thaisa storchi bergmann instituto de física, ufrgs, porto ...€¦ · thaisa storchi bergmann...

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

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Inflows

Outflows Stellar Population

Storchi-Bergmann – Science and Evolution of Gemini, San Francisco, July 2018

Thaisa Storchi Bergm annRogem ar A. RiffelRogério RiffelDinalva A. SalesJaderson Schim oiaDaniel Ruschell DutraAllan Schnorr Müller Guilherm e CoutoAstor Schönell Jr.Marlon DinizCarine BrumHekateline CarpesIzabel FreitasNatacha Z. DamettoFausto K. B. BarbosaBruno Dall’Agnol de OliveiraMarina BianchinNicolas D. MallmannJanaína NascimentoLuis Gabriel Dahmer HahnJohan Marques+Luis Colina Robledo (CAB, CSIC)Richard Davies (MPE)Andrew Robinson (RIT)Davide Lena (RIT)Martin Elvis (CfA)


§ Occur in Active Galactic Nuclei (AGN): fundamental phase in galaxy evolution

§ Why? SMBH growth connected to galaxy growth ->

§ How? Feeding and feedback of SMBH – needed to reproduce gal. lum. function

Madau & Dickinson 2014:

Black: SFR

Red: SM BH growth x 3,300

J. Silk:

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: 0.04”�0.1”¡ PSF ~ 0.1”¡ R~5500, Z, J, H, K


¡ 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 JanainaNascimento



HST F606W images of inner kpc(Simões Lopes+07, Malkan 98) :

§ Dusty nuclear spirals in all early-type 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 non-active


§ Sa, LINER/Seyfert 1

§ 0.7 kpc x 1 kpc

§ Nuclear spiral

§ 0.6”=60 pc


§ Stellar kinematics from absorption spectra (pPxf, Cappellari & Emsellem2004)

§ Gas kinematics from emission lines


§ Stellar velocity field: rotation

§ 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)

Gas kinematics Stellar kinematics


§ SO, Sy 2

§ FOV= 450 pc x 450 pc

§ 0.1”=15 pc

§ Gas kinematics: H2

§ Stellar kinematics: CO


Far

Near

§ Stellar velocity field: rotation

§ H2 velocity field: rotation + inflows + compact outflow

§ Warm (2000K) H2 mass ≈ 1400 M¤;

§ Warm H2: heated “skin” of cold gas; Cold H2 mass (Dale+05, Mazzalay +12) ~ 108-9 M¤

§ Warm H2 mass inflow rate ≈ 4 x 10-4

M¤ yr-1; estimated cold: > 1 M¤ yr-1


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 rapidlyabsorbs ionizing photons

§ HII masses: (0.03-4.4)x106M¤; surface

density ΣHII=0.2-36 M¤ pc-2

Warm molecular gas H2:§ H2: more uniform and extended: X-rays

penetrate the galactic plane in alldirections -> heat molecular gas

§ H2 masses: (0.05-3)x103M¤; surface density ΣH2=(0.2-14)x10-3 M¤ pc-2

§ Inflows in nuclear spirals, bars and disks, observed in H+ and H2; capture of dwarf companion (Fischer+15);

§ Inflow velocities: ~ 50-100 km/s;

§ Inflow rates: ~0.1 – few M¤yr-1 : 102-103 times the AGN accretion rate;

§ Total H+ masses in inner kpc ~ 105 - 108 M¤

§ Warm H2 masses: ~103 M¤; in cold H2: estimated 107-9 M¤(e.g. ALMA)

Øco-evolution: SMBH at 10-3 M¤yr-1 and galaxy at 1 M¤yr-1



§ NLRG, Sy 2

§ 0.6”= 700 pc

§ Extended [OIII] emission not aligned with radio jet (45deg)


§ 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 108 M¤

§ Mass outflow rate: ~0.1 M¤ yr-1

§ Outflow power: ~0.1% LAGN


[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


§ Rotation + equatorial outflow

§ Lateral expansion due to radio jet?

§ Mass outflow rate:~ 0.4 M¤ yr-1

§ HII mass: 1.3 ± 0.2 x 106 M¤

§ Warm H2 mass: 471 ± 58 M¤

Outflow

rotation


§ Sb, Seyfert 2

§ 500 pc x 500 pc

¡ 0.1”= 7 pc

¡ [FeII], J and H-band: bi-polar (bicome)

¡ H2: 100 pc off-centered ringD as e t a l. 2 0 0 6

HST [OIII]

[Fe II]: patchy outflow § Velocities up to 800 km/s§ Mass outflow rate: 4± 1 M¤ yr-1

§ Outflow power: ~0.1% LAGN

H2 ring: rotation+ expansion in the plane

§ -200 km/s < v < +200 km/s


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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


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


§ ~60% have non-circular motions (mostly outflows)

§ Mean outflow rate: ~0.3 M¤ yr-1 (range: 10-3-102 M¤ yr-1 )

§ Mean outflow power: P~1041 erg/s (range 1037 - 1043 erg/s)

§ Only 1/3 sample have P>1% LAGN-> meaning effective feedback on galaxy

§ 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 100-200 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)


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