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@ARTICLE{Liu:485765,
      author       = {Liu, Yijin and Ajello, M. and Atwood, W. B. and Baldini, L.
                      and Ballet, J. and Barbiellini, G. and Bastieri, D. and
                      Bellazzini, R. and Berretta, A. and Bhattacharyya, B. and
                      Bissaldi, E. and Blandford, R. D. and Bloom, E. and Bonino,
                      R. and Bruel, P. and Bühler, Rolf and Burns, E. and Buson,
                      S. and Cameron, R. A. and Caraveo, P. A. and Cavazzuti, E.
                      and Cibrario, N. and Ciprini, S. and Clark, C. J. and
                      Cognard, I. and Coronado-Blázquez, J. and Crnogorcevic, M.
                      and Cromartie, H. and Crowter, K. and Cutini, S. and
                      D'Ammando, F. and Gaetano, S. D. and Palma, F. d. and Digel,
                      S. W. and Lalla, N. D. and Fana Dirirsa, F. and Venere, L.
                      D. and Domínguez, A. and Ferrara, E. C. and Fiori, A. and
                      Franckowiak, A. and Fukazawa, Y. and Funk, S. and Fusco, P.
                      and Gammaldi, V. and Gargano, F. and Gasparrini, D. and
                      Giglietto, N. and Giordano, F. and Giroletti, M. and Green,
                      D. and Grenier, I. A. and Guillemot, L. and Guiriec, S. and
                      Gustafsson, M. and Harding, A. K. and Hays, E. and Hewitt,
                      J. W. and Horan, D. and Hou, X. and Jóhannesson, G. and
                      Keith, M. J. and Kerr, M. and Kramer, M. and Kuss, M. and
                      Larsson, S. and Latronico, L. and Li, J. and Longo, F. and
                      Loparco, F. and Lovellette, M. N. and Lubrano, P. and
                      Maldera, S. and Manfreda, A. and Martí-Devesa, G. and
                      Mazziotta, M. N. and Mereu, I. and Michelson, P. F. and
                      Mirabal, N. and Mitthumsiri, W. and Mizuno, T. and Monzani,
                      M. E. and Morselli, A. and Negro, M. and Nieder, L. and
                      Ojha, R. and Omodei, N. and Orienti, M. and Orlando, E. and
                      Ormes, J. F. and Paneque, D. and Parthasarathy, A. and Pei,
                      Z. and Persic, M. and Pesce-Rollins, M. and Pillera, R. and
                      Poon, H. and Porter, T. A. and Principe, G. and Racusin, J.
                      L. and Rainò, S. and Rando, R. and Rani, B. and Ransom, S.
                      M. and Ray, P. S. and Razzano, M. and Razzaque, S. and
                      Reimer, A. and Reimer, O. and Roy, J. and Sánchez-Conde, M.
                      and Parkinson, P. M. Sa. and Scargle, J. and Scotton, L. and
                      Serini, D. and Sgrò, C. and Siskind, E. J. and Smith, D. A.
                      and Spandre, G. and Spiewak, R. and Spinelli, P. and Stairs,
                      I. and Suson, D. J. and Swihart, S. J. and Tabassum, S. and
                      Thayer, J. B. and Theureau, G. and Torres, D. F. and Troja,
                      E. and Valverde, J. and Wadiasingh, Z. and Wood, K. and
                      Zaharijas, G.},
      collaboration = {Fermi-{LAT Collaboration}},
      title        = {{A} gamma-ray pulsar timing array constrains the nanohertz
                      gravitational wave background},
      reportid     = {PUBDB-2022-06831, arXiv:2204.05226},
      year         = {2022},
      note         = {ISSN 1095-9203 not unique: **3 hits**.3 figures in the main
                      text. 3 figures and 8 tables are in the supplementary
                      material},
      abstract     = {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 $t^{−13/6}_{obs}$.
                      This direct measurement provides an independent probe of the
                      GWB while offering a check on radio noise models.},
      keywords     = {gravitational radiation: background (INSPIRE) / pulsar
                      (INSPIRE) / gamma ray (INSPIRE) / binary (INSPIRE) / noise
                      (INSPIRE) / monitoring (INSPIRE) / black hole (INSPIRE) /
                      radio wave (INSPIRE) / GLAST (INSPIRE) / galaxy (INSPIRE)},
      cin          = {ZEU-EXP/AT},
      ddc          = {320},
      cid          = {$I:(DE-H253)ZEU-EXP_AT-20120731$},
      pnm          = {613 - Matter and Radiation from the Universe (POF4-613)},
      pid          = {G:(DE-HGF)POF4-613},
      experiment   = {EXP:(DE-H253)Fermi-20170101},
      typ          = {PUB:(DE-HGF)25},
      eprint       = {2204.05226},
      howpublished = {arXiv:2204.05226},
      archivePrefix = {arXiv},
      SLACcitation = {$\%\%CITATION$ = $arXiv:2204.05226;\%\%$},
      pubmed       = {pmid:35389746},
      url          = {https://bib-pubdb1.desy.de/record/485765},
}