Detecting Dark Clouds in the Galactic Plane with 2MASS data By : Luis Mercado. In collaboration with the part of GLIMPSE team (Christer Watson, Ed Churchwell and Bob Benjamin). Introduction / Background. What are Dark Clouds and why study them? Optically thick at visual and IR wavelengths
By : Luis Mercado
In collaboration with the part of GLIMPSE team (Christer Watson, Ed Churchwell and Bob Benjamin)
Image - Background
1.2’ radius for image
2.0’ radius for smoothing
H-Kave from l = 10°-15°
K stellar density
K-density contrastWhat it all looks like…
MSX image of same field
(l = 10°15°).
Notice the correlation between the dark blue objects on the contrast plot and high absorption areas (dark clouds) in the MSX image.
Also plotted are contours obtained from our selection method for the corresponding area.
Left: Histogram of # of dark clouds detected vs. galactic longitude. Notice a rise in detections at high longitudes, opposite to what would be expected
Right: Plot of noise and density versus longitude. Notice the similar behavior. It turns out noise seems to be proportional to the density, but in an unexpected way.