FINE-SCALE STRUCTURE OF THE QUASAR 3C 279 MEASURED WITH 1.3 mm VERY LONG BASELINE INTERFEROMETRY-猫眼课题宝

DOI：

10.1088/0004-637x/772/1/13

发表时间：

2013-05

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：

R. Lu;V. Fish;K. Akiyama;S. Doeleman;J. Algaba;G. Bower;C. Brinkerink;R. Chamberlin;G. Crew;R. Cappallo;M. Dexter;R. Freund;P. Friberg;M. Gurwell;P. Ho;M. Honma;M. Inoue;S. Jorstad;T. Krichbaum;L. Loinard;D. MacMahon;D. Marrone;A. Marscher;J. Moran;R. Plambeck;N. Pradel;R. Primiani;R. Tilanus;M. Titus;J. Weintroub;M. Wright;K. Young;L. Ziurys

我们报告了2011年在1.3毫米(230 GHz)对著名的类星体3C279进行的长达5天的基线干涉观测结果。在包括亚利桑那州、加利福尼亚州和夏威夷的台站在内的三角形上测量的非零闭合相位表明，震源结构是空间分辨的。我们在∼-1PC尺度上发现了一个异常的内喷流方向，沿着西北-东南方向延伸(P.A.=127°±3°)，而以前报道的一些尺度上的测量结果显示内喷流方向向西南延伸。1.3 mm的结构与在7 mm的准同步超分辨率甚长基线阵列图像的中心区域观察到的结构密切相关。与其他观测相比，最后一天的闭合位相发生了显著变化，表明内部急流结构在日时间尺度上可能是不同的。观测到的内喷流新方向与一类喷流进动模型的预测结果不一致。我们的观测表明，1.3mm芯的亮温为∼8×1010K，远低于厘米波长的亮温。在未来几年，具有更好的紫外线覆盖率和灵敏度的观测将允许区分不同的结构模型，并将提供20-30μAS(5-7光月)分辨率的喷流内部区域的直接图像。

We report results from five day very long baseline interferometry observations of the well-known quasar 3C 279 at 1.3 mm (230 GHz) in 2011. The measured nonzero closure phases on triangles including stations in Arizona, California, and Hawaii indicate that the source structure is spatially resolved. We find an unusual inner jet direction at scales of ∼1 pc extending along the northwest–southeast direction (P.A. = 127° ± 3°), as opposed to other (previously) reported measurements on scales of a few parsecs showing inner jet direction extending to the southwest. The 1.3 mm structure corresponds closely with that observed in the central region of quasi-simultaneous super-resolution Very Long Baseline Array images at 7 mm. The closure phase changed significantly on the last day when compared with the rest of observations, indicating that the inner jet structure may be variable on daily timescales. The observed new direction of the inner jet shows inconsistency with the prediction of a class of jet precession models. Our observations indicate a brightness temperature of ∼8 × 1010 K in the 1.3 mm core, much lower than that at centimeter wavelengths. Observations with better uv coverage and sensitivity in the coming years will allow the discrimination between different structure models and will provide direct images of the inner regions of the jet with 20–30 μas (5–7 light months) resolution.

FINE-SCALE STRUCTURE OF THE QUASAR 3C 279 MEASURED WITH 1.3 mm VERY LONG BASELINE INTERFEROMETRY

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