55 research outputs found
Absorption Line Survey of H3+ toward the Galactic Center Sources II. Eight Infrared Sources within 30 pc of the Galactic Center
Infrared absorption lines of H3+, including the metastable R(3,3)l line, have
been observed toward eight bright infrared sources associated with hot and
massive stars located in and between the Galactic Center Cluster and the
Quintuplet Cluster 30 pc to the east. The absorption lines with high velocity
dispersion arise in the Galaxy's Central Molecular Zone (CMZ) as well as in
foreground spiral arms. The temperature and density of the gas in the CMZ, as
determined from the relative strengths of the H3+ lines, are T=200-300K and
n=50-200cm^-3. The detection of high column densities of H3+ toward all eight
stars implies that this warm and diffuse gaseous environment is widespread in
the CMZ. The products of the ionization rate and path length for these sight
lines are 1000 and 10 times higher than in dense and diffuse clouds in the
Galactic disk, respectively, indicating that the ionization rate, zeta, is not
less than 10^-15 s^-1 and that L is at least on the order of 50 pc. The warm
and diffuse gas is an important component of the CMZ, in addition to the three
previously known gaseous environments: (1) cold molecular clouds observed by
radio emission of CO and other molecules, (2) hot (T=10^4-10^6K) and highly
ionized diffuse gas (n_e=10-100cm^-3) seen in radio recombination lines, far
infrared atomic lines, and radio-wave scattering, and (3) ultra-hot
(T=10^7-10^8K) X-ray emitting plasma. Its prevalence significantly changes the
understanding of the environment of the CMZ. The sight line toward GC IRS 3 is
unique in showing an additional H3+ absorption component, which is interpreted
as due to either a cloud associated with circumnuclear disk or the "50 km s^-1
cloud" known from radio observations. An infrared pumping scheme is examined as
a mechanism to populate the (3,3) metastable level in this cloud.Comment: 15 pages, 5 figures, 4 tables Accepted for publication in the
Astrophysical Journa
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