Figure 5 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 5.

The 95% upper limit on the GW strain amplitude from a circular SMBHB with ﹩{f}_{\mathrm{gw}}=8\,\mathrm{nHz}﹩ as a function of sky position from an analysis of the 11 yr data set, plotted in equatorial coordinates using the Mollweide projection. We used the DE436 ephemeris model with BAYESEPHEM to model uncertainty in the SSB. The positions of pulsars in our array are indicated by stars, and the most sensitive sky location is indicated by a red circle. The 95% upper limit ranged from 2.0(1) × 10⁻¹⁵ at our most sensitive sky location to ﹩1.34(4)\times {10}^{-14}﹩ at our least sensitive sky location.

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