1. Star Formation in GLIMPSE360

2. IRAC 3.6 & 4.5 pick out star formation regions
K (2MASS)
IRAC [3.6]
IRAC [4.5]
AFGL490, d=1 kpc
BG , d=10 kpc

3. IRAC 3.6 and 4.5 Catalogs pick out YSOs
“Empty field”
GL490 region
Catalog
stars
YSOs
Simulated cluster at 10 kpc using
YSO grid of models (Robitaille et al. 2006)

5. IRAC 4.5 discovers shocked outflows
New
Known
radio
outflow
GL490 with
Known
Molecular
outflow
New discoveries

6. Results and more to come
We can detect YSOs, outflows, PAH bubbles
The higher dynamic range than GLIMPSE allows detection of PAH emission at 3.6, faint outflows, and both massive and low-mass YSO
We easily detect star formation regions at 10 kpc
We detect much smaller SFRs, probably much more distant
More to come
Using SED fitting of Catalog stars to fit extinction and find Infrared Dark clouds
Determine star formation rate as a function of Galactocentric radius (Robitaille & Whitney 2010, Povich et al. 2009/10)