Thaisa Storchi Bergmann Instituto de Física, UFRGS, Porto Alegre, RS, Brazil

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1 [Fe II] and H 2 Outflows N Far side Inflows Stellar Population E Thaisa Storchi Bergmann Instituto de Física, UFRGS, Porto Alegre, RS, Brazil

Thaisa Storchi Bergmann Rogemar A. Riffel Rogério Riffel Dinalva A. Sales Jaderson Schimoia Daniel Ruschell Dutra Allan Schnorr Müller Guilherme Couto Astor Schönell Jr.

2 Thaisa Storchi Bergmann Rogemar A. Riffel Rogério Riffel Dinalva A. Sales Jaderson Schimoia Daniel Ruschell Dutra Allan Schnorr Müller Guilherme Couto Astor Schönell Jr. Marlon Diniz Carine Brum Hekateline Carpes Izabel Freitas Natacha Z. Dametto Fausto K. B. Barbosa Bruno Dall Agnol de Oliveira Marina Bianchin Nicolas D. Mallmann Janaína Nascimento Luis Gabriel Dahmer Hahn Johan Marques + Luis Colina Robledo (CAB, CSIC) Richard Davies (MPE) Andrew Robinson (RIT) Davide Lena (RIT) Martin Elvis (CfA)

3 Occur in Active Galactic Nuclei (AGN): fundamental phase in galaxy evolution Madau & Dickinson 2014: Why? SMBH growth connected to galaxy growth -> How? Feeding and feedback of SMBH needed to reproduce gal. lum. function Black: SFR Red: SMBH growth x 3,300 J. Silk:

4 Optical: GMOS IFU FOV: 3.5 x5 or 5 x7 Sampling 0.2 PSF ~ 0.6 R~2500 Near-IR NIFS + ALTAIR FOV: 3 x 3 Sampling: PSF ~ 0.1 R~5500, Z, J, H, K

5 Gemini NIFS survey of feeding and feedback in nearby active galaxies: Brazilian LLP2 29 AGN - with log(lx)>41.5 and closer than z=0.015 (Riffel+18) Ionised gas kinematics in local active galaxies using GMOS-IFU: local sample of 24 AGN (Ruschel- Dutra+18; poster by Gabriel Souza dos Santos); Follow up of MaNGA SDSS-IV AGN studies (Riffel+18, Wylezalek+17): presentation by Janaina Nascimento

spirals correlated with AGN: channels to feed the SMBH (Maciejewski 04, van de

7 HST F606W images of inner kpc (Simões Lopes+07, Malkan 98) : Dusty nuclear spirals in all earlytype AGN; But in only 25% of control sample; -> Nuclear spirals correlated with AGN: channels to feed the SMBH (Maciejewski 04, van de Ven & Fathi 10; Piñol-Ferrer+12; Hopkins+Quataert 10) active non-active active nonactive

8 Sa, LINER/Seyfert kpc x 1 kpc Nuclear spiral 0.6 =60 pc

9 Stellar kinematics from absorption spectra (ppxf, Cappellari & Emsellem2004) Gas kinematics from emission lines

Gas kinematics Stellar velocity field: rotation Stellar kinematics Gas velocity field: rotation + distortions correlated to spiral arms in structure map:

10 Gas kinematics Stellar velocity field: rotation Stellar kinematics Gas velocity field: rotation + distortions correlated to spiral arms in structure map: blueshifts in the far side and redshifts in the near side -> inflow if gas in the plane Mass inflow rate: 0.4 M yr -1 ; similar case: NGC1667: 2.4 M yr -1 (Schnorr-Müller+17)

11 SO, Sy 2 FOV= 450 pc x 450 pc 0.1 =15 pc Gas kinematics: H2 Stellar kinematics: CO

12 Stellar velocity field: rotation H2 velocity field: rotation + inflows + compact outflow Warm (2000K) H2 mass 1400 M ; Far Warm H2: heated skin of cold gas; Cold H2 mass (Dale+05, Mazzalay +12) ~ M Near Warm H2 mass inflow rate 4 x 10-4 M yr -1 ; estimated cold: > 1 M yr -1

13 NGC1097 nuclear spiral: Fathi+06 NGC6951 nuclear spiral: Storchi-Bergmann+07 NGC4051 nuclear spiral: Riffel+08 NGC7582 inflow from nuclear ring: Riffel+09 M81 nuclear spiral: Schnorr Müller+11 Mrk1066 nuclear spiral + compact disk: Riffel+11 Mrk79 nuclear spiral + compact disk: Riffel+13 Mrk766 compact H2 disk: Shönell+14 NGC3081 nuclear bar: Schorr Müller+16 NGC1358 nuclear spiral: Schnorr Müller+18

Ionised gas HII: HII more concentrated near the nucleus and along ionization axis: HI rapidly absorbs ionizing photons HII masses: (0.03-4.4)x10 6 M ; surface density ΣHII=0.

14 Ionised gas HII: HII more concentrated near the nucleus and along ionization axis: HI rapidly absorbs ionizing photons HII masses: ( )x10 6 M ; surface density ΣHII= M pc -2 Warm molecular gas H2: H2: more uniform and extended: X-rays penetrate the galactic plane in all directions -> heat molecular gas H2 masses: (0.05-3)x10 3 M ; surface density ΣH2=(0.2-14)x10-3 M pc -2

15 Inflows in nuclear spirals, bars and disks, observed in H + and H2; capture of dwarf companion (Fischer+15); Inflow velocities: ~ km/s; Inflow rates: ~0.1 few M yr -1 : times the AGN accretion rate; Total H + masses in inner kpc ~ M Warm H2 masses: ~10 3 M ; in cold H2: estimated M (e.g. ALMA) Øco-evolution: SMBH at 10-3 M yr -1 and galaxy at 1 M yr -1

17 NLRG, Sy = 700 pc Extended [OIII] emission not aligned with radio jet (45deg)

(1) Narrow, extended -> rotation Total gas mass: 4.1 ± 1.

18 High σ around the nucleus: 2 kinematic components: (1) Broad, perp. to radio jet -> outflow: lateral expansion? (1) Narrow, extended -> rotation Total gas mass: 4.1 ± 1.7 x 10 8 M Mass outflow rate: ~0.1 M yr -1 Outflow power: ~0.1% LAGN

19 [Fe II] flux [Fe II] σ Sab pec, Sy 2, 2 radio blobs 1 = 175 pc High σ perp. radio axis: double lines; also in two radio blobs Lower sigma elsewhere Gas counter rotating relative to the stars

20 Outflow Rotation + equatorial outflow Lateral expansion due to radio jet? Mass outflow rate:~ 0.4 M yr -1 HII mass: 1.3 ± 0.2 x 10 6 M Warm H2 mass: 471 ± 58 M rotation

21 HST [OIII] Sb, Seyfert pc x 500 pc 0.1 = 7 pc Das et al [FeII], J and H-band: bipolar (bicome) H2: 100 pc off-centered ring

[Fe II] and H 2 N Far side -600-520 E -440-360 [Fe II]: patchy outflow Velocities up to 800 km/s Mass outflow rate: 4± 1 M yr -1 2 1 0 1 2-280

22 [Fe II] and H 2 N Far side E [Fe II]: patchy outflow Velocities up to 800 km/s Mass outflow rate: 4± 1 M yr Outflow power: ~0.1% LAGN H2 ring: rotation+ expansion in the plane -200 km/s < v < +200 km/s

23 NGC4151: Storchi-Bergmann+10 hollow conical Mrk1066: Riffel+10 Mrk1157: Riffel+11 Mrk79: Riffel+13 Arp102B: Couto+13 NGC2110: Schnorr-Müller+14 NGC1386: Lena+15 NGC5548: Schönell+16 NGC1667: Schnorr-Müller+16

24 Outflows mapped via W80 (high. vel. wings): v=w80/1.3

3 M yr -1 (range: 10-3 -10 2 M yr -1 ) Mean outflow power:

25 ~60% have non-circular motions (mostly outflows) Mean outflow rate: ~0.3 M yr -1 (range: M yr -1 ) Mean outflow power: P~10 41 erg/s (range erg/s) Only 1/3 sample have P>1% LAGN-> meaning effective feedback on galaxy

26 Outflows with velocities: 200 (most) 800 (few) km s -1 and mass outflow rates of tenths to a few M yr -1 Geometry: (1) Unresolved compact (inner pc): need of better angular resolution (2) Extended perpendicularly to ionization/jet axis: lateral expansion of gas as jet progresses through it? (3) Resolved bi-polar (Fisher+13: ~ 1/3 of AGN) In all cases most extended emission does not originate in outflowing gas but in gas rotating in the galaxy disk ionized by the AGN Outflow power: <1% LAGN in 2/3 of the sample -> little effect on the galaxy On-going: study of farther and more luminous AGN (MaNGA, GMOS-IFU, NIFS)

Thaisa Storchi Bergmann Instituto de Física, UFRGS, Porto Alegre, RS, Brazil

[Fe II] and H 2 Outflows N Far side E Inflows -600-520 -440-360 -280-200 -120-40 2 1 0 1 2 40 120 200 280 360 440 520 600 2 1 0 1 2 Thaisa Storchi Bergmann Instituto de Física, UFRGS, Porto Alegre, RS,