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

Explore the intricate connection between gas dynamics, AGN activity, and star formation in nearby galaxies. Understand the role of various gas components, kinematics, and feedback mechanisms, shedding light on the evolution of galaxy structures.

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

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  1. 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

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

  3. Gas Kinematics Main Drivers Outer disk 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 … center

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

  5. 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

  6. Intensity Map Seyferts Velocity Field Intensity Map LINERs Velocity Field Intensity Map 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 Non-AGN Velocity Field

  7. HI Intensity Map Seyferts Velocity Field HI Intensity Map LINERs Velocity Field HI Intensity Map 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 Non-AGN Velocity Field

  8. Gas Dynamics within the DIsk Finding Inflows using Gravity Torques Stellar Potential Torque Maps Show In/Outflow Noncircular Motions = inflow Gas Distribution outflow Angular Momentum transfer Inflow Haan et al. (in prep.)

  9. Gas Dynamics within the DIsk Gas Flows and Mass Transfer Efficiencies 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.)

  10. NGC 6946 - Central Mass Build-Up Molecular Gas Kinematics And Star Formation Tracers at High Spatial Resolution

  11. IRAM, Plateau de Bure Molecular Gas at ~10pc Resolution mm-Interferometry 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

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

  13. Bar-Driven Fueling NGC6946 CO(2-1) Model Intensity 400pc long bar Redistributes gas ~ 107 Msun (r < 30 pc) CR @ 260 pc bar=510 km/s kpc-1 Velocity Schinnerer, Böker, Emsellem & Lisenfeld (2006)

  14. Star Formation in small Area over ~ 10 Myr Where and When Stars Form Central 50pc of NGC6946 3mm Continuum HCN(1-0) Pa Fueling via Inner bar Mass Build-Up of ~ 106 Msun In central 50pc (over last ~ 10 Myrs) 20pc SFR ~ 0.1 Msun/yr Age ~ couple Myr SFR ~ 0.1 Msun/yr Age ~ 5-10 Myr SFR ~ 0.06 Msun/yr Age ~ < Myr Schinnerer, Böker, Emsellem, Downes (2007)

  15. IC 342 - Nuclear Fueling & Star Formation Feedback Impact of Nuclear Star Formation Onto the Gas Flow

  16. Nuclear Cluster in IC342 A Late-Type Barred Spiral HST V Nuclear Stellar Cluster: star formation ~ 4 - 30 Myrs ago Cluster mass ~ 107 Msun D=3.3 Mpc; 1” ~ 16 pc PA ~ 35o; Incl. ~ 31o Bar Length ~ 11 kpc (Böker et al. 1997, 1999)

  17. OVRO CO (1-0) 110 pc Meier & Turner (2005) IC 342: Distribution of Molecular Gas H2 Mass (1’) ~ 4.4 x107 Msun Masses ~ 106 Msun Diameters ~ 20 - 50 pc (Wright et al. 1993, Levine et al. 1994)

  18. Zooming in - IC342 Gas vs. nuclear cluster 16pc Molecular Gas & Dust Coincide Gas reaches close To nuclear cluster (even more so in dense gas) (Schinnerer, Böker, Meier, Calzetti, in prep.)

  19. 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.)

  20. Self-Regulation of Star Formation What is happening - Suggested Scenario Nuclear SF changes Gas Flow Timescales: vwinds (15-20 km/s): ~ 3 Myrs ageSF ~ 4-30 Myrs Energies: Emech (SB99) ~ 5e52 erg EGMC (2e6Msun) ~ 3e52 erg Scenario plausible Nuclear Star Cluster (almost) Shuts Off Its Own Supply ---> Feedback process! Before SF after SF (Schinnerer, Böker, Meier, Calzetti, in prep.)

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

  22. Next Steps - NGC 6946 Chemistry Locate: star forming gas (chemically) fresh gas [from atomic reservoir] (chemically) altered gas (SF, Gas Dynamics) Census of multi-phase ISM Schinnerer, Meier, Böker, Downes, Emsellem in prep.

  23. (Gas) Kinematics & Star Formation Kinematics --- ionized Gas (different ISM Phase) --- Stellar Velocity Fields/Dispersion => Better Models of Kinematics (see Talk by G. Dumas) Star Formation --- History, Population, Location --- Energy Injection into ISM --- Feedback Processes

  24. Summary & Conclusion Gas Kinematics --- Ongoing Gas Redistribution within Disk --- bars work (in general, Small & Large) --- Sustained Nuclear fueling for > 10 Myr Nuclear Star Formation --- can alter gas flow --- self-regulated fueling => repetitive SF time-variable (models) Future Bright: ALMA ALMA test facility ALMA site

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