Figure 4 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 4.

Sky-averaged 95% upper limit on the GW strain amplitude from a circular SMBHB as a function of GW frequency, with and without BAYESEPHEM (solid blue curve and dashed red curve, respectively). At the lowest frequencies (﹩{f}_{\mathrm{gw}}\lesssim 4\,\mathrm{nHz}﹩), the analysis with BAYESEPHEM was more sensitive than the analysis without it, but there was no difference in sensitivity at higher frequencies.

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