Antarctic Submillimeter Telescope and Remote Observatory Observations of12CO \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10}{9}{7}{6} \begin{document} \landscape $J=4arrow 3$ \end{document} Emission from the N44 Complex in the Large Magellanic Cloud

Abstract

We present Antarctic Submillimeter Telescope and Remote Observatory (AST/RO) observations of 12CO J = 4 → 3 and [C I] emission in the N44 H II complex in the Large Magellanic Cloud. We detected strong 12CO J = 4 → 3 emission toward the H II region known as N44BC, which is located on the rim of an expanding giant shell in the N44 region. Analysis with a photodissociation region model showed that the 12CO J = 4 → 3 emitting cloud is very dense, with n0 ≈ 105 cm-3. We also note that there is a high-velocity component associated with the 12CO J = 4 → 3 emission. This probably originates from molecular material accelerated as a result of the motion induced by the expanding giant shell surrounding LH 47 in the N44 complex. We found that the kinetic energy of this high-velocity gas observed in the 12CO J = 4 → 3 emission toward the rim of the expanding H II shell is at least a factor of 4 higher than that derived for the H I and H II gas in this region.