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ohp_meeting_september_2018 [2018/09/22 22:16] admin-mist |
ohp_meeting_september_2018 [2018/09/22 22:17] (current) admin-mist |
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| Starting with the idea that the ISM is a multiphase turbulent medium, several observations | Starting with the idea that the ISM is a multiphase turbulent medium, several observations | ||
| may help us to understand | may help us to understand | ||
| - | - Pierre's shear | + | * Pierre's shear |
| - | - Edith's starburst | + | * Edith's starburst |
| Line 169: | Line 169: | ||
| • To trace the multiphase ISM | • To trace the multiphase ISM | ||
| - | - HI maps (mass of WNM+CNM) | + | - - HI maps (mass of WNM+CNM) |
| - | - ArH+ (tracer of purely atomic gas -> even better tracer than HI) | + | - - 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 fine structure (set the global thermal balance of CNM -> mass of CNM) |
| - | - CII and OI metastable lines (trace the mass of WNM) | + | - - CII and OI metastable lines (trace the mass of WNM) |
| - | - CI fine structure lines | + | - - CI fine structure lines |
| - | -> gives a measure of the gas thermal pressure | + | - -> gives a measure of the gas thermal pressure |
| - | -> may give the mass of unstable gas | + | - -> may give the mass of unstable gas |
| - | -> its relation with CO gives strong constrain on chemical models | + | - -> its relation with CO gives strong constrain on chemical models |
| - | - CS, C2H, OH, and H2O (tracers of PDR in diffuse ISM) | + | - - CS, C2H, OH, and H2O (tracers of PDR in diffuse ISM) |
| - | - HF (tracer of H2) | + | - - HF (tracer of H2) |
| - | - CH (tracer of PDR, except maybe at small column densities) | + | - - CH (tracer of PDR, except maybe at small column densities) |
| - | - OH+ and H2O+ (tracers of CR ionization and molecular fraction) | + | - - 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 | • To trace the dissipation of turbulent energy at small scales and / or the turbulent mixing of phases at all scales | ||
| - | - CH+ and SH+ | + | - - CH+ and SH+ |
| - | - excited H2 | + | - - excited H2 |
| - | - HCO+ and CO | + | - - HCO+ and CO |
| - | - CH (anomaly with PDR predictions at small column densities) | + | - - CH (anomaly with PDR predictions at small column densities) |
| - | - SH (not sure) | + | - - SH (not sure) |
| • For the DENSE GAS in starburst galaxies, we could try | • For the DENSE GAS in starburst galaxies, we could try | ||
| - | - SH+ | + | - - SH+ |
| - | - the rotational diagram of CH+ (as high as possible) -> this would be new by the way | + | - - 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. | + | - - CO, OH or H2O which behave oppositely to CH+ in irradiated shocks. |