The Laws of Formation: From the Cosmic Dawn to the Present Universe July 4, 2018 Outflows versus star formation in nearby AGN from the MAGNUM survey

Giacomo Venturi PhD student at University of Florence / INAF - Arcetri Astrophysical Observatory Visitor at Kavli Institute for Cosmology, Cambridge

A. Marconi (P.I.), M. Mingozzi, S. Carniani, R. Maiolino, G. Cresci, E. Nardini et al. evolution: the need for outflows

Stellar (SN) feedback accounts for the lack of low-mass

Feedback damps/quenches star formation

acting through outflows/jets

driven by SNe or AGN

AGN feedback accounts for the lack of massive galaxies Silk & Mamon 2012

G. Venturi Outflows vs star formation in nearby AGN from the MAGNUM survey 2 Detecting outflows Ionized outflows traced by broad wings in [OIII] in luminous AGN at z ~ 1–3

Brusa+2016 peak of AGN activity

[OIII] velocity Star Formation (Hα)

[OIII] wing map Star Formation (Hα)

Cresci+15a Carniani+16 Bongiorno+07 … but low-resolution, very difficult to measure outflow physical properties and study feedback in detail

G. Venturi Outflows vs star formation in nearby AGN from the MAGNUM survey 3 MAGNUM survey

Study in detail outflows and feedback in nearby (D < 50 Mpc) Seyfert galaxies with VLT/MUSE

FOV covers 1 to 15 kpc with resolution: 15 pc (@4Mpc) to 115 pc (@30Mpc)

VLT/MUSE FOV

1'⨉1'

Centaurus A Circinus IC 5063 NGC 1068 NGC 1365

NGC 1386 NGC 2992 NGC 4945 NGC 5643 NGC 6810 G. Venturi Outflows vs star formation in nearby AGN from the MAGNUM survey 4 Part 1: NGC 1365

Detailed study of ionized gas in the central kpcs of NGC 1365:

AGN vs star formation, mapping the outflow properties

from optical (MUSE) and X-ray (Chandra) data

(Venturi et al., subm.)

G. Venturi Outflows vs star formation in nearby AGN from the MAGNUM survey 5 NGC 1365: complex environment in central kpcs

Spatial res. —> ~60 pc

NW

MUSE FOV ~ 5 kpc [OIII] Hα SE Hα

Star formation (~7 M⊙/yr): Density[OIII] ⟂ from double [SII] cone doublet Hα follows dust lanes along up to 103 cm-3 in the ring SE less obscured ! above disk, Barred Seyfert 1.8 galaxy the bar + circumnuclear ring NW ! behind disk ⊙ Low-luminosity AGN: LAGN ~ 2×1043 erg/s (~5.6 M /yr)

G. Venturi Outflows vs star formation in nearby AGN from the MAGNUM survey 6 NGC 1365: source of gas ionization

Spatially resolved AGN AGN AGN BPT diagrams

LINER SF LINER SF SF log [OIII]/H β log [OIII]/H β log [OIII]/H β Double cone ionized by AGN Composite SF dominates along the bar log [SII]/Hα log [SII]/Hα log [SII]/Hα

[OIII] Hα

G. Venturi Outflows vs star formation in nearby AGN from the MAGNUM survey 7 NGC 1365: double-conical outflow Outflow spatially traced by motions deviating from rotation

Stellar velocity [OIII] velocity [OIII] vel. - Stellar vel. [OIII] lineline widthwidth

Stellar velocity and kinematically traced by asymmetric wings [OIII] in line profiles

G. Venturi Outflows vs star formation in nearby AGN from the MAGNUM survey 8 NGC 1365: mapping the mass outflow rate

NW cone: positive velocity [OIII] dominated by outflow, Hα by disk ! receding and outflow is not a broad wing SE cone: negative velocity as at low resolution in more powerful objects ! approaching

Left comp.: outflow blueshifted; Right comp.: disk Outflow sliced in a Stellar Hβ out velocity grid to separate [OIII] outflow from disk component in fitting

Hα [NII] out [SII]

G. Venturi Outflows vs star formation in nearby AGN from the MAGNUM survey 9 NGC 1365: outflow radial profiles

Radial profiles as a function of distance from the AGN Mass outflow rate of nuclear Decreasing trend with distance Ṁion SFR (7 M⊙/yr) blueshifted cone X-ray wind≪ (vout,X ~ 3000 km/s) redshifted cone from—>(see FeXXVoutflow also Karouzos+16a,16b, andunable FeXXVI to affect abs.Bae+17, SF lines (at leastCrenshaw+15, in its ionized Revalski+18) phase) • Energy-driven: Ėk,ion ≲ 10-3 Ėk,X • AGN more powerful recently —> would need too much neutral than in the past vout M˙ ion | | atomic + molecular for Ėk,tot ~ Ėk,X • Outflow does mass loading and SF ring scale (see Carniani+15, Fiore+17, Fluetsch+18) slows down (but we don’t see • Direct AGN radiation1kpc pressure on mass radially increasing) dustyNot clouds excluded (e.g. Thomson+15,that SF ring • We sample only ionized gas contributes to outflow, Ishibashi+18): ṗion ≲ 0.05 LAGN/c (lackingas we observeneutral atomic hard X-ray +

˙ ˙ 2 ˙ (models:emissionmolecular), ṗ totfrom ~ which 1-5 ring L dependsAGN tentatively/c) —> on in Ek,ion = Mionvout/2 p˙ion = Mionvout due to SNe producing shocked wind principleionizing could flux dropping be the driver as r -2 G. Venturi Outflows vs star formation in nearby AGN from the MAGNUM survey 10 Part 2: NGC 6810

Star formation within the outflow

in star-forming galaxy NGC 6810

(Venturi et al., in prep.)

G. Venturi Outflows vs star formation in nearby AGN from the MAGNUM survey 11 Con$nuum at λ=8140 Å Flux Hα(narrow) Gas velocity (narr. comp.) Gas σV (narrow comp.) Outflows can also form stars

First observational evidence of Models predict new mode of star formation, a)# creating stars with high velocities star formation inside an AGN-driven outflow Con$nuum at IRAS 2312λ=1400 -Å59 Flux Hα(broad) Gas velocity (broad comp.) Gas σV (broad comp.) on ~radial orbits, possibly contributing to Maiolino+17 spheroidal component (bulge) of galaxies (Silk+12,17, Ishibashi&Fabian14,15, Zubovas+13, Xshooter slit Zubovas&King13, Nayakshin&Zubovas 12, Gaibler+12) b)#

Hα [SII]6731 [OIII]5007 [SII]6717 Widespread evidence in our galaxy Hβ 8µm [NII]6584 Ha outflow [NII]6548 (PAH) So why not also See alsodiscs Gallagher+18 inside galactic outflows? Paβ R. Maiolino’s[FeII]1.64 talk later! HeI Brγ H2(1-0)S(1) (1-0)S(2) no 2

H [AlIX] no [FeII]1.25 [SIX] 24µm Stars HeII form in the

Zavagno+10, Lim+18, shocked front Dwarkadas+17, Duronea+17, Deharveng+15, Dewangan+12, b)# c)# Thompson+12, Brand+11 G. Venturi Outflows vs star formation in nearby AGN from the MAGNUM survey 12 NGC 6810

Soft X-rays Blue: stars (XMM-Newton) Star-forming galaxy: Bipolar no trace of AGN from Our MUSE starburst optical diagnostics, hard FOV outflow X-rays, MIR or radio ~8 kpc Red: Hα Green: [NII] Strickland+07 Stellar velocity Hα velocity Hα linewidth

LI(N)ER (old stars/ shocks) Cone has

Ionized by SF-like ionization log [OIII]/H β OB stars in star-forming regions

log [SII]/Hα G. Venturi Outflows vs star formation in nearby AGN from the MAGNUM survey 13 NGC 6810: stars forming within the outflow!

Stellar Contours: MaNGAvelocity BPT diagrams only for LI(N)ER/ Hα shocks SF galaxies outflow component [NII] outflow log [OIII]/H β log[OIII]/[SII] Star Grid to separate outflow forming from disk in fitting Outflowing cone has log [SII]/Hα Traces ionization parameter log ([OIII]+[SII])/Hα Low ionization Our points are consistent with SF-like ionization 1. Star formation within parameter expected, normal SF regionsif ionization —> ionizationcomes from outflow! from young starsdisk (dis >in 1 situ!kpc) 2. Ionizing photons simply come from SF in the disk… Star formation within the outflow! G. Venturi Outflows vs star formation in nearby AGN from the MAGNUM survey 14 Conclusions • MAGNUM survey: study ionized gas kinematics and ionization, outflows vs SF in central kpcs of nearby AGN down to ~10 pc with MUSE • NGC 1365 (Venturi et al., subm.)

✦ Hα traces star formation in disk/bar, [OIII] traces AGN-ionized double-conical kpc-scale outflow —> outflow not broad wing like at low-resolution in more powerful objects

✦ Ṁout << SFR —> ionized outflow not able to affect star formation

✦ Radial profiles of mass outflow rate, velocity, kinetic rate and momentum rate —> decrease at larger distance: AGN more powerful recently? mass loading? Molecular gas needed

✦ Comparison with AGN nuclear X-ray wind —> energy-driven scenario unlikely, rad. pres.-driven feasible • NGC 6810 (Venturi et al., in prep.)

✦ First detection of star formation within galactic outflow in an unambiguous star-forming galaxy (not AGN)

G. Venturi Outflows vs star formation in nearby AGN from the MAGNUM survey 15