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Cai RG, Guo ZK, Hu B, Liu C, Lu Y, Ni WT, Ruan WH, Seto N, Wang G, Wu YL. On networks of space-based gravitational-wave detectors. FUNDAMENTAL RESEARCH 2024; 4:1072-1085. [PMID: 39659501 PMCID: PMC11630722 DOI: 10.1016/j.fmre.2023.10.007] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/31/2023] [Revised: 08/01/2023] [Accepted: 10/10/2023] [Indexed: 12/12/2024] Open
Abstract
The space-based laser interferometers, LISA, Taiji and TianQin, are targeting to observe milliHz gravitational waves (GWs) in the 2030s. The joint observations from multiple space-based detectors yield significant advantages. In this work, we recap the studies and investigations for the joint space-based GW detector networks to highlight: 1) the high precision of sky localization for the massive binary black hole (BBH) coalescences and the GW sirens in the cosmological implication, 2) the effectiveness to test the parity violation in the stochastic GW background observations, 3) the efficiency of subtracting galactic foreground, 4) the improvement in stellar-mass BBH observations. We inspect alternative networks by trading off massive BBH observations and stochastic GW background observation.
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Affiliation(s)
- Rong-Gen Cai
- CAS Key Laboratory of Theoretical Physics, Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing 100190, China
- School of Physical Science and Technology, Ningbo University, Ningbo 315211, China
- School of Fundamental Physics and Mathematical Sciences, Hangzhou Institute for Advanced Study, University of Chinese Academy of Sciences, Hangzhou 310024, China
| | - Zong-Kuan Guo
- CAS Key Laboratory of Theoretical Physics, Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing 100190, China
- School of Fundamental Physics and Mathematical Sciences, Hangzhou Institute for Advanced Study, University of Chinese Academy of Sciences, Hangzhou 310024, China
- School of Physical Sciences, University of Chinese Academy of Sciences, Beijing 100049, China
| | - Bin Hu
- Department of Astronomy, Beijing Normal University, Beijing 100875, China
| | - Chang Liu
- School of Fundamental Physics and Mathematical Sciences, Hangzhou Institute for Advanced Study, University of Chinese Academy of Sciences, Hangzhou 310024, China
- School of Physical Sciences, University of Chinese Academy of Sciences, Beijing 100049, China
- Center for Gravitation and Cosmology, College of Physical Science and Technology, Yangzhou University, Yangzhou, 225009, China
| | - Youjun Lu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100101, China
- School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, 100049, China
| | - Wei-Tou Ni
- International Centre for Theoretical Physics Asia-Pacific, University of Chinese Academy of Sciences, Beijing 100049, China
- State Key Laboratory of Magnetic Resonance and Atomic and Molecular Physics, Innovation Academy for Precision Measurement Science and Technology (APM), Chinese Academy of Sciences, Wuhan 430071, China
| | - Wen-Hong Ruan
- School of Fundamental Physics and Mathematical Sciences, Hangzhou Institute for Advanced Study, University of Chinese Academy of Sciences, Hangzhou 310024, China
- School of Physical Sciences, University of Chinese Academy of Sciences, Beijing 100049, China
| | - Naoki Seto
- Department of Physics, Kyoto University, Kyoto 606–8502, Japan
| | - Gang Wang
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, 200030, China
| | - Yue-Liang Wu
- CAS Key Laboratory of Theoretical Physics, Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing 100190, China
- School of Fundamental Physics and Mathematical Sciences, Hangzhou Institute for Advanced Study, University of Chinese Academy of Sciences, Hangzhou 310024, China
- International Centre for Theoretical Physics Asia-Pacific, Beijing/Hangzhou, China
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Stegmann J, Zwick L, Vermeulen SM, Antonini F, Mayer L. Imprints of massive black-hole binaries on neighbouring decihertz gravitational-wave sources. NATURE ASTRONOMY 2024; 8:1321-1331. [PMID: 39430610 PMCID: PMC11486661 DOI: 10.1038/s41550-024-02338-0] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 01/31/2024] [Accepted: 07/12/2024] [Indexed: 10/22/2024]
Abstract
The most massive black holes in our Universe form binaries at the centre of merging galaxies. The recent evidence for a gravitational-wave (GW) background from pulsar timing may constitute the first observation that these supermassive black-hole binaries (SMBHBs) merge. Yet, the most massive SMBHBs are out of reach of interferometric GW detectors and are exceedingly difficult to resolve individually with pulsar timing. These limitations call for unexplored strategies to detect individual SMBHBs in the uncharted frequency band ≲10-5 Hz to establish their abundance and decipher the coevolution with their host galaxies. Here we show that SMBHBs imprint detectable long-term modulations on GWs from stellar-mass binaries residing in the same galaxy at a distance d ≲ 1 kpc. We determine that proposed decihertz GW interferometers sensitive to numerous stellar-mass binaries could uncover modulations from ~O(10-1-104) SMBHBs with masses ~O(107-108) M⊙out to redshift z ≈ 3.5. This offers a unique opportunity to map the population of SMBHBs through cosmic time, which might remain inaccessible otherwise.
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Affiliation(s)
- Jakob Stegmann
- Max Planck Institute for Astrophysics, Garching, Germany
- Gravity Exploration Institute, School of Physics and Astronomy, Cardiff University, Cardiff, UK
| | - Lorenz Zwick
- Niels Bohr International Academy, Niels Bohr Institute, Copenhagen, Denmark
- Center for Theoretical Astrophysics and Cosmology, Institute for Computational Science, University of Zurich, Zurich, Switzerland
| | - Sander M. Vermeulen
- Gravity Exploration Institute, School of Physics and Astronomy, Cardiff University, Cardiff, UK
- California Institute of Technology, Department of Physics, Pasadena, CA USA
| | - Fabio Antonini
- Gravity Exploration Institute, School of Physics and Astronomy, Cardiff University, Cardiff, UK
| | - Lucio Mayer
- Center for Theoretical Astrophysics and Cosmology, Institute for Computational Science, University of Zurich, Zurich, Switzerland
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Charisi M, Taylor SR, Witt CA, Runnoe J. Efficient Large-Scale, Targeted Gravitational-Wave Probes of Supermassive Black-Hole Binaries. PHYSICAL REVIEW LETTERS 2024; 132:061401. [PMID: 38394573 DOI: 10.1103/physrevlett.132.061401] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/05/2023] [Revised: 10/27/2023] [Accepted: 11/21/2023] [Indexed: 02/25/2024]
Abstract
Binary systems of supermassive black holes are promising sources of low-frequency gravitational waves (GWs) and bright electromagnetic emission. Pulsar timing array GW searches for individual binaries have been limited to only a few candidate systems due to computational demands, which get worse as more pulsars are added. By modeling the GW signal using only components from when the GW passes Earth (rather than also each pulsar), we find constraints on the binary's total mass and GW frequency that are similar to a full signal analysis, yet ∼70 times more efficient.
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Affiliation(s)
- Maria Charisi
- Department of Physics and Astronomy, Vanderbilt University, 2301 Vanderbilt Place, Nashville, Tennessee 37235, USA
| | - Stephen R Taylor
- Department of Physics and Astronomy, Vanderbilt University, 2301 Vanderbilt Place, Nashville, Tennessee 37235, USA
| | - Caitlin A Witt
- Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, Evanston, Illinois 60208, USA
- Adler Planetarium, 1300 S. DuSable Lake Shore Drive, Chicago, Illinois 60605, USA
| | - Jessie Runnoe
- Department of Physics and Astronomy, Vanderbilt University, 2301 Vanderbilt Place, Nashville, Tennessee 37235, USA
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Chen YC, Liu X, Foord A, Shen Y, Oguri M, Chen N, Di Matteo T, Holgado M, Hwang HC, Zakamska N. A close quasar pair in a disk-disk galaxy merger at z = 2.17. Nature 2023; 616:45-49. [PMID: 37020007 DOI: 10.1038/s41586-023-05766-6] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/13/2022] [Accepted: 01/26/2023] [Indexed: 04/07/2023]
Abstract
Galaxy mergers produce pairs of supermassive black holes (SMBHs), which may be witnessed as dual quasars if both SMBHs are rapidly accreting. The kiloparsec (kpc)-scale separation represents a physical regime sufficiently close for merger-induced effects to be important1 yet wide enough to be directly resolvable with the facilities currently available. Whereas many kpc-scale, dual active galactic nuclei-the low-luminosity counterparts of quasars-have been observed in low-redshift mergers2, no unambiguous dual quasar is known at cosmic noon (z ≈ 2), the peak of global star formation and quasar activity3,4. Here we report multiwavelength observations of Sloan Digital Sky Survey (SDSS) J0749 + 2255 as a kpc-scale, dual-quasar system hosted by a galaxy merger at cosmic noon (z = 2.17). We discover extended host galaxies associated with the much brighter compact quasar nuclei (separated by 0.46″ or 3.8 kpc) and low-surface-brightness tidal features as evidence for galactic interactions. Unlike its low-redshift and low-luminosity counterparts, SDSS J0749 + 2255 is hosted by massive compact disk-dominated galaxies. The apparent lack of stellar bulges and the fact that SDSS J0749 + 2255 already follows the local SMBH mass-host stellar mass relation, suggest that at least some SMBHs may have formed before their host stellar bulges. While still at kpc-scale separations where the host-galaxy gravitational potential dominates, the two SMBHs may evolve into a gravitationally bound binary system in around 0.22 Gyr.
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Affiliation(s)
- Yu-Ching Chen
- Department of Astronomy, University of Illinois at Urbana-Champaign, Urbana, IL, USA
- National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Champaign, IL, USA
| | - Xin Liu
- Department of Astronomy, University of Illinois at Urbana-Champaign, Urbana, IL, USA.
- National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Champaign, IL, USA.
| | - Adi Foord
- Kavli Institute of Particle Astrophysics and Cosmology, Stanford University, Stanford, CA, USA
| | - Yue Shen
- Department of Astronomy, University of Illinois at Urbana-Champaign, Urbana, IL, USA
- National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Champaign, IL, USA
| | - Masamune Oguri
- Center for Frontier Science, Chiba University, Chiba, Japan
- Department of Physics, Graduate School of Science, Chiba University, Chiba, Japan
| | - Nianyi Chen
- McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, Pittsburgh, PA, USA
| | - Tiziana Di Matteo
- McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, Pittsburgh, PA, USA
- NSF AI Planning Institute for Physics of the Future, Carnegie Mellon University, Pittsburgh, PA, USA
- OzGrav-Melbourne, Australian Research Council Centre of Excellence for Gravitational Wave Discovery, Melbourne, Victoria, Australia
| | - Miguel Holgado
- McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, Pittsburgh, PA, USA
| | - Hsiang-Chih Hwang
- School of Natural Sciences, Institute for Advanced Study, Princeton, NJ, USA
| | - Nadia Zakamska
- Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD, USA
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The Role of AGN in Luminous Infrared Galaxies from the Multiwavelength Perspective. UNIVERSE 2022. [DOI: 10.3390/universe8080392] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
Galaxy mergers provide a mechanism for galaxies to effectively funnel gas and materials toward their nuclei and fuel the central starbursts and accretion of supermassive black holes. In turn, the active nuclei drive galactic-scale outflows that subsequently impact the evolution of the host galaxies. The details of this transformative process as they pertain to the supermassive black holes remain ambiguous, partially due to the central obscuration commonly found in the dust-reddened merger hosts, and also because there are relatively few laboratories in the nearby universe where the process can be studied in depth. This review highlights the current state of the literature on the role of accreting supermassive black holes in local luminous infrared galaxies as seen from various windows within the electromagnetic spectrum. Specifically, we discuss the multiwavelength signatures of the active nucleus, its associated feeding and feedback processes, and the implications of multiple supermassive black holes found in nearby interacting galaxy systems for galaxy evolution from the observational perspective. We conclude with a future outlook on how the topic of active nuclei in low- and high-redshift galaxy mergers will benefit from the advent of next-generation observing facilities with unparalleled resolving power and sensitivity in the coming decade.
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