MULTI-WAVELENGTH LENS RECONSTRUCTION OF A PLANCK AND HERSCHEL-DETECTED STAR-BURSTING GALAXY-猫眼课题宝

DOI：

10.3847/0004-637x/829/1/21

发表时间：

2015-12

期刊：

The Astrophysical Journal

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

N. Timmons;A. Cooray;D. Riechers;H. Nayyeri;H. Fu;E. Jullo;M. Gladders;M. Baes;R. Bussmann;J. Calanog;D. Clements;E. D. Cunha;S. Dye;S. Eales;C. Furlanetto;J. González-Nuevo;J. Greenslade;M. Gurwell;H. Messias;M. Michałowski;I. Oteo;I. P'erez-Fournon;D. Scott;E. Valiante

我们提出了一个源平面重建的赫歇尔和普朗克探测引力透镜尘埃恒星形成星系（DSFG）在z = 1.68使用哈勃，亚毫米阵列（SMA），和凯克观测。背景亚毫米星系（SMG）被z = 0.997的前景星系团强烈透镜化，在光学图像中呈现为一个长度为1.15 ″的弧形。连续尘埃排放，如SMA所见，仅限于此弧内的单个结。我们提出了一个透镜模型与源平面重建在几个波长的恒星和尘埃之间的放大率的差异，并强调多波长透镜模型的重要性，涉及透镜DSFG的研究。我们通过拟合通量密度来估计星系的物理性质，以模拟光谱能量分布，导致放大率校正的恒星形成率（SFR）为390 ± 60 M yr−1，恒星质量为。这些值与已经形成大部分恒星的高红移大质量星系一致。估计的气体-重子比例、分子气体面密度和SFR面密度分别为0.43 ± 0.13、350 ± 200 pc−2和M yr−1 kpc−2。SFR表面密度与分子气体表面密度之比使其成为最具恒星形成的系统之一，类似于其他测量到的SMG和本地ULIRG。

We present a source-plane reconstruction of a Herschel and Planck-detected gravitationally lensed dusty star-forming galaxy (DSFG) at z = 1.68 using Hubble, Submillimeter Array (SMA), and Keck observations. The background submillimeter galaxy (SMG) is strongly lensed by a foreground galaxy cluster at z = 0.997 and appears as an arc with a length of ∼15″ in the optical images. The continuum dust emission, as seen by SMA, is limited to a single knot within this arc. We present a lens model with source-plane reconstructions at several wavelengths to show the difference in magnification between the stars and dust, and highlight the importance of multi-wavelength lens models for studies involving lensed DSFGs. We estimate the physical properties of the galaxy by fitting the flux densities to model spectral energy distributions leading to a magnification-corrected star-formation rate (SFR) of 390 ± 60 M yr−1 and a stellar mass of . These values are consistent with high-redshift massive galaxies that have formed most of their stars already. The estimated gas-to-baryon fraction, molecular gas surface density, and SFR surface density have values of 0.43 ± 0.13, 350 ± 200 pc−2, and M yr−1 kpc−2, respectively. The ratio of SFR surface density to molecular gas surface density puts this among the most star-forming systems, similar to other measured SMGs and local ULIRGs.

MULTI-WAVELENGTH LENS RECONSTRUCTION OF A PLANCK AND HERSCHEL-DETECTED STAR-BURSTING GALAXY

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