一种集成的光学瞬态应用
Towards An Integrated Optical Transient Utility
摘要：
正在进行的光学时域天文学调查每天晚上定期报告50个瞬态候选者。在这里，我调查了2019年向瞬态名称服务器报告的天文瞬变和超新星分类的人口统计数据。我发现只有十分之一的瞬变是光谱分类的。这个严重的“瓶颈”问题应该引起天文学家和资助机构的关注。一旦LSST上线，瓶颈将恶化20倍（或更多）。我们需要从根本上重新思考瞬变测量的目的。在这里，在对这个问题进行详细调查之后，我提供了一些解决方案。展望未来，天文学家将采用两种不同的方法：（1）多波段测光方法，非常适合于研究非常大的，成千上万的微弱瞬变样本;（2）在浅层和夜间节奏的宽场测光调查中发现的数千个明亮瞬变的光谱分类以及与本地宇宙中星系相关的瞬变。后一个计划，除了发掘新类型的瞬变和提供天文学家的机会，进行广泛的后续有趣的瞬变，需要为前者奠定基础。具体来说，我建议全球协调努力，对明亮超新星的完整样本进行光谱分类（< ~19.5等）和瞬变在本地宇宙（< 200 Mpc）拟议的计划是可以实现的--这要归功于正在进行的宽视场调查，为分类而调整的新型光谱仪的开发，摄谱仪产量的巨大提高和机器人望远镜的日益可用性。
英文摘要：
The ongoing optical time-domain astronomy surveys are routinely reporting fifty transient candidates per night. Here, I investigate the demographics of astronomical transients and supernova classifications reported to the Transient Name Server in the year 2019. I find that only a tenth of the transients were spectrally classified. This severe "bottleneck" problem should concern astronomers and also funding agencies. The bottleneck will get worse by a factor of 20 (or more) once LSST comes on line. We need to fundamentally rethink the purpose of surveys for transients. Here, after undertaking a detailed investigation of this issue I offer some solutions. Going forward, astronomers will employ two different methodologies: (1) multi-band photometric method which is well suited to the study of very large, many tens of thousands, samples of faint transients; (2) spectral classifications of thousands of bright transients found in shallow and nightly cadenced wide-field photometry surveys and transients associated with galaxies in the local Universe. The latter program, in addition to unearthing new types of transients and offering astronomers opportunities to undertake extensive follow up of interesting transients, is needed to set the stage for the former. Specifically, I suggest a globally coordinated effort to spectrally classify a complete sample of bright supernovae (< ~19.5 mag) and transients within the local Universe (< 200 Mpc) The proposed program is within reach -- thanks to the on-going wide-field surveys, the development of novel spectrographs tuned for classification, great improvements in throughput of spectrographs and the increasing availability of robotic telescopes.
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