ALMA deep field in SSA22: Blindly detected CO emitters and [C II] emitter candidates-猫眼课题宝

DOI：

10.1093/pasj/psx018

发表时间：

2017-02

期刊：

Publications of the Astronomical Society of Japan

影响因子：

2.3

通讯作者：

中科院分区：

物理与天体物理4区

文献类型：

作者：

N. H. Hayatsu;Y. Matsuda;H. Umehata;N. Yoshida;I. Smail;A. Swinbank;R. Ivison;K. Kohno;Y. Tamura;M. Kubo;D. Iono;B. Hatsukade;K. Nakanishi;R. Kawabe;T. Nagao;A. Inoue;T. Takeuchi;M. Lee;Y. Ao;S. Fujimoto;T. Izumi;Y. Yamaguchi;S. Ikarashi;T. Yamada

本文报道了利用阿塔卡马大毫/亚毫米阵列（阿尔马）在SSA 22视场（ADF 22）上对4个毫米线发射星系的识别。我们分析了阿尔马1.1毫米测量数据，有效测量面积为5弧分2，频率范围为253.1-256.8和269.1-272.8 GHz，角分辨率为0 "。.′′ 7和0.8 mJy波束−1在36 km s−1速度分辨率下的均方根噪声。我们检测到四个显着性水平高于6σ的线发射候选者。我们确定的四个源之一，作为CO（9-8）发射器在z = 3.1在该领域已知的原星系团的成员。具有光学对应物的另一个线发射体可能是z = 0.7的CO（4-3）发射体。没有任何毫米连续谱或光学/近红外对应物的其他两个源可能是z = 6.0和6.5的[C II]发射体候选者。[C II]候选者的等效宽度与已确认的高红移[C II]发射体和候选者的等效宽度一致，并且比在这次搜索中检测到的CO（9-8）发射体的等效宽度大10倍。候选者的[C Ⅱ]光度为4-7 × 108 L·cm ~（-1）。如果我们采用经验的[C II]光度-恒星形成率关系，这些源的星星形成率（SFR）估计为10-20 M yr−1。其中一个具有相对低的S/N比，但显示出发射线的特征。假设两个候选者中至少有一个是[C II]发射体，我们推导出z = 6时基于[C II]的星星形成率密度（SFRD）的下限。得到的数值>10−2 M yr−1 Mpc−3，与未修正的尘埃紫外线SFRD一致。未来的毫米波/亚毫米波巡天可以探测到大量的高红移线辐射源，从而研究早期宇宙中星星的形成历史。

We report the identification of four millimeter line-emitting galaxies with the Atacama Large Milli/submillimeter Array (ALMA) in SSA22 Field (ADF22). We analyze the ALMA 1.1-mm survey data, with an effective survey area of 5 arcmin2, frequency ranges of 253.1–256.8 and 269.1–272.8 GHz, angular resolution of 0 ′′. .′′ 7 and rms noise of 0.8 mJy beam−1 at 36 km s−1 velocity resolution. We detect four line-emitter candidates with significance levels above 6σ. We identify one of the four sources as a CO(9–8) emitter at z = 3.1 in a member of the proto-cluster known in this field. Another line emitter with an optical counterpart is likely a CO(4–3) emitter at z = 0.7. The other two sources without any millimeter continuum or optical/near-infrared counterpart are likely to be [C II] emitter candidates at z = 6.0 and 6.5. The equivalent widths of the [C II] candidates are consistent with those of confirmed high-redshift [C II] emitters and candidates, and are a factor of 10 times larger than that of the CO(9–8) emitter detected in this search. The [C II] luminosity of the candidates are 4–7 × 108 L⊙. The star formation rates (SFRs) of these sources are estimated to be 10–20 M⊙ yr−1 if we adopt an empirical [C II] luminosity–SFR relation. One of them has a relatively low S/N ratio, but shows features characteristic of emission lines. Assuming that at least one of the two candidates is a [C II] emitter, we derive a lower limit of [C II]-based star formation rate density (SFRD) at z ∼ 6. The resulting value of >10−2 M⊙ yr−1 Mpc−3 is consistent with the dust-uncorrected UV-based SFRD. Future millimeter/submillimeter surveys can be used to detect a number of high-redshift line emitters, with which to study the star formation history in the early universe.

ALMA deep field in SSA22: Blindly detected CO emitters and [C II] emitter candidates

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