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The Interstellar Medium and Star Formation Process in the Andromeda Galaxy

ESO 3D2014: Gas and Stars in Galaxies March 10, 2014. The Interstellar Medium and Star Formation Process in the Andromeda Galaxy. Andreas Schruba Max-Planck- Institut für extraterrestrische Physik. ESO 3D2014: Gas and Stars in Galaxies March 10, 2014. The CARMA Survey of Andromeda.

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The Interstellar Medium and Star Formation Process in the Andromeda Galaxy

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  1. ESO 3D2014: Gas and Stars in Galaxies March 10, 2014 The Interstellar Mediumand Star Formation Processin the Andromeda Galaxy Andreas Schruba Max-Planck-InstitutfürextraterrestrischePhysik

  2. ESO 3D2014: Gas and Stars in Galaxies March 10, 2014 The CARMA Survey of Andromeda Today’s largest (0.1 deg2) Interferometric Survey of CO(1-0) on Cloud Scale (20 pc x 1 km/s)

  3. ESO 3D2014: Gas and Stars in Galaxies March 10, 2014 1 • Where is the Molecular Gas in a ‘normal’ Spiral? 2 • What are the Properties of Molecular Clouds? 3 • Is there Concordance of Cloud Properties?

  4. 1 • Where is the Molecular Gas in a Spiral? … a 3D cloud-scale view of CO(1-0) in Andromeda Schruba+ (in prep)

  5. 1 • Where is the Molecular Gas in a Spiral? … a 2D cloud-scale view of CO(1-0) in Andromeda Peak Brightness Schruba+ (in prep)

  6. 1 • Where is the Molecular Gas in a Spiral? … PDFs of CO Pixel Brightness LMC M31 M51 ~ 0.33 dex Log width ~ 0.26 dex ~ 0.23 dex Most emission at low intensity (signal-to-noise) and thus often missed. Data at Common Resolution of 50 pc x 5 km/s Hughes+13; Gratier+12

  7. 1 • A Thick Disk of (diffuse) Molecular Gas M31: cumulative emission around local HI velocity Velocity Dispersion of HI and CO in 12 spirals at low inclination Caldu-Primo+ 13 M31 • 76% of flux within ~40 km/s • LOS dispersion ~18 km/s • … but M31 highly inclined Line Width of HI and CO comparable => Evidence for thick disk of diffuse H2 Caldu-Primo+13; Pety+13

  8. 2 • Mass Spectrum of Molecular Clouds … as described by truncated power-law M51 M33 M31 10-kpc ring 5-kpc ring All data: γ= -2.0 range: -1.5 … -2.3 All data: γ= -2.3 range: -1.3 … -2.6 10-kpc ring: γ= -2.0 5-kpc ring: γ= -1.4 Cloud mass spectrum steeper in low-density then high-density environments, … but cloud samples contain only ~50% of total mass, rest in diffuse phase Colombo+13; Gratier+12; Wong+11; Rosolowsky+05; Heyer+01

  9. 2 • Surface Density of Molecular Clouds … mass vs. radius for Milky Way and nearby SF galaxy clouds starbursts not shown Surface Density spirals Limit dwarfs Andromeda 10-kpc ring 5-kpc ring outer disk

  10. 2 • Turbulence of Molecular Clouds … line width vs. radius for Milky Way and nearby SF galaxy clouds VirialRatio Gravitational Stability Andromeda 10-kpc ring 5-kpc ring

  11. 2 • Turbulence of Molecular Clouds … how much of the line width can be explained by self-gravity? … concordance of properties (ieoffsets) of neighboring clouds? fixed external pressure (Field et al. 2011) Andromeda 10-kpc ring 5-kpc ring

  12. 3 • Concordance of Cloud Properties? 500pc Text avg cloud properties (σ2/l) for neighboring clouds

  13. 3 • Concordance of Cloud Internal Properties? 3rd 11th Distance H2 Surface Density @ 200pc 15th 7th SFR Surface Density @ 200pc Cloud Mass

  14. 3 • Concordance of Cloud-to-Cloud Motions?

  15. 3 • Concordance of Cloud-to-Cloud Motions? Distance H2 Surface Density @ 200pc SFR Surface Density @ 200pc Cloud Mass

  16. A Short Summary 1 • Evidence of diffuse molecular gas in thick disk 2 • Molecular Clouds don’t have uniform properties 3 • Neighboring Clouds have uncorrelated properties

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