The Impact of Quasar-Mode Feedback on the Ecosystems of Galaxies - - PowerPoint PPT Presentation

Sylvain Veilleux (U. Maryland, Joint Space-Science Institute)

Gemini Press Release (based on the results of Rupke+Veilleux 2011) Powerful wide-angle

• utflow in Mrk 231,

the nearest quasar

The Impact of Quasar-Mode Feedback

• n the Ecosystems of Galaxies

The Elephant in the Room

My Hat Today

1. What is the origin and fate of the CGM? 2. What are the morphological & physical properties of the CGM? 3. What are the physical processes that shape the CGM on both large (kpc) and small (pc) scales? 4. What is the relation between the CGM and galaxy properties? 5. How does the CGM evolve and what can we learn by comparing different epochs and tracers?

Key Questions

• Radiative energy:

– LAGN ~ (ε/0.10) (dMBH / dt) c2 ~ 1012 (ε/0.10) (dMBH / dt) Lsun – EAGN ~ (ε/0.10) MBH c2 ~ 1061 (ε/0.10) (MBH/108 Msun) ergs

• Binding energy of the bulge: Egal ~ Mgal σ2 (isothermal)
• BH – bulge relation: MBH ~ 0.0014 Mgal
• EAGN / Egal ~ 1.4 x 10-4 (c / σ)2 > 80 if σ < 400 km s-1 à

à potentially lethal!

• Radiative feedback

– Illuminate, ionize, and heat the ISM, CGM, and IGM

• Mechanical feedback: quasar-driven outflow

– Radiation pressure – Radiative heating → Compton-heated wind (T ~ 106 – 107 K) – Magnetic fields in accretion disks / BH → loosely collimated jets

in radio-quiet quasars

The Impact of Quasar-Mode Feedback

• n the Ecosystems of Galaxies

(e.g., SV, Cecil, Bland-Hawthorn+05; Fabian 12)

• Quasar Radiative Feedback
• Quasar Mechanical Feedback

Plan

• Quasar Radiative Feedback
• Quasar Mechanical Feedback

Plan

He II and Thermal Proximity Effects

(e.g., Boera+14; Khrykin+17)

• Photoionization of He II to He III à

à suprathermal electrons à à ΔT à à H I line broadening

• ΔT is sensitive to the initial He II ionization fraction, xHeII,0
• Sizes of proximity zones are sensitive to quasar lifetime, tQ

(e.g., Shull+10; Syphers+Shull14; Khrykin+16) He II Lyα Forest

Giant Lyα Nebulae fluorescently illuminated by Quasars

(Borisova+16) (Cantalupo+14)

Kinematically quiet, dense (> 1 cm-3), cool (~104 K), small (< 20 pc), metal-poor (< 0.1 Zsolar) clumps à à Mgas ~ 1011 – 1012 Msun

CGM Photoionized by “Quasars”: Asymmetric & Detached

(SV+03 [TTF]; Yoshida+02) NGC 1068 NGC 4388 NGC 7213 (Putman+03; Bland-Hawthorn+13) (Schawinski+10) 11 x 16 kpc

14 kpc Hanny’s Voorwerp MW: Magellanic Stream

50-100 kpc γ-bubble ~11 kpc ~35 kpc ~19 kpc

• 17.5
• 17.3
• 17.0

Δt ~ 1-3 Myr Δt < 70 kyr

• 18.5

(Kreimeyer & SV 13 [MMTF])

20 kpc ~15”

CGM Photoionized by Quasars: MR 2251-178 (z~0.06)

MMTF [O III] λ5007 140 kpc

• 18.0

Hα Cont [O III] Cont [N II]

Kinematically quiet + velocity gradient (distinct from inner quasar host) (0.7” ~ 900 pc)

ne ~ 0.1 cm-3, log U ~ [-3,-1], Z ~ 0.5-1 Zsolar , dust-free?, matter-bounded → fesc(ionizing radiation) ~ 65-95% (total)

(Kreimeyer & SV 13 [MMTF])

CGM Photoionized by Quasars: MR 2251-178 (z~0.06)

[O III]/Hβ

Dusty Dust-free

• Quasar Radiative Feedback
• Quasar Mechanical Feedback

Plan

Quasar-Mode Feedback à à tSZ Signal on CMB?

Ruan+15 Verdier+16 Crichton+16 Soergel+17

(Ruan+15; Crichton+16; Verdier+16; Spacek+16,17; Soergel+17; Chowdbury+Chatterjee17)

• Data from WMAP, Planck, ACT + Herschel, Akari
• Stacked maps of ~104 SDSS / BOSS RQ quasars:

à à stronger signal at z > 2 à à Eth ranges from (1 ± 0.2) Ÿ Ÿ 1062 to a few Ÿ Ÿ 1060 erg à à Eth (AGN) ranges from ~ Ebinding to negligible!

• Uncertainties: dust emission from the quasar host and

galaxies along the line of sight, including the MW

Extended Na I Outflow in Nearest Quasar Mrk 231

• Gemini/IFU: Na I D 5890, 5896 Å absorption
• R ≥ 2-3 kpc from the nucleus
• | Vout | in excess of 1100 km s-1
• dM/dt ≥ 160 Msun yr-1 ~ 1.1 SFR
• dp / dt ≥ 5 LSB / c , ≥ 3 LAGN / c, ≥ 2 LIR / c
• Lmech = dEkin/dt ≥ 1043.6 ergs s-1 ~ 1.1 x dESB/dt ~ 0.5% LEdd (AGN)

(Long-slit: Rupke, SV, & Sanders 05c; IFU: Rupke & SV 11, 13a) Mrk 231

2011 Gemini Press Release

à à AGN driving

• Herschel/PACS + Spitzer spectra: multiple OH transitions
• P-Cygni profiles!
• Outflow: |Vout | in excess of 1000 km s-1
• dM/dt ~ 620 - 1100 Msun yr-1
• dp/dt ~ 6 LBOL(AGN) / c
• dEkin/dt ~ 1% LEdd(AGN)
• Molecular Outflow in Mrk 231

Herschel: unresolved P-Cygni profiles of OH (e.g., Fischer+10; Sturm+11; Gonzalez-Alfonso+14, 17)

• Vout up to ~750 km s-1
• Mout ~ 6 x 108 Msun

(H2/CO ~ 0.1 x Galactic value)

• Kpc scale
• dM/dt ~ 700 Msun yr-1

IRAM: Spatially resolved molecular line emission (Feruglio+10; Aalto+12; Cicone+12; Alatalo+10; Feruglio+15; Lindberg+16; …)

Molecular Outflow in Mrk 231

Red Wing Blue Wing Feruglio+15

§

Statistics: ~70% of local U/LIRGs have molecular winds (Θ ~145o)

§

Outflow velocities: <v50> , <v84>, <vmax> ~ -200, -500, -925 km s-1

§

Energetics: Size ~ 0.1 – 10 kpc dM/dt ~ 10 – 1000 Msun yr-1 dp/dt ~ (0.1 – 20) LIR/c dE/dt < 2% LIR Molecular gas = energetically dominant phase of these

• utflows

§

Trends with SFR and AGN luminosities: suggest that we are seeing starburst + quasar feedback in action Herschel Surveys: unresolved P-Cygni profiles of OH (e.g., SV, Melendez+13; Spoon+13; Gonzalez-Alfonso+14, 15, 17; Stone, SV+16) MM-wave Interferometric Surveys: kpc-scale CO line emission (e.g., Feruglio +10,+15; Aalto+12ab; 15, 16; Alatalo+11, 15; Cicone+12, 14; Garcia-Burillo+14,15; Lindberg+16; SV, Bolatto+17)

Molecular Outflows in U/LIRGs & Quasars

(SV, Melendez+13; Cicone+14; Stone, SV+16) Red = ULIRGs Blue = BAT AGN à AGN driving of the most extreme molecular winds

OH CO

Molecular Outflows in U/LIRGs & Quasars

(Rupke, Gultekin, & SV 2017)

dE/dt ~ MBH

1.66±0.45 dE/dt ~ σ9.0±3.8

Multi-Phase Outflows in Local Quasars and Seyferts

u u Seyfert galaxies

Extreme Warm (T ~ 104 K) Ionized Outflows

(Alexander+10; Liu+13ab, 14; Greene+14; Hainline+14; Husemann+15; Harrison+12, 14,16; Carniani+15, 16; Perna+15; Cresci+15; Brusa+16; Rupke + SV 2013, 2017) (Bischetti+17) (Zakamska+16)

log LAGN dEkin/dt Dusty Outflows in Red Quasars

vmax([O III]) à à3000+ km s-1 Ekin ~ 1059 (ne/102 cm-3)-1 erg W90([O III])

§ ALMA: CO (1 – 0) emission from rotating disk + outflow

• Aperture photometry & UV plane fitting: Rmax ~ 15 kpc

12

Sizes: Quasar-Driven Molecular Outflow in F11119+3257

(SV, Bolatto, Tombesi+17)

[-820, -380] km/s [+280, +800] km/s

15 kpc

Sizes: Neutral Outflows from Resonant Na I Emission

(Rupke & SV 2015)

Mrk 231

Type-2 Quasar / ULIRG F05189-2524

§

Complementary to Na I D absorption (no need for background galaxy continuum emission)

§

Provide new constraints on the sizes of local winds à à So far, R < 5 – 10 kpc (limited by IFU FOV)

galaxy clumpy outflow Blueshifted absorption Redshifted emission

(Hailey Finley’s talk: Fe II)

Matter-bounded?

log R-15 (pc) log (L 8 µm) log R-15 (pc)

10 kpc 30 kpc

Sizes: Warm Ionized Outflows

(Alexander+10; Liu+13ab, 14; Greene+14; Hainline+14; Husemann+15; Harrison+14; Carniani+15, 16; Perna+15; Cresci+15; Brusa+16; Rupke + SV 2013, 2017; Bischetti+17)

13 kpc

[O III] blue wing (Liu+14; Hainline+14) z ~ 0.6 z ~ 2 (Cresci+15)

850 µm

Mrk 231

SV, Teng+14

20 kpc ~ 40”

65 x 50 kpc 110 x 80 kpc Starburst-driven outflow Quasar-driven outflow

Nardini+13 Yoshida+16

NGC 6240

X-rays Hα + X-rays

Sizes: Hot Ionized CGM

850 µm

Koda+06

Sizes: Hot Ionized CGM

Hα + X-rays

Yoshida+16

Mrk 231 NGC 6240

Major galaxy mergers

R band R band

Predictions from Numerical Simulations of Major Galaxy Mergers

(Cox, di Matteo+06) ~0.4 keV ~ 4.6 million K ~0.2 keV ~ 2.3 million K 1 0.5 0.1

(Nardini+13; Wang+14)

20 kpc ~ 40”

Two-phase plasma: (1) T ~ 8 x 106 K, Fe ~ 0.5 solar (dominant; SB-processed) (2) T ~ 3 x 106 K, Fe ~ 0.1 solar (fainter; pre-existing) Ethermal ~ 5 x 1058 erg Extended Fe XXV 6.7 keV à àfast ~2200 km s-1 shocks (Si, O, Mg) / Fe = 4-5 x solar (~ uniform) Starburst-processed gas is slowly expanding into, and mixing with, a preexisting halo medium of lower metallicity and temperature

Hot Ionized CGM: NGC 6240

(SV, Teng+14)

20 kpc ~ 40”

Two-phase plasma: T ~ 3 and 8 x 106 K

Fe ~ 0.4 solar Ethermal ~ 2 x 1058 erg (Si, O, Mg) / Fe = 2-4 x solar (~ uniform) à à mixed by on-going & past (~108 yrs)

• utflow events

Hot Ionized CGM: Mrk 231

Single-phase plasma: T ~ 8 x 106 K only Ethermal ~ 1 x 1057 erg < Ewind, ESB, EAGN Absorbing screen à à Na I D outflow? Extended Fe XXV 6.7 keV à àfast shocks?

R = 6 – 30 kpc R < 6 kpc

§ Quasar-mode radiative feedback

• He II Proximity and Thermal Effects: Out to several 10’s of Mpc
• MR 2251-178: A local analog to giant Lyα nebulae around high-z quasars
• Beware: Environmental effects (tidal debris, stripped satellites, ram-

pressure filaments) + quasar ionization cones and flaring complicate the interpretation of these nebulae

§ Quasar-mode mechanical feedback

• Globally: tSZ effect from radio-quiet quasars gives Eth(AGN) ~ 0 à

à Ebinding Stay tuned for the jury’s decision…

• Ubiquitous outflows: Multi-phase, fast (up to ~3000 km s-1), massive

(10 – 1000+ Msun yr-1), and powerful (up to ~5% LAGN)

• Sizes: R ~ 1 – 15 kpc à

à 30+ kpc (at high z)

• Hot Ionized CGM of Mrk 231: Evidence for heating from fast shocks as

well as metal transport by the on-going and past outflow event(s)

Summary