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arXiv 2409.06100astro-ph.GA
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使用 $\textit{JWST}$ CEERS 数据研究 $z \sim$ 4 处棒状星系的丰度与性质

The Abundance and Properties of Barred Galaxies out to $z \sim$ 4 Using $\textit{JWST}$ CEERS Data

Yuchen Guo, Shardha Jogee, Eden Wise, Keith Pritchett, Elizabeth J. McGrath, Steven L. Finkelstein, Kartheik G. Iyer, Pablo Arrabal Haro, Micaela B. Bagley, Mar… 展开作者

Yuchen Guo, Shardha Jogee, Eden Wise, Keith Pritchett, Elizabeth J. McGrath, Steven L. Finkelstein, Kartheik G. Iyer, Pablo Arrabal Haro, Micaela B. Bagley, Mark Dickinson, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, L. Y. Aaron Yung, Bren E. Backhaus, Eric F. Bell, Rachana Bhatawdekar, Yingjie Cheng, Luca Costantin, Alexander de la Vega, Mauro Giavalisco, Nimish P. Hathi, Benne W. Holwerda, Peter Kurczynski, Ray A. Lucas, Bahram Mobasher, Pablo G. Pérez-González, Fabio Pacucci

备注：
25 pages, 16 figures, Accepted for publication in ApJ
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AI总结：

利用JWST CEERS数据首次估算z~4处棒状星系比例，发现z~2-4大棒比例低（<10%），棒在z~4已出现，且随红移降低棒比例、长度和强度增加。

摘要：

我们利用 $\textit{JWST}$ CEERS NIRCam 图像，首次估算了 $z\sim4$ 处棒状星系的观测比例及其性质。我们分析了 $0.5 \leq z \leq 4$ 范围内 1770 个 $M_\star > 10^{10} M_\odot$ 的星系，并通过椭圆拟合以及对 F200W 和 F444W 图像的视觉分类，从 839 个中等倾斜盘状星系中识别出棒状星系。我们的结果主要适用于投影半长轴 $a_{\rm bar}$ $> 1.5$ kpc（约为 F200W 图像中 PSF 的 2 倍）的棒，这些棒可以通过椭圆拟合被稳健地追踪。对于此类棒，$z\sim$ 2-4 处的观测棒比例较低（$\lesssim 10\\%$），且它们至少在 $z\sim4$ 时就已经出现。我们的观测棒比例与 TNG50 模拟在 $z \sim$ 0.5-4 处预测的 $a_{\rm bar}$ $> 1.5$ kpc 的大棒比例一致，也与 Auriga 模拟预测的直至 $z \sim$ 1.5 的棒比例一致。然而，TNG50 模拟预测存在大量较小的棒，而我们的数据无法稳健地探测到它们。如果这些较小的棒确实存在，那么 $z \sim$ 2-4 处的真实棒比例可能显著高于我们的结果。在 $z \ge 1.5$ 处，许多棒状星系显示出邻近伴星系，这表明棒可能受到潮汐触发。从 $z \sim$ 4 到 0.5，观测棒比例、平均投影棒长度和投影棒强度均有所上升。我们的结果突显了棒状星系的早期出现与演化，以及从 $z \sim$ 4 至今棒驱动的盘面长期演化日益增长的重要性。

英文摘要：

We present the first estimate of the observed fraction and properties of bars out to $ z\sim4$ using $\textit{JWST}$ CEERS NIRCam images. We analyze 1770 galaxies with $M_\star > 10^{10} M_\odot$ at $0.5 \leq z \leq 4$ and identify barred galaxies from 839 moderately inclined disk galaxies via ellipse fits and visual classification of both F200W and F444W images. Our results apply mainly to bars with projected semi-major axis $a_{\rm bar}$ $> 1.5 $ kpc ($\sim$ 2 $\times$ PSF in F200W images) that can be robustly traced by ellipse fits. For such bars, the observed bar fraction at $z\sim$ 2-4 is low ($\lesssim 10\%$), and they appear to be emerging at least as early as $z\sim 4$. Our observed bar fraction is consistent with the bar fraction predicted by TNG50 simulations for large bars with $a_{\rm bar}$ $> 1.5$ kpc at $z \sim$ 0.5-4 and with the bar fraction from Auriga simulations out to $z \sim$ 1.5. However, TNG50 simulations predict a large population of smaller bars that our data cannot robustly detect. If such bars exist, the true bar fraction at $z \sim$ 2-4 may be significantly higher than our results. At $z \ge 1.5$, many barred galaxies show nearby neighbors, suggesting bars may be tidally triggered. From $z \sim$ 4-0.5, the observed bar fraction, average projected bar length, and projected bar strength rise. Our results highlight the early emergence and evolution of barred galaxies and the rising importance of bar-driven secular evolution from $z \sim$4 to today.

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