The H_2/CO ratio in the Large Magellanic Cloud

Details The H_2/CO ratio in the Large Magellanic Cloud The H_2/CO ratio in the Large Magellanic Cloud

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8320b&link_type=abstract

HST Proposal ID #8320

Physics

Hst Proposal Id #8320 Interstellar And Intergalactic Matter

Scientific paper

Little is known about real abundance ratios of the two most abundant molecules H_2 and CO in the interstellar matter of the Large Magellanic Cloud. Because of their abundance, both molecules play a crucial role in the physics of molecular gas. The only possibility to observe the homoeopolar molecule H_2 in its cool phase is the measurement of its far UV resonance lines with absorption spectroscopy. So far, of 4 observed lines of sight to the LMC, only the one to LH 10:3120 showed a significant amount of the H_2 molecule at LMC velocities. The CO molecule also has resonance lines in the far UV, but due to its much smaller amount and the relatively poor signal to noise ratio in the ORFEUS spectrum of LH 10:3120, the presence of CO could not be established from those measurements. With its high resolution spectrograph {STIS}, the Hubble Space Telescope provides the possibility to measure several strong CO absorption bands near 1500 Angstrom due to the LMC gas. We propose to observe LH 10:3120 and make the direct determination of the H_2/CO ratio for the LMC possible for the very first time.

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