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Starburst Galaxies: Outflows of Metal and Energy into the IGM

Starburst Galaxies: Outflows of Metal and Energy into the IGM. Sun Wei 4/15/2009. Superwind Feedback. Galaxy Formation Galactic Winds (Veilleux et al. 2005) Plasma in the Halo Pollution of Intergalactic Medium (IGM) (Songaila 1997; Simcoe et al. 2003). Key Question:.

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Starburst Galaxies: Outflows of Metal and Energy into the IGM

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  1. Starburst Galaxies: Outflows of Metal and Energy into the IGM Sun Wei 4/15/2009

  2. Superwind Feedback • Galaxy Formation • Galactic Winds (Veilleux et al. 2005) • Plasma in the Halo • Pollution of Intergalactic Medium (IGM) (Songaila 1997; Simcoe et al. 2003)

  3. Key Question: • What is the contribution of mass, metals and energy from starburst galaxies to the Intergalactic Medium?

  4. Outline • Intro to Superwind Feedback • Feedback from Starburst-Driven Superwinds to IGM • Creating a Future for Superwind Studies • Some Recent Works on M82

  5. Superwind • Power: Massive star winds Core collapse SNe (Type II) • Creation: Metal-enriched plasma Cool entrained gas (Howk & Savage 1999) • Feedback to IGM powerful superwind in lower mass galaxies? (Ferrara & Tolstoy 2000; Keeney et al. 2006 vs Strickland et al. 2006)

  6. Key Information • Velocity • Chemical Composition Chemical feedback Plasma in the halo Metal enrichment of the IGM Cooling efficiency

  7. Velocity

  8. Velocity • Warm neutral and ionized gas: 200~1000km s-1 (Shapley et al. 2003; Rupke et al. 2005; Martin 2005) near galactic escape velocity! • Hot gas: no direct observational measurement Require better spectral resolution

  9. a Schematic Diagram Face-on: line centroid shifts line broadening Edge-0n: Spatially-resolved X-ray spectroscopy

  10. Observation Requirement • Better spectral resolution! chemical composition velocity information • Same good spatial resolution • International X-ray Obervatory?

  11. Recent Work on M82 • Starburst-driven superwind (observation & model) Mass-loading Metallicity of plasma in the halo/Cap Entrained cool gas • Ref: Strickland & Heckman 2007, ApJ 658,258 Strickland & Heckman 2009, arXiv 0903.4175 Tsuru et al. 2007, PASJ 59, 269

  12. Abundance • O & Fe are lower than Si & S in Cap from ASCA &XMM-Newton • Weak 6.69 keV Fe Heα line: too weak even treated Fe as solar abundance Explanation: 1. plasma is multi-phase; 2. plasma is not in collisional ionization equilibrium (CIE).

  13. Key Question: • What is the contribution of mass, metals and energy from starburst galaxies to the Intergalactic Medium? • A high sensitivity X-ray imaging spectrometer with a velocity accuracy of for composition, energetics and flow rates diagnostics. Experimental Requirement:

  14. Thanks!

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