利用南希·格蕾丝·罗曼太空望远镜开展千新星科学研究
Enabling Kilonova Science with Nancy Grace Roman Space Telescope
AI总结：
本研究分析南希·格蕾丝·罗曼太空望远镜的观测优势，提出引力波后续观测、巡天配置及协同观测的建议，预计可发现多例千新星，助力r-过程核合成等多领域研究。
摘要：
双中子星并合与中子星-黑洞并合是可通过引力波和电磁辐射探测的多信使源。中子星并合抛射物的低电子丰度有利于通过快中子俘获（r-过程）生成镧系元素、锕系元素等重元素。这些不稳定原子核的衰变会为一种被称为“千新星（kilonova）”的亮红外暂现源提供能量。发现一批千新星样本将帮助我们确定中子星并合是否是r-过程元素核合成的主要场所，约束核物质的状态方程，并对哈勃常数进行独立测量。南希·格蕾丝·罗曼太空望远镜（Roman）将兼具深度、近红外灵敏度和宽视场的独特优势。这些特性将使Roman能够发现光学望远镜会遗漏的引力波对应体，例如与大距离、高镧系元素丰度、高双星质量比、视线方向上的大尘埃消光相关的千新星，或是从赤道视角观测到的千新星。我们的分析建议：（i）为引力波后续观测提供快速（约1周）的机遇目标（Target of Opportunity, ToO）模式；（ii）在高纬时域巡天天区中至少使用两个滤光片（优先选用F158和F213滤光片）开展观测，观测频率小于8天；（iii）与鲁宾天文台（Rubin Observatory）协同运行。遵循这些建议，我们预计在LIGO-Virgo-KAGRA第五次观测运行的1.5年期间，Roman可通过对定位良好（90%置信度下定位面积A<10平方度）的中子星并合事件开展ToO观测，识别出1-6个千新星（在第六次观测运行期间约为4-21个）。在为期5年的高纬巡天中，可收集到5-40个偶然发现的千新星样本。
英文摘要：
Binary neutron star mergers and neutron star-black hole mergers are multi-messenger sources that can be detected in gravitational waves and in electromagnetic radiation. The low electron fraction of neutron star merger ejecta favors the production of heavy elements such as lanthanides and actinides via rapid neutron capture (r-process). The decay of these unstable nuclei powers an infrared-bright transient called a "kilonova". The discovery of a population of kilonovae will allow us to determine if neutron star mergers are the dominant sites for r-process element nucleosynthesis, constrain the equation of state of nuclear matter, and make independent measurements of the Hubble constant. The Nancy Grace Roman Space Telescope (Roman) will have a unique combination of depth, near-infrared sensitivity, and wide field of view. These characteristics will enable Roman's discovery of GW counterparts that will be missed by optical telescopes, such as kilonova that are associated with large distances, high lanthanide fractions, high binary mass-ratios, large dust extinction in the line of sight, or that are observed from equatorial viewing angles. Our analysis suggests to (i) make available a rapid (about 1 week) Target of Opportunity mode for GW follow-up; (ii) include observations of the High Latitude Time-Domain survey footprint in at least two filters (preferably the F158 and F213 filters) with a cadence of < 8 days; (iii) operate in synergy with Rubin Observatory. Following these recommendations, we expect that 1-6 kilonovae can be identified by Roman via ToO observations of well localized (A < 10 sq. deg., 90% C.I.) neutron star mergers during 1.5 years of the LIGO-Virgo-KAGRA fifth (or about 4-21 in during the sixth) observing run. A sample of 5-40 serendipitously discovered kilonovae can be collected in a 5-year high latitude survey.
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