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Physical processes in the ISM

21–25 Oct 2013
MPE
Europe/Berlin timezone

Session

ISM on Galactic Scales

24 Oct 2013, 11:30
MPE

MPE

Gießenbachstraße 1 85748 Garching

Conveners

ISM on Galactic Scales

  • Rowan Smith

ISM on Galactic Scales

  • Mordecai-Mark MacLow

Presentation materials

There are no materials yet.

  1. 131. ISM on galactic scales: Observations
    Alberto Bolatto (University of Maryland)
    24/10/2013, 11:30
    review talk
  2. 127. ISM on galactic scales: Theory
    Andreas Burkert (USM/LMU)
    24/10/2013, 12:00
    review talk
  3. 50. Dust luminosity as a tracer of gas mass and gas heating
    Brent Groves (MPIA)
    24/10/2013, 14:00
    contributed talk
    In the local universe the mass of gas in galaxies is usually measured through the combination of the 21cm HI line, tracing the atomic gas, and the CO sub-millimeter lines that trace the molecular interstellar medium (ISM). However, the dust infrared continuum provides another tracer of the ISM mass, through two paths; the correlation of dust and gas mass, and the association of the total IR...
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  4. 23. Structure formation and evolution in gas-rich disk systems
    Manuel Behrendt (MPE, Garching)
    24/10/2013, 14:15
    contributed talk
    We perform high resolution hydrodynamical simulations of gas-rich disks to get a better understanding of the origin and peculiar properties of the dominating structures in z=2 massive disk galaxies. Their structure is irregular, they have highly turbulent motions and high gas fractions of 30-80%. Stars form with enormous rates of a factor of 10-100 higher than in the Milky Way. The star...
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  5. 61. The Survey of Lines in M31 (SLIM): Investigating the Origins of [CII] Emission
    Maria Kapala (Max Planck Institute for Astronomy)
    24/10/2013, 14:30
    contributed talk
    The [CII] 158 micron line is typically the brightest emission line from star-forming galaxies and arises from both the ionized and neutral phases of the ISM. As a strong line it has been suggested both as a tracer of star-formation and a diagnostic of the ISM, but first we must distinguish the ISM phases it arises from and understand how it is excited. To address these issues we have...
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  6. 65. Evolution of molecular gas in spiral galaxies
    Jin Koda (Stony Brook University)
    24/10/2013, 14:45
    contributed talk
    I will discuss the formation and evolution of giant molecular clouds (GMCs) in spiral galaxies. The evolution appears quite different between the molecule-rich and atom-rich galaxies. GMCs exist almost exclusively along HI spiral arms and filaments in atom-rich galaxies, suggesting that they form and finish their short lifetimes within the HI arms. However, in molecular-rich galaxies, GMCs are...
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  7. 67. Superbubbles as a physical process in the ISM
    Dr Martin Krause (Max-Planck-Institut für extraterrestrische Physik)
    24/10/2013, 15:00
    contributed talk
    With sizes from below 100 pc to just above 1kpc, superbubbles are structuring the ISM on scales in between the larger scale spiral arms and the smaller, turbulent molecular cloud scales. With 3D hydrodynamics simulation of the entire stellar evolution of and the interaction between an ensemble of massive stars we are able to explain at least some of the apparent width of observed bubbles...
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  8. 73. Star formation and molecular gas outside galaxies
    Ute Lisenfeld (Universidad Granada)
    24/10/2013, 15:15
    contributed talk
    In galaxy collisions gas and stars can be torn out of the parent galaxies, giving rise to tails and bridges of gas and to intergalactic star forming region of different sizes. These regions are ideal to study the conditions for the onset of star formation in very simple environments which are different from those in spiral galaxies. I will describe and compare the molecular gas properties...
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  9. 92. The resolved ISM of our nearest spiral galaxy
    Andreas Schruba (MPE, Garching)
    24/10/2013, 16:00
    contributed talk
    I summarize first results from a large CARMA survey to image CO(1-0) emission at high sensitivity and resolution (20pc, 1km/s) in the nearby Andromeda galaxy (M31). This survey augments a new extensive set of multi-wavelength data including Hubble, Spitzer, Herschel, VLA photometry and spectroscopy that provide an unprecedented knowledge of the stars, dust, and gas in M31. We are able to...
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  10. 95. The sub-linear and non-universal Kennicutt-Schmidt relationship
    Rahul Shetty (ZAH/ITA, University of Heidelberg)
    24/10/2013, 16:15
    contributed talk
    The star formation rate is observed to be strongly correlated with the gas surface density. This correlation is well described as a power-law with index N, now known as the Kennicutt-Schmidt (KS) relationship. Previous efforts have inferred N=1.5 when considering both resolved observations of galaxies as well as unresolved starbursting systems. More recently, analysis of resolved observations...
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  11. 108. Two regimes of star formation
    Javier Zaragoza-Cardiel (Instituto de Astrofísica de Canarias)
    24/10/2013, 16:30
    contributed talk
    We have used interacting galaxies to explore the properties of high luminosity star forming zones. With the GHaFaS Fabry-Perot spectrometer on the 4.2m William Herschel Telescope (La Palma) we have used Halpha emission to obtain complete 2D mapping in surface brightness, velocity, and velocity dispersion of 8 paris of interecting galaxies. The detailed kinematics reveal global features such as...
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