The Bubbling Galactic Disk. II. The Inner 20°

Details The Bubbling Galactic Disk. II. The Inner 20° The Bubbling Galactic Disk. II. The Inner 20°

Nov 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007apj...670..428c&link_type=abstract

The Astrophysical Journal, Volume 670, Issue 1, pp. 428-441.

Astronomy and Astrophysics

Astronomy

41

Ism: H Ii Regions, Ism: Bubbles, Stars: Formation

Scientific paper

We report 269 mid-infrared bubbles within 10° of the Galactic center from visual inspection of the Spitzer GLIMPSE II Legacy Science program images. The surface density of bubbles is ~5 deg-2 or about 3 times that detected in longitudes |l|=10deg-65°, because the inner 10° of longitude were more thoroughly searched for small bubbles. There is a gradient in the number of bubbles with longitude with an increase of about a factor of 2 from 2° to 10° this is probably the result of several factors, including decreasing diffuse background brightness, confusion, and opacity with longitude. Bubble eccentricities are typically between 0.6 and 0.8, and >50% show evidence for blowouts, which we suggest result from local density fluctuations of the ISM and/or anisotropic stellar winds and radiation fields. The fraction of bubbles identified with H II regions and clusters is only about half that found at |l|>10deg. This is largely a result of the much smaller angular diameter of bubbles cataloged in the inner Galaxy than in the outer Galaxy. At least 12% of the bubbles have morphologies suggestive of triggered star formation. Most of the bubbles that show evidence for triggered star formation in the inner Galaxy have not formed secondary bubbles; it is postulated that this may be because they are too young to have had time for this to occur.

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