Paul Fulda

University of Florida

H-index: 109

North America-United States

About Paul Fulda

Paul Fulda, With an exceptional h-index of 109 and a recent h-index of 87 (since 2020), a distinguished researcher at University of Florida, specializes in the field of Gravitational waves.

His recent articles reflect a diverse array of research interests and contributions to the field:

GWTC-2.1: Deep extended catalog of compact binary coalescences observed by LIGO and Virgo during the first half of the third observing run

Tilt-to-length coupling calibration in the LISA mission: uncertainty and biases

Experimental demonstrations of alignment and mode matching in optical cavities with higher-order Hermite-Gauss modes

arXiv: Ultralight vector dark matter search using data from the KAGRA O3GK run

Ultralight vector dark matter search using data from the KAGRA O3GK run

LIGO operates with quantum noise below the Standard Quantum Limit

A joint Fermi-GBM and Swift-BAT analysis of Gravitational-wave candidates from the third Gravitational-wave Observing Run

Beam displacement tolerances on a segmented mirror for higher-order Hermite–Gauss modes

Paul Fulda Information

University	University of Florida
Position	___
Citations(all)	97256
Citations(since 2020)	71523
Cited By	54155
hIndex(all)	109
hIndex(since 2020)	87
i10Index(all)	218
i10Index(since 2020)	207
Email	Access Email
University Profile Page	University of Florida

Paul Fulda Skills & Research Interests

Gravitational waves

Top articles of Paul Fulda

GWTC-2.1: Deep extended catalog of compact binary coalescences observed by LIGO and Virgo during the first half of the third observing run

Authors

R Abbott,TD Abbott,F Acernese,K Ackley,C Adams,N Adhikari,RX Adhikari,VB Adya,C Affeldt,D Agarwal,M Agathos,K Agatsuma,N Aggarwal,OD Aguiar,L Aiello,A Ain,P Ajith,S Albanesi,A Allocca,PA Altin,A Amato,C Anand,S Anand,A Ananyeva,SB Anderson,WG Anderson,T Andrade,N Andres,T Andrić,SV Angelova,S Ansoldi,JM Antelis,S Antier,S Appert,K Arai,MC Araya,JS Areeda,M Arène,N Arnaud,SM Aronson,KG Arun,Y Asali,G Ashton,M Assiduo,SM Aston,P Astone,F Aubin,C Austin,S Babak,F Badaracco,MKM Bader,C Badger,S Bae,AM Baer,S Bagnasco,Y Bai,J Baird,M Ball,G Ballardin,SW Ballmer,A Balsamo,G Baltus,S Banagiri,D Bankar,JC Barayoga,C Barbieri,BC Barish,D Barker,P Barneo,F Barone,B Barr,L Barsotti,M Barsuglia,D Barta,J Bartlett,MA Barton,I Bartos,R Bassiri,A Basti,M Bawaj,JC Bayley,AC Baylor,M Bazzan,B Bécsy,VM Bedakihale,M Bejger,I Belahcene,V Benedetto,D Beniwal,TF Bennett,JD Bentley,M Benyaala,F Bergamin,BK Berger,S Bernuzzi,CPL Berry,D Bersanetti,A Bertolini,J Betzwieser,D Beveridge,R Bhandare,U Bhardwaj,D Bhattacharjee,S Bhaumik,IA Bilenko,G Billingsley,S Bini,R Birney,O Birnholtz,S Biscans,M Bischi,S Biscoveanu,A Bisht,B Biswas,M Bitossi,M-A Bizouard,JK Blackburn,CD Blair,DG Blair,RM Blair,F Bobba,N Bode,M Boer,G Bogaert,M Boldrini,LD Bonavena,F Bondu,E Bonilla,R Bonnand,P Booker,BA Boom,R Bork,V Boschi,N Bose,S Bose,V Bossilkov,V Boudart,Y Bouffanais,A Bozzi,C Bradaschia,PR Brady,A Bramley,A Branch,M Branchesi,JE Brau,M Breschi,T Briant,JH Briggs,A Brillet,M Brinkmann

Journal

Physical Review D

Published Date

2024/1/5

The second Gravitational-Wave Transient Catalog, GWTC-2, reported on 39 compact binary coalescences observed by the Advanced LIGO and Advanced Virgo detectors between 1 April 2019 15∶ 00 UTC and 1 October 2019 15∶ 00 UTC. Here, we present GWTC-2.1, which reports on a deeper list of candidate events observed over the same period. We analyze the final version of the strain data over this period with improved calibration and better subtraction of excess noise, which has been publicly released. We employ three matched-filter search pipelines for candidate identification, and estimate the probability of astrophysical origin for each candidate event. While GWTC-2 used a false alarm rate threshold of 2 per year, we include in GWTC-2.1, 1201 candidates that pass a false alarm rate threshold of 2 per day. We calculate the source properties of a subset of 44 high-significance candidates that have a …

Tilt-to-length coupling calibration in the LISA mission: uncertainty and biases

Authors

Marie-Sophie Hartig,Jose Sanjuan Munoz,Daniel George,Paul Fulda

Journal

Bulletin of the American Physical Society

Published Date

2024/4/6

R05. 00007: Tilt-to-length coupling calibration in the LISA mission: uncertainty and biases*

Experimental demonstrations of alignment and mode matching in optical cavities with higher-order Hermite-Gauss modes

Authors

Liu Tao,Paul Fulda

Journal

arXiv preprint arXiv:2310.14902

Published Date

2023/10/23

Higher-order spatial laser modes have recently been investigated as candidates for reducing test-mass thermal noise in ground-based gravitational-wave detectors such as advanced LIGO. In particular, higher-order Hermite-Gauss (HG) modes have gained attention within the community for their more robust behaviors against random test-mass surface deformations and stronger sensing and control capacities. In this letter we offer experimental investigations on various aspects of HG mode interferometry. We have generated purified HG modes up to the 12-th order mode, with a power conversion efficiency of 38.8% and 27.7% for the and modes respectively. We demonstrated for the first time the misalignment and mode mismatch-induced power coupling loss measurements for HG modes up to the . We report an excellent agreement with the extended numerical power loss factors that in the ``small power loss'' region converge to or for a misaligned or mode mismatched mode. We also demonstrated the wavefront sensing (WFS) signal measurement for HG modes up to the . The measurement result is accurately in accordance with theoretical WFS gain for an mode, with being the beat coefficient of the adjacent and modes on a split photodetector.

arXiv: Ultralight vector dark matter search using data from the KAGRA O3GK run

Authors

AG Abac,ML Chiofalo,G Nieradka,R Pegna,C North,R Bhandare,G Pierra,A Amato,JG Baier,D Chen,B Haskell,F Robinet,M Fyffe,M Arogeti,P Stevens,DD White,TF Davies,E Payne,M Wright,K Johansmeyer,K Hayama,P-F Cohadon,CG Collette,D Sellers,S Hoang,V Sipala,H Heitmann,T O'Hanlon,B Edelman,G McCarrol,AD Huddart,KD Sullivan,T Harder,A Garron,TA Clarke,YT Huang,J Junker,M Hennig,N Hirata,J Portell,R McCarthy,M Weinert,R Poulton,G Ballardin,D Bankar,A Bianchi,M Montani,CD Panzer,X Chen,R Takahashi,J Lange,K Schouteden,Yitian Chen,A Sasli,F Yang,LM Modafferi,ME Zucker,J O'Dell,D Lumaca,AP Spencer,M Millhouse,G Quéméner,M Norman,MJ Szczepańczyk,S-C Hsu,ST Countryman,C Chatterjee,AL James,KN Nagler,E Chassande-Mottin,W Kiendrebeogo,M Tacca,FJ Raab,TR Saravanan,VP Mitrofanov,S Bernuzzi,C Adamcewicz,L Conti,C Tong-Yu,J Golomb,X Li,A Perego,ERG von Reis,J Woehler,G Bogaert,F Fidecaro,B Shen,JM Ezquiaga,D Macri,V Juste,S Sachdev,JD Bentley,R Sturani,TP Lott IV,K Takatani,D Beniwal,U Dupletsa,A Boumerdassi,F Glotin,Y Lee,R Bhatt,A Couineaux,M Wade,N Kanda,J Novak,S Bini,I Ferrante,RA Alfaidi,N Johny,LE Sanchez,J Heinze,J Zhang,M Kinley-Hanlon,AJ Weinstein,T Sainrat,NN Janthalur,A Trovato,A Romero,K Tomita,DE McClelland,B Fornal,M Heurs,AM Gretarsson,A Chincarini,BB Lane,AE Romano,V Fafone,FY Khalili,F Linde,C Messick,A Heffernan,J Gargiulo,V JaberianHamedan,SW Reid,D Moraru,D Pathak,M Iwaya,G Grignani,T Yan,K AultONeal,SA Pai,Y Xu,IM Pinto,KW Chung,C Palomba,J Tissino,T Klinger,Ll M Mir,K Kwan,C Posnansky

Published Date

2024/3/5

Among the various candidates for dark matter (DM), ultralight vector DM can be probed by laser interferometric gravitational wave detectors through the measurement of oscillating length changes in the arm cavities. In this context, KAGRA has a unique feature due to differing compositions of its mirrors, enhancing the signal of vector DM in the length change in the auxiliary channels. Here we present the result of a search for U (1) B− L gauge boson DM using the KAGRA data from auxiliary length channels during the first joint observation run together with GEO600. By applying our search pipeline, which takes into account the stochastic nature of ultralight DM, upper bounds on the coupling strength between the U (1) B− L gauge boson and ordinary matter are obtained for a range of DM masses. While our constraints are less stringent than those derived from previous experiments, this study demonstrates the applicability of our method to the lower-mass vector DM search, which is made difficult in this measurement by the short observation time compared to the auto-correlation time scale of DM.

Ultralight vector dark matter search using data from the KAGRA O3GK run

Authors

AG Abac,R Abbott,H Abe,I Abouelfettouh,F Acernese,K Ackley,C Adamcewicz,S Adhicary,N Adhikari,RX Adhikari,VK Adkins,VB Adya,C Affeldt,D Agarwal,M Agathos,OD Aguiar,I Aguilar,L Aiello,A Ain,P Ajith,T Akutsu,S Albanesi,RA Alfaidi,A Al-Jodah,C Alléné,A Allocca,S Al-Shammari,PA Altin,S Alvarez-Lopez,A Amato,L Amez-Droz,A Amorosi,C Amra,S Anand,A Ananyeva,SB Anderson,WG Anderson,M Andia,M Ando,T Andrade,N Andres,M Andrés-Carcasona,T Andrić,J Anglin,S Ansoldi,JM Antelis,S Antier,M Aoumi,EZ Appavuravther,S Appert,SK Apple,K Arai,A Araya,MC Araya,JS Areeda,N Aritomi,F Armato,N Arnaud,M Arogeti,SM Aronson,KG Arun,G Ashton,Y Aso,M Assiduo,S Melo,SM Aston,P Astone,F Aubin,K AultONeal,G Avallone,S Babak,F Badaracco,C Badger,S Bae,S Bagnasco,E Bagui,Y Bai,JG Baier,R Bajpai,T Baka,M Ball,G Ballardin,SW Ballmer,S Banagiri,B Banerjee,D Bankar,P Baral,JC Barayoga,BC Barish,D Barker,P Barneo,F Barone,B Barr,L Barsotti,M Barsuglia,D Barta,SD Barthelmy,MA Barton,I Bartos,S Basak,A Basalaev,R Bassiri,A Basti,M Bawaj,P Baxi,JC Bayley,AC Baylor,M Bazzan,B Bécsy,VM Bedakihale,F Beirnaert,M Bejger,D Belardinelli,AS Bell,V Benedetto,D Beniwal,W Benoit,JD Bentley,M Ben Yaala,S Bera,M Berbel,F Bergamin,BK Berger,S Bernuzzi,M Beroiz,D Bersanetti,A Bertolini,J Betzwieser,D Beveridge,N Bevins,R Bhandare,U Bhardwaj,R Bhatt,D Bhattacharjee,S Bhaumik,S Bhowmick,A Bianchi,IA Bilenko,G Billingsley,A Binetti,S Bini,O Birnholtz,S Biscoveanu,A Bisht,M Bitossi,M-A Bizouard,JK Blackburn,CD Blair,DG Blair,F Bobba

Journal

arXiv preprint arXiv:2403.03004

Published Date

2024/3/5

Among the various candidates for dark matter (DM), ultralight vector DM can be probed by laser interferometric gravitational wave detectors through the measurement of oscillating length changes in the arm cavities. In this context, KAGRA has a unique feature due to differing compositions of its mirrors, enhancing the signal of vector DM in the length change in the auxiliary channels. Here we present the result of a search for gauge boson DM using the KAGRA data from auxiliary length channels during the first joint observation run together with GEO600. By applying our search pipeline, which takes into account the stochastic nature of ultralight DM, upper bounds on the coupling strength between the gauge boson and ordinary matter are obtained for a range of DM masses. While our constraints are less stringent than those derived from previous experiments, this study demonstrates the applicability of our method to the lower-mass vector DM search, which is made difficult in this measurement by the short observation time compared to the auto-correlation time scale of DM.

LIGO operates with quantum noise below the Standard Quantum Limit

Authors

Wenxuan Jia,Victoria Xu,Kevin Kuns,Masayuki Nakano,Lisa Barsotti,Matthew Evans,Nergis Mavalvala,Rich Abbott,Ibrahim Abouelfettouh,Rana Adhikari,Alena Ananyeva,Stephen Appert,Koji Arai,Naoki Aritomi,Stuart Aston,Matthew Ball,Stefan Ballmer,David Barker,Beverly Berger,Joseph Betzwieser,Dripta Bhattacharjee,Garilynn Billingsley,Nina Bode,Edgard Bonilla,Vladimir Bossilkov,Adam Branch,Aidan Brooks,Daniel Brown,John Bryant,Craig Cahillane,Huy-tuong Cao,Elenna Capote,Yanbei Chen,Filiberto Clara,Josh Collins,Camilla Compton,Robert Cottingham,Dennis Coyne,Ryan Crouch,Janos Csizmazia,Torrey Cullen,Louis Dartez,Nicholas Demos,Ezekiel Dohmen,Jenne Driggers,Sheila Dwyer,Anamaria Effler,Aldo Ejlli,Todd Etzel,Jon Feicht,Raymond Frey,William Frischhertz,Peter Fritschel,Valery Frolov,Paul Fulda,Michael Fyffe,Dhruva Ganapathy,Bubba Gateley,Joe Giaime,Dwayne Giardina,Jane Glanzer,Evan Goetz,Aaron Jones,Slawomir Gras,Corey Gray,Don Griffith,Hartmut Grote,Tyler Guidry,Evan Hall,Jonathan Hanks,Joe Hanson,Matthew Heintze,Adrian Helmling-cornell,Hsiang-yu Huang,Yuki Inoue,Alasdair James,Austin Jennings,Srinath Karat,Marie Kasprzack,Keita Kawabe,Nutsinee Kijbunchoo,Jeffrey Kissel,Antonios Kontos,Rahul Kumar,Michael Landry,Brian Lantz,Michael Laxen,Kyung-ha Lee,Madeline Lesovsky,Francisco Llamas,Marc Lormand,Hudsonalexander Loughlin,Ronaldas Macas,Myron Macinnis,Camille Makarem,Benjaminrobert Mannix,Georgia Mansell,Rodica Martin,Nyath Maxwell,Garrett Mccarrol,Richard Mccarthy,David Mcclelland,Scott Mccormick,Lee Mcculler,Terry Mcrae,Fernando Mera,Edmond Merilh,Fabian Meylahn,Richard Mittleman,Dan Moraru,Gerardo Moreno,Matthew Mould,Adam Mullavey,Timothy Nelson,Ansel Neunzert,Jason Oberling,Timothy Ohanlon,Charles Osthelder,David Ottaway,Harry Overmier,William Parker,Arnaud Pele,Huyen Pham,Marc Pirello,Volker Quetschke,Karla Ramirez,Jonathan Reyes,Jonathan Richardson,Mitchell Robinson,Jameson Rollins,Janeen Romie,Michael Ross,Travis Sadecki,Anthony Sanchez,Eduardo Sanchez,Luis Sanchez,Richard Savage,Dean Schaetzl,Mitchell Schiworski,Roman Schnabel,Robert Schofield,Eyal Schwartz,Danny Sellers,Thomas Shaffer,Ryan Short,Daniel Sigg,Bram Slagmolen,Siddharth Soni,Ling Sun,David Tanner

Journal

arXiv preprint arXiv:2404.14569

Published Date

2024/4/22

Precision measurements of space and time, like those made by the detectors of the Laser Interferometer Gravitational-wave Observatory (LIGO), are often confronted with fundamental limitations imposed by quantum mechanics. The Heisenberg uncertainty principle dictates that the position and momentum of an object cannot both be precisely measured, giving rise to an apparent limitation called the Standard Quantum Limit (SQL). Reducing quantum noise below the SQL in gravitational-wave detectors, where photons are used to continuously measure the positions of freely falling mirrors, has been an active area of research for decades. Here we show how the LIGO A+ upgrade reduced the detectors' quantum noise below the SQL by up to 3 dB while achieving a broadband sensitivity improvement, more than two decades after this possibility was first presented.

A joint Fermi-GBM and Swift-BAT analysis of Gravitational-wave candidates from the third Gravitational-wave Observing Run

Authors

C Fletcher,J Wood,R Hamburg,P Veres,CM Hui,E Bissaldi,MS Briggs,E Burns,WH Cleveland,MM Giles,A Goldstein,BA Hristov,D Kocevski,S Lesage,B Mailyan,C Malacaria,S Poolakkil,A von Kienlin,CA Wilson-Hodge,M Crnogorčević,J DeLaunay,A Tohuvavohu,R Caputo,SB Cenko,S Laha,T Parsotan,R Abbott,H Abe,F Acernese,K Ackley,N Adhikari,RX Adhikari,VK Adkins,VB Adya,C Affeldt,D Agarwal,M Agathos,K Agatsuma,N Aggarwal,OD Aguiar,Luca Aiello,A Ain,P Ajith,T Akutsu,S Albanesi,RA Alfaidi,A Allocca,PA Altin,A Amato,C Anand,S Anand,A Ananyeva,SB Anderson,WG Anderson,M Ando,T Andrade,N Andres,M Andrés-Carcasona,T Andríc,SV Angelova,S Ansoldi,JM Antelis,S Antier,T Apostolatos,EZ Appavuravther,S Appert,SK Apple,K Arai,A Araya,MC Araya,JS Areeda,M Arène,N Aritomi,N Arnaud,M Arogeti,SM Aronson,KG Arun,H Asada,Y Asali,G Ashton,Y Aso,M Assiduo,S Melo,SM Aston,P Astone,F Aubin,K AultONeal,C Austin,S Babak,F Badaracco,MKM Bader,C Badger,S Bae,Y Bae,AM Baer,S Bagnasco,Y Bai,J Baird,R Bajpai,T Baka,M Ball,G Ballardin,SW Ballmer,A Balsamo,G Baltus,S Banagiri,B Banerjee,D Bankar,JC Barayoga,C Barbieri,BC Barish,D Barker,P Barneo,F Barone,B Barr,L Barsotti,M Barsuglia,D Barta,J Bartlett,MA Barton,I Bartos,S Basak,R Bassiri,A Basti,M Bawaj,JC Bayley,M Bazzan,BR Becher,B Bécsy,VM Bedakihale,F Beirnaert,M Bejger,I Belahcene,V Benedetto,D Beniwal,MG Benjamin,TF Bennett,JD Bentley,M BenYaala,S Bera,M Berbel,F Bergamin,BK Berger,S Bernuzzi,CPL Berry,D Bersanetti,A Bertolini,J Betzwieser,D Beveridge,R Bhandare

Journal

arXiv preprint arXiv:2308.13666

Published Date

2023/8/25

The detection of GW170817 (Abbott et al. 2017b) coincident with the short gamma-ray burst GRB 170817A (Goldstein et al. 2017; Savchenko et al. 2017) was a groundbreaking discovery for the multimessenger era. Not only was it the first binary neutron star (BNS) merger detected by the gravitational-wave (GW) instruments Advanced LIGO (Aasi et al. 2015) and Advanced Virgo (Acernese et al. 2014), it was also the first, and to date only, GW detection with a confirmed electromagnetic (EM) counterpart. Since then, the search for EM emission from more of these extreme events has been at the forefront of multimessenger astronomy, particularly in the gamma-ray energy band, since GRB 170817A demonstrated that BNS mergers are a progenitor of short gamma-ray bursts (GRBs; Abbott et al. 2017a). GWs have also been observed from the mergers of other compact objects, such as binary black hole (BBH) and …

Beam displacement tolerances on a segmented mirror for higher-order Hermite–Gauss modes

Authors

Liu Tao,Nina Brown,Paul Fulda

Journal

arXiv preprint arXiv:2305.03681

Published Date

2023/5/5

Odd-indexed higher-order Hermite–Gauss (HG) modes are compatible with four-quadrant segmented mirrors due to their intensity nulls along the principal axes, which guarantees minimum beam intensity illuminating the bond lines between the segments thus leading to low power loss. However, a misplaced HG beam can cause extra power loss due to the bright intensity spots probing the bond lines. This paper analytically and numerically studies the beam displacement tolerances on a segmented mirror for the

Calculating the precision of tilt-to-length coupling estimation and noise subtraction in LISA using Fisher information

Authors

Daniel George,Jose Sanjuan,Paul Fulda,Guido Mueller

Journal

Physical Review D

Published Date

2023/1/18

Tilt-to-length (TTL) noise from angular jitter in LISA is projected to be the dominant noise source in the milli-Hertz band unless corrected in post-processing. The correction is only possible after removing the overwhelming laser phase noise using time-delay interferometry (TDI). We present here a frequency domain model that describes the effect of angular motion of all three spacecraft on the interferometric signals after propagating through TDI. We then apply a Fisher information matrix analysis to this model to calculate the minimum uncertainty with which TTL coupling coefficients may be estimated. Furthermore, we show the impact of these uncertainties on the residual TTL noise in the gravitational wave readout channel, and compare it to the impact of the angular witness sensors’ readout noise. We show that the residual TTL noise post-subtraction in the TDI variables for a case using the LISA angular jitter …

Searching for the causes of anomalous Advanced LIGO noise

Authors

BK Berger,JS Areeda,JD Barker,A Effler,E Goetz,AF Helmling-Cornell,B Lantz,AP Lundgren,DM Macleod,J McIver,R Mittleman,P Nguyen,A Pele,H Pham,P Rangnekar,K Rink,RMS Schofield,JR Smith,S Soni,J Warner,R Abbott,RX Adhikari,A Ananyeva,S Appert,K Arai,Y Asali,SM Aston,AM Baer,M Ball,SW Ballmer,S Banagiri,D Barker,L Barsotti,J Betzwieser,D Bhattacharjee,G Billingsley,S Biscans,CD Blair,RM Blair,N Bode,P Booker,R Bork,AF Brooks,DD Brown,C Cahillane,X Chen,AA Ciobanu,F Clara,CM Compton,SJ Cooper,KR Corley,ST Countryman,PB Covas,DC Coyne,LEH Datrier,D Davis,C Di Fronzo,KL Dooley,JC Driggers,SE Dwyer,T Etzel,M Evans,TM Evans,J Feicht,A Fernandez-Galiana,P Fritschel,VV Frolov,P Fulda,M Fyffe,JA Giaime,KD Giardina,P Godwin,S Gras,C Gray,R Gray,AC Green,A Gupta,EK Gustafson,R Gustafson,J Hanks,J Hanson,RK Hasskew,MC Heintze,NA Holland,S Kandhasamy,S Karki,M Kasprzack,K Kawabe,N Kijbunchoo,PJ King,JS Kissel,Rahul Kumar,M Landry,BB Lane,M Laxen,YK Lecoeuche,J Leviton,J Liu,M Lormand,R Macas,M MacInnis,GL Mansell,S Márka,Z Márka,DV Martynov,K Mason,F Matichard,N Mavalvala,R McCarthy,DE McClelland,S McCormick,L McCuller,T McRae,G Mendell,K Merfeld,EL Merilh,F Meylahn,T Mistry,G Moreno,CM Mow-Lowry,S Mozzon,A Mullavey,TJN Nelson,LK Nuttall,J Oberling,Richard J Oram,C Osthelder,DJ Ottaway,H Overmier,W Parker,E Payne,R Penhorwood,CJ Perez,M Pirello,KE Ramirez,JW Richardson,K Riles,NA Robertson,JG Rollins,CL Romel,JH Romie,MP Ross,K Ryan,T Sadecki,EJ Sanchez,LE Sanchez,TR Saravanan,RL Savage,D Schaetzl,R Schnabel

Journal

Applied Physics Letters

Published Date

2023/5/1

Advanced LIGO and Advanced Virgo have detected gravitational waves from astronomical sources to open a new window on the Universe. To explore this new realm requires an exquisite level of detector sensitivity, meaning that the much stronger signal from instrumental and environmental noise must be rejected. Selected examples of unwanted noise in Advanced LIGO are presented. The initial focus is on how the existence of this noise (characterized by particular frequencies or time intervals) was discovered. Then, a variety of methods are used to track down the source of the noise, eg, a fault within the instruments or coupling from an external source. The ultimate goal of this effort is to mitigate the noise by either fixing equipment or by augmenting methods to suppress the coupling to the environment.The Advanced LIGO instruments 1 at LIGO Hanford Observatory (LHO) and LIGO Livingston Observatory (LLO …

arXiv: Search for Eccentric Black Hole Coalescences during the Third Observing Run of LIGO and Virgo

Authors

AG Abac,ML Chiofalo,G Nieradka,R Pegna,C North,R Bhandare,G Pierra,A Amato,JG Baier,D Chen,B Haskell,F Robinet,M Fyffe,M Arogeti,N Raza,DD White,E Payne,M Wright,K Johansmeyer,K Hayama,P-F Cohadon,CG Collette,D Sellers,S Hoang,V Sipala,H Heitmann,T O'Hanlon,B Edelman,G McCarrol,GS Bonilla,T Harder,TA Clarke,YT Huang,J Junker,M Hennig,N Hirata,J Portell,R McCarthy,M Weinert,Y-C Yang,R Poulton,G Ballardin,D Bankar,A Bianchi,M Montani,R Goetz,CD Panzer,X Chen,R Takahashi,J Lange,K Schouteden,A Sasli,LM Modafferi,ME Zucker,J O'Dell,D Lumaca,AP Spencer,M Millhouse,M Norman,MJ Szczepańczyk,S-C Hsu,ST Countryman,C Chatterjee,AL James,E Chassande-Mottin,M Tacca,FJ Raab,TR Saravanan,VP Mitrofanov,S Bernuzzi,C Adamcewicz,L Conti,J Golomb,X Li,ERG von Reis,J Woehler,G Bogaert,F Fidecaro,B Shen,JM Ezquiaga,V Juste,S Sachdev,JD Bentley,YA Kas-danouche,R Sturani,M Toscani,K Takatani,D Beniwal,U Dupletsa,F Glotin,Y Lee,R Bhatt,A Couineaux,M Wade,N Kanda,J Novak,S Bini,I Ferrante,RA Alfaidi,N Johny,LE Sanchez,J Heinze,J Zhang,M Kinley-Hanlon,M Pegoraro,A Van de Walle,T Sainrat,NN Janthalur,A Trovato,A Romero,K Tomita,DE McClelland,B Fornal,M Heurs,AM Gretarsson,ND Koliadko,A Chincarini,BB Lane,AE Romano,M Martinez,V Fafone,FY Khalili,F Linde,C Messick,A Heffernan,J Gargiulo,V JaberianHamedan,SW Reid,D Moraru,D Pathak,M Iwaya,G Grignani,T Karydas,K AultONeal,SA Pai,IM Pinto,KW Chung,C Palomba,J Tissino,T Klinger,Ll M Mir,K Kwan,JK Katsuren,TP Lott,C Posnansky,S Di Pace,F Badaracco,NA Johnson,VA Martinez,A Ain

Published Date

2023/8/7

Despite the growing number of candidates and the insight they have provided, the astrophysical sites and processes that produce the observed merging binaries remain uncertain. Multiple viable scenarios exist. The binary black holes could have formed in an isolated stellar binary (eg, Bethe & Brown 1998; Dominik et al. 2015; Inayoshi et al. 2017; Marchant et al. 2016; de Mink & Mandel 2016; Gallegos-Garcia et al. 2021), via dynamical interactions in dense stellar clusters (eg, Portegies Zwart & McMillan 2000; Banerjee et al. 2010; Ziosi et al. 2014; Morscher et al. 2015; Mapelli 2016; Rodriguez et al. 2016a; Askar et al. 2017) or triple systems (eg, Antonini et al. 2017; Martinez et al. 2020; Vigna-Gómez et al. 2021), or via gas capture in the disks of active galactic nuclei (AGN; eg, McKernan et al. 2012; Bartos et al. 2017; Fragione et al. 2019; Tagawa et al. 2020).

GWTC-3: compact binary coalescences observed by LIGO and Virgo during the second part of the third observing run

Authors

Richard Abbott,TD Abbott,F Acernese,K Ackley,C Adams,N Adhikari,RX Adhikari,VB Adya,C Affeldt,D Agarwal,M Agathos,Kazuhiro Agatsuma,N Aggarwal,OD Aguiar,L Aiello,A Ain,P Ajith,S Akcay,T Akutsu,S Albanesi,A Allocca,PA Altin,A Amato,C Anand,S Anand,A Ananyeva,SB Anderson,WG Anderson,M Ando,T Andrade,N Andres,T Andrić,SV Angelova,S Ansoldi,JM Antelis,S Antier,S Appert,Koji Arai,Koya Arai,Y Arai,S Araki,A Araya,MC Araya,JS Areeda,M Arène,N Aritomi,N Arnaud,M Arogeti,SM Aronson,KG Arun,H Asada,Y Asali,G Ashton,Y Aso,M Assiduo,SM Aston,P Astone,F Aubin,C Austin,S Babak,F Badaracco,MKM Bader,C Badger,S Bae,Y Bae,AM Baer,S Bagnasco,Y Bai,L Baiotti,J Baird,R Bajpai,M Ball,G Ballardin,SW Ballmer,A Balsamo,G Baltus,S Banagiri,D Bankar,JC Barayoga,C Barbieri,BC Barish,D Barker,P Barneo,F Barone,B Barr,L Barsotti,M Barsuglia,D Barta,J Bartlett,MA Barton,I Bartos,R Bassiri,A Basti,M Bawaj,JC Bayley,AC Baylor,M Bazzan,B Bécsy,VM Bedakihale,M Bejger,I Belahcene,V Benedetto,D Beniwal,TF Bennett,JD Bentley,M BenYaala,F Bergamin,BK Berger,S Bernuzzi,CPL Berry,D Bersanetti,A Bertolini,J Betzwieser,D Beveridge,R Bhandare,U Bhardwaj,D Bhattacharjee,S Bhaumik,IA Bilenko,G Billingsley,S Bini,R Birney,O Birnholtz,S Biscans,M Bischi,S Biscoveanu,A Bisht,B Biswas,M Bitossi,M-A Bizouard,JK Blackburn,CD Blair,DG Blair,RM Blair,F Bobba,N Bode,M Boer,G Bogaert,M Boldrini,LD Bonavena,F Bondu,E Bonilla,R Bonnand,P Booker,BA Boom,R Bork,V Boschi,N Bose,S Bose,V Bossilkov

Journal

Physical Review X

Published Date

2023/12/4

The third Gravitational-Wave Transient Catalog (GWTC-3) describes signals detected with Advanced LIGO and Advanced Virgo up to the end of their third observing run. Updating the previous GWTC-2.1, we present candidate gravitational waves from compact binary coalescences during the second half of the third observing run (O3b) between 1 November 2019, 15∶ 00 Coordinated Universal Time (UTC) and 27 March 2020, 17∶ 00 UTC. There are 35 compact binary coalescence candidates identified by at least one of our search algorithms with a probability of astrophysical origin p astro> 0.5. Of these, 18 were previously reported as low-latency public alerts, and 17 are reported here for the first time. Based upon estimates for the component masses, our O3b candidates with p astro> 0.5 are consistent with gravitational-wave signals from binary black holes or neutron-star–black-hole binaries, and we identify …

Experimental investigations on the Higher-order Hermite-Gauss mode interferometry

Authors

Liu Tao,Paul Fulda

Journal

Bulletin of the American Physical Society

Published Date

2023/4/15

Thermal noise of the test masses is one of the limiting noise sources in advanced gravitational wave (GW) detectors. It is expected to remain a limiting noise source in future detectors, despite radical changes to the design including cryogenic operations, new materials, and the use of longer laser wavelengths. The so-calledflat beams' such as higher-order Hermite-Gaussian (HG) beams have been studied for thermal noise reduction in GW detectors. They help by better averaging over the random mirror surface fluctuations caused by thermal motions. We have started the experimental investigations on the HG mode interferometry with HG3, 3 mode, and we will report on the latest results and progress.

Detection of the gravitational memory effect in LISA using triggers from ground-based detectors

Authors

Sourath Ghosh,Alexander Weaver,Jose Sanjuan,Paul Fulda,Guido Mueller

Journal

Physical Review D

Published Date

2023/4/28

The LIGO-Virgo-KAGRA (LVK) Collaboration has detected gravitational waves (GWs) from 90 compact binary coalescences. In addition to fortifying the linearized theory of general relativity (GR), the statistical ensemble of detections also provides prospects of detecting nonlinear effects predicted by GR, one such prediction being the nonlinear gravitational memory effect. For detected stellar and intermediate mass compact binaries, the induced strain from the memory effect is 1 or 2 orders below the detector noise background. Additionally, since most of the energy is radiated at merger the strain induced by the memory effect resembles a step function at the merger time. These facts motivate the idea of coherently stacking up data streams from recorded GW events at these merger times so that the cumulative memory strain is detected with a sufficient signal to noise ratio (SNR). GW detectors essentially record the …

Search for eccentric black hole coalescences during the third observing run of LIGO and virgo

Authors

AG Abac,R Abbott,H Abe,F Acernese,K Ackley,C Adamcewicz,S Adhicary,N Adhikari,RX Adhikari,VK Adkins,VB Adya,C Affeldt,D Agarwal,M Agathos,OD Aguiar,I Aguilar,L Aiello,A Ain,P Ajith,T Akutsu,S Albanesi,RA Alfaidi,A Al-Jodah,C Alléné,A Allocca,M Almualla,PA Altin,S Álvarez-López,A Amato,L Amez-Droz,A Amorosi,S Anand,A Ananyeva,R Andersen,SB Anderson,WG Anderson,M Andia,M Ando,T Andrade,N Andres,M Andrés-Carcasona,T Andrić,S Ansoldi,JM Antelis,S Antier,M Aoumi,T Apostolatos,EZ Appavuravther,S Appert,SK Apple,K Arai,A Araya,MC Araya,JS Areeda,N Aritomi,F Armato,N Arnaud,M Arogeti,SM Aronson,KG Arun,G Ashton,Y Aso,M Assiduo,S Melo,SM Aston,P Astone,F Aubin,K AultONeal,S Babak,A Badalyan,F Badaracco,C Badger,S Bae,S Bagnasco,Y Bai,JG Baier,R Bajpai,T Baka,M Ball,G Ballardin,SW Ballmer,G Baltus,S Banagiri,B Banerjee,D Bankar,P Baral,JC Barayoga,J Barber,BC Barish,D Barker,P Barneo,F Barone,B Barr,L Barsotti,M Barsuglia,D Barta,SD Barthelmy,MA Barton,I Bartos,S Basak,A Basalaev,R Bassiri,A Basti,M Bawaj,P Baxi,JC Bayley,AC Baylor,M Bazzan,B Bécsy,VM Bedakihale,F Beirnaert,M Bejger,AS Bell,V Benedetto,D Beniwal,W Benoit,JD Bentley,M Ben Yaala,S Bera,M Berbel,F Bergamin,BK Berger,S Bernuzzi,M Beroiz,CPL Berry,D Bersanetti,A Bertolini,J Betzwieser,D Beveridge,N Bevins,R Bhandare,AV Bhandari,U Bhardwaj,R Bhatt,D Bhattacharjee,S Bhaumik,A Bianchi,IA Bilenko,M Bilicki,G Billingsley,A Binetti,S Bini,O Birnholtz,S Biscans,M Bischi,S Biscoveanu,A Bisht,M Bitossi,M-A Bizouard,JK Blackburn

Journal

arXiv preprint arXiv:2308.03822

Published Date

2023/8/7

Despite the growing number of confident binary black hole coalescences observed through gravitational waves so far, the astrophysical origin of these binaries remains uncertain. Orbital eccentricity is one of the clearest tracers of binary formation channels. Identifying binary eccentricity, however, remains challenging due to the limited availability of gravitational waveforms that include effects of eccentricity. Here, we present observational results for a waveform-independent search sensitive to eccentric black hole coalescences, covering the third observing run (O3) of the LIGO and Virgo detectors. We identified no new high-significance candidates beyond those that were already identified with searches focusing on quasi-circular binaries. We determine the sensitivity of our search to high-mass (total mass ) binaries covering eccentricities up to 0.3 at 15 Hz orbital frequency, and use this to compare model predictions to search results. Assuming all detections are indeed quasi-circular, for our fiducial population model, we place an upper limit for the merger rate density of high-mass binaries with eccentricities at Gpc yr at 90\% confidence level.

Sideband Locking for the LISA Optical Truss Interferometer Readout

Authors

Paul Edwards,Paul Fulda

Journal

Bulletin of the American Physical Society

Published Date

2023/4/15

In LISA, the optical truss interferometer (OTI) is a subsystem proposed to track pathlength variations in the telescope and ensure the telescope structure meets the required picometer stability. An OTI would be located at each of the six LISA telescopes, with each OTI comprising three separate linear cavities in a triangular configuration. If a telescope is not picometer stable, on-mission cavity length measurements serve as a potential witness channel for spurious length fluctuations. A simple method of cavity length measurements would involve three separate lasers, each locked to a respective OTI cavity. However, one alternative which uses a pick-off from a single, pre-existing laser source at each telescope is sideband locking, which would lock pairs of sidebands to each of the three cavities. Via this sideband locking, a voltage-controlled oscillator (VCO) signal, applied to a broadband electro-optic modulator (EOM …

Search for gravitational-lensing signatures in the full third observing run of the LIGO-Virgo network

Authors

R Abbott,H Abe,F Acernese,K Ackley,S Adhicary,N Adhikari,RX Adhikari,VK Adkins,VB Adya,C Affeldt,D Agarwal,M Agathos,OD Aguiar,L Aiello,A Ain,P Ajith,T Akutsu,S Albanesi,RA Alfaidi,C Alléné,A Allocca,PA Altin,A Amato,S Anand,A Ananyeva,SB Anderson,WG Anderson,M Ando,T Andrade,N Andres,M Andrés-Carcasona,T Andrić,S Ansoldi,JM Antelis,S Antier,T Apostolatos,EZ Appavuravther,S Appert,SK Apple,K Arai,A Araya,MC Araya,JS Areeda,M Arène,N Aritomi,N Arnaud,M Arogeti,SM Aronson,H Asada,G Ashton,Y Aso,M Assiduo,S Melo,SM Aston,P Astone,F Aubin,K AultONeal,S Babak,F Badaracco,C Badger,S Bae,Y Bae,S Bagnasco,Y Bai,JG Baier,J Baird,R Bajpai,T Baka,M Ball,G Ballardin,SW Ballmer,G Baltus,S Banagiri,B Banerjee,D Bankar,JC Barayoga,BC Barish,D Barker,P Barneo,F Barone,B Barr,L Barsotti,M Barsuglia,D Barta,J Bartlett,MA Barton,I Bartos,S Basak,R Bassiri,A Basti,M Bawaj,JC Bayley,M Bazzan,B Bécsy,VM Bedakihale,F Beirnaert,M Bejger,I Belahcene,AS Bell,V Benedetto,D Beniwal,W Benoit,JD Bentley,M BenYaala,S Bera,M Berbel,F Bergamin,BK Berger,S Bernuzzi,M Beroiz,CPL Berry,D Bersanetti,A Bertolini,J Betzwieser,D Beveridge,R Bhandare,AV Bhandari,U Bhardwaj,R Bhatt,D Bhattacharjee,S Bhaumik,A Bianchi,IA Bilenko,M Bilicki,G Billingsley,S Bini,O Birnholtz,S Biscans,M Bischi,S Biscoveanu,A Bisht,B Biswas,M Bitossi,M-A Bizouard,JK Blackburn,CD Blair,DG Blair,RM Blair,F Bobba,N Bode,M Boër,G Bogaert,M Boldrini,GN Bolingbroke,LD Bonavena,R Bondarescu,F Bondu,E Bonilla,R Bonnand,P Booker

Journal

arXiv preprint arXiv:2304.08393

Published Date

2023/4/17

Gravitational lensing by massive objects along the line of sight to the source causes distortions of gravitational wave-signals; such distortions may reveal information about fundamental physics, cosmology and astrophysics. In this work, we have extended the search for lensing signatures to all binary black hole events from the third observing run of the LIGO--Virgo network. We search for repeated signals from strong lensing by 1) performing targeted searches for subthreshold signals, 2) calculating the degree of overlap amongst the intrinsic parameters and sky location of pairs of signals, 3) comparing the similarities of the spectrograms amongst pairs of signals, and 4) performing dual-signal Bayesian analysis that takes into account selection effects and astrophysical knowledge. We also search for distortions to the gravitational waveform caused by 1) frequency-independent phase shifts in strongly lensed images, and 2) frequency-dependent modulation of the amplitude and phase due to point masses. None of these searches yields significant evidence for lensing. Finally, we use the non-detection of gravitational-wave lensing to constrain the lensing rate based on the latest merger-rate estimates and the fraction of dark matter composed of compact objects.

Broadband quantum enhancement of the LIGO detectors with frequency-dependent squeezing

Authors

D Ganapathy,W Jia,M Nakano,V Xu,N Aritomi,T Cullen,N Kijbunchoo,SE Dwyer,A Mullavey,L McCuller,R Abbott,I Abouelfettouh,RX Adhikari,A Ananyeva,S Appert,K Arai,SM Aston,M Ball,SW Ballmer,D Barker,L Barsotti,BK Berger,J Betzwieser,D Bhattacharjee,G Billingsley,S Biscans,N Bode,E Bonilla,V Bossilkov,A Branch,AF Brooks,DD Brown,J Bryant,C Cahillane,H Cao,E Capote,F Clara,J Collins,CM Compton,R Cottingham,DC Coyne,R Crouch,J Csizmazia,LP Dartez,N Demos,E Dohmen,JC Driggers,A Effler,A Ejlli,T Etzel,M Evans,J Feicht,R Frey,W Frischhertz,P Fritschel,VV Frolov,P Fulda,M Fyffe,B Gateley,JA Giaime,KD Giardina,J Glanzer,E Goetz,R Goetz,AW Goodwin-Jones,S Gras,C Gray,D Griffith,H Grote,T Guidry,ED Hall,J Hanks,J Hanson,MC Heintze,AF Helmling-Cornell,NA Holland,D Hoyland,HY Huang,Y Inoue,AL James,A Jennings,S Karat,S Karki,M Kasprzack,K Kawabe,PJ King,JS Kissel,K Komori,A Kontos,R Kumar,K Kuns,M Landry,B Lantz,M Laxen,K Lee,M Lesovsky,F Llamas,M Lormand,HA Loughlin,R Macas,M MacInnis,CN Makarem,B Mannix,GL Mansell,RM Martin,K Mason,F Matichard,N Mavalvala,N Maxwell,G McCarrol,R McCarthy,DE McClelland,S McCormick,T McRae,F Mera,EL Merilh,F Meylahn,R Mittleman,D Moraru,G Moreno,TJN Nelson,A Neunzert,J Notte,J Oberling,T O’Hanlon,C Osthelder,DJ Ottaway,H Overmier,W Parker,A Pele,H Pham,M Pirello,V Quetschke,KE Ramirez,J Reyes,JW Richardson,M Robinson,JG Rollins,CL Romel,JH Romie,MP Ross,K Ryan,T Sadecki,A Sanchez,EJ Sanchez,LE Sanchez,RL Savage,D Schaetzl,MG Schiworski,R Schnabel

Journal

Physical Review X

Published Date

2023/10/30

Quantum noise imposes a fundamental limitation on the sensitivity of interferometric gravitational-wave detectors like LIGO, manifesting as shot noise and quantum radiation pressure noise. Here, we present the first realization of frequency-dependent squeezing in full-scale gravitational-wave detectors, resulting in the reduction of both shot noise and quantum radiation pressure noise, with broadband detector enhancement from tens of hertz to several kilohertz. In the LIGO Hanford detector, squeezing reduced the detector noise amplitude by a factor of 1.6 (4.0 dB) near 1 kHz; in the Livingston detector, the noise reduction was a factor of 1.9 (5.8 dB). These improvements directly impact LIGO’s scientific output for high-frequency sources (eg, binary neutron star postmerger physics). The improved low-frequency sensitivity, which boosted the detector range by 15%–18% with respect to no squeezing, corresponds to an …

Search for gravitational waves associated with fast radio bursts detected by CHIME/FRB during the LIGO–Virgo observing run O3a

Authors

R Abbott,TD Abbott,F Acernese,K Ackley,C Adams,N Adhikari,RX Adhikari,VB Adya,C Affeldt,D Agarwal,M Agathos,K Agatsuma,N Aggarwal,OD Aguiar,L Aiello,A Ain,P Ajith,T Akutsu,S Albanesi,A Allocca,PA Altin,A Amato,C Anand,S Anand,A Ananyeva,SB Anderson,WG Anderson,M Ando,T Andrade,N Andres,T Andrić,SV Angelova,S Ansoldi,JM Antelis,S Antier,S Appert,Koji Arai,Koya Arai,Y Arai,S Araki,A Araya,MC Araya,JS Areeda,M Arène,N Aritomi,N Arnaud,SM Aronson,KG Arun,H Asada,Y Asali,G Ashton,Y Aso,M Assiduo,SM Aston,P Astone,F Aubin,C Austin,S Babak,F Badaracco,MKM Bader,C Badger,S Bae,Y Bae,AM Baer,S Bagnasco,Y Bai,L Baiotti,J Baird,R Bajpai,M Ball,G Ballardin,SW Ballmer,A Balsamo,G Baltus,S Banagiri,D Bankar,JC Barayoga,C Barbieri,BC Barish,D Barker,P Barneo,F Barone,B Barr,L Barsotti,M Barsuglia,D Barta,J Bartlett,MA Barton,I Bartos,R Bassiri,A Basti,M Bawaj,JC Bayley,AC Baylor,M Bazzan,B Bécsy,VM Bedakihale,M Bejger,I Belahcene,V Benedetto,D Beniwal,TF Bennett,JD Bentley,M Benyaala,F Bergamin,BK Berger,S Bernuzzi,CPL Berry,D Bersanetti,A Bertolini,J Betzwieser,D Beveridge,R Bhandare,U Bhardwaj,D Bhattacharjee,S Bhaumik,IA Bilenko,G Billingsley,S Bini,R Birney,O Birnholtz,S Biscans,M Bischi,S Biscoveanu,A Bisht,B Biswas,M Bitossi,M-A Bizouard,JK Blackburn,CD Blair,DG Blair,RM Blair,F Bobba,N Bode,M Boer,G Bogaert,M Boldrini,LD Bonavena,F Bondu,E Bonilla,R Bonnand,P Booker,BA Boom,R Bork,V Boschi,N Bose,S Bose,V Bossilkov,V Boudart,Y Bouffanais

Journal

The Astrophysical Journal

Published Date

2023/10/1

Fast radio bursts (FRBs) are millisecond duration radio pulses that have been observed out to cosmological distances, several with inferred redshifts greater than unity (Lorimer et al. 2007; Cordes & Chatterjee 2019; Petroff et al. 2019). Although intensely studied for more than a decade, the emission mechanisms and progenitor populations of FRBs are still one of the outstanding questions in astronomy. Some FRBs have been shown to repeat (Amiri et al. 2019a; CHIME/FRB Collaboration et al. 2019; Kumar et al. 2019), and the recent association of an FRB with the Galactic magnetar SGR 1935+ 2154 proves that magnetars can produce FRBs (Bochenek et al. 2020; CHIME/FRB Collaboration et al. 2020). Alternative progenitors and mechanisms to produce nonrepeating FRBs are still credible and have so far not been ruled out (Zhang 2020a). Data currently suggest that both repeating and nonrepeating classes of …

Cosmic Explorer: A Submission to the NSF MPSAC ngGW Subcommittee

Authors

Matthew Evans,Alessandra Corsi,Chaitanya Afle,Alena Ananyeva,KG Arun,Stefan Ballmer,Ananya Bandopadhyay,Lisa Barsotti,Masha Baryakhtar,Edo Berger,Emanuele Berti,Sylvia Biscoveanu,Ssohrab Borhanian,Floor Broekgaarden,Duncan A Brown,Craig Cahillane,Lorna Campbell,Hsin-Yu Chen,Kathryne J Daniel,Arnab Dhani,Jennifer C Driggers,Anamaria Effler,Robert Eisenstein,Stephen Fairhurst,Jon Feicht,Peter Fritschel,Paul Fulda,Ish Gupta,Evan D Hall,Giles Hammond,Otto A Hannuksela,Hannah Hansen,Carl-Johan Haster,Keisi Kacanja,Brittany Kamai,Rahul Kashyap,Joey Shapiro Key,Sanika Khadkikar,Antonios Kontos,Kevin Kuns,Michael Landry,Philippe Landry,Brian Lantz,Tjonnie GF Li,Geoffrey Lovelace,Vuk Mandic,Georgia L Mansell,Denys Martynov,Lee McCuller,Andrew L Miller,Alexander Harvey Nitz,Benjamin J Owen,Cristiano Palomba,Jocelyn Read,Hemantakumar Phurailatpam,Sanjay Reddy,Jonathan Richardson,Jameson Rollins,Joseph D Romano,Bangalore S Sathyaprakash,Robert Schofield,David H Shoemaker,Daniel Sigg,Divya Singh,Bram Slagmolen,Piper Sledge,Joshua Smith,Marcelle Soares-Santos,Amber Strunk,Ling Sun,David Tanner,Lieke AC van Son,Salvatore Vitale,Benno Willke,Hiro Yamamoto,Michael Zucker

Journal

arXiv preprint arXiv:2306.13745

Published Date

2023/6/23

Gravitational-wave astronomy has revolutionized humanity's view of the universe, a revolution driven by observations that no other field can make. This white paper describes an observatory that builds on decades of investment by the National Science Foundation and that will drive discovery for decades to come: Cosmic Explorer. Major discoveries in astronomy are driven by three related improvements: better sensitivity, higher precision, and opening new observational windows. Cosmic Explorer promises all three and will deliver an order-of-magnitude greater sensitivity than LIGO. Cosmic Explorer will push the gravitational-wave frontier to almost the edge of the observable universe using technologies that have been proven by LIGO during its development. With the unprecedented sensitivity that only a new facility can deliver, Cosmic Explorer will make discoveries that cannot yet be anticipated, especially since gravitational waves are both synergistic with electromagnetic observations and can reach into regions of the universe that electromagnetic observations cannot explore. With Cosmic Explorer, scientists can use the universe as a laboratory to test the laws of physics and study the nature of matter. Cosmic Explorer allows the United States to continue its leading role in gravitational-wave science and the international network of next-generation observatories. With its extraordinary discovery potential, Cosmic Explorer will deliver revolutionary observations across astronomy, physics, and cosmology including: Black Holes and Neutron Stars Throughout Cosmic Time, Multi-Messenger Astrophysics and Dynamics of Dense Matter, New Probes …

See List of Professors in Paul Fulda University(University of Florida)

Paul Fulda FAQs

What is Paul Fulda's h-index at University of Florida?

The h-index of Paul Fulda has been 87 since 2020 and 109 in total.

What are Paul Fulda's top articles?

The articles with the titles of