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ohp_meeting_september_2018 [2018/09/22 22:08] admin-mist |
ohp_meeting_september_2018 [2018/09/22 22:17] (current) admin-mist |
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| - | ====== Notes taken by FL | + | ==== Presentations ==== |
| - | ====== | + | |
| + | {{ :ohp_lehmann.pdf |Andrew}} | ||
| + | {{ :ohp-lesaffre.pdf |Pierre L}} | ||
| + | {{ :mist-ohp.pdf |François L}} | ||
| + | |||
| + | ==== Notes taken by FL ==== | ||
| **EDITH FALGARONE | **EDITH FALGARONE | ||
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| * Turbulence increase pushes more gas away from the thermal equilibrium curve. | * Turbulence increase pushes more gas away from the thermal equilibrium curve. | ||
| * Increase of B prevents the formation of dense structures. | * Increase of B prevents the formation of dense structures. | ||
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| + | |||
| + | ==== Afterthoughts by BG ==== | ||
| + | |||
| + | Starting with the idea that the ISM is a multiphase turbulent medium, several observations | ||
| + | may help us to understand | ||
| + | * Pierre's shear | ||
| + | * Edith's starburst | ||
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| + | |||
| + | I'm no observer so I'll just throw ideas even if they are ridiculous or not completely correct | ||
| + | |||
| + | • To trace the multiphase ISM | ||
| + | - - HI maps (mass of WNM+CNM) | ||
| + | - - ArH+ (tracer of purely atomic gas -> even better tracer than HI) | ||
| + | - - CII and OI fine structure (set the global thermal balance of CNM -> mass of CNM) | ||
| + | - - CII and OI metastable lines (trace the mass of WNM) | ||
| + | - - CI fine structure lines | ||
| + | - -> gives a measure of the gas thermal pressure | ||
| + | - -> may give the mass of unstable gas | ||
| + | - -> its relation with CO gives strong constrain on chemical models | ||
| + | - - CS, C2H, OH, and H2O (tracers of PDR in diffuse ISM) | ||
| + | - - HF (tracer of H2) | ||
| + | - - CH (tracer of PDR, except maybe at small column densities) | ||
| + | - - OH+ and H2O+ (tracers of CR ionization and molecular fraction) | ||
| + | |||
| + | |||
| + | • To trace the dissipation of turbulent energy at small scales and / or the turbulent mixing of phases at all scales | ||
| + | - - CH+ and SH+ | ||
| + | - - excited H2 | ||
| + | - - HCO+ and CO | ||
| + | - - CH (anomaly with PDR predictions at small column densities) | ||
| + | - - SH (not sure) | ||
| + | |||
| + | |||
| + | • For the DENSE GAS in starburst galaxies, we could try | ||
| + | - - SH+ | ||
| + | - - the rotational diagram of CH+ (as high as possible) -> this would be new by the way | ||
| + | - - CO, OH or H2O which behave oppositely to CH+ in irradiated shocks. | ||