(radio-mode) AGN feedback in semi- analytics Nikos Fanidakis - PowerPoint PPT Presentation

(radio-mode) AGN feedback in semi- analytics Nikos Fanidakis Quenching & Quiescence With: Andrea Macciò (MPIA), Alvaro Orsi (PUC), Salvo Cielo (MPIA), George Mountrichas (NOA), Antonis Georgakakis (MPE), Carlton Baugh (Durham), Mirko Krumpe (ESO), Cedric Lacey (Durham), Carlos Frenk (Durham)

Motivation for introducing AGN feedback Stellar feedback AGN feedback Maximum galaxy formation efficiency Log 10 (M stellar /M halo ) � Moster et al. (2010) Log 10 (M halo /M ! ) � Nikos Fanidakis – ITP Zurich 4.3.2014 Nikos Fanidakis – Marseille 12.06.2014 Nikos Fanidakis – Q&Q 15.07.2014

“Radio mode” AGN feedback Standard AGN feedback scheme in semi-analytics Rapid-cooling regime Static-halo regime M halo ~10 11.5 M ! ! " Gas in > 10 11.5 M ! haloes is in blue% quasi-hydrostatic equilibrium. " Outflows (jets?) driven by the r cool ! central AGN heat the halo and r cool = r ( τ cool = τ H ) ! supress the cooling of gas. τ cool ~ τ ff τ cool >> τ ff Only gas in quasi- hydrostatic equilibrium can be efficiently heated red% See Croton et al (2006); Bower et al. by the central AGN. (2006); Monaco et al. (2007); Somerville et al (2008); Lagos et al. (2008) Nikos Fanidakis – ITP Zurich 4.3.2014 Nikos Fanidakis – Q&Q 15.07.2014

Implementation in SAMs MUNICH model (Croton et al. 2006): ! 3 ⇒ L jet = 0.1 ! M BH c 2 M BH ∝ M BH f hot V vir L jet m cool = ! ! ! m cool − 2 0.5 V vir See also Rachel Somerville’s (2008) model and MORGANA model (Monaco et al. 2007) GALFORM model (Bower et al 2006): Cooling in massive haloes is suppressed if: L jet = f jet L Edd , f jet ~ 0.04 M BH = L cool L jet ≥ L cool ⇒ ! ε r c 2 Typical accretion rates are below 1-10% of the Eddington accretion rate. Nikos Fanidakis – ITP Zurich 4.3.2014 Nikos Fanidakis – Q&Q 15.07.2014

Effect on gas cooling Average cooling rate Cooling flow suppression is most efficient in massive haloes at late epochs. ! m heat ∝ M BH V vir Croton et al. (2006) Nikos Fanidakis – ITP Zurich 4.3.2014 Nikos Fanidakis – Q&Q 15.07.2014

Effect on stellar mass Moster et al. (2011) z = 0 with AGN feedback w/o AGN feedback AGN feedback is necessary for reproducing the correct stellar mass in massive haloes! GALFORM Nikos Fanidakis – ITP Zurich 4.3.2014 Nikos Fanidakis – Q&Q 15.07.2014

With AGN feedback we reproduce � The paucity of galaxies in the bright end of the LF. � The colour bimodality of galaxies. Croton et al. (2006) See also: Monaco et al. (2007), Lagos et al. (2008), Somerville et al. (2008) Nikos Fanidakis – ITP Zurich 4.3.2014 Nikos Fanidakis – Q&Q 15.07.2014

With AGN feedback we reproduce Bower et al. 2006 � The paucity of galaxies in the bright end of the LF. � The colour bimodality of galaxies. Bower et al. (2006) See also: Monaco et al. (2007), Lagos et al. (2008), Somerville et al. (2008) Nikos Fanidakis – ITP Zurich 4.3.2014 Nikos Fanidakis – Q&Q 15.07.2014

Linking feedback to AGN: BH growth in GALFORM Hot-halo (radio) mode Starburst (quasar) mode 1. Disk instabilities 2. Galaxy mergers M halo > 10 11.5 M ! ! t 1 t 1 t 2 t 2 M BH = L cool ! M BH = Δ M acc ε r c 2 ! f q t dyn t 3 t 3 We trace the evolution of BH mass, spin and accretion rate from z >> 20 to z = 0 Quasar Hot gas Cold gas/Stars Dark matter NF et al. (2011, 2012) See also: Malbon et al. (2007), Marulli et al (2008), Somerville et al (2008), Hirschmann et al (2012) Nikos Fanidakis – ITP Zurich 4.3.2014 Nikos Fanidakis – Q&Q 15.07.2014

Linking feedback to AGN: Modelling the accretion flow Blandford – Znajek mechanism hot halo for Jet formation: AGN ADAF ~10 − 100 L jet 2 α 2 , with L jet L jet ∝ ( H / R ) 2 M BH TD Central engine jet ! R H BH ! DM halo accretion disk Thin disk ADAF m = ! M / ! ! M Edd < 0.01 luminous disks under-luminous disks TD , ε ADAF = 0.01 − 0.1 ADAF = ε ADAF L disk L disk (NF et al 2011) % Nikos Fanidakis – ITP Zurich 4.3.2014 Nikos Fanidakis – Q&Q 15.07.2014

Linking feedback to AGN: Luminosity functions NF et al. (2013a) Hot-Haloes Starbursts Optical LF Super-Eddington Log 10 ( Φ (L HX ) ) [Mpc -3 dex -1 ] X-ray LF z = 1 NF et al. (2012) Nikos Fanidakis – ITP Zurich 4.3.2014 Nikos Fanidakis – Q&Q 15.07.2014

Effects of feedback on AGN: The AGN colour bimodality Contours = galaxies Red cloud: Red and poor in gas galaxies The model predicts a bimodal distribution of AGN on the BV — stellar mass plane. Blue cloud: star forming and rich in gas galaxies NF & Georgakakis (in prep) Nikos Fanidakis – ITP Zurich 4.3.2014 Nikos Fanidakis – Q&Q 15.07.2014

Effects of feedback on AGN: The AGN colour bimodality Contours = galaxies Points = AGN Red cloud: Red and poor in gas galaxies The model predicts a bimodal distribution of AGN on the BV — stellar mass plane. Blue cloud: star forming and rich in gas galaxies NF & Georgakakis (in prep) Nikos Fanidakis – ITP Zurich 4.3.2014 Nikos Fanidakis – Q&Q 15.07.2014

Effects of feedback on AGN: The clustering of moderate luminosity AGN Hot-halo accretion is essential for reproducing the halo mass of moderate luminosity AGN! L xray = 10 42 -10 44 erg/sec ! NF+(2013a) Nikos Fanidakis – ITP Zurich 4.3.2014 Nikos Fanidakis – Q&Q 15.07.2014

Effects of feedback on AGN: The clustering of Quasars NF+(2013b) most massive halo The AGN feedback shapes the halo environment of luminous Quasars! Luminous Quasars 2QZ survey Croom et al. (2004) See also: Ross et al. (2009), White et al. (2012), Shen et al. (2013) Nikos Fanidakis – ITP Zurich 4.3.2014 Nikos Fanidakis – Q&Q 15.07.2014

Effects of feedback on AGN: The Radio Galaxy Luminosity Function Radio LF dominated by NF +(2011) rapidly rotating BHs accreting in the hot-halo mode! L jet ∝ ( H / R ) 2 B φ 2 M BH ˙ a 2 m jet ! Blandford & Znajek 1977 R H BH ! accretion disk Nikos Fanidakis – ITP Zurich 4.3.2014 Nikos Fanidakis – Q&Q 15.07.2014

Effects of feedback on AGN: The clustering of Radio Galaxies z = 2 ! The dependence of BH parameters on the Millennium simulation environment creates the right conditions for reproducing the clustering of Radio Galaxies NF (PhD thesis) Radio galaxies trace the peaks of the Dark-Matter distribution z = 2 ! See also: Wake et al. (2008); Donoso et al. (2008) Nikos Fanidakis – ITP Zurich 4.3.2014 Nikos Fanidakis – Q&Q 15.07.2014

Summary With a phenomenological calculation for the accretion rate that is linked to AGN feedback we get: 1. The correct evolution of AGN 2. The colour bimodality of AGN 3. The clustering of moderate luminosity AGN and luminous Quasars The abundance & clustering of Radio Galaxies 4. Take away message: AGN feedback & associated growth mode crucial for reproducing key AGN properties Nikos Fanidakis – ITP Zurich 4.3.2014 Nikos Fanidakis – Q&Q 15.07.2014