phangs-jwst首先结果：跨NGC 628的反馈驱动气泡（幻影空隙）的多波长视图

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phangs-jwst首先结果：跨NGC 628的反馈驱动气泡（幻影空隙）的多波长视图

PHANGS-JWST First Results: Multi-wavelength view of feedback-driven bubbles (The Phantom Voids) across NGC 628

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Barnes, Ashley T., Watkins, Elizabeth J., Meidt, Sharon E., Kreckel, Kathryn, Sormani, Mattia C., Tress, Robin G., Glover, Simon C. O., Bigiel, Frank, Chandar, Rupali, Emsellem, Eric, Lee, Janice C., Leroy, Adam K., Sandstrom, Karin M., Schinnerer, Eva, Rosolowsky, Erik W., Belfiore, Francesco, Blanc, Guillermo, Boquien, Mederic, Brok, Jakob S. den, Cao, Yixian, Chevance, Mélanie, Dale, Daniel A., Egorov, Oleg, Eibensteiner, Cosima, Grasha, Kathryn, Groves, Brent, Hassani, Hamid, Henshaw, Jonathan, Jeffreson, Sarah, Jimenez-Donaire, Maria Jesus, Keller, Benjamin W., Klessen, Ralf S., Koch, Eric W., Kruijssen, J. M. Diederik, Larson, Kirsten L., Li, Jing, Liu, Daizhong, Lopez, Laura A., Murphy, Eric J., Neumann, Lukas, Pety, Jerome, Pinna, Francesca, Querejeta, Miguel, Renaud, Florent, Saito, Toshiki, Sarbadhicary, Sumit, Sardone, Amy, Smith, Rowan J., Stuber, Sophia K., Sun, Jiayi, Thilker, David A., Usero, Antonio, Whitmore, Bradley C., Williams, Thomas G.

论文摘要

我们提供了幻影星系内气泡的高分辨率视图（NGC 628）；附近的（〜10mpc），星形（〜2mmun/yr），面对面（I〜9DEG）大设计的螺旋星系。通过作为Phangs-JWST国库计划的一部分获得的新数据，我们对两个感兴趣的区域进行了详细的案例研究，其中一个包含星系中最大，最突出的气泡（幻影效果；直径超过1KPC），另一个是较小的区域，可能是一个大型Bubble（Corporsor aise over Bubble）（versor）的ph phantom（v）。与来自哈勃太空望远镜（HST）的匹配的分辨率HALPHA观测值相比，我们看到两个气泡的壳中的电离气体是最亮的，并且与最年轻的（〜1myr）和最大的（〜100,000msun）的恒星关联是一致的。我们还发现，幻影空隙的气泡中存在着老一代（〜20myr）。从我们对幻影空隙的HI，H2（CO）和HII气体的运动学分析中，我们推断出高约15至50km/s的高膨胀速度。幻影空隙的较大尺寸和高膨胀速度表明，由于多种机制，驾驶机制是持续的恒星反馈，在这种机制中，早期的反馈首先清除了气泡（正如我们现在在前体幻影空隙中观察到的那样），从那时起，SNE就在腔内爆炸了，并加速了壳。 Finally, comparison to simulations shows a striking resemblance to our JWST observations, and suggests that such large-scale stellar feedback-driven bubbles should be common within other galaxies.

We present a high-resolution view of bubbles within The Phantom Galaxy (NGC 628); a nearby (~10Mpc), star-forming (~2Msun/yr), face-on (i~9deg) grand-design spiral galaxy. With new data obtained as part of the PHANGS-JWST treasury program, we perform a detailed case-study of two regions of interest, one of which contains the largest and most prominent bubble in the galaxy (The Phantom Void; over 1kpc in diameter), and the other being a smaller region that may be the precursor to such a large bubble (The Precursor Phantom Void). When comparing to matched resolution Halpha observations from the Hubble Space Telescope (HST), we see that the ionized gas is brightest in the shells of both bubbles, and is coincident with the youngest (~1Myr) and most massive (~100,000Msun) stellar associations. We also find an older generation (~20Myr) of stellar associations is present within the bubble of The Phantom Void. From our kinematic analysis of the HI, H2 (CO) and HII gas across The Phantom Void, we infer a high expansion speed of around 15 to 50km/s. The large size and high expansion speed of The Phantom Void suggest that the driving mechanism is sustained stellar feedback due to multiple mechanisms, where early feedback first cleared a bubble (as we observe now in The Precursor Phantom Void), and since then SNe have been exploding within the cavity, and have accelerated the shell. Finally, comparison to simulations shows a striking resemblance to our JWST observations, and suggests that such large-scale stellar feedback-driven bubbles should be common within other galaxies.

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