AJELLO, M.; ATWOOD, W.B.; BALDINI, L.; BALLET, J.; BARBIELLINI, G.; BASTIERI, D.; BELLAZZINI, R.; BERRETTA, A.; BHATTACHARYYA, B.; BISSALDI, E.; BLANDFORD, R.D.; BLOOM, E.; BONINO, R.; BRUEL, P.; BUEHLER, R.; BURNS, E.; BUSON, S.; CAMERON, R.A.; CARAVEO, P.A.; CAVAZZUTI, E.; CIBRARIO, N.; CIPRINI, S.; CLARK, C.J.; COGNARD, I.; CORONADO-BLAZQUEZ, J.; CRNOGORCEVIC, M.; CROMARTIE, H.; CROWTER, K.; CUTINI, S.; D'AMMANDO, F.; DE GAETANO, S.; DE PALMA, F.; DIGEL, S.W.; DI LALLA, N.; DIRIRSA, F. Fana; DI VENERE, L.; DOMÍNGUEZ, A.; FERRARA, E.C.; FIORI, A.; FRANCKOWIAK, A.; FUKAZAWA, Y.; FUNK, S.; FUSCO, P.; GAMMALDI, V.; GARGANO, F.; GASPARRINI, D.; GIGLIETTO, N.; GIORDANO, F.; GIROLETTI, M.; GREEN, D.; GRENIER, I.A.; GUILLEMOT, L.; GUIRIEC, S.; GUSTAFSSON, M.; HARDING, A.K.; HAYS, E.; HEWITT, J.W.; HORAN, D.; HOU, X.; JOHANNESSON, G.; KEITH, M.J.; KERR, M.; KRAMER, M.; KUSS, M.; LARSSON, S.; LATRONICO, L.; LI, J.; LONGO, F.; LOPARCO, F.; LOVELLETTE, M.N.; LUBRANO, P.; MALDERA, S.; MANFREDA, A.; MARTÍ-DEVESA, G.; MAZZIOTTA, M.N.; MEREU, I.; MICHELSON, P.F.; MIRABAL, N.; MITTHUMSIRI, W.; MIZUNO, T.; MONZANI, M.E.; MORSELLI, A.; NEGRO, M.; NIEDER, L.; OJHA, R.; OMODEI, N.; ORIENTI, M.; ORLANDO, E.; ORMES, J.F.; PANEQUE, D.; PARTHASARATHY, A.; PEI, Z.; PERSIC, M.; PESCE-ROLLINS, M.; PILLERA, R.; POON, H.; PORTER, T.A.; PRINCIPE, G.; RACUSIN, J.L.; RAINO, S.; RANDO, R.; RANI, B.; RANSOM, S.M.; RAY, P.S.; RAZZANO, M.; RAZZAQUE, S.; REIMER, A.; REIMER, O.; ROY, J.; SANCHEZ-CONDE, M.; SAZ PARKINSON, P.M.; SCARGLE, J.; SCOTTON, L.; SERINI, D.; SGRO, C.; SISKIND, E.J.; SMITH, D.A.; SPANDRE, G.; SPIEWAK, R.; SPINELLI, P.; STAIRS, I.; SUSON, D.J.; SWIHART, S.J.; TABASSUM, S.; THAYER, J.B.; THEUREAU, G.; TORRES, D.F.; TROJA, E.; VALVERDE, J.; WADIASINGH, Z.; WOOD, K.; ZAHARIJAS, G.

doi:10.1126/science.abm3231

Métadonnées

Afficher la notice complète

Licence d’utilisation du document

Langue

Article de revue

Ce document a été publié dans

Science. 2022, vol. 376, n° 6592, p. abm3231

Résumé en anglais

After large galaxies merge, their central supermassive black holes are expected to form binary systems. Their orbital motion should generate a gravitational wave background (GWB) at nanohertz frequencies. Searches for this background use pulsar timing arrays, which perform long-term monitoring of millisecond pulsars at radio wavelengths. We used 12.5 years of Fermi Large Area Telescope data to form a gamma-ray pulsar timing array. Results from 35 bright gamma-ray pulsars place a 95% credible limit on the GWB characteristic strain of 1.0 × 10−14 at a frequency of 1 year–1. The sensitivity is expected to scale with tobs, the observing time span, as t−13/6obs. This direct measurement provides an independent probe of the GWB while offering a check on radio noise models.< Réduire

Mots clés en anglais

gravitational radiation: background

pulsar

gamma ray

binary

noise

monitoring

black hole

radio wave

GLAST

galaxy

Métadonnées

Partager cette publication !

Licence d’utilisation du document

A gamma-ray pulsar timing array constrains the nanohertz gravitational wave background

Langue

Ce document a été publié dans

Résumé en anglais

Mots clés en anglais

URI

DOI

Origine

Unités de recherche