Quest for Galaxy-Wide Quasar Feedback

Transcription

1 Quest for Galaxy-Wide Quasar Feedback Guilin Liu 刘桂琳 University of Science and Technology of China

2 Main collaborators Nadia L. Zakamska Jenny E. Greene Nicole P. H. Nesvadba Xin Liu ( 刘昕 ) Johns Hopkins Univ. Princeton Univ. Université Paris-Sud 11 Univ. of Illinois The USTC company: 王挺贵, 周宏岩, 孔旭 Graduate students at USTC: Michael A. Strauss Princeton Univ. - 何志成, 高玉龙, 赵沁园

3 Outline - Why we need quasar feedback - Luminous z~0.5 quasars are outflowing ubiquitously - Case studies of low-z quasars - BAL quasars: IFU mapping - BAL quasars: absorption troughs - Red quasars at z~0.5 and z>2 - Summary

4 Thirst for Quasar Feedback: Ultimate questions: how do galaxies co-evolve with black holes? Large-scale outflow blows gas away Quasar Mrk 509 (Liu et al. 2015) Black hole BH grows by accreting gas gas collapses to form stars Quasars = active supermassive black holes M16 KPNO 2.1m)

5 Thirst for Quasar Feedback: Galaxy luminosity function Bright end needs mass-dependent quasar feedback to quench star formation! Croton et al (taken from G. Kauffmann's talk)

6 Thirst for Quasar Feedback: Galaxy luminosity function Bright end needs mass-dependent quasar feedback to quench star formation! + SNe Croton et al (taken from G. Kauffmann's talk)

7 Thirst for Quasar Feedback: Galaxy luminosity function Bright end needs mass-dependent quasar feedback to quench star formation! + SNe + SNe + AGN Croton et al (taken from G. Kauffmann's talk)

8 Thirst for Quasar Feedback: Galaxy luminosity function Bright end needs mass-dependent quasar feedback to quench star formation! + SNe + SNe + AGN + SNe + AGN + Reionization Croton et al (taken from G. Kauffmann's talk)

9 Fact Thirst for Quasar Feedback: BH mass-buldge correlation BH masses in nearby galaxies strongly correlate with many galaxy properties L Buldge / M sph / σ c / r e... Implication BH evolution has profound effects on galaxy formation M BH Puzzles Physical mechanism? masses / sptial scales vastly different need galaxy-wide feedback σ (km s -1 ) Gultekin et al. 2009

10 Thirst for Quasar Feedback: To reproduce BH-galaxy correlation... ~0.5-5% of quasar energy Thermal heating? 5%, Hopkins et al Momentum-driven? ~1%, Zubovas & King 2012, J. Ostriker and his group Radiatively-driven? Proga et al. 2000, but scales? Radio jets? strong: radio galaxies / RL quasars weak (?): NGC 3079 Hopkins et al. 2006

11 unobscured (Type 1) Radio-loud objects Jets can destroy host galaxies Jet-driven winds induces bow-shock and cocoon, deposit mechanic energy into ISM/IGM - both in observations and simulations Urry & Padovani 1995 Cyg 5GHz, Perley Gaibler 2011

12 Radio-loud objects Jets can do serious damage to galaxy Turbulent outflows detected at z~2 Emission regions follow the jet Physical scales are tens of kpc Velocity ~ 1000 km/s, dispersion ~ 1000 km/s Kinetic energy ~10 60 ergs Velocity Velocity dispersion Nesvadba et al. 2006, 2008

13 Radio-loud objects Jets can even do serious damage to galaxy clusters! Cluster MS z = 0.22 Size = 550 kpc (radio) Power = ergs McNamara+ 2007

14 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

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17 Our Gemini IFU Observations Strategy 11 SDSS RQ (+3 RL) quasars obscured (type 2) most luminous at z~0.5 L bol ~ erg/s 12 SDSS RQ quasars: unobscured (type 1) z, L [OIII] matched to type 2s Integral field spectroscopy FoV: 5" 7" seeing 0.4"-0.6" spectral resolution FWHM~130 km/s IFU data cube Credit: Durham University FoV

18 Our Gemini IFU Observations Strategy 11 SDSS RQ (+3 RL) quasars obscured (type 2) most luminous at z~0.5 L bol ~ erg/s 12 SDSS RQ quasars: unobscured (type 1) z, L [OIII] matched to type 2s Integral field Gemini FoV: 5" 7" seeing 0.4"-0.6" spectral resolution FWHM~130 km/s IFU data cube

19 [O III]5007Å intensity maps Radio-Quiet Quasars extended ionized nebulae seen in EVERY case Smooth and round!! kpc across All objects are spatially resolved Radio-Loud Quasars Liu, Zakamska, Greene+ 2013a

20 Ellipticity RQ vs. RL Quasar Nebulae: Morphology RQ quasars are smoother and rounder, inconsistent with illuminated merger debris ε=0.25 Liu, Zakamska, Greene, et al, 2013a, MNRAS

21 Kinematics: Non-Parametric Measurements for Each Spatial Pixel V med W 80 V med W 80

22 Well-organized velocity field, high velocity dispersion, blueshifted asymmetry, heavy wings: RQ type 2 quasars "smoking gun" evidence for gaseous outflows Liu, Zakamska, Greene+ 2013b

23 W 80 ~1000 km/s in the center, slightly decline W (~3% per kpc) High gas dispersion on >10 kpc scales Liu, Zakamska, Greene+ 2013b

24 RQ quasar outflows: Why not observed before? Sensitivity? narrow-band imaging shallower than long-slit spectroscopy and IFU Dependence on luminosity? Villar-Martin, Humphrey et al. found <20% at lower luminosities 0.8 dex increase in [O III], detection fraction changes from <20% to >50% Fooled by long-slit data? limited spatial information Humphrey+ 2010

25 Luminous RQ type 2 (obscured) quasars ubiquitously drive outflows galaxy-wide, quasi-spherical, energetic outflows Are type 1 & 2 (unobscured & obscured) quasars in a different evolutionary stage? Blow-out phase? e.g. Sanders, 1988

26 Type 1 quasars sample Direct comparison with type 2 quasars same redshift z~0.5 matched L [OIII] same telescope, instrument and setting similar seeing 0.4"-0.6" Need to remove Fe II -- template: Boroson [O III]4959Å is recovered after Fe II removal Liu, Zakamska, Greene 2014

27 Type 1 & 2 quasar nebulae are surprisingly similar! Galaxy-wide kpc 27±4 kpc Smooth & round K-S tests give high chance Liu, Zakamska, Greene+ 2014

28 Type 1 & 2 quasars are surprisingly similar! Gas dispersion W 80 ~1000 km/s Well-organized velocity fields Liu, Zakamska, Greene+ 2014

29 Interpretation & Energetics Low Δv and no correlation => quasi-spherical Velocity dispersion ~ constant in a quasi-spherical model => link W 80 to outflow velocity directly Quasi-spherical outflows with physical v~800 km/s Hβ => gas mass ~ M sun or higher Kinetic energy ~ erg (no extinction correction) Liu, Zakamska, Greene+ 2013b

30 Interpretation & Energetics Energy flow kinetic luminosity erg/s Mass flow ~10 3 M /yr L bol estimated from WISE 12μm and extrapolation from Richards Energy is too high to originate from star formation (suggested by Spitzer observations, Zakamska+ 2008) Magic number: L kin ~ 2% L bol Liu, Zakamska, Greene+ 2013b

31 Our Poster Child : SDSS J A pair of super-bubbles X in IFU maps Post-starburst galaxy, W 80 ~2000 km/s Liu, Zakamska, Greene+ 2013b Gemini long-slit spectroscopy (Xin Liu+, unpublished)

32 Our Poster Child : SDSS J A pair of super-bubbles X in IFU maps Post-starburst galaxy, W 80 ~2000 km/s Liu, Zakamska, Greene+ 2013b Gemini long-slit spectroscopy (Xin Liu+, unpublished) American Astronomical Society direct evidence for AGN-driven outflows proved for the first time that feedback from AGN is occurring on 10 kpc scales.

33 Blue scattered light + host GALFIT Data model Their host galaxies as seen by HST

34 Connecting with the tradition: direct test of BAL analysis Blue-shifted broad absortpion line: traditional outflow indicator R=?? outflow location indirectly derived from ionization models (multiple assumptions) ~10 years of debate ~kpc: engulf the whole host galaxy ~tens of pc: energy insufficient

35 Low-z case study 1: IRAS F04250 Rotation =170 km/s z~0.1 Opening angle ~70 v outflow ~600 km/s v rot ~170 km/s MW: v rot =220, v esc =550 IFU s results: R=2.9 kpc, dm/dt~1.3 M /yr, de k /dt~ erg/s Edmonds+ 2011: R 3 kpc, dm/dt~1.2 M /yr, de k /dt~ erg/s Liu, Arav, Rupke, 2015, ApJS

36 Low-z case study 2: Mrk 509 ~5.4 kpc Liu, Arav, Rupke, 2015, ApJS

37 Original-tail Tail Original Low-z case study 2: Mrk peaked [O III] => remove tail Quasi-spherical outflow v outflow ~300 km/s Hβ traces star formation IFU results: R = 1 kpc, dm/dt~5.2 M /yr, de k /dt~ erg/s Arav+ 2001: R>0.2 kpc, dm/dt~3.3 M /yr, de k /dt~ erg/s Liu, Arav, Rupke, 2015, ApJS

38 BAL: Small-scale outflows The Physical Picture - Spatial location of quasar outflows remains a challenging and contradictory issue, existing methods are complementary - Spiky Lyɑ 1216 emission line, nearly black N V 1240 absorption trough, deemed as broad emission line regions not fully obscured and Lyɑ emission leaks out, can estimate spatial scale from Lyɑ FWHM Three SDSS quasars with these features - 3 prominent quasars from SDSS (z~3), outflow size 3-26 pc New method, new view angle. He ZC, Liu GL, Wang TG+ 2017

39 SDSS/BOSS VLT BAL: Large-scale outflows - Absorption line analysis: most robust way is using troughs from excited states SDSS/BOSS quasar spectra (z>2.6, r<18.5) + 13 quasar spectra from VLT - Identify SIV 1063/SIV* 1073, from ~same physical regions as C IV - At least 50% quasar outflows at R>100 pc, 12% at R>1 kpc!!! Paper under review

40 Marching towards cosmic noon Cosmic SFR & quasar activity peak at z=2-3, the epoch when galaxy properties were largely regulated Our collaboration recently discovered ~300 extremely red quasars at 2-3 in BOSS 1. Extremely high IR/optical ratio 2. Type 2? (high equivalent width of emission lines) 3. Type 1? (UV blue, emission lines >2000 km/s) 4. N V/Lyα ~ 3:1, not ~1:40! Madau & Dickinson, 2014 SDSS J , z=2.366, Ross+ 2015, Hamann+ 2017

41 Marching towards cosmic noon Driving dusty, galaxywide, energetic winds? Blow-out phase? 1. Dust causes high IR/optical ratio 2. Patchy obscuration allows UV photons to escape 3. C IV + N V emission & absorption within differentially moving winds produce extraordinary line shapes 4. Blue-shifted N V absorption suppresses Lyα VLT/Xshooter IR spectra: [O III]+Hβ complex, Zakamska+ 2017

42 Puzzles remain there z~0.5 red quasars Spectacular super-bubbles! -- Step stone towards high z -- Criticism: PSF domination? Beam smearing? Look at the answer! Liu, Zakamska, Greene, Glikman, in prep.

43 Puzzles remain there z~0.5 red quasars Spectacular super-bubbles! -- Step stone towards high z -- Criticism: PSF domination? Beam smearing? Look at the answer! Origin of gas? HST COS has detected 150-kpc HI halo gas commonly surrounding all galaxies, red or blue Liu, Zakamska, Greene, Glikman, in prep. Bimodal metallicity distribution: metal-rich gas from outflows + metal-poor gas from cold accretion streams (Lehner+ 2013) Dekel+ 2009

44 Summary Galaxy-wide quasar feedback will save theorists, but jets are rare -- radio-quiet quasars? Our pioneering work shows that luminous RQ quasars ubiquitously drive >10-kpc scale outflows that are galaxy-wide and energetic Long-sought direct evidence for accretion energy reaching gas far away First direct test of absorption line analysis consistent within 2-3! Type 1 & 2 quasars at z~0.5 both at advanced evolutionary stages. Red quasars more likely caught in the blow-out phase. Super-bubbles seen in z~0.5 red quasars. High-z extremely red quasars at cosmic noon are the signpost of quasar feedback?

45 Quasar ionization A transition from ionization to matter-bounded [O III]/Hβ radial profiles Size-luminosity relation Existence of a maximum size

46 [O III]/Hβ He II/Hβ [O III]/Hβ break radius ~7 kpc He II/Hβ rises beyond ~7 kpc Outer regions: pressure falls, clouds expand, become overionized ("fried") Liu, Zakamska, Greene 2013a

47 Size-Luminosity Relation: [O III] isophotal radius at /(1+z) 4 erg/s/cm 2 / " power index = 0.25 ± 0.02 theoretical expectation: 0.5 matter-bounded Liu, Zakamska, Greene 2013a

48 Size-Luminosity Relation: [O III] isophotal radius at /(1+z) 4 erg/s/cm 2 / " power index = 0.23 ± 0.02 theoretical expectation: 0.5 matter-bounded Liu, Zakamska, Greene 2014

49 Size-Luminosity Relation: 8 μm isophotal radius at /(1+z) 4 erg/s/cm 2 / " [O III] nebulae have a maximum radius of ~15 kpc Liu, Zakamska, Greene 2014; (also see Hainline+ 2013)

50 Quasar ionization A transition from ionization to matter-bounded [O III]/Hβ radial profiles -- Persists at a constant ~10, then decline Size-luminosity relation -- Flatter then expected Existence of a maximum size -- no larger than ~30 kpc quasar nebulae exist