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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >ALMA deep field in SSA22: Blindly detected CO emitters and [C II] emitter candidates
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ALMA deep field in SSA22: Blindly detected CO emitters and [C II] emitter candidates

机译：SSA22中的Alma Deep Field：盲目地检测到CO发射器和[C II]发射器候选人

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摘要

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 arcmin(2), 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 kms(-1) velocity resolution. We detect four line-emitter candidates with significance levels above 6 sigma. 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 anymillimeter 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 x 10(8) L-circle dot. The star formation rates (SFRs) of these sources are estimated to be 10-20 M-circle dot 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 similar to 6. The resulting value of > 10(-2) M-circle dot 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.
机译：我们在SSA22场（ADF22）中举报了与Atacama大型毫米/亚颌骨阵列（ALMA）的四毫米线发射星系的识别。我们分析了Alma 1.1-MM测量数据，有效的调查面积为5 Accmin（2），频率范围为253.1-256.8和269.1-272.8 GHz，角度分辨率为0''7和RMS噪声为0.8米米的梁（ - 1）在36公里（-1）速度分辨率下。我们检测到四个线发射器候选者，其具有高于6 sigma的显着性水平。我们将四个源中的一个识别为CO（9-8）发射器，在该字段中已知的原始簇的成员中z = 3.1。具有光学对应物的另一个线发射器可能是Z = 0.7的CO（4-3）发射器。其他两个没有含有的连续或光/近红外对应物的来源可能是z = 6.0和6.5的发射器候选者。 [C II]候选者的等效宽度与确认的高射频[C II]发射器和候选者一致，并且比在该搜索中检测到的CO（9-8）发射器的倍数为10倍。候选物的[C II]亮度是4-7×10（8）升圆点。如果我们采用经验[C II]亮度-SFR关系，这些来源的星形成速率（SFR）估计为10-20 m圆点Yr（-1）。其中一个具有相对较低的S / N比，但显示了发射线的特征特征。假设两个候选者中的至少一个是发射器，我们在z类似于6的基于z的基于恒星形成速率密度（sfrd）的下限。结果> 10（ - 2）M圆点YR（-1）MPC（-3）与粉尘未校正的UV的SFRD一致。未来毫米/亚丘疹调查可用于检测许多高射频线发射器，其中研究早期宇宙中的星形形成历史。

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    Hayatsu Natsuki H.; Matsuda Yuichi; Umehata Hideki; Yoshida Naoki; Smail Ian; Swinbank A. Mark; Ivison Rob; Kohno Kotaro; Tamura Yoichi; Kubo Mariko; Iono Daisuke; Hatsukade Bunyo; Nakanishi Kouichiro; Kawabe Ryohei; Nagao Tohru; Inoue Akio K.; Takeuchi Tsutomu T.; Lee Minju; Ao Yiping; Fujimoto Seiji; Izumi Takuma; Yamaguchi Yuki; Ikarashi Soh; Yamada Toru;

  • 作者单位

    Univ Tokyo Dept Phys Bunkyo Ku 7-3-1 Hongo Tokyo 1130033 Japan;

    Natl Astron Observ Japan Osawa 2-21-1 Mitaka Tokyo 1818588 Japan;

    Open Univ Japan Mihama Ku 2-11 Wakaba Chiba 2618586 Japan;

    Univ Tokyo Dept Phys Bunkyo Ku 7-3-1 Hongo Tokyo 1130033 Japan;

    Univ Durham Dept Phys Ctr Extragalact Astron South Rd Durham DH1 3LE England;

    Univ Durham Dept Phys Ctr Extragalact Astron South Rd Durham DH1 3LE England;

    European Southern Observ Karl Schwarzschild Str 2 D-85748 Garching Germany;

    Univ Tokyo Sch Sci Inst Astron 2-21-1 Osawa Mitaka Tokyo 1810015 Japan;

    Univ Tokyo Sch Sci Inst Astron 2-21-1 Osawa Mitaka Tokyo 1810015 Japan;

    Natl Astron Observ Japan TMT Project Off 2-21-1 Osawa Mitaka Tokyo 1818588 Japan;

    Natl Astron Observ Japan Osawa 2-21-1 Mitaka Tokyo 1818588 Japan;

    Natl Astron Observ Japan Osawa 2-21-1 Mitaka Tokyo 1818588 Japan;

    Natl Astron Observ Japan Osawa 2-21-1 Mitaka Tokyo 1818588 Japan;

    Natl Astron Observ Japan Osawa 2-21-1 Mitaka Tokyo 1818588 Japan;

    Ehime Univ Res Ctr Space &

    Cosm Evolut 2-5 Bunkyo Cho Matsuyama Ehime 7908577 Japan;

    Osaka Sangyo Univ Coll Gen Educ 3-1-1 Nakagaito Daito Osaka 5748530 Japan;

    Nagoya Univ Div Particle &

    Astrophys Sci Chikusa Ku Furo Cho Nagoya Aichi 4648602 Japan;

    Natl Astron Observ Japan Osawa 2-21-1 Mitaka Tokyo 1818588 Japan;

    Natl Astron Observ Japan Osawa 2-21-1 Mitaka Tokyo 1818588 Japan;

    Univ Tokyo Grad Sch Sci Dept Astron Bunkyo Ku 7-3-1 Hongo Tokyo 1330033 Japan;

    Univ Tokyo Sch Sci Inst Astron 2-21-1 Osawa Mitaka Tokyo 1810015 Japan;

    Univ Tokyo Sch Sci Inst Astron 2-21-1 Osawa Mitaka Tokyo 1810015 Japan;

    Univ Groningen Kapteyn Astron Inst POB 800 NL-9700 AV Groningen Netherlands;

    Tohoku Univ Astron Inst Aoba Ku 6-3 Aoba Sendai Miyagi 9808578 Japan;

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  • 原文格式 PDF
  • 正文语种 eng
  • 中图分类 天文学;
  • 关键词

    early universe; galaxies: clusters: individual (SSA22); galaxies: formation;

    机译：早期宇宙;星系：群集：个人（SSA22）;星系：形成;

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