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arXiv 2103.01958astro-ph.GAastro-ph.SR
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M33-ike螺旋线中Wolf-Rayet星的可探测性达30 Mpc

The detectability of Wolf-Rayet Stars in M33-ike spirals up to 30 Mpc

J. L. Pledger, A. J. Sharp, A. E. Sansom

备注：
14 pages, 7 figures, 5 tables. Accepted for publication in MNRAS
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摘要：

我们分析的影响，空间分辨率上推断的数量和类型的沃尔夫-拉叶（WR）和其他大质量恒星在外部星系。附近星系M33的连续体和线状影像越来越模糊，以模拟从8.4Mpc到30 Mpc的不同距离的效果，以获得恒定的可见度。我们使用连续谱和氦II线图像之间的幅度差异，加上图像的目视检查，通过其电离氦过剩来识别WR候选人。结果是WR探测到的数量惊人地大幅度减少，只有15%的已知WR恒星被预测在30 Mpc时被探测到。WR亚型的混合物也显示出随着距离的增加而显着变化（分辨率较差），较冷的WN星比其他亚型更容易检测。我们讨论了如何空间聚类的不同亚型和线稀释可能会导致这些差异和它们的年龄的影响，这将是有用的校准在当前的调查中发现的大质量恒星的数量。我们调查的能力ELT/HARMONI进行WR调查，并表明，通过使用自适应光学在可见光波长，即使是最微弱的（Mv =-3等）WR星将检测到30 Mpc。

英文摘要：

We analyse the impact that spatial resolution has on the inferred numbers and types of Wolf-Rayet (WR) and other massive stars in external galaxies. Continuum and line images of the nearby galaxy M33 are increasingly blurred to mimic effects of different distances from 8.4Mpc to 30Mpc, for a constant level of seeing. We use differences in magnitudes between continuum and Helium II line images, plus visual inspection of images, to identify WR candidates via their ionized helium excess. The result is a surprisingly large decrease in the numbers of WR detections, with only 15% of the known WR stars predicted to be detected at 30Mpc. The mixture of WR sub-types is also shown to vary significantly with increasing distance (poorer resolution), with cooler WN stars more easily detectable than other subtypes. We discuss how spatial clustering of different subtypes and line dilution could cause these differences and the implications for their ages, this will be useful for calibrating numbers of massive stars detected in current surveys. We investigate the ability of ELT/HARMONI to undertake WR surveys and show that by using adaptive optics at visible wavelengths even the faintest (Mv = -3mag) WR stars will be detectable out to 30Mpc.

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