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

被引：8

作者：

Gupta, Ish ^{[1
]}

Afle, Chaitanya ^{[2
]}

Arun, K. G. ^{[1
,3
]}

Bandopadhyay, Ananya ^{[2
]}

Baryakhtar, Masha ^{[4
]}

Biscoveanu, Sylvia ^{[5
]}

Borhanian, Ssohrab ^{[6
]}

Broekgaarden, Floor ^{[7
]}

Corsi, Alessandra ^{[8
]}

Dhani, Arnab ^{[9
]}

Evans, Matthew ^{[5
]}

Hall, Evan D. ^{[5
]}

Hannuksela, Otto A. ^{[10
]}

Kacanja, Keisi ^{[2
]}

Kashyap, Rahul ^{[1
]}

Khadkikar, Sanika ^{[1
]}

Kuns, Kevin ^{[5
]}

Li, Tjonnie G. F. ^{[11
,12
]}

Miller, Andrew L. ^{[13
,14
]}

Nitz, Alexander Harvey ^{[2
]}

Owen, Benjamin J. ^{[8
]}

Palomba, Cristiano ^{[15
]}

Pearce, Anthony ^{[8
]}

Phurailatpam, Hemantakumar ^{[10
]}

Rajbhandari, Binod ^{[8
]}

Read, Jocelyn ^{[16
]}

Romano, Joseph D. ^{[8
]}

Sathyaprakash, Bangalore S. ^{[1
,17
]}

Shoemaker, David H. ^{[5
]}

Singh, Divya ^{[1
]}

Vitale, Salvatore ^{[5
]}

Barsotti, Lisa ^{[5
]}

Berti, Emanuele ^{[18
]}

Cahillane, Craig ^{[2
]}

Chen, Hsin-Yu ^{[19
]}

Fritschel, Peter ^{[5
]}

Haster, Carl-Johan ^{[20
]}

Landry, Philippe ^{[21
]}

Lovelace, Geoffrey ^{[16
]}

McClelland, David ^{[22
]}

Slagmolen, Bram J. J. ^{[22
]}

Smith, Joshua R. ^{[16
]}

Soares-Santos, Marcelle ^{[23
]}

Sun, Ling ^{[22
]}

Tanner, David ^{[24
]}

Yamamoto, Hiro ^{[25
]}

Zucker, Michael ^{[5
,25
]}

机构：

[1] Penn State Univ, Inst Gravitat & Cosmos, Dept Phys, University Pk, PA 16802 USA

[2] Syracuse Univ, Syracuse, NY USA

[3] Chennai Math Inst, Chennai, India

[4] UNIV WASHINGTON, Seattle, WA USA

[5] MIT CSAIL, Cambridge, MA USA

[6] Friedrich Schiller Univ Jena, Theoret Phys Inst, D-07743 Jena, Germany

[7] Harvard & Smithsonian, Ctr Astrophys, Batavia, IL 60510 USA

[8] Texas Tech Univ, Dept Phys & Astron, Lubbock, TX 79409 USA

[9] Albert Einstein Inst, Max Planck Inst Grav Phys, D-14476 Potsdam, Germany

[10] Chinese Univ Hong Kong, Dept Phys, Shatin, Hong Kong, Peoples R China

[11] Katholieke Univ Leuven, Inst Theoret Phys, Dept Phys & Astron, B-3001 Heverlee, Belgium

[12] Katholieke Univ Leuven, Dept Elect Engn ESAT, STADIUS, B-3001 Heverlee, Belgium

[13] Nikhef Natl Inst Subatom Phys, NL-1098 XG Amsterdam, Netherlands

[14] Univ Utrecht, Inst Gravitat & Subatom Phys, NL-3584 CC Utrecht, Netherlands

[15] Ist Nazl Fis Nucl, Sez Roma, Rome, Italy

[16] Calif State Univ Fullerton, Nicholas & Lee Begovich Ctr Gravitat Wave Phys & A, Fullerton, CA 92831 USA

[17] Univ Wales Coll Cardiff, Cardiff CF24 3AA, Wales

[18] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[19] Univ Texas Austin, Dept Phys, Austin, TX 78712 USA

[20] Univ Nevada, Las Vegas, NV USA

[21] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada

[22] Australian Natl Univ, Canberra, 2601, Australia

[23] Univ Michigan, Ann Arbor, ND 48109 USA

[24] Univ Florida, Dept Phys, Gainesville, FL 32611 USA

[25] CALTECH, LIGO Lab, Pasadena, CA 91125 USA

来源：

CLASSICAL AND QUANTUM GRAVITY | 2024年 / 41卷 / 24期

基金：

澳大利亚研究理事会;

关键词：

cosmic explorer; Einstein telescope; gravitational waves; next generation; GAMMA-RAY BURST; ACCRETING NEUTRON-STARS; RADIO FLARES; BLACK-HOLES; RADIATION; EMISSION; KILONOVA; PULSAR; NUCLEOSYNTHESIS; COUNTERPART;

D O I：

10.1088/1361-6382/ad7b99

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.

引用

页数：68

共 250 条

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