Vera C. Rubin天文台的时空遗产巡天（LSST）将对多达1亿个类星体的光变曲线进行编目。其中大约有100个超紧凑大质量黑洞（MBH）双星，它们在5-15年后可被激光干涉空间天线（LISA）通过引力波（GWs）探测到。在此我们假设LISA已探测到来自一个MBH双星的引力波，并评估其电磁（EM）对应体能否在归档LSST数据中被唯一识别为周期性类星体。我们利用从LISA波形推导出的双星属性，如其轨道频率的过去演化、总质量、距离和天空定位，来预测归档LSST数据中预期类星体的红移、星等和历史周期性。然后我们使用蒙特卡洛模拟来计算误报概率，即LSST星表中偶然匹配这些属性的类星体数量，该计算基于（外推的）类星体光度函数、LSST的采样节奏以及内在的“阻尼随机游走（DRW）”类星体变率。我们对四个基准LISA双星进行分析，其总质量和红移为$(M_{\rm bin}/{\rm M_{\odot}},z) = (3\times10^5,0.3)$、$(3\times10^6,0.3)$、$(10^7,0.3)$和$(10^7,1)$。虽然DRW噪声和LSST采样节奏导致的混叠可能偶然产生虚假周期性，但我们发现LISA源在LSST观测期间的频率啁啾会消除这些噪声峰，使真实源在Lomb-Scargle周期图中凸显出来。我们发现所有四个基准双星都有极好的机会被唯一识别，在合并前一周或更早时其误报概率低于$10^{-5}$。这使得在双星旋近阶段能够对单个电磁对应体进行深度后续电磁观测。
英文摘要：
The Vera C. Rubin Observatory's Legacy Survey of Space and Time (LSST) will catalogue the light-curves of up to 100 million quasars. Among these there can be up to approximately 100 ultra-compact massive black hole (MBH) binaries, which 5-15 years later can be detected in gravitational waves (GWs) by the Laser Interferometer Space Antenna (LISA). Here we assume that GWs from a MBH binary have been detected by LISA, and we assess whether or not its electromagnetic (EM) counterpart can be uniquely identified in archival LSST data as a periodic quasar. We use the binary's properties derived from the LISA waveform, such as the past evolution of its orbital frequency, its total mass, distance and sky localization, to predict the redshift, magnitude and historical periodicity of the quasar expected in the archival LSST data. We then use Monte Carlo simulations to compute the false alarm probability, i.e. the number of quasars in the LSST catalogue matching these properties by chance, based on the (extrapolated) quasar luminosity function, the sampling cadence of LSST, and intrinsic ``damped random walk (DRW)" quasar variability. We perform our analysis on four fiducial LISA binaries, with total masses and redshifts of $(M_{\rm bin}/{\rm M_{\odot}},z) = (3\times10^5,0.3)$, $(3\times10^6,0.3)$, $(10^7,0.3)$ and $(10^7,1)$. While DRW noise and aliasing due to LSST's cadence can produce false periodicities by chance, we find that the frequency chirp of the LISA source during the LSST observations washes out these noise peaks and allows the genuine source to stand out in Lomb-Scargle periodograms. We find that all four fiducial binaries yield excellent chances to be uniquely identified, with false alarm probabilities below $10^{-5}$, a week or more before their merger. This then enables deep follow-up EM observations targeting the individual EM counterparts during their inspiral stage.
Double white dwarf (DWD) binaries are expected to be very common in the Milky Way, but their intrinsic faintness challenges the detection of these systems. Currently, only a few tens of detached DWDs are know. Such systems offer the best chance of extracting the physical properties that would allow us to address a wealth of outstanding questions ranging from the nature of white dwarfs, over stellar and binary evolution to mapping the Galaxy. In this paper we explore the prospects for detections of ultra-compact (with binary separations of a few solar radii or less) detached DWDs in: 1) optical…
The Legacy Survey of Space and Time (LSST) by the Vera C. Rubin Observatory is expected to discover tens of millions of quasars. A significant fraction of these could be powered by coalescing massive black hole (MBH) binaries, since many quasars are believed to be triggered by mergers. We show that under plausible assumptions about the luminosity functions, lifetimes, and binary fractions of quasars, we expect the full LSST quasar catalogue to contain between 20-100 million compact MBH binaries with masses $M=10^{5-9}M_{\odot}$, redshifts $z=0-6$, and orbital periods $P=1-70$ days. Their light…
Stellar-mass binary black holes will sweep through the frequency band of the Laser Interferometer Space Antenna (LISA) for months to years before appearing in the audio-band of ground-based gravitational-wave detectors. One can expect several tens of these events up to a distance of $500 \,\mathrm{Mpc}$ each year. The LISA signal-to-noise ratio for such sources even at these close distances will be too small for a blind search to confidently detect them. However, next generation ground-based gravitational-wave detectors, expected to be operational at the time of LISA, will observe them with si…
The planned Laser Interferometric Space Antenna (LISA) will be able to detect gravitational waves (GWs) from intermediate mass binary black holes (IMBBHs) in the mass range $\sim 10^{2} \mbox{-} 10^{4}\,M_{\odot}$ up to a redshift $z\sim20$. Modulation effects due to orbital motion of LISA around the Sun facilitate precise premerger localization of the sources, which in turn would help in electromagnetic (EM) followups. In this work, we calculate the uncertainties in sky position, luminosity distance, and time of coalescence as a function of time to coalescence. For representative masses of th…
Multiband observations of coalescing stellar-mass black holes binaries could deliver valuable information on the formation of those sources and potential deviations from General Relativity. Some of these binaries might be first detected by the space-based detector LISA and, then, several years later, observed with ground-based detectors. Due to large uncertainties in astrophysical models, it is hard to predict the population of such binaries that LISA could observe. In this work, we assess the ability of LISA to detect the events of the third catalogue of gravitational wave sources released by…
Presaging Doppler beaming discoveries of double white dwarfs during the Rubin LSST era
Johns Hopkins University（约翰斯·霍普金斯大学）；Astrophysics Research Center of the Open University (ARCO)（开放大学天体物理研究中心）；Institute for Advanced Study, Princeton（普林斯顿高等研究院）；The Observatories of the Carnegie Institution for Science（卡内基科学研究所天文台）
Archival Multiband Gravitational-Wave Signals from Massive Black Hole Binary Mergers
Vanderbilt University（范德堡大学）；Fisk University（菲斯克大学）；University of Southern California（南加州大学）；Universitá degli Studi di Milano-Bicocca（米兰比可卡大学）；INAF, Osservatorio Astronomico di Brera（意大利国家天体物理研究所，布雷拉天文台）；INFN, Sezione di Milano-Bicocca（意大利国家核物理研究所，米兰比可卡分部）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所）；Donostia International Physics Centre (DIPC)（圣塞巴斯蒂安国际物理中心）；IKERBASQUE, Basque Foundation for Science（伊克尔巴斯基克，巴斯克科学基金会）；Universitá degli Studi dell’Insubria（因苏布里亚大学）
With the discovery of both binary black hole mergers and a binary neutron star merger the field of Gravitational Wave Astrophysics has really begun. The current advanced LIGO and Virgo detectors are laser interferometers that will improve their sensitivity in the coming years. In the long run, new detectors such as LISA and the Einstein Telescope will have sensitivities that allow the detection of many thousands of sources and ET can observe essentially the whole observable Universe, for heavy black holes. All these measurements will provide new answers to open questions in binary evolution, r…
We argue that the recent groundbreaking discovery by Badenes et al. (2009) of a nearby (~50 pc) white dwarf-neutron star (or black hole) binary (SDSS 1257+5428) with a merger timescale ~500 Myr implies that such systems are common; we estimate that there are of order 10^6 in the Galaxy. Although subject to large uncertainties, the nominal derived merger rate is ~5 x 10^-4 per yr in the Milky Way, just ~3-6 and ~20-40 times less than the Type Ia and core-collapse supernova (SN) rates, respectively. This implies that the merger rate is ~0.5-1 x 10^4 per Gpc^3 per yr in the local universe, ~5000-…
Supermassive black hole binaries (SMBHBs) should be an inevitable consequence of the hierarchical growth of massive galaxies through mergers, and the strongest sirens of gravitational waves (GWs) in the cosmos. And yet, their direct detection has remained elusive due to the compact (sub-parsec) orbital separations of gravitationally bound SMBHBs. Here we exploit a theoretically predicted signature of a SMBHB in the time domain: periodic variability caused by a mass accretion rate that is modulated by the binary's orbital motion. We report our first significant periodically varying quasar detec…
Gas-induced gravitational-wave dephasing and accretion periodicities of live post-Newtonian massive black hole binaries: warm disk
Center for Cosmology and Particle Physics, Physics Department, New York University（纽约大学物理系宇宙学与粒子物理中心）；Dipartimento di Fisica A. Pontremoli, Università degli Studi di Milano（米兰大学A. Pontremoli物理系）；DiSAT, Università degli Studi dell’Insubria（因苏布里亚大学DiSAT）；INFN, Sezione di Milano-Bicocca（意大利国家核物理研究所米兰-比可卡分部）
Searching for core-collapse supernovae in binaries with ZTF
Deutsches Elektronen-Synchrotron (DESY)（德国电子同步辐射研究所）；Institut für Physik, Humboldt-Universität zu Berlin（柏林洪堡大学物理研究所）；Argelander Institut für Astronomie（阿尔兰德尔天文学研究所）
McFACTS. IV. Electromagnetic Counterparts to AGN-disk-embedded Binary Black Hole Mergers
Graduate Center, City University of New York（纽约市立大学研究生院）；Department of Astrophysics, American Museum of Natural History（美国自然历史博物馆天体物理系）；Department of Physics and Astronomy, Stony Brook University（石溪大学物理与天文系）；Department of Science, BMCC, City University of New York（纽约市立大学巴鲁克学院科学系）；Center for Computational Astrophysics, Flatiron Institute（平顿研究所计算天体物理中心）；New Mexico State University（新墨西哥州立大学）；Canadian Institute for Theoretical Astrophysics, University of Toronto（多伦多大学加拿大理论天体物理研究所）；Center for Computational Relativity and Gravitation, Rochester Institute of Technology（罗切斯特理工学院计算相对论与引力中心）；Data Science Institute, University of Chicago（芝加哥大学数据科学研究所）
We study the interaction of a supermassive black hole (SMBH) binary and a standard radiatively efficient thin accretion disk. We examine steady-state configurations of the disk and migrating SMBH system, self-consistently accounting for tidal and viscous torques and heating, radiative diffusion limited cooling, gas and radiation pressure, and the decay of the binary's orbit. We obtain a "phase diagram" of the system as a function of binary parameters, showing regimes in which both the disk structure and migration have a different character. Although massive binaries can create a central gap in…
Searching for Binary Black Hole Merger Emission in AGN Disks: Optical and Spectroscopic Follow-up of S240413p
Artificial Intelligence for Physics Laboratory (Lab-IA) and Centro Brasileiro de Pesquisas Físicas（物理人工智能实验室（Lab-IA）和巴西物理研究中心）；Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) Northwestern University（西北大学天体物理学跨学科探索与研究中心）；International Gemini Observatory/NSF NOIRLab（国际双子座天文台/美国国家科学基金会NOIR实验室）；Universidade de São Paulo, IAG（圣保罗大学天文学、地球学和气象学院）；Departamento de Física, Universidade Federal de Santa Catarina（圣卡塔琳娜联邦大学物理系）；Departamento de Astronomia, Instituto de Física（物理系天文学系）
A survey of ultra-compact high-state AM CVn binaries with ZTF and Gaia: New discoveries and observational constraints on Galactic space density
Kazan Federal University（喀山联邦大学）；Department of Astronomy, California Institute of Technology（加利福尼亚理工学院天文系）；Institut für Astronomie und Astrophysik, Kepler Center for Astro and Particle Physics, Universität Tübingen（蒂宾根大学天文与天体物理研究所、开普勒天体与粒子物理中心）；Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院卡弗里天体物理学与空间研究研究所）；Anton Pannekoek Institute for Astronomy, University of Amsterdam（阿姆斯特丹大学安东·潘内库克天文学研究所）；Institute of Science and Technology Austria（奥地利科学技术研究院）
