Disclaimer ❖ Just slightly scientific ❖ Pretty pictures are key! ❖ Talk to me about: ❖ HI ❖ Observational multiphase ISM ❖ CIB/CMB component separation ❖ Dust/Reddening ❖ Machine learning, Bayesian models, python, Mac OS
On Galactic HI ❖ Very abundant, easy to detect ❖ Key to understanding galaxy evolution ❖ How do galaxies replenish their star-formation fuel? ❖ Important for foreground modeling of cosmological signals
Multiphase ISM -15.9797 184.878 K km s 1 -1 3.8 log10 (Rayleighs) -1.00791 1.24339 log10 (Counts) ❖ There is so much more! ❖ No need for more data, just need to be smarter H⍺ -rays CII
The Cosmic Infrared Background ❖ Made up from dust in star- forming galaxies at z = 1..2 ❖ Used for ❖ cosmic evolution of the star formation rate ❖ tracer of the density field Lagache+ (2005)
Reddening ❖ E(B-V) = Extinction in B band - Extinction in V band ❖ More dust => larger E(B-V) ❖ E(B-V) maps essential for correcting observations for Galactic reddening ❖ Schlegel, Finkbeiner, Davis (1998) still state-of-the-art
Reddening ❖ E(B-V) = Extinction in B band - Extinction in V band ❖ More dust => larger E(B-V) ❖ E(B-V) maps essential for correcting observations for Galactic reddening ❖ Schlegel, Finkbeiner, Davis (1998) still state-of-the-art
Thanks! ❖ Talk to me about: ❖ HI ❖ Observational multiphase ISM ❖ CIB/CMB component separation ❖ Dust/Reddening ❖ Machine learning, Bayesian models, python, Mac OS