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Mentasti G, Contaldi CR, Peloso M. Intrinsic Limits on the Detection of the Anisotropies of the Stochastic Gravitational Wave Background. PHYSICAL REVIEW LETTERS 2023; 131:221403. [PMID: 38101358 DOI: 10.1103/physrevlett.131.221403] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/26/2023] [Revised: 07/19/2023] [Accepted: 10/31/2023] [Indexed: 12/17/2023]
Abstract
For any given network of detectors, and for any given integration time, even in the idealized limit of negligible instrumental noise, the intrinsic time variation of the isotropic component of the stochastic gravitational wave background (SGWB) induces a limit on how accurately the anisotropies in the SGWB can be measured. We show here how this sample limit can be calculated and apply this to three separate configurations of ground-based detectors placed at existing and planned sites. Our results show that in the idealized, best-case scenario, individual multipoles of the anisotropies at ℓ≤8 can only be measured to ∼10^{-5}-10^{-4} level over five years of observation as a fraction of the isotropic component. As the sensitivity improves as the square root of the observation time, this poses a very serious challenge for measuring the anisotropies of SGWB of cosmological origin, even in the case of idealized detectors with arbitrarily low instrumental noise.
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Affiliation(s)
- Giorgio Mentasti
- Blackett Laboratory, Imperial College London, SW7 2AZ, London, United Kingdom
| | - Carlo R Contaldi
- Blackett Laboratory, Imperial College London, SW7 2AZ, London, United Kingdom
| | - Marco Peloso
- Dipartimento di Fisica e Astronomia "Galileo Galilei", Università di Padova, 35131 Padova, Italy and INFN, Sezione di Padova, 35131 Padova, Italy
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2
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Valbusa Dall'Armi L, Nishizawa A, Ricciardone A, Matarrese S. Circular Polarization of the Astrophysical Gravitational Wave Background. PHYSICAL REVIEW LETTERS 2023; 131:041401. [PMID: 37566858 DOI: 10.1103/physrevlett.131.041401] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/25/2023] [Revised: 05/08/2023] [Accepted: 06/29/2023] [Indexed: 08/13/2023]
Abstract
The circular polarization of gravitational waves is a powerful observable to test parity violation in gravity and to distinguish between the primordial or the astrophysical origin of the stochastic background. This property comes from the expected unpolarized nature of the homogeneous and isotropic astrophysical background, contrary to some specific cosmological sources that can produce a polarized background. However, in this work we show that there is also a non-negligible amount of circular polarization in the astrophysical background, generated by Poisson fluctuations in the number of unresolved sources, which is present in the third-generation interferometers with signal-to-noise ratio larger than 2. We also explain in which cases the gravitational wave maps can be cleaned from this extra source of noise, exploiting the frequency and the angular dependence, in order to search for signals from the early Universe. Future studies about the detection of polarized cosmological backgrounds with ground- and space-based interferometers should account for the presence of such a foreground contribution.
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Affiliation(s)
- L Valbusa Dall'Armi
- Dipartimento di Fisica e Astronomia "G. Galilei", Università degli Studi di Padova, via Marzolo 8, I-35131 Padova, Italy
- INFN, Sezione di Padova, via Marzolo 8, I-35131 Padova, Italy
| | - A Nishizawa
- Research Center for the Early Universe (RESCEU), School of Science, The University of Tokyo, Tokyo 113-0033, Japan
| | - A Ricciardone
- Dipartimento di Fisica e Astronomia "G. Galilei", Università degli Studi di Padova, via Marzolo 8, I-35131 Padova, Italy
- INFN, Sezione di Padova, via Marzolo 8, I-35131 Padova, Italy
- Dipartimento di Fisica "E. Fermi," Università di Pisa, I-56127 Pisa, Italy
| | - S Matarrese
- Dipartimento di Fisica e Astronomia "G. Galilei", Università degli Studi di Padova, via Marzolo 8, I-35131 Padova, Italy
- INFN, Sezione di Padova, via Marzolo 8, I-35131 Padova, Italy
- INFN, Sezione di Padova, via Marzolo 8, I-35131 Padova, Italy
- Gran Sasso Science Institute, Viale F. Crispi 7, I-67100 L'Aquila, Italy
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Caldwell R, Cui Y, Guo HK, Mandic V, Mariotti A, No JM, Ramsey-Musolf MJ, Sakellariadou M, Sinha K, Wang LT, White G, Zhao Y, An H, Bian L, Caprini C, Clesse S, Cline JM, Cusin G, Fornal B, Jinno R, Laurent B, Levi N, Lyu KF, Martinez M, Miller AL, Redigolo D, Scarlata C, Sevrin A, Haghi BSE, Shu J, Siemens X, Steer DA, Sundrum R, Tamarit C, Weir DJ, Xie KP, Yang FW, Zhou S. Detection of early-universe gravitational-wave signatures and fundamental physics. GENERAL RELATIVITY AND GRAVITATION 2022; 54:156. [PMID: 36465478 PMCID: PMC9712380 DOI: 10.1007/s10714-022-03027-x] [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: 04/23/2022] [Accepted: 10/20/2022] [Indexed: 06/17/2023]
Abstract
Detection of a gravitational-wave signal of non-astrophysical origin would be a landmark discovery, potentially providing a significant clue to some of our most basic, big-picture scientific questions about the Universe. In this white paper, we survey the leading early-Universe mechanisms that may produce a detectable signal-including inflation, phase transitions, topological defects, as well as primordial black holes-and highlight the connections to fundamental physics. We review the complementarity with collider searches for new physics, and multimessenger probes of the large-scale structure of the Universe.
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Affiliation(s)
- Robert Caldwell
- Department of Physics and Astronomy, Dartmouth College, Hanover, NH 03755 USA
| | - Yanou Cui
- Department of Physics and Astronomy, University of California, Riverside, CA 92521 USA
| | - Huai-Ke Guo
- Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112 USA
| | - Vuk Mandic
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455 USA
| | - Alberto Mariotti
- Theoretische Natuurkunde and IIHE/ELEM, Vrije Universiteit Brussel, and International Solvay Institutes, Pleinlaan 2, 1050 Brussels, Belgium
| | - Jose Miguel No
- Instituto de Física Teórica UAM/CSIC, C/ Nicolás Cabrera 13- 15, Campus de Cantoblanco, 28049 Madrid, Spain
| | - Michael J. Ramsey-Musolf
- Tsung Dao Lee Institute/Shanghai Jiao Tong University, Shanghai, 200120 People’s Republic of China
- University of Massachusetts, Amherst, MA 01003 USA
| | | | - Kuver Sinha
- Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019 USA
| | - Lian-Tao Wang
- Department of Physics, University of Chicago, Chicago, IL 60637 USA
| | - Graham White
- Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583 Japan
| | - Yue Zhao
- Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112 USA
| | - Haipeng An
- Department of Physics, Tsinghua University, Beijing, 100084 People’s Republic of China
- Center for High Energy Physics, Tsinghua University, Beijing, 100084 People’s Republic of China
- Center for High Energy Physics, Peking University, Beijing, 100871 People’s Republic of China
| | - Ligong Bian
- Center for High Energy Physics, Peking University, Beijing, 100871 People’s Republic of China
- Department of Physics and Chongqing Key Laboratory for Strongly Coupled Physics, Chongqing University, Chongqing, 401331 People’s Republic of China
| | - Chiara Caprini
- Theoretical Physics Department, University of Geneva, 1211 Geneva, Switzerland
- CERN, Theoretical Physics Department, 1 Esplanade des Particules, 1211 Genève 23, Switzerland
| | - Sebastien Clesse
- Service de Physique Théorique (CP225), University of Brussels (ULB), Boulevard du Triomphe, 1050 Brussels, Belgium
| | - James M. Cline
- Department of Physics, McGill University, Montréal, QC H3A2T8 Canada
| | - Giulia Cusin
- Theoretical Physics Department, University of Geneva, 1211 Geneva, Switzerland
- Sorbonne Université, CNRS, UMR 7095, Institut d’Astrophysique de Paris, 75014 Paris, France
| | - Bartosz Fornal
- Department of Chemistry and Physics, Barry University, Miami Shores, FL 33161 USA
| | - Ryusuke Jinno
- Instituto de Física Teórica UAM/CSIC, C/ Nicolás Cabrera 13- 15, Campus de Cantoblanco, 28049 Madrid, Spain
| | - Benoit Laurent
- Department of Physics, McGill University, Montréal, QC H3A2T8 Canada
| | - Noam Levi
- Raymond and Beverly Sackler School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv, 69978 Israel
| | - Kun-Feng Lyu
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455 USA
| | - Mario Martinez
- Institut de Física d’Altes Energies, Barcelona Institute of Science and Technology and ICREA, 08193 Barcelona, Spain
| | - Andrew L. Miller
- Université catholique de Louvain, 1348 Louvain-la-Neuve, Belgium
| | - Diego Redigolo
- INFN, Sezione di Firenze Via G. Sansone 1, 50019 Sesto Fiorentino, Italy
| | - Claudia Scarlata
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455 USA
| | - Alexander Sevrin
- Theoretische Natuurkunde and IIHE/ELEM, Vrije Universiteit Brussel, and International Solvay Institutes, Pleinlaan 2, 1050 Brussels, Belgium
| | - Barmak Shams Es Haghi
- Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112 USA
| | - Jing Shu
- CAS Key Laboratory of Theoretical Physics, Insitute of Theoretical Physics, Chinese Academy of Sciences, Beijing, 100190 People’s Republic of China
- School of Physical Sciences, University of Chinese Academy of Sciences, Beijing, 100049 People’s Republic of China
- School of Fundamental Physics and Mathematical Sciences, Hangzhou Institute for Advanced Study, University of Chinese Academy of Sciences, Hangzhou, 310024 People’s Republic of China
- International Center for Theoretical Physics Asia-Pacific, Beijing, Hanzhou, People’s Republic of China
| | - Xavier Siemens
- Department of Physics, Oregon State University, Corvallis, OR 97331 USA
| | - Danièle A. Steer
- Laboratoire Astroparticule et Cosmologie, CNRS, Université Paris Cité, 75013 Paris, France
| | | | - Carlos Tamarit
- Physik-Department T70, Technische Universität München, James-Franck-Straße, 85748 Garching, Germany
| | - David J. Weir
- Department of Physics and Helsinki Institute of Physics, University of Helsinki, P.O. Box 64, 00014 Helsinki, Finland
| | - Ke-Pan Xie
- Department of Physics and Astronomy, University of Nebraska, Lincoln, NE 68588 USA
| | - Feng-Wei Yang
- Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112 USA
| | - Siyi Zhou
- Department of Physics, Kobe University, Kobe, 657-8501 Japan
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Detectability of the Cross-Correlation between CMB Lensing and Stochastic GW Background from Compact Object Mergers. UNIVERSE 2022. [DOI: 10.3390/universe8030160] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 01/27/2023]
Abstract
The anisotropies of the Stochastic Gravitational-Wave Background (SGWB), produced by merging compact binaries, constitute a possible new probe of the Large-Scale Structure (LSS). However, the significant shot noise contribution caused by the discreteness of the GW sources and the poor angular resolution of the instruments hampers the detection of the intrinsic anisotropies induced by the LSS. In this work, we investigate the potential of cross-correlating forthcoming high precision measurements of the SGWB energy density and the Cosmic Microwave Background (CMB) lensing convergence to mitigate the effect of shot noise. Combining a detailed model of stellar and galactic astrophysics with a novel framework to distribute the GW emitters in the sky, we compute the auto- and cross-correlation power spectra for the two cosmic fields, evaluate the shot noise contribution and predict the signal-to-noise ratio. The results of our analysis show that the SGWB energy density correlates significantly with the CMB lensing convergence and that the cross-correlation between these two cosmic fields reduces the impact of instrumental and shot noise. Unfortunately, the S/N is not high enough to detect the intrinsic SGWB anisotropies. Nevertheless, a network composed of both present and future generation GW interferometers, operating for at least 10 yrs, should be able to measure the shot noise contribution.
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