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Absorption Line Survey of H3+ toward the Galactic Center Sources I. GCS 3-2 and GC IRS3 | | M. Goto
; B. J. McCall
; T. R. Geballe
; T. Usuda
; N. Kobayashi
; H. Terada
; T. Oka
; | | Date: |
6 Dec 2002 | | Subject: | astro-ph | | Affiliation: | 1,2), B. J. McCall , T. R. Geballe , T. Usuda , N. Kobayashi , H. Terada , T. Oka ( Subaru Telescope, University of Hawaii, University of California, Berkeley, Gemini Observatory, University of Chicago | | Abstract: | We present high-resolution (R = 20000) spectroscopy of H3+ absorption toward the luminous Galactic center sources GCS 3-2 and GC IRS 3. With the efficient wavelength coverage afforded by Subaru IRCS, six absorption lines of H3+ have been detected in each source from 3.5 to 4.0 um, three of which are new. In particular the 3.543 um absorption line of the R(3, 3)^l transition arising from the metastable (J, K) = (3, 3) state has been tentatively detected for the first time in the interstellar medium, where previous observations of H3+ had been limited to absorption lines from the lowest levels: (J, K) = (1, 0) of ortho-H3+ and (1, 1) of para-H3+. The H3+ absorption toward the Galactic center takes place in dense and diffuse clouds along the line of sight as well as the molecular complex close to the Galactic nucleus. At least four kinematic components are found in the H3+ absorption lines. We suggest identifications of the velocity components with those of HI, CO, and H2CO previously reported from radio and infrared observations. H3+ components with velocities that match those of weak and sharp CO and H2CO lines are attributed to diffuse clouds. Our observation has revealed a striking difference between the absorption profiles of H3+ and CO, demonstrating that the spectroscopy of H3+ provides information complementary to that obtained from CO spectroscopy. The tentative detection of the R(3, 3)^l line and the non-detection of spectral lines from other J > 1 levels provide observational evidence for the metastability of the (3, 3) level, which is theoretically expected. This suggests that other metastable J = K levels with higher J may also be populated. | | Source: | arXiv, astro-ph/0212159 | | Services: | Forum | Review | PDF | Favorites | |
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