An Infrared Search for Kilonovae with the WINTER Telescope. I. Binary Neutron Star Mergers
An Infrared Search for Kilonovae with the WINTER Telescope. I. Binary Neutron Star Mergers
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DOI：
10.3847/1538-4357/ac4508
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发表时间：
2021-10
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通讯作者：
Danielle Frostig;S. Biscoveanu;G. Mo;V. Karambelkar;T. Dal Canton;Hsin-Yu Chen;M. Kasliwal;E. Katsavounidis;N. Lourie;R. Simcoe;S. Vitale
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作者：
Danielle Frostig;S. Biscoveanu;G. Mo;V. Karambelkar;T. Dal Canton;Hsin-Yu Chen;M. Kasliwal;E. Katsavounidis;N. Lourie;R. Simcoe;S. Vitale
宽视场红外瞬变探测器（WINTER）是一种新型的1度限视时域巡天仪器，专门用于对双中子星（BNS）和中子星-黑洞并合产生的千新星进行近红外跟踪。WINTER将在Palomar天文台的专用1米望远镜上观测近红外Y， J和短h波段（0.9-1.7 μm，到J AB = 21等）。迄今为止，大多数快速的千新星追踪都是在光学波长；然而，与光学发射相比，近红外发射衰减更慢，对几何形状和视角的依赖更小。我们对LIGO、Virgo和KAGRA干涉仪第四次观测期间的后续活动进行了端到端模拟，包括模拟625个BNS合并，它们在引力波中的探测，低延迟和全参数估计的天图，以及来自两个不同模型网格的一套千新星光曲线。考虑到现实的BNS合并率，我们预测在O4期间，WINTER将独立发现多达5个新的千新星。使用更大的千新星参数网格，我们发现千新星发射的寿命约为光学的2倍，红色千新星在红外中的探测距离约为光学的1.5倍。对于90%的定位区域小于150（450）摄氏度，WINTER将对超过10%的千诺瓦模型网格敏感到350（200）摄氏度。我们开发了一个通用的工具包来创建任何电磁望远镜的最佳BNS后续策略，并在此框架下提出了WINTER的观测策略。这个工具包，所有的模拟引力波事件和天空地图都可供社区使用。
The Wide-Field Infrared Transient Explorer (WINTER) is a new 1 deg2 seeing-limited time-domain survey instrument designed for dedicated near-infrared follow-up of kilonovae from binary neutron star (BNS) and neutron star–black hole mergers. WINTER will observe in the near-infrared Y, J, and short-H bands (0.9–1.7 μm, to J AB = 21 mag) on a dedicated 1 m telescope at Palomar Observatory. To date, most prompt kilonova follow-up has been in optical wavelengths; however, near-infrared emission fades more slowly and depends less on geometry and viewing angle than optical emission. We present an end-to-end simulation of a follow-up campaign during the fourth observing run (O4) of the LIGO, Virgo, and KAGRA interferometers, including simulating 625 BNS mergers, their detection in gravitational waves, low-latency and full parameter estimation skymaps, and a suite of kilonova lightcurves from two different model grids. We predict up to five new kilonovae independently discovered by WINTER during O4, given a realistic BNS merger rate. Using a larger grid of kilonova parameters, we find that kilonova emission is ≈2 times longer lived and red kilonovae are detected ≈1.5 times further in the infrared than in the optical. For 90% localization areas smaller than 150 (450) deg2, WINTER will be sensitive to more than 10% of the kilonova model grid out to 350 (200) Mpc. We develop a generalized toolkit to create an optimal BNS follow-up strategy with any electromagnetic telescope and present WINTER’s observing strategy with this framework. This toolkit, all simulated gravitational-wave events, and skymaps are made available for use by the community.