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ALMA-QUARKS View of W49N: Multipolar Episodic Outflow Associated with the Most Energetic Galactic Water Maser

  • Authors: Yunfan Jiao, Tie Liu, Wenyu Jiao, Fengwei Xu, Qilao Gu, Xindi Tang, Xiaofeng Mai, Qiuyi Luo, Siju Zhang, Paul F. Goldsmith, Chang Won Lee, Guido Garay, Yuhan Yang, Prasanta Gorai, Manuel Merello, Pablo García, Sami Dib, Jihye Hwang, Ariful Hoque, Mika Juvela, Yankun Zhang, Patricio Sanhueza, Jixiang Weng, Kee-Tae Kim, Swagat R. Das, Archana Soam, Tapas Baug, Jianjun Zhou, Leonardo Bronfman, Aiyuan Yang, Lei Zhu

Yunfan Jiao et al 2026 The Astronomical Journal 172 .

  • Provider: AAS Journals

Caption: Figure 3.

Left: PV diagrams of 12CO emission. The PV cuts of panels (a), (b), and (c) are along the connection of the two curved arrows “Bn” and “Bse”, the curved arrow “Bsw” in Figure 1 panel (a), and “Rs” in Figure 2 panel (a), respectively. Low velocity (less than ∼10 km s−1 relative to the systemic velocity) parts are chopped out. The black dashed vertical lines indicate the position of source G2a. The smoothed contours in blue and red indicate 10 times the rms value of the PV diagram background. The colored dots on the smoothed contour denote the knots in four different newly found outflow lobes, which can be distinctly recognized by eye with the assistance of the gray-dotted integrated intensity curve. The intensity of the curve in panel (c) is integrated from the velocity channels higher than 40 km s−1 only to avoid contamination. Right: dynamical timescale for each knot without inclination angle correction. The x-axis represents distance between each knot and the source.

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