A DECam Search for an Optical Counterpart to the LIGO Gravitational Wave Event GW151226
P. S. Cowperthwaite, E. Berger, M. Soares-Santos, J. Annis, D. Brout, D. A. Brown, E. Buckley-Geer, S. B. Cenko, H. Y. Chen, R. Chornock, H. T. Diehl, Z. Doctor… 展开作者
P. S. Cowperthwaite, E. Berger, M. Soares-Santos, J. Annis, D. Brout, D. A. Brown, E. Buckley-Geer, S. B. Cenko, H. Y. Chen, R. Chornock, H. T. Diehl, Z. Doctor, A. Drlica-Wagner, M. R. Drout, B. Farr, D. A. Finley, R. J. Foley, W. Fong, D. B. Fox, J. Frieman, J. Garcia-Bellido, M. S. S. Gill, R. A. Gruendl, K. Herner, D. E. Holz, D. Kasen, R. Kessler, H. Lin, R. Margutti, J. Marriner, T. Matheson, B. D. Metzger, E. H. Neilsen, E. Quataert, A. Rest, M. Sako, D. Scolnic, N. Smith, F. Sobreira, G. M. Strampelli, V. A. Villar, A. R. Walker, W. Wester, P. K. G. Williams, B. Yanny, T. M. C. Abbott, F. B. Abdalla, S. Allam, R. Armstrong, K. Bechtol, A. Benoit-Levy, E. Bertin, D. Brooks, D. L. Burke, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, C. E. Cunha, C. B. D'Andrea, L. N. da Costa, S. Desai, J. P. Dietrich, A. E. Evrard, A. Fausti Neto, P. Fosalba, D. W. Gerdes, T. Giannantonio, D. A. Goldstein, D. Gruen, G. Gutierrez, K. Honscheid, D. J. James, M. W. G. Johnson, M. D. Johnson, E. Krause, K. Kuehn, N. Kuropatkin, M. Lima, M. A. G. Maia, J. L. Marshall, F. Menanteau, R. Miquel, J. J. Mohr, R. C. Nichol, B. Nord, R. Ogando, A. A. Plazas, K. Reil, A. K. Romer, E. Sanchez, V. Scarpine, I. Sevilla-Noarbe, R. C. Smith, E. Suchyta, G. Tarle, D. Thomas, R. C. Thomas, D. L. Tucker, J. Weller
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7 Pages, 2 Figures, 1 Table. Accepted to ApJL, updated to better match published version
We report the results of a Dark Energy Camera (DECam) optical follow-up of the gravitational wave (GW) event GW151226, discovered by the Advanced LIGO detectors. Our observations cover 28.8 deg$^2$ of the localization region in the $i$ and $z$ bands (containing 3% of the BAYESTAR localization probability), starting 10 hours after the event was announced and spanning four epochs at $2-24$ days after the GW detection. We achieve $5σ$ point-source limiting magnitudes of $i\approx21.7$ and $z\approx21.5$, with a scatter of $0.4$ mag, in our difference images. Given the two day delay, we search this area for a rapidly declining optical counterpart with $\gtrsim 3σ$ significance steady decline between the first and final observations. We recover four sources that pass our selection criteria, of which three are cataloged AGN. The fourth source is offset by $5.8$ arcsec from the center of a galaxy at a distance of 187 Mpc, exhibits a rapid decline by $0.5$ mag over $4$ days, and has a red color of $i-z\approx 0.3$ mag. These properties roughly match the expectations for a kilonova. However, this source was detected several times, starting $94$ days prior to GW151226, in the Pan-STARRS Survey for Transients (dubbed as PS15cdi) and is therefore unrelated to the GW event. Given its long-term behavior, PS15cdi is likely a Type IIP supernova that transitioned out of its plateau phase during our observations, mimicking a kilonova-like behavior. We comment on the implications of this detection for contamination in future optical follow-up observations.
Detecting electromagnetic counterparts to LIGO/Virgo/KAGRA gravitational wave events with DECam: Neutron Star Mergers
Carnegie Mellon University（卡内基梅隆大学）；University of Chicago（芝加哥大学）；University of Ferrara（费拉拉大学）；INFN, Sezione di Ferrara（意大利国家核物理研究所费拉拉分部）；INAF, Osservatorio Astronomico d’Abruzzo（意大利国家天体物理研究所阿布鲁佐天文台）；Universität Potsdam（波茨坦大学）；Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理学研究所（爱因斯坦研究所））；Utrecht University（乌得勒支大学）；Nikhef（荷兰国家核物理与粒子物理研究所）；California Institute of Technology（加州理工学院）；University of North Carolina at Chapel Hill（北卡罗来纳大学教堂山分校）
GROWTH on S190426c. II. Real-Time Search for a Counterpart to the Probable Neutron Star-Black Hole Merger using an Automated Difference Imaging Pipeline for DECam
A Joint Search for the Electromagnetic Counterpart to the Gravitational-Wave Binary Black-Hole Merger Candidate S250328ae with the Dark Energy Camera and the Prime Focus Spectrograph
Archival Search for IceCube Sub-TeV Neutrino Counterparts to Sub-Threshold Gravitational Wave Events from the Third Observing Run of the LIGO-Virgo-KAGRA
Bright in the Black: Searching for Electromagnetic Counterparts to Gravitational-Wave Candidates in LIGO-Virgo-KAGRA Observation Runs with AstroSat-CZTI
介绍了LIGO双星黑洞合并事件GW 170104的\emph{Fermi}伽马射线暴监测器（GBM）和大视场望远镜（LAT）观测结果。GBM或LAT均未检测到候选电磁对应物。GBM和LAT数据的时间尺度从秒到天覆盖LIGO本地化区域的详细分析。在10-1000千电子伏范围内，由GBM得到的通量上限为（5.2- 9.4）$\times$ 10 $^{-7}$ erg cm $^{-2}$ s $^{-1}$，由LAT得到的通量上限为（0.2- 13）$\times$ 10 $^{-9}$ erg cm $^{-2}$ s $^{-1}$ s 0.1- 1 GeV。我们还描述了我们的自动化管道和分析技术的改进，用于搜索和表征未来高级LIGO/VIRGO的引力波事件的潜在电磁对应物。
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/VIRGO GW170817. VIII. A Comparison to Cosmological Short-duration Gamma-ray Bursts
Implications of the search for optical counterparts during the second part of the Advanced LIGO's and Advanced Virgo's third observing run: lessons learned for future follow-up observations
Detectability of Gravitational-wave counterparts of EP-FXTs observed during the O4b LIGO-Virgo-KAGRA Observing Run
Gran Sasso Science Institute (GSSI)（格兰萨索科学研究所）；INFN, Laboratori Nazionali del Gran Sasso（意大利国家核物理研究所，格兰萨索国家实验室）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所（ICE, CSIC））；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究学院（IEEC））；Department of Astrophysics/IMAPP, Radboud University（拉德堡德大学天体物理学/IMAPP系）；INAF – Osservatorio Astronomico di Brera（意大利国家天体物理研究所-布里拉天文台）
Implications of the search for optical counterparts during the first six months of the Advanced LIGO's and Advanced Virgo's third observing run: possible limits on the ejecta mass and binary properties
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/VIRGO GW170817. VI. Radio Constraints on a Relativistic Jet and Predictions for Late-Time Emission from the Kilonova Ejecta
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/VIRGO GW170817. III. Optical and UV Spectra of a Blue Kilonova From Fast Polar Ejecta
我们目前的光学和紫外光谱的第一个电磁对应的引力波（GW）源，二中子星合并GW 170817。在合并后1.5至9.5天之间，使用SOAR和麦哲伦望远镜每晚获得光谱;紫外光谱在5.5天时使用\textit{Hubble Space Telescope}获得。我们的数据揭示了一个快速褪色的蓝色成分（$T\approx5500$ K在1.5天），迅速变红;光谱晚于$\gtrsim 4.5$天超出光学制度的峰值。光谱大多是无特征的，虽然我们确定了一个可能的弱发射线在$\sim 7900$在$t\lesssim 4.5$天。其颜色、快速演化和无特征的光谱与来自极地喷出物的“蓝色”千诺娃一致，主要由原子质量数为$A\lesssim 140$的轻$r$过程核组成。这表明视线在眶轴的$θ_{\rm obs}\lesssim 45^{\circ}$范围内。与模型的比较表明，蓝色喷出物的$\sim0.03$ M $_\odot$，速度为$\sim 0.3c$。所需的镧系元素部分是$\sim 10^{-4}$，但在最外面的喷出物中下降到$<10^{-5}$。大的速度指向一个动力学的起源，而不是盘风，对于这个蓝色的分量，这表明这两个双星组成是中子星（而不是由中子星和黑洞组成的双星）。对于动态喷出物，高质量有利于一个小的中子星半径$\lesssim 12$公里。这个质量也支持了中子星合并是$r$过程核合成的主…
WFST Follow-up of S251112cm: Searching for an Optical Counterpart to a Subsolar-mass Compact-binary Merger Candidate
University of Science and Technology of China（中国科学技术大学）；National Astronomical Observatory of Japan, National Institutes of Natural Sciences（日本国立天文台，国立自然科学研究院）；Guizhou University（贵州大学）
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/VIRGO GW170817. VII. Properties of the Host Galaxy and Constraints on the Merger Timescale
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/VIRGO GW170817. IV. Detection of Near-infrared Signatures of r-process Nucleosynthesis with Gemini-South
