CO Observations of the Host Galaxy of GRB000418 at Z=1.1
CO Observations of the Host Galaxy of GRB000418 at Z=1.1
复制标题
GRB000418 宿主星系 Z=1.1 处的 CO 观测
DOI：
10.1088/0004-637x/748/2/108
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发表时间：
2011
影响因子：
4.9
通讯作者：
et al
中科院分区：
文献类型：
--
作者：
Hatsukade;B.;et al
我们提出的结果，16厘米波段连续观测的四个宿主星系的伽玛射线暴（GRB）990705，021211，041006，和051022使用澳大利亚望远镜紧凑阵列。在任何一个宿主星系中都没有发现射电辐射。由主星系的射电观测得出的星星形成速率的2σ上限分别为23、45、27和26百万年− 1，这还不到由紫外/光学观测得出的结果的10倍，表明它们没有明显的尘埃遮蔽的星星形成。伽玛暴021211和051022被称为所谓的暗伽玛暴，我们的结果意味着暗伽玛暴并不总是发生在被尘埃笼罩的星系中。由于在GRB 021211的余辉中没有观察到大的尘埃消光，我们的结果表明暗GRB的原因可能是光学余辉的内在模糊。另一方面，考虑到在GRB 051022的余辉中观察到的高柱密度，暗GRB的可能原因是GRB视线中的尘埃消光。
We present the results of the 16 cm wave band continuum observations of four host galaxies of gamma-ray bursts (GRBs) 990705, 021211, 041006, and 051022 using the Australia Telescope Compact Array. Radio emission was not detected in any of the host galaxies. The 2σ upper limits on star formation rates derived from the radio observations of the host galaxies are 23, 45, 27, and 26 M☉ yr− 1, respectively, which are less than about 10 times those derived from UV/optical observations, suggesting that they have no significant dust-obscured star formation. GRBs 021211 and 051022 are known as the so-called dark GRBs and our results imply that dark GRBs do not always occur in galaxies enshrouded by dust. Because large dust extinction was not observed in the afterglow of GRB 021211, our result suggests the possibility that the cause of the dark GRB is the intrinsic faintness of the optical afterglow. On the other hand, by considering the high column density observed in the afterglow of GRB 051022, the likely cause of the dark GRB is the dust extinction in the line of sight of the GRB.