Figure 6 from The NANOGrav 11 yr Data Set: Limits on Gravitational Waves from Individual Supermassive Black Hole Binaries

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The NANOGrav 11 yr Data Set: Limits on Gravitational Waves from Individual Supermassive Black Hole Binaries

Authors: K. Aggarwal, Z. Arzoumanian, P. T. Baker, A. Brazier, M. R. Brinson, P. R. Brook, S. Burke-Spolaor, S. Chatterjee, J. M. Cordes, N. J. Cornish, F. Crawford, K. Crowter, H. T. Cromartie, M. DeCesar, P. B. Demorest, T. Dolch, J. A. Ellis, R. D. Ferdman, E. Ferrara, E. Fonseca, N. Garver-Daniels, P. Gentile, J. S. Hazboun, A. M. Holgado, E. A. Huerta, K. Islo, G. Jones, M. L. Jones, A. R. Kaiser, D. L. Kaplan, J. S. Key, M. T. Lam, T. J. W. Lazio, L. Levin, D. R. Lorimer, J. Luo, R. S. Lynch, D. R. Madison, M. A. McLaughlin, S. T. McWilliams, C. M. F. Mingarelli, C. Ng, D. J. Nice, T. T. Pennucci, N. S. Pol, S. M. Ransom, P. S. Ray, X. Siemens, J. Simon, R. Spiewak, I. H. Stairs, D. R. Stinebring, K. Stovall, J. Swiggum, S. R. Taylor, J. E. Turner, M. Vallisneri, R. van Haasteren, S. J. Vigeland, C. A. Witt, and W. W. Zhu

2019 The Astrophysical Journal 880 116.

Provider: AAS Journals

Caption: Figure 6.

Comparison between a search at ﹩{f}_{\mathrm{gw}}=15\,\mathrm{nHz}﹩ performed on the 9 yr data set with all pulsars (orange) and excluding PSR J0613−0200 (purple). There was very little difference between the Bayes factors (﹩{{ \mathcal B }}_{10}=1.4(1)﹩ with all pulsars, and ﹩{{ \mathcal B }}_{10}=1.11(4)﹩ excluding PSR J0613−0200), but there was a significant difference in the 95% strain upper limit. We found an upper limit of 4.1(2) × 10⁻¹⁴ with all pulsars, compared with 3.2(3) × 10⁻¹⁴ without PSR J0613−0200.

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