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This material is based upon work supported by NSF's LIGO Laboratory, which is a major facility fully funded by the National Science Foundation. The authors also gratefully acknowledge the support of the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO 600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS), and the Netherlands Organization for Scientific Research (NWO) for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India, the Science and Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigacion (AEI), the Spanish Ministerio de Ciencia, Innovacion, y Universidades, the European Union NextGenerationEU/PRTR (PRTR-C17.I1), the ICSC-CentroNazionale di Ricerca in High Performance Computing, Big Data, and Quantum Computing, funded by the European Union NextGenerationEU, the Comunitat Autonma de les Illes Balears through the Conselleria d'Educacio i Universitats, the Conselleria d'Innovacio, Universitats, Ciencia i Societat Digital de la Generalitat Valenciana, and the CERCA Programme Generalitat de Catalunya, Spain, the Polish National Agency for Academic Exchange, the National Science Centre of Poland and the European Union-European Regional Development Fund; the Foundation for Polish Science (FNP), the Polish Ministry of Science and Higher Education, the Swiss National Science Foundation (SNSF), the Russian Science Foundation, the European Commission, the European Social Funds (ESF), the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the French Lyon Institute of Origins (LIO), the Belgian Fonds de la Recherche Scientifique (FRS-FNRS), Actions de Recherche Concertees (ARC) and Fonds Wetenschappelijk Onderzoek-Vlaanderen (FWO), Belgium, the Paris ile-de-France Region, the National Research, Development and Innovation Office of Hungary (NKFIH), the National Research Foundation of Korea, the Natural Sciences and Engineering Research Council of Canada (NSERC), the Canadian Foundation for Innovation (CFI), the Brazilian Ministry of Science, Technology, and Innovations, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Israel Science Foundation (ISF), the US-Israel Binational Science Fund (BSF), the Leverhulme Trust, the Research Corporation, the National Science and Technology Council (NSTC), Taiwan, the United States Department of Energy, and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, INFN, and CNRS for provision of computational resources. This work was supported by MEXT, the JSPS Leading-edge Research Infrastructure Program, JSPS Grant-in-Aid for Specially Promoted Research 26000005, JSPS Grant-in-Aid for Scientific Research on Innovative Areas 2905: JP17H06358, JP17H06361, and JP17H06364, JSPS Core-to-Core Program A, Advanced Research Networks, JSPS Grants-in-Aid for Scientific Research (S) 17H06133 and 20H05639, JSPS Grant-in-Aid for Transformative Research Areas (A) 20A203: JP20H05854, the joint research program of the Institute for Cosmic Ray Research, the University of Tokyo, the National Research Foundation (NRF), the Computing Infrastructure Project of Global Science experimental Data hub Center (GSDC) at KISTI, the Korea Astronomy and Space Science Institute (KASI), the Ministry of Science and ICT (MSIT) in Korea, Academia Sinica (AS), the AS Grid Center (ASGC) and the National Science and Technology Council (NSTC) in Taiwan under grants including the Rising Star Program and Science Vanguard Research Program, the Advanced Technology Center (ATC) of NAOJ, and the Mechanical Engineering Center of KEK. C.M.E. acknowledges support from ANID/FONDECYT, grant 1211964. S. Guillot acknowledges the support of the CNES. W.C.G.H. acknowledges support through grant 80NSSC22K1305 from NASA. This work is supported by NASA through the NICER mission and the Astrophysics Explorers Program and uses data and software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. The Nancay radio Observatory is operated by the Paris Observatory, associated with the French Centre National de la Recherche Scientifique (CNRS), and partially supported by the Region Centre in France. We acknowledge financial support from "Programme National de Cosmologie and Galaxies" (PNCG), and "Programme National Hautes Energies" (PNHE) funded by CNRS/INSU-IN2P3-INP, CEA, and CNES, France. A.B.P. is a Banting Fellow, a McGill Space Institute (MSI) Fellow, and a Fonds de Recherche du Quebec-Nature et Technologies (FRQNT) postdoctoral fellow. E. Fonseca is supported by the NSF grant AST-2407399. The activities at the Instituto Argentino de Radioastronomia (IAR) are supported by the national agency CONICET, the Province of Buenos Aires agency CIC, and the National University of La Plata (UNLP).

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Search for Continuous Gravitational Waves from Known Pulsars in the First Part of the Fourth LIGO-Virgo-KAGRA Observing Run

Publicado en:Astrophysical Journal. 983 (2): 99- - 2025-04-20 983(2), DOI: 10.3847/1538-4357/adb3a0

Autores: Abac, A G; Abbott, R; Abouelfettouh, I; Acernese, F; Ackley, K; Adhicary, S; Adhikari, N; Adhikari, R X; Adkins, V K; Agarwal, D; Agathos, M; Abchouyeh, M Aghaei; Aguiar, O D; Aguilar, I; Aiello, L; Ain, A; Ajith, P; Akutsu, T; Albanesi, S; Alfaidi, R A; Al-Jodah, A; Allene, C; Allocca, A; Al-Shammari, S; Altin, P A; Alvarez-Lopez, S; Amato, A; Amez-Droz, L; Amorosi, A; Amra, C; Ananyeva, A; Anderson, S B; Anderson, W G; Andia, M; Ando, M; Andrade, T; Andres, N; Andres-Carcasona, M; Andric, T; Anglin, J; Ansoldi, S; Antelis, J M; Antier, S; Aoumi, M; Appavuravther, E Z; Appert, S; Apple, S K; Arai, K; Araya, A; Araya, M C; Areeda, J S; Argianas, L; Aritomi, N; Armato, F; Arnaud, N; Arogeti, M; Aronson, S M; Ashton, G; Aso, Y; Assiduo, M; Melo, S Assis de Souza; Aston, S M; Astone, P; Attadio, F; Aubin, F; AultONeal, K; Avallone, G; Babak, S; Badaracco, F; Badger, C; Bae, S; Bagnasco, S; Bagui, E; Baier, J G; Baiotti, L; Bajpai, R; Baka, T; Ball, M; Ballardin, G; Ballmer, S W; Banagiri, S; Banerjee, B; Bankar, D; Baral, P; Barayoga, J C; Barish, B C; Barker, D; Barneo, P; Barone, F; Barr, B; Barsotti, L; Barsuglia, M; Barta, D; Bartoletti, A M; Barton, M A; Bartos, I; Basak, S; Basalaev, A; Bassiri, R; Basti, A; Bates, D E; Bawaj, M; Baxi, P; Bayley, J C; Baylor, A C; Baynard, P A, II; Bazzan, M; Bedakihale, V M; Beirnaert, F; Bejger, M; Belardinelli, D; Bell, A S; Benedetto, V; Benoit, W; Bentley, J D; Ben Yaala, M; Bera, S; Berbel, M; Bergamin, F; Berger, B K; Bernuzzi, S; Beroiz, M; Bersanetti, D; Bertolini, A; Betzwieser, J; Beveridge, D; Bevins, N; Bhandare, R; Bhardwaj, U; Bhatt, R; Bhattacharjee, D; Bhaumik, S; Bhowmick, S; Bianchi, A; Bilenko, I A; Billingsley, G; Binetti, A; Bini, S; Birnholtz, O; Biscoveanu, S; Bisht, A; Bitossi, M; Bizouard, M -A; Blackburn, J K; Blagg, L A; Blair, C D; Blair, D G; Bobba, F; Bode, N; Boileau, G; Boldrini, M; Bolingbroke, G N; Bolliand, A; Bonavena, L D; Bondarescu, R; Bondu, F; Bonilla, E; Bonilla, M S; Bonino, A; Bonnand, R; Booker, P; Borchers, A; Boschi, V; Bose, S; Bossilkov, V; Boudart, V; Boudon, A; Bozzi, A; Bradaschia, C; Brady, P R; Braglia, M; Branch, A; Branchesi, M; Brandt, J; Braun, I; Breschi, M; Briant, T; Brillet, A; Brinkmann, M; Brockill, P; Brockmueller, E; Brooks, A F; Brown, B C; Brown, D D; Brozzetti, M L; Brunett, S; Bruno, G; Bruntz, R; Bryant, J; Bucci, F; Buchanan, J; Bulashenko, O; Bulik, T; Bulten, H J; Buonanno, A; Burtnyk, K; Buscicchio, R; Buskulic, D; Buy, C; Byer, R L; Davies, G S Cabourn; Cabras, G; Cabrita, R; Caceres-Barbosa, V; Cadonati, L; Cagnoli, G; Cahillane, C; Calderon Bustillo, J; Callister, T A; Calloni, E; Camp, J B; Canepa, M; Santoro, G Caneva; Cannon, K C; Cao, H; Capistran, L A; Capocasa, E; Capote, E; Carapella, G; Carbognani, F; Carlassara, M; Carlin, J B; Carpinelli, M; Carrillo, G; Carter, J J; Carullo, G; Diaz, J Casanueva; Casentini, C; Castro-Lucas, S Y; Caudill, S; Cavaglia, M; Cavalieri, R; Cella, G; Cerda-Duran, P; Cesarini, E; Chaibi, W; Chakraborty, P; Subrahmanya, S Chalathadka; Chan, J C L; Chan, M; Chandra, K; Chang, R -J; Chao, S; Charlton, E L; Charlton, P; Chassande-Mottin, E; Chatterjee, C; Chatterjee, Debarati; Chatterjee, Deep; Chaturvedi, M; Chaty, S; Chen, A; Chen, A H -Y; Chen, D; Chen, H; Chen, H Y; Chen, J; Chen, K H; Chen, Y; Chen, Yanbei; Chen, Yitian; Cheng, H P; Chessa, P; Cheung, H T; Cheung, S Y; Chiadini, F; Chiarini, G; Chierici, R; Chincarini, A; Chiofalo, M L; Chiummo, A; Chou, C; Choudhary, S; Christensen, N; Chua, S S Y; Chugh, P; Ciani, G; Ciecielag, P; Cieslar, M; Cifaldi, M; Ciolfi, R; Clara, F; Clark, J A; Clarke, J; Clarke, T A; Clearwater, P; Clesse, S; Coccia, E; Codazzo, E; Cohadon, P -F; Colace, S; Colleoni, M; Collette, C G; Collins, J; Colloms, S; Colombo, A; Colpi, M; Compton, C M; Connolly, G; Conti, L; Corbitt, T R; Cordero-Carrion, I; Corezzi, S; Cornish, N J; Corsi, A; Cortese, S; Costa, C A; Cottingham, R; Coughlin, M W; Couineaux, A; Coulon, J -P; Countryman, S T; Coupechoux, J -F; 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Resumen

Continuous gravitational waves (CWs) emission from neutron stars carries information about their internal structure and equation of state, and it can provide tests of general relativity. We present a search for CWs from a set of 45 known pulsars in the first part of the fourth LIGO-Virgo-KAGRA observing run, known as O4a. We conducted a targeted search for each pulsar using three independent analysis methods considering single-harmonic and dual-harmonic emission models. We find no evidence of a CW signal in O4a data for both models and set upper limits on the signal amplitude and on the ellipticity, which quantifies the asymmetry in the neutron star mass distribution. For the single-harmonic emission model, 29 targets have the upper limit on the amplitude below the theoretical spin-down limit. The lowest upper limit on the amplitude is 6.4 x 10(-27) for the young energetic pulsar J0537-6910, while the lowest constraint on the ellipticity is 8.8 x 10(-9) for the bright nearby millisecond pulsar J0437-4715. Additionally, for a subset of 16 targets, we performed a narrowband search that is more robust regarding the emission model, with no evidence of a signal. We also found no evidence of nonstandard polarizations as predicted by the Brans-Dicke theory.

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