Galaxy feedback in 3D

Roberto Maiolino

Feedback is the key:- reducing SF efficiency

(gas heating+turbulence)- removing baryons

Discrepancy between halo mass functions and stellar/baryons mass function

Star formation feedback

SNe

Radiation pressure

Photoionization

TurbulenceVelocity dispersion

AGN feedbackQuasar mode

Radio mode

Blast wave

Radiation pressure

(Q>1)

Star formation feedback

SNe & radiation pressuredriven outflows

Herschel PACSM82

velocity field velocity dispersiongalaxyrotation

turbulentoutflow

X-rays(Chandra)

NIRNGC 253

Ha

X-rays

CO~170 km/s(ALMA)

Mout ~ 1-2 SFR.

Contursi+13, Kreckel+14

Bolatto+13

PAH(Spitzer)

[CII]158um (Herschel)

The importance of tracingoutflows in multiple phases

Investigating outflows as a function of M* and SFR(breaking the M*-SFR degernarcy)

160,000 SDSS galaxies sorted into 50 bins in the M*- SFR parameter space

Lowest M* ≈ 2 x 107 M Lowest SFR ≈ 2 x 10-3 Myr-1

Cicone+14

MainSequence

7

THE LINE-OF-SIGHT VELOCITY DISTRIBUTIONS

[OIII]

Hα+[NII]

STARS

v [km/s]

Trends with M*

at a fixed SFR

Cicone+14

8

THE LINE-OF-SIGHT VELOCITY DISTRIBUTIONS

[OIII]

Hα+[NII]

STARS

v [km/s]

Trends with SFR

at a fixed M*

9

OUTFLOW PROPERTIES

Stacking grid colour-coded with the excess of gas velocity with respect to stars which traces non-virial motion of gas (due to outflows)

• vGAS – vSTAR increases with SFR and sSFR Expected for star formation-

driven outflows

• vGAS – vSTAR decreases with M* for fixed SFR Qualitatively agrees with

models

Agreement with indirect observations of feedback (e.g. mass-metallicity relation)

v[OIII] - vSTARS

vHα- vSTARS

[OIII]

Hα

10

OUTFLOW PROPERTIES

Outflows are detected only above the main sequence of star formation

• Sharp increase of outflows at SFR > SFRMS

• Outflows eventually quench star formation and lower the SFR, bringing the galaxy back on the MS

Self-adjusting mechanism that may explain the tightness of the MS

v[OIII] - vSTARS

v [OIII

] – v

STAR

S [k

m/s

]

ΔMS = offset from the Main Sequence

Cicone+14

11

Next steps:- 3D on large samples of galaxies required to obtain outflow rate and PK SDSS4-MANGA- Investigate the Atomic (NaI) and Molecular components

in 3D

v [OIII

] – v

STAR

S [k

m/s

]

ΔMS = offset from the Main Sequence

• Sharp increase of outflows at SFR > SFRMS

• Outflows eventually quench star formation and lower the SFR, bringing the galaxy back on the MS

Self-adjusting mechanism that may explain the tightness of the MS

v[OIII] - vSTARS

Star formation feedback

at high redshift

Steidel+10Bradshaw+13Diamond-Stanic+12

z~3

Integrated

Outflow load factor M

SFR~ 1-2

.

3D resolved

z~2

Genzel+12

The need of feedback becomes dramatic at high-z

Photoionization the main driver?

Need to trace both ionized and neutral ISM at high-z

e.g. Lya, Ha e.g. [CII], [CI], CO

Feedback in the early Universe

[CII]158mm (ALMA)

Lya emitter at z=4.7SFR ~ 20 M/yr

Williams+14

QSO

SMG

Neutral-cold gas ([CII]) probably account just for a small fraction of the whole galaxy traced by Lya

Lya

Ly a (FORS2)

But peculiar environment (QSO)…

Y-band(Lya+UV)

Vanzella+12

Star forminggalaxy at z=7.1(reionization

epoch)

SFR ~ 9 M/yr

[CII]158mm(~neutral cold gas)detected at z=7.1with ALMA

5 kpc

beam 0.5”x0.7”

Maiolino+14

Y-band(Lya+UV)

Star forminggalaxy at z=7.1(reionization

epoch)

SFR ~ 9 M/yr

FWHM8 km/s!

5 kpc

beam 0.5”x0.7”

[CII](ALMA)

Star forminggalaxy at z=7.1(reionization

epoch)

SFR ~ 9 M/yr

FWHM8 km/s!

5 kpc

beam 0.5”x0.7”

velocity vel. dispersion

km/s

km/s

Mdyn ~ 3 107 M

[CII](ALMA)

FWHM8 km/s!

[CII]

Lya+UV

5 kpc

3 kpc

beam

[CII](ALMA)

offset~3 kpc

…as expectedby modelsof primeval

galaxiesVallini+13

galaxy mostlyphotoionized+ accreting

clumpsof cold gas

AGN feedback

“Quasar mode”

Quasar-driven outflows detected in theatomic neutral and ionized component

Rupke+11,13, Spoon+11, Muller-Sanchez+11

Wavelength (Å)

Narrow Ha

[NII][NII]

Broad H a (outflow)

F l (n

orm

alize

d)

Mrk231Mrk231

NaI

2kpcve

loci

ty [k

m/s

]

lambda6100 6160

1200 km/s

velo

city

[km

/s]

Evidence for massive quasar-drivenmolecular outflows

CO(1-0) high velocity wings

Massive molecular outflows (~1000 M/yr)Extended on kpc scalesPK ~ 0.05 LAGN

Momentum rate ~ 20 LAGN/c

OH P-Cygni profiles

Fischer+10Sturm+11

1200 km/s

5kpc

Feruglio+10,13Cicone+14

blue wing

…as expected(and required)by models

l (mm)

Mrk231

The importance of high resolution3D spectroscopy

Recurrent explosive processEnergy driven quasar outflows

1kpc

1kpc600 – 800 km/s 800 – 1000 km/s

Mrk231

600 – 800 km/s

CO(1-0)

CO(1-0)

CO(2-1)Feruglio+, in prep.

IRAM - PdBI

Simulations: only diffuse gas is ejected, no dense gas… AGN not really capable of quenching star formation?

Gabor+14

Actually a lot of dense (~105 cm-3) gas is observed in the outflow…

Aalto+12

…actually there is more dense gas in the outflow(relative to diffuse) than in the disk!

Alternative scenario: molecular outflowing cloudscondensed out of the shocked ouflowing gas…… would be consistent with AGN only ejecting diffusegas and the detection of dense outflowing gas…

Zubovas & King ‘13

Expected Observed

log (critical density) [cm-3]

outf

low

size

[kp

c]

Cicone+12

but 3D info:

n n

AGN feedbackat high-z

(that’s what is reallyneeded to account for

local massive ellipticals)

V[OIII] >300 km/s(outflow)

H a (SFR)

Cano Diaz+12

Alexander+10Forster-Schreiber+13Cimatti et al. 13Weiss+13

Bourget + 2012, 2013

z=3.0 z=2.4

z=3

z=6.4

Maiolino+12, Cicone+14

[CII] Moutflow up to >3000 M/yr .

Sizes >10 kpc

Depletion timescales < 107 yr

Keeping the galaxy clean

“Radio mode”

“Quasar mode”

Cleaning the galaxy

radio

optical + radio

Evidence for radio-mode AGN feedback in LOCAL galaxies(maintenance mode)

Heating ~ CoolingIt works!

… Really?

Having, ON AVERAGE, balance betweenheating and cooling does not

mean that some regions cannot undergooverheating and other OVERCOOLING

Salome’+11Russel+14Hamer+14

Streams ofcooling molecular gas

towards the centerof Perseus

“Quasar-feedback” phase driven by jets?

Wagner & Bicknell 2011, 2012

4C12.50

SCIENCE (today)

blueshifted 21cmabsorption

see alsoMorganti+03,05, Emonts+03

ALMA CO(1-0)

Observational evidence and characterizationof feedback in galaxies:

green field

lots of open questions

rapid growth expected in the coming few yearsthanks to the new 3D facilities