Gas Dynamics, AGN, Star Formation and ISM in Nearby Galaxies

Eva Schinnerer (MPIA)Eva Schinnerer (MPIA)

S. Haan, F. Combes, S. Garcia-Burillo, C.G. Mundell,S. Haan, F. Combes, S. Garcia-Burillo, C.G. Mundell,T. Böker, D.S. Meier , E. Emsellem, U. Lisenfeld, T. Böker, D.S. Meier , E. Emsellem, U. Lisenfeld,

D. Downes, D. CalzettiD. Downes, D. Calzetti

ISM in Nearby GalaxiesISM in Nearby GalaxiesWhy do we care?Why do we care?

Star Formation (SF)

Active Galactic Nuclei (AGN)

Gas Kinematics & ISM Properties

PDRs -- Photon Dominated RegionsXDRs -- X-ray Dominated RegionsShocks

Neutral Gas(Atomic &Molecular)

fuel

feedback

Spiral Arms (i.e. Density Waves)Large-scale Stellar barsDouble/Inner/Nuclear Barsnuclear Spiral Density Waves

Fueling nearby AGNs (e.g.NUGA - see talk by M. Krips): m=1 modes warps viscosity …

Gas Kinematics Main DriversOuter disk

center

Gas in BarsGas in BarsBasicsBasics

Meier & Turner (2004)

2

1

NGC 4303Schinnerer et al. (2002)

CO(1-0)

Roberts & StewarT (1987)

HI-NUGAHI-NUGA--

Gas Dynamics Gas Dynamics Over the Entire DiskOver the Entire Disk

VLA HI Survey of 16 Nearby Active GalaxiesVLA HI Survey of 16 Nearby Active Galaxies

AIM:AIM: Trace Gas Flow from Outer Disk to Very CenterTrace Gas Flow from Outer Disk to Very Center

S. Haan, PhD ThesisS. Haan, PhD Thesis

Seyferts

LINERs

Non-AGN

Inte

nsity

Map

Inte

nsity

Map

Inte

nsity

Map

Velo

city

Field

Velo

city

Field

Velo

city

Field

Findings (haan et al. 2008):LINERs - more large HI rings - more kinematically disturbed specialTime for Gas Flow in Barred Galaxies AGN activity linked to overall Disk

kinematics

22. Jan. 2008

Seyferts

LINERs

Non-AGN

HI

Inte

nsity

Map

HI

Inte

nsity

Map

HI

Inte

nsity

Map

Velo

city

Field

Velo

city

Field

Velo

city

Field

Findings (haan et al. 2008):LINERs - more large HI rings - more kinematically disturbed particular time for gas flow in bars

AGN activity linked to overall Disk kinematics

Finding Inflows using Gravity TorquesGas Dynamics within the DIsk

Haan et al. (in prep.)

Stellar Potential

Gas Distribution

Torque MapsShow In/Outflow

Angular MomentumtransferInflow

outflow

Noncircular Motions = inflow

Gas Flows and Mass Transfer EfficienciesGas Dynamics within the DIsk

Significant Gas Mass RedistributionLarger Gas Inflow Rates in Centers

Gas Flow Across Corotation Resonance

=> Strong Secular Evolution within Disks

Haan et al. (in prep.)

NGC 6946NGC 6946--

Central Mass Build-UpCentral Mass Build-Up

Molecular Gas Kinematics Molecular Gas Kinematics And And

Star Formation Tracers Star Formation Tracers at High Spatial Resolutionat High Spatial Resolution

Molecular Gas at ~10pc Resolutionmm-Interferometry

IRAM, Plateau de Bure

High Spectral (few km/s) & Spatial (<1’’) Resolution

Up-graded IRAM Plateau de Bure Interferometer:~ 0.3” resolution (at 1mm)3x more sensitive ~ 10x fasterMulti-Line Observations --> Chemistry

New Band: 2mm

Nuclear Region of NGC 6946Stars vs. Molecular Gas D=5.5 Mpc; 1” ~ 25 pc D=5.5 Mpc; 1” ~ 25 pc

PA ~ 35PA ~ 35oo; Incl. ~ 35; Incl. ~ 35oo

Large-Scale BarLarge-Scale Bar

50pc

HST H bandHST H band

Stellar Bar in NIR w/Length ~ 10” - 15”

PdBI 12CO(2-1)

20pc

Schinnerer, Böker, Emsellem, Lisenfeld (2006)

Gas Shows Classical Response Pattern for a Bar

Bar-Driven FuelingNGC6946

CO(2-1) Model

Inte

nsi

tyV

elo

city

400pc long barRedistributes gas

~ 107 Msun (r < 30 pc)

CR @ 260 pcbar=510 km/s kpc-1

Schinnerer, Böker, Emsellem & Lisenfeld (2006)

Where and When Stars Form Central 50pc of NGC6946

Schinnerer, Böker, Emsellem, Downes (2007)

PaPa HCN(1-0)HCN(1-0)3mm Continuum3mm Continuum

SFR ~ 0.1 Msun/yrAge ~ 5-10 Myr

SFR ~ 0.06 Msun/yrAge ~ < Myr

SFR ~ 0.1 Msun/yrAge ~ couple Myr

Star Formation in small Area over ~ 10 Myr

Fueling via Inner barMass Build-Up of ~ 106 Msun

In central 50pc(over last ~ 10 Myrs)

20pc

IC 342IC 342--

Nuclear Fueling &Nuclear Fueling &Star Formation FeedbackStar Formation Feedback

Impact of Nuclear Star FormationImpact of Nuclear Star FormationOnto the Gas FlowOnto the Gas Flow

Nuclear Cluster in IC342A Late-Type Barred Spiral

(Böker et al. 1997, 1999)(Böker et al. 1997, 1999)

Nuclear Stellar Cluster:

star formation~ 4 - 30 Myrs ago

Cluster mass ~ 107 Msun

HST V

D=3.3 Mpc; 1” ~ 16 pcPA ~ 35o; Incl. ~ 31o

Bar Length ~ 11 kpc

IC 342: Distribution of Molecular Gas

110 pc

OVRO CO (1-0)

H2 Mass (1’) ~ 4.4 x107 Msun

Masses ~ 106 Msun

Diameters ~ 20 - 50 pc(Wright et al. 1993, Levine et al. 1994)

Meier & Turner (2005)

Zooming in - IC342Gas vs. nuclear cluster

(Schinnerer, Böker, Meier, Calzetti, in prep.)

16pc

Molecular Gas & Dust CoincideGas reaches close To nuclear cluster(even more so in dense gas)

Ongoing Fueling? - IC342

H Bubble fills CO Cavity

stellar winds/SN appear to Shape inner edge of Eastern spiral arm

(obscured) HII region

(Schinnerer, Böker, Meier, Calzetti, in prep.)

Self-Regulation of Star FormationWhat is happening - Suggested Scenario

Before SF after SF

Nuclear SF changesNuclear SF changesGas FlowGas Flow

Timescales:vwinds (15-20 km/s): ~ 3 MyrsageSF ~ 4-30 Myrs

Energies:Emech (SB99) ~ 5e52 ergEGMC (2e6Msun) ~ 3e52 erg

Scenario plausible

(Schinnerer, Böker, Meier, Calzetti, in prep.)

Nuclear Star ClusterNuclear Star Cluster(almost) Shuts Off (almost) Shuts Off

Its Own SupplyIts Own Supply---> Feedback process!---> Feedback process!

What’s Next:What’s Next:--

Star Formation, ISM Star Formation, ISM And Gas KinematicsAnd Gas Kinematics

Molecular Gas ChemistryMolecular Gas ChemistryUtilizing Multiple MoleculesUtilizing Multiple Molecules

Next Steps - NGC 6946Chemistry

Schinnerer, Meier, Böker, Downes, Emsellem in prep.Schinnerer, Meier, Böker, Downes, Emsellem in prep.

Locate: star forming gas(chemically) fresh gas [from atomic reservoir](chemically) altered gas (SF, Gas Dynamics)

Census of multi-phase ISM

(Gas) Kinematics & Star Formation

KinematicsKinematics --- ionized Gas (different ISM Phase)--- ionized Gas (different ISM Phase) --- Stellar Velocity Fields/Dispersion--- Stellar Velocity Fields/Dispersion => Better Models of Kinematics => Better Models of Kinematics (see Talk by G. Dumas)(see Talk by G. Dumas)

Star FormationStar Formation --- History, Population, Location--- History, Population, Location --- Energy Injection into ISM--- Energy Injection into ISM --- Feedback Processes --- Feedback Processes

Summary & Conclusion Gas KinematicsGas Kinematics --- Ongoing Gas Redistribution within Disk--- Ongoing Gas Redistribution within Disk --- bars work (in general, Small & Large)--- bars work (in general, Small & Large) --- Sustained Nuclear fueling for > 10 Myr--- Sustained Nuclear fueling for > 10 Myr Nuclear Star FormationNuclear Star Formation --- can alter gas flow--- can alter gas flow --- self-regulated fueling--- self-regulated fueling => repetitive SF=> repetitive SF time-variable time-variable (models)(models)

Future BrightFuture Bright:: ALMAALMA

ALMA siteALMA site

ALMA test facilityALMA test facility