Subaru Observations Of Warm And Diffuse Gas Near The Galactic Center Probed By Metastable H3+

Details Subaru Observations Of Warm And Diffuse Gas Near The Galactic Center Probed By Metastable H3+ Subaru Observations Of Warm And Diffuse Gas Near The Galactic Center Probed By Metastable H3+

Jul 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21012104o&link_type=abstract

American Astronomical Society Meeting 210, #121.04; Bulletin of the American Astronomical Society, Vol. 39, p.328

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Scientific paper

Our previous infrared observations of H3+ and CO toward the brightest quintuplet star GCS 3-2 has established presence of a vast amount of high temperature (T 250 K) and low density (n 100 cm-3) gas in the Central Molecular Zone (CMZ) of the Galaxy.a The observations have been extended to seven other young stars within 30 pc of the Galactic center (GC). All sightlines show high H3+ column densities of N(H3+) = (2.3 - 4.5) × 1015 cm-2 and temperatures of 220 K- 400 K and density 100 cm-3 demonstrating the ubiquity of the warm and diffuse gas in the CMZ.
The average value of the observed N(H3+) = 3.6 × 1015 cm-2 gives a product of the ionization rate ζ and pathlength L as ζL (2.5 - 8.4) × 1015 cm-2, where the large uncertainty reflects the uncertainty of the reduction of the H/C ratio near the GC compared to solar vicinity, by a factor of RX = 3 - 10 reported by COBE DIRBE. Separation of ζ and L is difficult but even if we use a high ζ value of 10-15 s-1, the estimated cloud dimension is L = 80 pc - 270 pc indicating a large volume filling factor of the warm and diffuse gas.
The newly found gas is thought to fill significant fraction of the space between dense clouds which has been mostly observed by radio CO emission spectra of molecules. The gas cannot coexist with the ultra-hot (T 107-8 K) gas emitting X-rays and the hot (T 106 K) and high density electron gas (ne 10 cm-3) causing hyper-strong radio-wave scattering. Their relation and the possible heating mechanism of the warm and diffuse gas will be discussed.

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