论文标题
区分“模棱两可”合并系统的性质，该系统托有中子星：低延期中的GW190425
Distinguishing the nature of ''ambiguous'' merging systems hosting a neutron star: GW190425 in low-latency
论文作者
论文摘要
GW190425是新发现的重力波（GW）源，与中子星形中子星星合并一致，其chirp质量为$ 1.44 \ pm0.02 cm_ \ odot。$此值仅在GW信号中属于$ abiguliund $ nettair in GW信号，我们不能仅仅排除Black of Black of Black in the Black hole by bilary binary binary byary bartion bartion bartion bartion by bartial byarn的含量。在这种情况下，该系统将拥有一个中子星和一个非常轻的恒星黑洞，质量接近中子星的最大值，填充了$ $ $ $ $ GAP $。与GW/GRB170817相比，由于信息的本地化且距离较大，因此没有电磁对应物与此事件牢固相关。我们在这里为GW190425的Kilonova Light曲线模型构建，用于双中性恒星和黑洞中的星系系统，考虑到两个状态方程与GW170817/GW190425信号的当前限制一致，以及NICER的结果，以及黑洞旋转效果，包括新的exta for eementa of eementa。与双中性恒星盒相比，GW190425中的浅黑洞的假定会产生更明亮的Kilonova发射，使我们能够区分中子星的同伴性质。关于GW190425的候选对应物，后来被分类为超新星，我们的模型本可以在其早期的$ r $ band Evolution中丢弃两个瞬态。将GW信号的CHIRP质量和光度距离信息与Kilonova光曲线库相结合，有助于早期识别电磁对应物。我们指出，在此间隔的$模棱两可$值的间隔中，chirp质量的低潜伏期释放对于成功的电磁随访至关重要。
GW190425 is the newly discovered gravitational wave (GW) source consistent with a neutron star-neutron star merger with chirp mass of $1.44\pm0.02M_\odot.$ This value falls in the $ambiguous$ interval as from the GW signal alone we can not rule out the presence of a black hole in the binary. In this case, the system would host a neutron star and a very light stellar black hole, with mass close to the maximum value for neutron stars, filling the $mass$ $gap$. No electromagnetic counterpart is firmly associated with this event, due to the poorly informative sky localisation and larger distance, compared to GW/GRB170817. We construct here kilonova light curve models for GW190425, for both double neutron star and black hole-neutron star systems, considering two equations of state consistent with current constraints from the signals of GW170817/GW190425 and the NICER results, including black hole spin effects and assuming a new formula for the mass of the ejecta. The putative presence of a light black hole in GW190425 would have produced a brighter kilonova emission compared to the double neutron star case, letting us to distinguish the nature of the companion to the neutron star. Concerning candidate counterparts of GW190425, classified later on as supernovae, our models could have discarded two transients detected in their early $r$-band evolution. Combining the chirp mass and luminosity distance information from the GW signal with a library of kilonova light curves helps identifying the electromagnetic counterpart early on. We remark that the release in low latency of the chirp mass in this interval of $ambiguous$ values appears to be vital for successful electromagnetic follow-ups.
