory) Cold clouds can form the BLR/NLR or HVC & induce rapid variability in L AGN Tight symbiosis between the BH and the whole galaxy: Fast communication time BH - galaxy and boosted accretion M BH M cold M Ṁ BH CCA main driver of agn feedback Ṁcool

15 Feedback FLASH4 simulations MG Cluster Group Elliptical large-scale runs: 100 pc - 2 Mpc Dark matter + central galaxy potential Radiative cooling M vir M,R vir 2.5 Mpc M vir M,R vir 0.9 Mpc M M,R eff 10 kpc Stellar evolution: heating + mass loss Bipolar AGN outflows + self-regulation: 1 2ṁjetv 2 jet = P jet = ɛ Ṁaccc 2 Ṁ acc Ṁcool

16 AGN feedback Cycle MG+2012 L > H z (kpc) t cool/t ff 10 thermal instabilities cold clumps DENS x (kpc) feed SMBH Log n Log n feedback boosted L < H PHASE PLOT Log T

17 agn outflows + cca feedback galaxy group NGC 5044 MG+2012 pure CF INJECTED ENERGY AGN feedback Quenched cooling: < 5-10% CF JET POWER DENS Cool core preserved Mechanical efficiencies: ~ 5x x10-3 X-ray TEMP isolated galaxies ---> clusters Pout = f M cool c2 Lx M cool T c2s /f c2 JET VELOCITY

18 32 b. 32 f. AGN imprints cocoon shocks turbulence bubbles ~ 5-10 kpc metal uplift DENS X-ray TEMP X-ray SB IRON 32 l. 32 p Gitti HCG Outer Cavity Randall NGC 5813 Edge 20 Kpc David NGC NE Cavity NW Cavity Middle Cavity Edge kpc Inner Cavities Middle Cavity S Cavity

19 quenching the soft x-ray spectrum MG 2015 X-ray data constraints simulations: 1. AGN outflows deposits relatively more heat in the inner cooler phase 2. turbulence becomes transonic in the cooler phase => stronger diffusion

20 SIMS L x - T x (core) L x - T x (no core) SIMS can agn feedback break self-similarity? MG+2014 solid line: stacking central brightest galaxies (X-ray flux-limited) Anderson, Gaspari, White+2015 central cooling time COOL CORE DESTROYED X-ray data: cool-core structure must be preserved for several Gyr COOL CORE PRESERVED black filled points: AGN feedback simulations

21 SELF-REGULATED AGN FEEDBACK L > H MG > 2015 chaotic COLD mode (flat T X profile) t cool/ t ff < 10 extended TI chaotic collisions: Ta t < 1 subsonic turbulence ~ 100 km/s clumpy torus & filaments (< 10 kpc) (obs.: McDonald et al. 2011,2012, Werner et al. 2013, Wong et al. 2014) tight and fast symbiosis BH - M bulge Ṁ BH 100 ṀBondi Ṁcool mechanical feedback quench the cooling flow and SF bubbles, shocks, metal uplift disc COLD mode stifled HOT mode (cuspy T X profile) Ta t > 1 t cool/ t ff >> 10 Ṁ BH < L < H ṀBondi residual cold disc: system overheated Ṁ BH Ta 1 (obs.: Young et al. 2011, Alatalo et al. 2013, Werner et al. 2013) (obs.: Humphrey et al. 2008, 2009) t