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Gemini IFU Observations of Feedback from Radio-Quiet Quasars at z~0.5 Black Hole Feedback 2012 Guilin Liu JHU/CAS Nadia L. Zakamska JHU/CAS Jenny E. Greene Princeton Nicole P. H. Nesvadba Insitut d'Astrophysique Spatiale Xin Liu CfA/Hubble Fellow Thirst for Quasar Feedback: Galaxy luminosity function Bright end needs mass-dependent quasar feedback to quench SF! + SNe + SNe + AGN Croton et al. 2006 (as taken from Guinevere Kauffmann's talk) + SNe + AGN + Reionization Thirst for Quasar Feedback: BH mass-buldge correlation • Fact – BH masses in nearby galaxies strongly correlate with many galaxy properties • Implication – BH evolution has profound effects on galaxy formation MBH • LBuldge / Msph / σc / re ... • Puzzle – Physical mechanism? – masses / sptial scales vastly different – need galaxy-wide feedback σ (km s-1) Gultekin et al. 2009 Thirst for Quasar Feedback: To reproduce BH-galaxy correlation... • Thermal heating? – 5% × quasar energy is sufficient to expell gas and quench SF – Hopkins et al. 2006, ClaudeAndre Faucher-Giguere's talk • Momentum-driven? – < 1% × quasar energy is sufficient – Zubovas & King 2012, J. Ostriker and his group • Radio jets? – strong: radio galaxies / RL quasars – weak: NGC 3079 (?) Hopkins et al. 2006 unobscured (Type 1) Radio-loud objects Jets can do serious damage to galaxy r ed u c ) obs pe 2 (Ty Jet-driven winds induces bow-shock and cocoon, deposit mechanic energy into ISM/IGM - both in observations and simulations Urry & Padovani 1995 Geibler 2011 Radio-loud objects Jets can do serious damage to galaxy turbulent outflows detected at z~2 emision regions follow the jet physical scales are tens of kpc velocity ~ 1000 km/s, dispersion ~ 1000 km/s kinetic energy ~1060 erg Nesvadba et al. 2006, 2008 Standard wisdom Stockton & MacKenty found ~30% RL quasars have "extended emission line regions" (~50 kpc) RQ quasars don't have them photoionized by nucleus galaxy-scale winds driven by radiation? But only ~10% quasars are radio-loud... Stockton & MacKenty 1987 Our Gemini IFU Observations 11 SDSS RQ (+3 RL) quasars that are: – obscured (type 2) – highly luminous • Lbol~1047 erg/s or higher • mass dependent feedback expected – from Zakamska et al. (2003) and Reyes et al. (2008) catalogs Integral field spectroscopy @ Gemini – FoV: 5"×7" – seeing 0.4"-0.6" – spectral resolution ~50 km/s Credit: Durham Univ. [O III] 5007Å Intensity Maps Radio-Quiet Quasars extended ionized nebulae seen in EVERY case; regular and round morphology physical extents of 20-40 kpc All objects are spatially resolved Radio-Loud Quasars Liu et al, in prep RQ Quasars Zakamska et al, in prep Well-organized velocity fields, signature of outflows (| Δv| ≤ 100 km/s) [O III] 5007Å Radial Velocity Maps Radial Velocity FWHM duoL- oi da R Nesvadba et al. 2008 RQ vs. RL Quasar Outflows • Comparable outflow extent: – 20 - 40 kpc • Similar velocity dispersion: – up to ~1000 km/s ei u Q- oi da R • RQ quasars have larger opening angles Zakamska et al, in prep RQ vs. RL Quasar Nebulae • 3 RL objects at z=2-3 – Nesvadba et al. 2008 • Size – similar at z~0.5 – smaller than z=2-3 RLs • Ellipticity – RQ: ε < 0.25 – RL: ε > 0.25 or irregular – one exception Liu et al, in prep Galaxy-Wide Outflowing Gas Ionized Gas vs. Host Galaxy • Size: [OIII] > continuum • Ellipticity: ~ same – only one exception – [OIII] ~ 2.1 × Continuum – regular and round – ε ~ 0.1 Liu et al, in prep Size-Luminosity Relation isophotal radius at 10-15/(1+z)4 erg/s/cm2/□" power index = 0.24 ± 0.02 theoretical expectation: 0.5 matter-bounded? asar u q ured c s b o 0.6 1 . z=0 s es laxi a g y-2 S l loca T HS na a -b w rro nd g gin a im Liu et al, in prep RQ quasar outflow: Why not observed before? • Sensitivity? – narrow-band imaging shallower than long-slit spectroscopy and IFU • Luminosity dependence? – Villar-Martin, Humphrey et al. found <20% at lower luminosities – 0.8 dex increase in [OIII], detection fraction changes <20% to >50% • Viewing angle? – type 2's more favorable? • Fooled by long-slit data? – limited spatial information Humphrey et al, 2010 Next Steps • Go for unobscured quasars – Evolution? • Gemini IFU (PI: Liu) - approved • Continue observing low-z high-L obscured quasars – star formation: • Herschel (PI: Zakamska) - approved – molecular outflow: • ALMA (PI: Greene) - approved – weak jets? • Karl G. Jansky VLA (PI: Liu) - approved • Probe higher redshifts – newly identified obscured quasars at z=2-3 from BOSS • HST (PI: Michael Strauss) - approved • ALMA (PI: Zakamska) - pending Summary Galaxy-wide quasar feedback will save theorists Jets from RL objects are seen to have strong effect on ISM/IGM RL objects are rare, what about RQ quasars? RQ quasars at highest luminosity commonly have outflows that are galaxy-wide, round, and likely energetic