PART I Galaxy Formation Models Darren Croton Centre for - - PowerPoint PPT Presentation

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PART I Galaxy Formation Models Darren Croton Centre for - - PowerPoint PPT Presentation

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PART I Galaxy Formation Models Darren Croton Centre for Astrophysics and Supercomputing Swinburne University dcroton@astro.swin.edu.au PART I: Building synthetic universes PART II: The parameters of galaxy formation PART III: The universe in

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PART I Galaxy Formation Models

Darren Croton Centre for Astrophysics and Supercomputing Swinburne University dcroton@astro.swin.edu.au

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PART I: Building synthetic universes PART II: The parameters of galaxy formation PART III: The universe in the cloud

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The basics of how galaxies are built and evolve The uses and limitations of semi-analytic galaxy models The challenge of data access and delivery

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$20 z=1 $30 z=2 $40 z=3

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Galaxy formation primer

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The skeleton The flesh

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  • 1. The skeleton: N-body simulations
  • 2. The flesh: interwoven analytic models of

the physics of galaxy formation

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%& %& %&

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SLIDE 15 cluster milky-way Wechsler et al. 2002 z=0 z=1 z=6 z=3
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  • 1. The skeleton: N-body simulations
  • 2. The flesh: interwoven analytic models of

the physics of galaxy formation

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Galaxies, why we care ...

  • highly non-linear evolution
  • home of internal phenomena
  • shaped by external influences
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Star formation

M31

Kennicutt 1998
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M82

Supernova feedback

Martin 1999
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Satellite galaxies

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NGC 2207 & IC 2163

Morphological evolution

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... and assembly

Seyfert’s Sextet

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... and death

M87 (Virgo cluster)

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Black holes

NGC 6240

Haring & Rix 2005
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AGN jets

M87 (Virgo cluster)

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AGN bubbles

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SLIDE 28 GEMS (Rix et al. 2004)
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iPad

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  • Schmidt law star formation
  • SFR dependent SN winds
  • satellite gas stripping
  • morphological transformation
  • assembly through mergers
  • starbursts through mergers
  • Magorrian relation BH growth
  • jet & bubble AGN feedback

Croton et al. 2006

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z=0 dark matter

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Remember:

Numerical Simulation + Analytic Simulation
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z=0 galaxy light

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Galaxy spatial and luminosity distributions

  • clustering- -luminosity function-
Croton et al. 2006
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  • model- -SDSS-

Galaxy colour distribution

Croton et al. 2006 Baldry et all. 2005
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Physical consequences

AGN SN AGN

Croton et al. 2006

(∝mBHσ3) (∝SFR)

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AGN SN

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AGN SN

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Our model is only as good as the questions we ask For systems with infinite levels of complexity, our model can never be “correct”

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...and the story continues in the next lecture with “Model parameterisation”...