[C ii] Properties and Far-infrared Variability of a z = 7 Blazar

Eduardo Bañados, Yana Khusanova, Roberto Decarli, Emmanuel Momjian, Fabian Walter, Thomas Connor, Christopher L. Carilli, Chiara Mazzucchelli, Sofía Rojas-Ruiz and Bram P. Venemans
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Abstract

We present millimeter observations of the host galaxy of the most distant blazar known, VLASS J041009.05−013919.88 (hereafter J0410–0139) at z = 7, using Atacama Large Millimeter/submillimeter Array (ALMA) and NOrthern Extended Millimeter Array (NOEMA) observations. The ALMA data reveal a (2.02 ± 0.36) × 1042 erg s−1 [C ii] 158 μm emission line at z = 6.9964 with a [C ii]-inferred star formation rate (SFR) of 58 ± 9 M⊙ yr−1. We estimate a dynamical mass of Mdyn,[C ii] = (4.6 ± 2.0) × 109M⊙, implying a black hole mass to host a dynamical mass ratio of . The 238 GHz continuum (rest-frame IR) decreased by ∼33% from the NOEMA to the ALMA observations taken ∼10 months apart. The Very Large Array 3–10 GHz radio flux densities showed a ∼37% decrease in a similar time frame, suggesting a causal connection. At face value, J0410–0139 would have the lowest [C ii]-to-IR luminosity ratio of a z > 5.7 quasar reported to date (∼10−4). However, if only <20% of the measured IR luminosity was due to thermal emission from dust, the [C ii]-to-IR luminosity ratio would be typical of (U)LIRGs, and the SFRs derived from [C ii] and IR luminosities would be consistent. These results provide further evidence that synchrotron emission significantly contributes to the observed rest-frame IR emission of J0410–0139, similar to what has been reported in some radio-loud active galactic nuclei at z < 1.
我们利用阿塔卡马大型毫米波/亚毫米波阵列(ALMA)和诺尔斯南部扩展毫米波阵列(NOEMA)的观测数据,对z = 7的已知最遥远的类星体VLASS J041009.05-013919.88(以下简称J0410-0139)的主星系进行了毫米波观测。ALMA数据显示,在z = 6.9964处有一条(2.02 ± 0.36) × 1042 erg s-1 [C ii] 158 μm发射线,[C ii]推断的恒星形成率(SFR)为58 ± 9 M⊙ yr-1。我们估计其动力学质量为 Mdyn,[C ii] = (4.6 ± 2.0) × 109M⊙,这意味着黑洞质量与所承载的动力学质量比为......。 从 NOEMA 到 ALMA 的观测结果相隔 10 个月,238 GHz 的连续波(静帧红外)减少了 ∼ 33%。超大阵列3-10 GHz射电通量密度在类似的时间范围内下降了37%,这表明两者之间存在因果关系。从表面上看,J0410-0139是迄今为止报道的z > 5.7类星体中[C ii]-红外发光比最低的(∼10-4)。然而,如果测得的红外发光度中只有小于20%是由尘埃的热辐射引起的,那么[C ii]-红外发光度比将是典型的(U)LIRG,而根据[C ii]和红外发光度得出的SFR也将是一致的。这些结果进一步证明,同步辐射对观测到的J0410-0139的静帧红外辐射有很大的贡献,这与一些z < 1的射电大声活星系核的情况类似。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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