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arXiv 2103.13285astro-ph.CO
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HST见变更程序：I.勘测设计、管道和超新星发现

The HST See Change Program: I. Survey Design, Pipeline, and Supernova Discoveries

Brian Hayden, David Rubin, Kyle Boone, Greg Aldering, Jakob Nordin, Mark Brodwin, Susana Deustua, Sam Dixon, Parker Fagrelius, Andy Fruchter, Peter Eisenhardt, … 展开作者

Brian Hayden, David Rubin, Kyle Boone, Greg Aldering, Jakob Nordin, Mark Brodwin, Susana Deustua, Sam Dixon, Parker Fagrelius, Andy Fruchter, Peter Eisenhardt, Anthony Gonzalez, Ravi Gupta, Isobel Hook, Chris Lidman, Kyle Luther, Adam Muzzin, Zachary Raha, Pilar Ruiz-Lapuente, Clare Saunders, Caroline Sofiatti, Adam Stanford, Nao Suzuki, Tracy Webb, Steven C. Williams, Gillian Wilson, Mike Yen, Rahman Amanullah, Kyle Barbary, Hans Bohringer, Greta Chappell, Carlos Cunha, Miles Currie, Rene Fassbender, Michael Gladders, Ariel Goobar, Hendrik Hildenrandt, Henk Hoekstra, Xiaosheng Huang, Dragan Huterer, M. James Jee, Alex Kim, Marek Kowalski, Eric Linder, Joshua E. Meyers, Reynald Pain, Saul Perlmutter, Johan Richard, Piero Rosati, Eduardo Rozo, Eli Rykoff, Joana Santos, Anthony Spadafora, Daniel Stern, Risa Wechsler, The Supernova Cosmology Project

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摘要：

See Change巡天的目的是通过有效地发现高红移Ia型超新星（SNe Ia）并通过弱透镜改善星团质量测量来进行$z>1$宇宙学测量。这次巡天用哈勃太空望远镜观测了12个星系团，它们的红移范围从$z=1.13$到$1.75$，在$z\sim 0.8-2.3$发现了57个可能的瞬变和27个可能的Ia型超新星。与之前类似的巡天（Dawson et al. 2009）一样，这被证明是一个非常有效的使用HST进行SN观测的方法; See Change巡天还测试了在更高的红移下保持或进一步提高效率的可行性，在那里我们对预期的星团质量和恒星形成率的详细信息较少。我们发现，每个轨道的超新星Ia的数量是一个$\sim 8$的因子高于现场搜索，和45%的轨道包含一个活跃的超新星Ia在22休息帧天的峰值，与一个集群本身产生6个超新星Ia。我们提出了调查设计，管道和SN发现。新功能包括全盲SN搜索，第一个随机森林候选分类器，用于欠采样IR数据（50%的检测阈值在人类搜索者的0.05量级内），候选人的实时前向建模测光，以及半自动光度分类和后续预测。我们还描述了光谱的后续行动，在测量主机星系红移。我们样本的宇宙学分析将在配套论文中介绍。

英文摘要：

The See Change survey was designed to make $z>1$ cosmological measurements by efficiently discovering high-redshift Type Ia supernovae (SNe Ia) and improving cluster mass measurements through weak lensing. This survey observed twelve galaxy clusters with the Hubble Space Telescope spanning the redshift range $z=1.13$ to $1.75$, discovering 57 likely transients and 27 likely SNe Ia at $z\sim 0.8-2.3$. As in similar previous surveys (Dawson et al. 2009), this proved to be a highly efficient use of HST for SN observations; the See Change survey additionally tested the feasibility of maintaining, or further increasing, the efficiency at yet higher redshifts, where we have less detailed information on the expected cluster masses and star-formation rates. We find that the resulting number of SNe Ia per orbit is a factor of $\sim 8$ higher than for a field search, and 45% of our orbits contained an active SN Ia within 22 rest-frame days of peak, with one of the clusters by itself yielding 6 of the SNe Ia. We present the survey design, pipeline, and SN discoveries. Novel features include fully blinded SN searches, the first random forest candidate classifier for undersampled IR data (with a 50% detection threshold within 0.05 magnitudes of human searchers), real-time forward-modeling photometry of candidates, and semi-automated photometric classifications and follow-up forecasts. We also describe the spectroscopic follow-up, instrumental in measuring host-galaxy redshifts. The cosmology analysis of our sample will be presented in a companion paper.

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