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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >ALMA band 8 observations of DLA 2233+131 at z=3.150
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ALMA band 8 observations of DLA 2233+131 at z=3.150

机译：ALMA带8在Z = 3.150处观察2233 + 131

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We present our ALMA Band 8 observations of a damped Lya absorption (DLA) system at z= 3.150 observed in the spectrum of the quasar Q2233+131 at z= 3.295. The optical counterpart of this DLA has been identified and it shows a double-peaked Lya emission line. Since one possible origin of DLAs at high redshift is an outflowing gas from starforming galaxies, DLA 2233+131 provides a good laboratory to investigate the nature of high-z DLAs. Motivated by this, we have carried out ALMA band 8 observations to study the [C-II] line in this system. However, we do not detect any significant emission line in the observed pass bands. Instead, we have serendipitously found three submm continuum sources in the observed sky area. One appears to be the quasar Q2233+131 itself while the other two sources are newly identified submm galaxies (SMGs), called SMG1 and SMG2 in this paper. They are located at a separation of 4 '' 7 and 8 '' 1 from Q2233+131, respectively. Their 646 mu m fluxes are 6.35 mJy and 6.43 mJy, respectively, being higher than that of Q2233+131, 3.62 mJy. Since these two SMGs are not detected in the optical images obtained with the Hubble Space Telescope and the Subaru Telescope, they have a very red spectral energy distribution. It is, therefore, suggested that they are high-redshift galaxies or very dusty galaxies at intermediate redshift, although we cannot rule out the possibility that they are optically very faint SMG analogs at low redshift. Follow-up observations will be necessary to explore the nature of this interesting region.
机译：我们在Z = 3.295的Z = 3.295的谱中观察到的Z = 3.150的Z = 3.150的阻尼Lya吸收（DLA）系统的Alma带8观察。已经识别了该DLA的光学对应物，并显示了双峰值的Lya排放线。由于高射频的DLA一起可能起源是来自恒星星系的流出气体，因此DLA 2233 + 131提供了良好的实验室来研究高Z DLA的性质。由此激励，我们已经开展了Alma Band 8观察，以研究该系统中的[C-II]线。但是，我们在观察到的通带中没有检测到任何重要的排放线。相反，我们在观察到的天空地区终于发现了三个提交的连续源。一个似乎是标准Q2233 + 131本身，而另一个两个来源是新识别的子造工组星系（SMG），称为SMG1和SMG2。它们位于Q2233 + 131的4''7和8'1的分离处。他们的646亩M次助焊剂分别为6.35米米，分别为6.43米，高于Q2233 + 131,3.62 MJY。由于在用哈勃空间望远镜和底座望远镜获得的光学图像中未检测到这两个SMG，因此它们具有非常红的光谱能量分布。因此，它表明它们是中间红移的高射频星系或非常尘土飞扬的星系，尽管我们不能排除它们在低射频处是光学非常微弱的SMG类似物的可能性。有必要进行后续观察来探索这个有趣区域的性质。

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