What Controls the Star Formation in Luminous Starburst Mergers?
What Controls the Star Formation in Luminous Starburst Mergers?
复制标题
是什么控制着发光星暴合并中恒星的形成？
DOI：
10.1086/311779
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发表时间：
1998
期刊：
影响因子：
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通讯作者：
Y. Ohyama
中科院分区：
文献类型：
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作者：
Y. Taniguchi;Y. Ohyama
为了了解是什么控制了发光星暴合并中的星星形成过程（例如，NGC 6240，阿普220，等等），我们分别使用欧文斯谷射电天文台（Scoville et al.）和IRAM干涉仪（Downes &所罗门）。我们发现，远红外发光度的表面密度（FIR）与两个样品的H2表面质量密度（H2）成线性比例; FIR的表面质量密度（H2）为1.01 ± 0.06，相关系数为0.96。通常认为，单位面积的星星形成率（SFR）可以很好地度量。我们还知道，在明亮的星暴合并中，分子气体主要存在于核周区域;即，氢气（H2）。因此，上述关系表明了一个星星形成规律：SFR（气体）。我们认为，这种星星形成规律有利于引力不稳定的情况下，而不是云-云碰撞之一。
In order to understand what controls the star formation process in luminous starburst mergers (e.g., NGC 6240, Arp 220, and so on), we investigate observational properties of two samples of high-luminosity starburst galaxies mapped in CO J=1-0 independently using both the Owens Valley Radio Observatory (Scoville et al.) and the IRAM interferometer (Downes & Solomon). We find that the surface density of far-infrared luminosity, Σ(FIR), is proportional linearly to the H2 surface mass density, Σ(H2), for the two samples; Σ(FIR)∝Σ(H2)1.01 ± 0.06 with a correlation coefficient of 0.96. It is often considered that Σ(FIR) provides a good measure of the star formation rate per unit area, Σ(SFR). It is also known that molecular gas is dominated in circumnuclear regions in the luminous starburst mergers; i.e., Σ(gas)≃Σ(H2). Therefore, the above relationship suggests a star formation law; Σ(SFR)∝Σ(gas). We suggest that this star formation law favors the gravitational instability scenario rather than the cloud-cloud collision one.