基于DECam后续观测的暗能量巡天模拟对GW190814物理性质的约束
Constraints on the Physical Properties of GW190814 through Simulations based on DECam Follow-up Observations by the Dark Energy Survey
摘要：
2019年8月14日，LIGO和Virgo合作探测到来自黑洞和2.6太阳质量致密物体的引力波，这可能是第一个中子星-黑洞（NSBH）合并。为了寻找光学对应物，暗能量调查（DES）在合并后的第0、1、2、3、6和16天晚上用Blanco/DECam获得了整个90%置信水平定位区域的深度成像。DES管道检测到亮度不同的物体，我们通过目录匹配，光变曲线特性，宿主星系光度红移，SOAR光谱后续观测和基于机器学习的光度分类系统地减少了候选对应物。所有候选人都被拒绝作为合并的对手。为了量化我们搜索的灵敏度，我们将我们的选择标准应用于超新星和千新星的全光变曲线模拟，因为它们将出现在DECam观测中。由于合并的源类是不确定的，我们利用了一个不可知的，三个组件kilonova模型的基础上潮汐中断NS喷出物的属性来量化我们的检测效率的对应物，如果合并包括NS。我们发现，如果在合并过程中发生的kilonova，配置喷射的物质是大于0.07太阳质量，具有镧系元素丰度小于$10^{-8.56}$，并具有$0.18c$和$0.21c$之间的速度是不利的$2σ$水平。此外，我们估计，我们的背景减少的方法是能够关联的引力波信号与探测到的电磁对应物在$4σ$水平在$95\%$未来的后续观测。
英文摘要：
On 14 August 2019, the LIGO and Virgo Collaborations detected gravitational waves from a black hole and a 2.6 solar mass compact object, possibly the first neutron star -- black hole (NSBH) merger. In search of an optical counterpart, the Dark Energy Survey (DES) obtained deep imaging of the entire 90 percent confidence level localization area with Blanco/DECam 0, 1, 2, 3, 6, and 16 nights after the merger. Objects with varying brightness were detected by the DES Pipeline and we systematically reduced the candidate counterparts through catalog matching, light curve properties, host-galaxy photometric redshifts, SOAR spectroscopic follow-up observations, and machine-learning-based photometric classification. All candidates were rejected as counterparts to the merger. To quantify the sensitivity of our search, we applied our selection criteria to full light curve simulations of supernovae and kilonovae as they would appear in the DECam observations. Since the source class of the merger was uncertain, we utilized an agnostic, three-component kilonova model based on tidally-disrupted NS ejecta properties to quantify our detection efficiency of a counterpart if the merger included a NS. We find that if a kilonova occurred during this merger, configurations where the ejected matter is greater than 0.07 solar masses, has lanthanide abundance less than $10^{-8.56}$, and has a velocity between $0.18c$ and $0.21c$ are disfavored at the $2σ$ level. Furthermore, we estimate that our background reduction methods are capable of associating gravitational wave signals with a detected electromagnetic counterpart at the $4σ$ level in $95\%$ of future follow-up observations.
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