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Band-9 ALMA Observations of the N II 122 μm Line and FIR Continuum in Two High-z Galaxies

机译：两个高z星系中N II 122μm谱线和FIR连续谱的Band-9 ALMA观测

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摘要

We present Atacama Large Millimeter Array (ALMA) observations of two high-redshift systems (SMMJ02399-0136 at z_1 ~ 2.8 and the Cloverleaf QSO at z_1 ~ 2.5) in their rest-frame 122 μm continuum (νsky ~ 650 GHz, λsky ~ 450 μm) and [N ii] 122 μm line emission. The continuum observations with a synthesized beam of ~0."25 resolve both sources and recover the expected flux. The Cloverleaf is resolved into a partial Einstein ring, while SMMJ02399-0136 is unambiguously separated into two components: a point source associated with an active galactic nucleus and an extended region at the location of a previously identified dusty starburst. We detect the [N ii] line in both systems, though significantly weaker than our previous detections made with the first generation z (Redshift) and Early Universe Spectrometer. We show that this discrepancy is mostly explained if the line flux is resolved out due to significantly more extended emission and longer ALMA baselines than expected. Based on the ALMA observations we determine that ≥75% of the total [N ii] line flux in each source is produced via star formation. We use the [N ii] line flux that is recovered by ALMA to constrain the N/H abundance, ionized gas mass, hydrogen- ionizing photon rate, and star formation rate. In SMMJ02399-0136 we discover it contains a significant amount (~1000 M_⊙ yr^(−1)) of unobscured star formation in addition to its dusty starburst and argue that SMMJ02399-0136 may be similar to the Antennae Galaxies (Arp 244) locally. In total these observations provide a new look at two well-studied systems while demonstrating the power and challenges of Band-9 ALMA observations of high-z systems.
机译：我们在其静止帧122μm连续体（νsky〜650 GHz，λsky〜450）中展示了两个高红移系统（z_1〜2.8处的SMMJ02399-0136和z_1〜2.5处的苜蓿叶形QSO）的Atacama大毫米波阵列（ALMA）观测结果。 [n ii] 122μm的线发射。用〜0。“ 25的合成光束进行的连续观测可解析两个源并恢复预期的通量。苜蓿叶形立叶解析为部分爱因斯坦环，而SMMJ02399-0136则明确地分为两个部分：与有源点相关的点源星系核和先前发现的尘埃爆发的位置的一个扩展区域，我们在两个系统中都检测到了[N ii]线，尽管比我们使用第一代z（Redshift）和早期宇宙光谱仪进行的检测要弱得多。结果表明，这种差异主要是由于延长了发射时间和更长的ALMA基线比预期消除了线通量所导致的，根据ALMA的观察，我们确定每个源中总[N ii]线通量的≥75％是通过恒星形成而产生的，我们使用ALMA回收的[N ii]线通量来约束N / H丰度，电离气体质量，氢电离光子速率和恒星形成率。在SMMJ02399-0136中，我们发现它除了尘土飞扬的星尘外，还包含大量（〜1000M_⊙yr ^（-1））隐蔽的恒星形成，并指出SMMJ02399-0136可能类似于天线星系（Arp 244）本地。总体而言，这些观测结果为两个经过充分研究的系统提供了新的视角，同时展示了高z系统的Band-9 ALMA观测结果的功能和挑战。

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