Designing an Optimal Kilonova Search Using DECam for Gravitational-wave Events
Designing an Optimal Kilonova Search Using DECam for Gravitational-wave Events
复制标题
DOI：
10.3847/1538-4357/ad0462
复制
发表时间：
2023-02
期刊：
影响因子：
--
通讯作者：
C. Bom;J. Annis;A. Garcia;A. Palmese;N. Sherman;M. Soares-Santos;L. Santana-Silva;R. Morgan;K. Bechtol;T. Davis;H. Diehl;S. Allam;T. Bachmann;B. Fraga;J. García-Bellido;M. Gill;K. Herner;C. Kilpatrick;M. Makler;E. F.Olivares;M. Pereira;J. Pineda;A. Santos;D. Tucker;M. Wiesner;M. Aguena;O. Alves;D. Bacon;P. Bernardinelli;E. Bertin;S. Bocquet;D. Brooks;M. Kind;J. Carretero;C. Conselice;M. Costanzi;L. Costa;J. Vicente;S. Desai;P. Doel;S. Everett;I. Ferrero;J. Frieman;M. Gatti;D. Gerdes;D. Gruen;R. Gruendl;G. Gutiérrez;S. Hinton;D. Hollowood;K. Honscheid;D. James;K. Kuehn;N. Kuropatkin;Peter Melchior;J. Mena-Fernández;F. Menanteau;A. Pieres;A. P. Malagón;M. Raveri;M. Rodríguez-Monroy;E. Sanchez;B. Santiago;I. Sevilla-Noarbe;M. Smith;E. Suchyta;M. Swanson;G. Tarlé;C. To;N. Weaverdyck
中科院分区：
文献类型：
--
作者：
C. Bom;J. Annis;A. Garcia;A. Palmese;N. Sherman;M. Soares-Santos;L. Santana-Silva;R. Morgan;K. Bechtol;T. Davis;H. Diehl;S. Allam;T. Bachmann;B. Fraga;J. García-Bellido;M. Gill;K. Herner;C. Kilpatrick;M. Makler;E. F.Olivares;M. Pereira;J. Pineda;A. Santos;D. Tucker;M. Wiesner;M. Aguena;O. Alves;D. Bacon;P. Bernardinelli;E. Bertin;S. Bocquet;D. Brooks;M. Kind;J. Carretero;C. Conselice;M. Costanzi;L. Costa;J. Vicente;S. Desai;P. Doel;S. Everett;I. Ferrero;J. Frieman;M. Gatti;D. Gerdes;D. Gruen;R. Gruendl;G. Gutiérrez;S. Hinton;D. Hollowood;K. Honscheid;D. James;K. Kuehn;N. Kuropatkin;Peter Melchior;J. Mena-Fernández;F. Menanteau;A. Pieres;A. P. Malagón;M. Raveri;M. Rodríguez-Monroy;E. Sanchez;B. Santiago;I. Sevilla-Noarbe;M. Smith;E. Suchyta;M. Swanson;G. Tarlé;C. To;N. Weaverdyck
我们解决的问题，最佳识别所有kilonovae检测到通过引力波发射在即将到来的LIGO/处女座/KAGRA观测运行，O 4，这是预计将是敏感的一个因素的107倍以上的二进制中子星星（BNS）警报比以前。除了最明亮的事件之外，对所有这些新事件的电磁跟踪将需要>1米的望远镜，这是有限的时间。我们提出了一个优化的观察策略DECam在O 4。我们的研究基于O 4和宽先验kilonova模拟的引力波事件的模拟。我们推导出的事件的可探测性为现实的观测条件。我们优化我们的策略，以确认一个kilonova，同时尽量减少望远镜的时间。对于宽范围的kilonova参数，对应于与GW 170817/AT 2017 gfo相比更暗的kilonova，我们发现，采用这种最佳策略，在O 4的标称BNS引力波检测极限（190 Mpc）下，DECam的电磁对应物的发现概率为1080%，这对应于与在先前的观察运行期间采用的策略相比的大约30%的改进。对于更远的事件（0.330兆秒差距），我们的检测概率达到0.60%，增加了0.2倍。对于再现GW 170817/AT 2017 gfo观测结果的以蓝色分量为主的更亮的千诺瓦模型，我们发现在330 Mpc的范围内，我们可以达到0.90%的检测概率，即增加0.20%，同时还减少了跟踪事件所需的总望远镜时间0.20%。
We address the problem of optimally identifying all kilonovae detected via gravitational-wave emission in the upcoming LIGO/Virgo/KAGRA observing run, O4, which is expected to be sensitive to a factor of ∼7 more binary neutron star (BNS) alerts than previously. Electromagnetic follow-up of all but the brightest of these new events will require >1 m telescopes, for which limited time is available. We present an optimized observing strategy for the DECam during O4. We base our study on simulations of gravitational-wave events expected for O4 and wide-prior kilonova simulations. We derive the detectabilities of events for realistic observing conditions. We optimize our strategy for confirming a kilonova while minimizing telescope time. For a wide range of kilonova parameters, corresponding to a fainter kilonova compared to GW170817/AT 2017gfo, we find that, with this optimal strategy, the discovery probability for electromagnetic counterparts with the DECam is ∼80% at the nominal BNS gravitational-wave detection limit for O4 (190 Mpc), which corresponds to an ∼30% improvement compared to the strategy adopted during the previous observing run. For more distant events (∼330 Mpc), we reach an ∼60% probability of detection, a factor of ∼2 increase. For a brighter kilonova model dominated by the blue component that reproduces the observations of GW170817/AT 2017gfo, we find that we can reach ∼90% probability of detection out to 330 Mpc, representing an increase of ∼20%, while also reducing the total telescope time required to follow up events by ∼20%.