Characterizing gravitational wave detector networks: from A# to cosmic explorer

Ish Gupta; Chaitanya Afle; K. G. Arun; Ananya Bandopadhyay; Masha Baryakhtar; Sylvia Biscoveanu; Ssohrab Borhanian; Floor Broekgaarden; Alessandra Corsi; Arnab Dhani; Matthew Evans; Evan D. Hall; Otto A. Hannuksela; Keisi Kacanja; Rahul Kashyap; Sanika Khadkikar; Kevin Kuns; Tjonnie G.F. Li; Andrew L. Miller; Alexander Harvey Nitz; Benjamin J. Owen; Cristiano Palomba; Anthony Pearce; Hemantakumar Phurailatpam; Binod Rajbhandari; Jocelyn Read; Joseph D. Romano; Bangalore S. Sathyaprakash; David H. Shoemaker; Divya Singh; Salvatore Vitale; Lisa Barsotti; Emanuele Berti; Craig Cahillane; Hsin Yu Chen; Peter Fritschel; Carl Johan Haster; Philippe Landry; Geoffrey Lovelace; David McClelland; Bram J.J. Slagmolen; Joshua R. Smith; Marcelle Soares-Santos; Ling Sun; David Tanner; Hiro Yamamoto; Michael Zucker

doi:10.1088/1361-6382/ad7b99

Characterizing gravitational wave detector networks: from A^# to cosmic explorer

Ish Gupta^*, Chaitanya Afle, K. G. Arun, Ananya Bandopadhyay, Masha Baryakhtar, Sylvia Biscoveanu, Ssohrab Borhanian, Floor Broekgaarden, Alessandra Corsi, Arnab Dhani, Matthew Evans, Evan D. Hall, Otto A. Hannuksela, Keisi Kacanja, Rahul Kashyap, Sanika Khadkikar, Kevin Kuns, Tjonnie G.F. Li, Andrew L. Miller, Alexander Harvey NitzBenjamin J. Owen, Cristiano Palomba, Anthony Pearce, Hemantakumar Phurailatpam, Binod Rajbhandari, Jocelyn Read, Joseph D. Romano, Bangalore S. Sathyaprakash, David H. Shoemaker, Divya Singh, Salvatore Vitale, Lisa Barsotti, Emanuele Berti, Craig Cahillane, Hsin Yu Chen, Peter Fritschel, Carl Johan Haster, Philippe Landry, Geoffrey Lovelace, David McClelland, Bram J.J. Slagmolen, Joshua R. Smith, Marcelle Soares-Santos, Ling Sun, David Tanner, Hiro Yamamoto, Michael Zucker

^*Corresponding author for this work

Research output: Contribution to journal › Article › Academic › peer-review

Abstract

Gravitational-wave observations by the laser interferometer gravitational-wave observatory (LIGO) and Virgo have provided us a new tool to explore the Universe on all scales from nuclear physics to the cosmos and have the massive potential to further impact fundamental physics, astrophysics, and cosmology for decades to come. In this paper we have studied the science capabilities of a network of LIGO detectors when they reach their best possible sensitivity, called A^#, given the infrastructure in which they exist and a new generation of observatories that are factor of 10 to 100 times more sensitive (depending on the frequency), in particular a pair of L-shaped cosmic explorer (CE) observatories (one 40 km and one 20 km arm length) in the US and the triangular Einstein telescope with 10 km arms in Europe. We use a set of science metrics derived from the top priorities of several funding agencies to characterize the science capabilities of different networks. The presence of one or two A^# observatories in a network containing two or one next generation observatories, respectively, will provide good localization capabilities for facilitating multimessenger astronomy (MMA) and precision measurement of the Hubble parameter. Two CE observatories are indispensable for achieving precise localization of binary neutron star events, facilitating detection of electromagnetic counterparts and transforming MMA. Their combined operation is even more important in the detection and localization of high-redshift sources, such as binary neutron stars, beyond the star-formation peak, and primordial black hole mergers, which may occur roughly 100 million years after the Big Bang. The addition of the Einstein Telescope to a network of two CE observatories is critical for accomplishing all the identified science metrics including the nuclear equation of state, cosmological parameters, the growth of black holes through cosmic history, but also make new discoveries such as the presence of dark matter within or around neutron stars and black holes, continuous gravitational waves from rotating neutron stars, transient signals from supernovae, and the production of stellar-mass black holes in the early Universe. For most metrics the triple network of next generation terrestrial observatories are a factor 100 better than what can be accomplished by a network of three A^# observatories.

Original language	English
Article number	245001
Journal	Classical and Quantum Gravity
Volume	41
Issue number	24
DOIs	https://doi.org/10.1088/1361-6382/ad7b99
Publication status	Published - 19 Dec 2024

Bibliographical note

Publisher Copyright:
© 2024 The Author(s).

Funding

We thank the members of the Cosmic Explorer Project and the Scientific Advisory Committee for their input and feedback. We thank Kara Merfeld for pointing out the omission of the assumption for binary neutron stars that leads to more mass-symmetric binaries. I G, A D, B S S, R K, and D S were supported by NSF Grant Numbers AST-2006384, AST-2307147, PHY-2012083, PHY-2207638, PHY-2308886, and PHYS-2309064 to B.S.S. S B acknowledges support from the Deutsche Forschungsgemeinschaft, DFG, Project MEMI number BE 6301/2-1. K G A acknowledges support from the Department of Science and Technology and Science and Engineering Research Board (SERB) of India via the following grants: Swarnajayanti Fellowship Grant DST/SJF/PSA-01/2017-18 and Core Research Grant CRG/2021/004565 K G A, E B and B S S acknowledge the support of the Indo-US Science and Technology Forum through the Indo-US Centre for Gravitational-Physics and Astronomy, grant IUSSTF/JC-142/2019. A B and K K acknowledge support from NSF award PHY-2207264. E B is supported by NSF Grants No. AST-2006538, PHY-2207502, PHY-090003 and PHY-20043, and by NASA Grant Nos. 20-LPS20-0011 and 21-ATP21-0010. E B acknowledges support from the ITA-USA Science and Technology Cooperation program (CUP: D13C23000290001), supported by the Ministry of Foreign Affairs of Italy (MAECI). M B acknowledges support from DOE under Award Number DE- SC0022348 G L acknowledges NSF award PHY-2208014, Nicholas and Lee Begovich, and the Dan Black Family Trust. A Corsi acknowledges support from NSF grant PHYS-2011608. AHN acknowledges support from NSF grant PHY-2309240. OAH and HP acknowledge support by grants from the Research Grants Council of Hong Kong (Project Nos. CUHK 2130822 and 4443086), and the Direct Grant for Research from the Research Committee of The Chinese University of Hong Kong. T G F L acknowledge support by grants from the Research Foundation-Flanders (G086722N, I002123N) and KU Leuven (STG/21/061). D E M, B J J S, and L S acknowledge the support of the Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), Project No. CE170100004. C P acknowledges research support from the Italian Istituto Nazionale di Fisica Nucleare (INFN). B J O, A P, and B R acknowledge support from NSF grants PHY-1912625, PHY-2309305, and AST-1907975. JDR acknowledges support from NSF grant PHY-2207270. J R S and G L acknowledge support from NSF Grant 2308985, Nicholas and Lee Begovich, and the Dan Black Family Trust. S V acknowledges support from NSF award PHY-2207387.

Funders	Funder number
High Energy Physicshttp://dx.doi.org/10.13039/100006208	PHY-2207387
NSF	BE 6301/2-1
Deutsche Forschungsgemeinschaft, DFG	DST/SJF/PSA-01/2017-18, CRG/2021/004565 K G A
Department of Science and Technology and Science and Engineering Research Board (SERB) of India	IUSSTF/JC-142/2019
Indo-US Science and Technology Forum through the Indo-US Centre for Gravitational-Physics and Astronomy	20-LPS20-0011, 21-ATP21-0010
NASA	CUP: D13C23000290001
ITA-USA Science and Technology Cooperation program
Ministry of Foreign Affairs of Italy (MAECI)	DE- SC0022348
DOE
Dan Black Family Trust	CUHK 2130822, 4443086
Research Grants Council of Hong Kong
Direct Grant for Research from the Research Committee of The Chinese University of Hong Kong	G086722N, I002123N
Research Foundation-Flanders	STG/21/061
KU Leuven	CE170100004
Australian Research Council Centre of Excellence for Gravitational Wave Discovery
Italian Istituto Nazionale di Fisica Nucleare (INFN)

Keywords

cosmic explorer
Einstein telescope
gravitational waves
next generation

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Cite this

Gupta, I., Afle, C., Arun, K. G., Bandopadhyay, A., Baryakhtar, M., Biscoveanu, S., Borhanian, S., Broekgaarden, F., Corsi, A., Dhani, A., Evans, M., Hall, E. D., Hannuksela, O. A., Kacanja, K., Kashyap, R., Khadkikar, S., Kuns, K., Li, T. G. F., Miller, A. L., ... Zucker, M. (2024). Characterizing gravitational wave detector networks: from A^# to cosmic explorer. Classical and Quantum Gravity, 41(24), Article 245001. https://doi.org/10.1088/1361-6382/ad7b99

@article{904d8979df2a4ff3aa6b25f8afbbcc55,

title = "Characterizing gravitational wave detector networks: from A\# to cosmic explorer",

abstract = "Gravitational-wave observations by the laser interferometer gravitational-wave observatory (LIGO) and Virgo have provided us a new tool to explore the Universe on all scales from nuclear physics to the cosmos and have the massive potential to further impact fundamental physics, astrophysics, and cosmology for decades to come. In this paper we have studied the science capabilities of a network of LIGO detectors when they reach their best possible sensitivity, called A\#, given the infrastructure in which they exist and a new generation of observatories that are factor of 10 to 100 times more sensitive (depending on the frequency), in particular a pair of L-shaped cosmic explorer (CE) observatories (one 40 km and one 20 km arm length) in the US and the triangular Einstein telescope with 10 km arms in Europe. We use a set of science metrics derived from the top priorities of several funding agencies to characterize the science capabilities of different networks. The presence of one or two A\# observatories in a network containing two or one next generation observatories, respectively, will provide good localization capabilities for facilitating multimessenger astronomy (MMA) and precision measurement of the Hubble parameter. Two CE observatories are indispensable for achieving precise localization of binary neutron star events, facilitating detection of electromagnetic counterparts and transforming MMA. Their combined operation is even more important in the detection and localization of high-redshift sources, such as binary neutron stars, beyond the star-formation peak, and primordial black hole mergers, which may occur roughly 100 million years after the Big Bang. The addition of the Einstein Telescope to a network of two CE observatories is critical for accomplishing all the identified science metrics including the nuclear equation of state, cosmological parameters, the growth of black holes through cosmic history, but also make new discoveries such as the presence of dark matter within or around neutron stars and black holes, continuous gravitational waves from rotating neutron stars, transient signals from supernovae, and the production of stellar-mass black holes in the early Universe. For most metrics the triple network of next generation terrestrial observatories are a factor 100 better than what can be accomplished by a network of three A\# observatories.",

keywords = "cosmic explorer, Einstein telescope, gravitational waves, next generation",

author = "Ish Gupta and Chaitanya Afle and Arun, \{K. G.\} and Ananya Bandopadhyay and Masha Baryakhtar and Sylvia Biscoveanu and Ssohrab Borhanian and Floor Broekgaarden and Alessandra Corsi and Arnab Dhani and Matthew Evans and Hall, \{Evan D.\} and Hannuksela, \{Otto A.\} and Keisi Kacanja and Rahul Kashyap and Sanika Khadkikar and Kevin Kuns and Li, \{Tjonnie G.F.\} and Miller, \{Andrew L.\} and Nitz, \{Alexander Harvey\} and Owen, \{Benjamin J.\} and Cristiano Palomba and Anthony Pearce and Hemantakumar Phurailatpam and Binod Rajbhandari and Jocelyn Read and Romano, \{Joseph D.\} and Sathyaprakash, \{Bangalore S.\} and Shoemaker, \{David H.\} and Divya Singh and Salvatore Vitale and Lisa Barsotti and Emanuele Berti and Craig Cahillane and Chen, \{Hsin Yu\} and Peter Fritschel and Haster, \{Carl Johan\} and Philippe Landry and Geoffrey Lovelace and David McClelland and Slagmolen, \{Bram J.J.\} and Smith, \{Joshua R.\} and Marcelle Soares-Santos and Ling Sun and David Tanner and Hiro Yamamoto and Michael Zucker",

note = "Publisher Copyright: {\textcopyright} 2024 The Author(s).",

year = "2024",

month = dec,

day = "19",

doi = "10.1088/1361-6382/ad7b99",

language = "English",

volume = "41",

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Gupta, I, Afle, C, Arun, KG, Bandopadhyay, A, Baryakhtar, M, Biscoveanu, S, Borhanian, S, Broekgaarden, F, Corsi, A, Dhani, A, Evans, M, Hall, ED, Hannuksela, OA, Kacanja, K, Kashyap, R, Khadkikar, S, Kuns, K, Li, TGF, Miller, AL, Nitz, AH, Owen, BJ, Palomba, C, Pearce, A, Phurailatpam, H, Rajbhandari, B, Read, J, Romano, JD, Sathyaprakash, BS, Shoemaker, DH, Singh, D, Vitale, S, Barsotti, L, Berti, E, Cahillane, C, Chen, HY, Fritschel, P, Haster, CJ, Landry, P, Lovelace, G, McClelland, D, Slagmolen, BJJ, Smith, JR, Soares-Santos, M, Sun, L, Tanner, D, Yamamoto, H & Zucker, M 2024, 'Characterizing gravitational wave detector networks: from A^# to cosmic explorer', Classical and Quantum Gravity, vol. 41, no. 24, 245001. https://doi.org/10.1088/1361-6382/ad7b99

TY - JOUR

T1 - Characterizing gravitational wave detector networks

T2 - from A# to cosmic explorer

AU - Gupta, Ish

AU - Afle, Chaitanya

AU - Arun, K. G.

AU - Bandopadhyay, Ananya

AU - Baryakhtar, Masha

AU - Biscoveanu, Sylvia

AU - Borhanian, Ssohrab

AU - Broekgaarden, Floor

AU - Corsi, Alessandra

AU - Dhani, Arnab

AU - Evans, Matthew

AU - Hall, Evan D.

AU - Hannuksela, Otto A.

AU - Kacanja, Keisi

AU - Kashyap, Rahul

AU - Khadkikar, Sanika

AU - Kuns, Kevin

AU - Li, Tjonnie G.F.

AU - Miller, Andrew L.

AU - Nitz, Alexander Harvey

AU - Owen, Benjamin J.

AU - Palomba, Cristiano

AU - Pearce, Anthony

AU - Phurailatpam, Hemantakumar

AU - Rajbhandari, Binod

AU - Read, Jocelyn

AU - Romano, Joseph D.

AU - Sathyaprakash, Bangalore S.

AU - Shoemaker, David H.

AU - Singh, Divya

AU - Vitale, Salvatore

AU - Barsotti, Lisa

AU - Berti, Emanuele

AU - Cahillane, Craig

AU - Chen, Hsin Yu

AU - Fritschel, Peter

AU - Haster, Carl Johan

AU - Landry, Philippe

AU - Lovelace, Geoffrey

AU - McClelland, David

AU - Slagmolen, Bram J.J.

AU - Smith, Joshua R.

AU - Soares-Santos, Marcelle

AU - Sun, Ling

AU - Tanner, David

AU - Yamamoto, Hiro

AU - Zucker, Michael

PY - 2024/12/19

Y1 - 2024/12/19

N2 - Gravitational-wave observations by the laser interferometer gravitational-wave observatory (LIGO) and Virgo have provided us a new tool to explore the Universe on all scales from nuclear physics to the cosmos and have the massive potential to further impact fundamental physics, astrophysics, and cosmology for decades to come. In this paper we have studied the science capabilities of a network of LIGO detectors when they reach their best possible sensitivity, called A#, given the infrastructure in which they exist and a new generation of observatories that are factor of 10 to 100 times more sensitive (depending on the frequency), in particular a pair of L-shaped cosmic explorer (CE) observatories (one 40 km and one 20 km arm length) in the US and the triangular Einstein telescope with 10 km arms in Europe. We use a set of science metrics derived from the top priorities of several funding agencies to characterize the science capabilities of different networks. The presence of one or two A# observatories in a network containing two or one next generation observatories, respectively, will provide good localization capabilities for facilitating multimessenger astronomy (MMA) and precision measurement of the Hubble parameter. Two CE observatories are indispensable for achieving precise localization of binary neutron star events, facilitating detection of electromagnetic counterparts and transforming MMA. Their combined operation is even more important in the detection and localization of high-redshift sources, such as binary neutron stars, beyond the star-formation peak, and primordial black hole mergers, which may occur roughly 100 million years after the Big Bang. The addition of the Einstein Telescope to a network of two CE observatories is critical for accomplishing all the identified science metrics including the nuclear equation of state, cosmological parameters, the growth of black holes through cosmic history, but also make new discoveries such as the presence of dark matter within or around neutron stars and black holes, continuous gravitational waves from rotating neutron stars, transient signals from supernovae, and the production of stellar-mass black holes in the early Universe. For most metrics the triple network of next generation terrestrial observatories are a factor 100 better than what can be accomplished by a network of three A# observatories.

AB - Gravitational-wave observations by the laser interferometer gravitational-wave observatory (LIGO) and Virgo have provided us a new tool to explore the Universe on all scales from nuclear physics to the cosmos and have the massive potential to further impact fundamental physics, astrophysics, and cosmology for decades to come. In this paper we have studied the science capabilities of a network of LIGO detectors when they reach their best possible sensitivity, called A#, given the infrastructure in which they exist and a new generation of observatories that are factor of 10 to 100 times more sensitive (depending on the frequency), in particular a pair of L-shaped cosmic explorer (CE) observatories (one 40 km and one 20 km arm length) in the US and the triangular Einstein telescope with 10 km arms in Europe. We use a set of science metrics derived from the top priorities of several funding agencies to characterize the science capabilities of different networks. The presence of one or two A# observatories in a network containing two or one next generation observatories, respectively, will provide good localization capabilities for facilitating multimessenger astronomy (MMA) and precision measurement of the Hubble parameter. Two CE observatories are indispensable for achieving precise localization of binary neutron star events, facilitating detection of electromagnetic counterparts and transforming MMA. Their combined operation is even more important in the detection and localization of high-redshift sources, such as binary neutron stars, beyond the star-formation peak, and primordial black hole mergers, which may occur roughly 100 million years after the Big Bang. The addition of the Einstein Telescope to a network of two CE observatories is critical for accomplishing all the identified science metrics including the nuclear equation of state, cosmological parameters, the growth of black holes through cosmic history, but also make new discoveries such as the presence of dark matter within or around neutron stars and black holes, continuous gravitational waves from rotating neutron stars, transient signals from supernovae, and the production of stellar-mass black holes in the early Universe. For most metrics the triple network of next generation terrestrial observatories are a factor 100 better than what can be accomplished by a network of three A# observatories.

KW - cosmic explorer

KW - Einstein telescope

KW - gravitational waves

KW - next generation

UR - https://www.scopus.com/pages/publications/85209756709

U2 - 10.1088/1361-6382/ad7b99

DO - 10.1088/1361-6382/ad7b99

M3 - Article

AN - SCOPUS:85209756709

SN - 0264-9381

VL - 41

JO - Classical and Quantum Gravity

JF - Classical and Quantum Gravity

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