T-ReX:通过 X 射线揭示的狼蛛

Leisa K. Townsley, Patrick S. Broos and Matthew S. Povich
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摘要

蜘蛛星云(30 Doradus,30 Dor)是本星系群中最重要的恒星形成复合体,是研究星爆天体物理学的显微镜。它的中心是异常丰富的年轻恒星群R136,其中包含了已知质量最大的恒星。恒星风和超新星将 30 Dor 星雕刻成令人惊叹的弧形、柱形和气泡。我们将介绍钱德拉 X 射线愿景项目 "X 射线揭示的狼蛛(T-Revealed by X-rays,T-ReX)"的首批成果和高级数据处理产品。T-ReX 星表中的 3615 个点源包括大质量恒星、紧凑天体、双星、明亮的前主序恒星和 30 Dor 中紧凑的年轻恒星(子)星团。剔除点源和异常明亮的超新星残余物 N157B(30 Dor B)后,全球漫射 X 射线图显示了 1-10 pc 尺度的热等离子体结构,吸收校正后的总波段(0.5-7 keV)X 射线光度为 2.110 × 1037 erg s-1。空间分辨光谱建模为界面上电荷交换过程增强的发射线提供了证据。我们在一个新解析的弧状X射线风星云--Manta Ray--内发现了一颗迄今为止在30 Dor探测到的最古老的X射线脉冲星的候选者--PSR J0538-6902。T-ReX 的长时间基线允许对数十颗大质量恒星进行监测,其中几颗恒星显示出与双星轨道周期相关的周期性变化,并捕捉到至少三颗低质量银河系前景恒星的强烈耀斑。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
T-ReX: The Tarantula—Revealed by X-Rays
The Tarantula Nebula (30 Doradus, 30 Dor) is the most important star-forming complex in the Local Group, offering a microscope on starburst astrophysics. At its heart lies the exceptionally rich young stellar cluster R136, containing the most massive stars known. Stellar winds and supernovae have carved 30 Dor into an amazing display of arcs, pillars, and bubbles. We present first results and advanced data-processing products from the 2 Ms Chandra X-ray Visionary Project, “The Tarantula—Revealed by X-rays” (T-ReX). The 3615 point sources in the T-ReX catalog include massive stars, compact objects, binaries, bright pre-main-sequence stars, and compact young stellar (sub)clusters in 30 Dor. After removing point sources and excluding the exceptionally bright supernova remnant N157B (30 Dor B), the global diffuse X-ray maps reveal hot plasma structures resolved at 1–10 pc scales, with an absorption-corrected total-band (0.5–7 keV) X-ray luminosity of 2.110 × 1037 erg s−1. Spatially resolved spectral modeling provides evidence for emission lines enhanced by charge-exchange processes at the interfaces. We identify a candidate for the oldest X-ray pulsar detected to date in 30 Dor, PSR J0538-6902, inside a newly resolved arcuate X-ray wind nebula, the Manta Ray. The long temporal baseline of T-ReX allowed monitoring of dozens of massive stars, several showing periodic variability tied to binary orbital periods, and captured strong flares from at least three low-mass Galactic foreground stars.
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