Gas Dynamics, AGN, Star Formation and ISM in Nearby Galaxies Eva Schinnerer (MPIA) S. Haan, F. Combes, S. Garcia-Burillo, C.G. Mundell, T. Böker, D.S. Meier, E. Emsellem, U. Lisenfeld, D. Downes, D. Calzetti

ISM in Nearby Galaxies Why do we care? Star Formation (SF) Active Galactic Nuclei (AGN) Gas Kinematics & ISM Properties PDRs -- Photon Dominated Regions XDRs -- X-ray Dominated Regions Shocks Neutral Gas (Atomic & Molecular) fuel feedback

Spiral Arms (i.e. Density Waves) Large-scale Stellar bars Double/Inner/Nuclear Bars nuclear Spiral Density Waves Fueling nearby AGNs (e.g.NUGA - see talk by M. Krips): m=1 modes warps viscosity … Gas Kinematics Main Drivers Outer disk center

Gas in Bars Gas in Bars Basics Meier & Turner (2004) 2 1 NGC 4303 Schinnerer et al. (2002) CO(1-0) Roberts & StewarT (1987)

HI-NUGA- Gas Dynamics Over the Entire Disk VLA HI Survey of 16 Nearby Active Galaxies AIM: Trace Gas Flow from Outer Disk to Very Center S. Haan, PhD Thesis

Seyferts LINERs Non-AGN Intensity Map Intensity Map Intensity Map Velocity Field Velocity Field Velocity 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 Seyferts LINERs Non-AGN HI Intensity Map HI Intensity Map HI Intensity Map Velocity Field Velocity Field Velocity 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 Torques Gas Dynamics within the DIsk Haan et al. (in prep.) Stellar Potential Gas Distribution Torque Maps Show In/Outflow Angular Momentum transfer Inflow outflow Noncircular Motions = inflow

Gas Flows and Mass Transfer Efficiencies Gas Dynamics within the DIsk Significant Gas Mass Redistribution Larger Gas Inflow Rates in Centers Gas Flow Across Corotation Resonance => Strong Secular Evolution within Disks Haan et al. (in prep.)

NGC Central Mass Build-Up Molecular Gas Kinematics And Star Formation Tracers at High Spatial Resolution

Molecular Gas at ~10pc Resolution mm-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 faster Multi-Line Observations --> Chemistry New Band: 2mm

Nuclear Region of NGC 6946 Stars vs. Molecular Gas D=5.5 Mpc; 1” ~ 25 pc D=5.5 Mpc; 1” ~ 25 pc PA ~ 35 o ; Incl. ~ 35 o PA ~ 35 o ; Incl. ~ 35 o Large-Scale Bar Large-Scale Bar 50pc HST H band Stellar Bar in NIR w/ Length ~ 10” - 15” PdBI 12 CO(2-1) 20pc Schinnerer, Böker, Emsellem, Lisenfeld (2006) Gas Shows Classical Response Pattern for a Bar

Bar-Driven Fueling NGC6946 CO(2-1) Model Intensity Velocity 400pc long bar Redistributes gas ~ 10 7 M sun (r < 30 pc) 260 pc  bar =510 km/s kpc -1 Schinnerer, Böker, Emsellem & Lisenfeld (2006)

Where and When Stars Form Central 50pc of NGC6946 Schinnerer, Böker, Emsellem, Downes (2007) Pa  HCN(1-0) 3mm Continuum SFR ~ 0.1 M sun /yr Age ~ 5-10 Myr SFR ~ 0.06 M sun /yr Age ~ < Myr SFR ~ 0.1 M sun /yr Age ~ couple Myr Star Formation in small Area over ~ 10 Myr Fueling via Inner bar Mass Build-Up of ~ 10 6 M sun In central 50pc (over last ~ 10 Myrs) 20pc

IC Nuclear Fueling & Star Formation Feedback Impact of Nuclear Star Formation Onto the Gas Flow

Nuclear Cluster in IC342 A Late-Type Barred Spiral (Böker et al. 1997, 1999) Nuclear Stellar Cluster: star formation ~ Myrs ago Cluster mass ~ 10 7 M sun HST V D=3.3 Mpc; 1” ~ 16 pc PA ~ 35 o ; Incl. ~ 31 o Bar Length ~ 11 kpc

IC 342: Distribution of Molecular Gas 110 pc OVRO CO (1-0) H 2 Mass (1’) ~ 4.4 x10 7 M sun Masses ~ 10 6 M sun Diameters ~ pc (Wright et al. 1993, Levine et al. 1994) Meier & Turner (2005)

Zooming in - IC342 Gas vs. nuclear cluster (Schinnerer, Böker, Meier, Calzetti, in prep.) 16pc Molecular Gas & Dust Coincide Gas 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 Formation What is happening - Suggested Scenario Before SF after SF Nuclear SF changes Gas Flow Timescales: v winds (15-20 km/s): ~ 3 Myrs age SF ~ 4-30 Myrs Energies: E mech (SB99) ~ 5e52 erg E GMC (2e6M sun ) ~ 3e52 erg Scenario plausible (Schinnerer, Böker, Meier, Calzetti, in prep.) Nuclear Star Cluster (almost) Shuts Off Its Own Supply ---> Feedback process!

What’s Next: - Star Formation, ISM And Gas Kinematics Molecular Gas Chemistry Utilizing Multiple Molecules

Next Steps - NGC 6946 Chemistry 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 Kinematics Kinematics --- 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 Formation Star Formation --- History, Population, Location --- History, Population, Location --- Energy Injection into ISM --- Energy Injection into ISM --- Feedback Processes --- Feedback Processes

Summary & Conclusion Gas Kinematics Gas 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 Formation Nuclear 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 Bright : ALMA ALMA ALMA site ALMA test facility