HI-distribution in the MW

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Presentation transcript:

HI-distribution in the MW Supervisor: Peter Kalberla Group #1 Bitten Gullberg Maria Louise Strandet Sarolta Zahorecz Valentina Vacca

OUTLINE 1. Scientific aim and method 2. Theoretical background 3. Data presentation 4. Discussion

Scientific aim and method Scientific aim: To explore the HI distribution in the Milky Way and to determine the kinetic spin temperature of filaments Method: We fit the emission and absorption lines by means of gaussian curves

OUTLINE 1. Scientific aim and method 2. Theoretical background 3. Data presentation 4. Discussion

Self absorbing HI clouds Background continuum Have been subtracted in our data Foreground HI emission Can be ignored because we are close (125 pc) to the self absorbing cloud Background HI emission

OUTLINE 1. Scientific aim and method 2. Theoretical background 3. Data presentation 4. Discussion

Parkes Telescope Location: Australia, NSW Diameter: 64 m Telescope and survey Parkes Telescope Location: Australia, NSW Diameter: 64 m Galactic All Sky Survey

Data presentation

Data presentation

Data presentation

Data presentation

Data presentation

Data presentation

Data presentation

Data presentation

Data presentation

Data presentation

Data presentation

Data presentation

OUTLINE 1. Scientific aim and method 2. Theoretical background 3. Data presentation 4. Discussion

The kinetic spin temperature The kinetic spin temperature is calculated as Where σ is the actual velocity dispersion, where the instrumental broadening has been taken into account For GASS the instrumental broadening is

The kinetic spin temperature Range: 203 – 325 K Average: 247 K Range: 101 – 275 K Average: 170 K Very turbulent!

The kinetic spin temperature T = 65 K T=14 K Montgomery et al. (1995)

Thank you!