Atacama Large Millimeter Array (ALMA) observations of CO(1-0) emission in the interacting galaxies IC 2163 and NGC 2207 are used to determine the properties of molecular clouds and their association with star-forming regions observed with the Hubble Space Telescope. Half of the CO mass is in 249 clouds, each more massive than . The mass distribution functions for the CO clouds and star complexes in a galactic-scale shock front in IC 2163 both have a slope on a log–log plot of ?0.7, similar to what is observed in Milky Way clouds. The molecular cloud mass function is steeper in NGC 2207. The CO distribution in NGC 2207 also includes a nuclear ring, a mini-bar, and a mini-starburst region that dominates the , radio, and Hα emission in both galaxies. The ratio of the sum of the masses of star complexes younger than 30 Myr to the associated molecular cloud masses is ~4%. The maximum age of star complexes in the galactic-scale shock front in IC 2163 is about 200 Myr, the same as the interaction time of the two galaxies, suggesting the destruction of older complexes in the eyelids.
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机译：阿塔卡马相互作用毫米星系IC 2163和NGC 2207中的CO（1-0）发射的大毫米波阵列（ALMA）观测值用于确定分子云的性质以及它们与哈勃太空望远镜观测到的恒星形成区域的关联。一氧化碳质量的一半位于249个云中，每个云的质量均大于。 IC 2163中银河级激波锋中CO云和恒星复合体的质量分布函数在对数-对数图上的斜率均为0.7，类似于银河系云中所观察到的。在NGC 2207中，分子云的质量函数更加陡峭。在NGC 2207中，CO分布还包括一个核环，一个迷你条和一个迷你星暴区域，该区域主导着两个星系中的，放射和Hα发射。小于30 Myr的恒星复合物的质量总和与相关分子云质量的比率为〜4％。 IC 2163的银河系规模激波锋中恒星复合物的最大年龄约为200 Myr，与两个星系的相互作用时间相同，这表明双眼皮中较老的复合物被破坏了。
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