Intergalactic cold dust in the NGC 4631 group.
Intergalactic cold dust in the NGC 4631 group.
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NGC 4631 群中的星系间冷尘埃。
DOI：
10.1073/pnas.96.10.5360
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发表时间：
1999
影响因子：
11.1
通讯作者：
M. Dumke
中科院分区：
文献类型：
--
作者：
N. Neininger;M. Dumke
我们已经探测到了距离超过10千秒差距的面外冷尘埃，位于相互作用星系NGC 4631的晕中。尘埃排放盘比翘曲的HI盘薄得多，并且出现了新的结构。特别是，已经发现了一个巨大的弧，它与原子气体运动学结构的异常有关。大多数的面外尘埃与早先发现的HI毛刺密切相关[Weliachew，L.，桑西西河& Guelin，M. 03 The Dog of the Woman（1978）65，37-45;兰德，R. J.（1994）Astron. Astrophys. 285，833-856]。这些毛刺显然是相互作用的痕迹[Combes，F。03 The Dog of the Woman（1978）65，47-55]。平面内的灰尘排放到达光盘的边界。NGC 4631的盘的活动被相互作用适度地增强，但是没有发现在z方向上移动的气体[兰德，R. J.，库尔卡尼山R. & Hester，J. J.（1992）Astrophys. J.396，97-103; Golla，G.，德特马尔河- J. & Domgorgen，H. 03 The Dog（1996）313，439-447]。因此，强风似乎不太可能沉积高z尘埃。相反，与HI特征的巧合表明我们看到了相互作用留下的痕迹。此外，HI显示了由撞击形成的超壳层[兰德，R. J. & Stone，J. M.（1996）Astron. J. 111，190-196]在尘埃轨迹穿过圆盘的区域。该区域的特征还在于Halpha光分布的扰动。尘埃的质量只能根据现有的数据进行粗略的估计，它们大约是气体圈中几个10（9）M的中点。
We have detected extraplanar cold dust at distances out to >10 kiloparsecs, situated in the halo of the interacting galaxy NGC 4631. The dust emission disk is much thinner than the warped HI disk, and new structures emerge. In particular, a giant arc has been found that is linked to anomalies in the kinematical structure of the atomic gas. Most of the extraplanar dust is closely associated with HI spurs that have been found earlier [Weliachew, L., Sancisi, R. & Guelin, M. (1978) Astron. Astrophys. 65, 37-45; Rand, R. J. (1994) Astron. Astrophys. 285, 833-856]. These spurs obviously are traces of the interaction [Combes, F. (1978) Astron. Astrophys. 65, 47-55]. The dust emission within the plane reaches the border of the optical disk. The activity of the disk of NGC 4631 is moderately enhanced by the interaction, but no gas moving in the z-direction could be found [Rand, R. J., Kulkarni, S. R. & Hester, J. J. (1992) Astrophys. J. 396, 97-103; Golla, G., Dettmar, R.-J. & Domgorgen, H. (1996) Astron. Astrophys. 313, 439-447]. Hence, it seems unlikely that strong winds have deposited the high-z dust. Instead, the coincidence with the HI features suggests that we see a track left behind by the interaction. In addition, the HI shows a supershell formed by an impact [Rand, R. J. & Stone, J. M. (1996) Astron. J. 111, 190-196] in the zone where the dust trail crosses the disk. This region is also characterized by disturbances in the distribution of the Halpha light. The masses associated with the dust can be estimated only very roughly on the basis of the existing data; they are of the order of a few 10(9) M middle dot in circle of gas.