@article{oai:soar-ir.repo.nii.ac.jp:00015871,
 author = {Jones,  Therese M. and Misawa,  Toru and Charlton,  Jane C. and Mshar,  Andrew C. and Ferland,  Gary J.},
 issue = {2},
 journal = {The Astrophysical Journal},
 month = {Jun},
 note = {Several neutral species (Mg I, Si I, Ca I, Fe I) have been detected in a weak Mg II absorption line system (W-r (2796) similar to 0.15 angstrom) at z similar to 0.45 along the sightline toward HE0001-2340. These observations require extreme physical conditions, as noted in D'Odorico. We place further constraints on the properties of this system by running a wide grid of photoionization models, determining that the absorbing cloud that produces the neutral absorption is extremely dense (similar to 100-1000 cm(-3)), cold (<100 K), and has significant molecular content (similar to 72%-94%). Structures of this size and temperature have been detected in Milky Way CO surveys and have been predicted in hydrodynamic simulations of turbulent gas. In order to explain the observed line profiles in all neutral and singly ionized chemical transitions, the lines must suffer from unresolved saturation and/or the absorber must partially cover the broad emission line region of the background quasar. In addition to this highly unusual cloud, three other ordinary weak Mg II clouds (within densities of similar to 0.005 cm(-3) and temperatures of similar to 10,000 K) lie within 500 km s(-1) along the same sightline. We suggest that the "bare molecular cloud," which appears to reside outside of a galaxy disk, may have had in situ star formation and may evolve into an ordinary weak Mg II absorbing cloud., The Astrophysical Journal. 715(2):1497-1507 (2010)},
 pages = {1497--1507},
 title = {A BARE MOLECULAR CLOUD AT z similar to 0.45},
 volume = {715},
 year = {2010}
}