The Ionized Structure of the Local Spur

Details The Ionized Structure of the Local Spur The Ionized Structure of the Local Spur

Jul 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009apj...699..716c&link_type=abstract

The Astrophysical Journal, Volume 699, Issue 1, pp. 716-721 (2009).

Astronomy and Astrophysics

Astronomy

Galaxies: Structure, H Ii Regions, Ism: Clouds, Radio Lines: Ism

Scientific paper

The distribution of the H166α radio recombination line emission at the end of the first quadrant is obtained and compared with the distribution of H I and other young objects. The data analyzed lie in the Galactic longitude range between l = 60° and l = 91° and was observed with single dish antenna at 1.4 GHz. The extended low-density warm ionized medium (ELDWIM) is used to trace the Local Spur (LS), which is strongly correlated with neutral hydrogen and low-brightness H II regions. The Galactic distribution of gas in the (X, Y, z) Galactic coordinates yields the location of ionized hydrogen in an arclike structure at an almost constant distance of 8 kpc from the galactic center. The ELDWIM and the low-brightness H II region define the LS; it is located between r sime 0.5 and 5 kpc from the Sun. We found sources of ionized gas at larger distances; they are probably located in the Perseus arm. The structure of the LS does not seem to join the Perseus arm at farther distances, a fact gleaned from the H I emission. The LS is very thick between 2 and 5 kpc, where the ionized gas spreads from z sime -150 to +250 pc. The z distribution of the ionized gas appears tilted with respect to the Galactic plane, which starts at 3 kpc from the Sun and runs toward higher galactocentric radii on the Perseus arm.

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