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Pulsar timing arrays have found evidence for a low-frequency gravitationalwave background (GWB). Assuming the GWB is produced by supermassive black holebinaries (SMBHBs), the next gravitational wave (GW) signals astronomersanticipate are Continuous Waves (CWs) from single SMBHBs and their associatedGWB anisotropy. The prospects for detecting CWs and anisotropy are highlydependent on the astrophysics of SMBHB populations. Thus, information fromsingle sources can break degeneracies in astrophysical models and place muchmore stringent constraints than the GWB alone. We simulate and evolve SMBHBpopulations, model their GWs, and calculate their anisotropy and detectability.We investigate how varying components of our semi-analytic model, including thegalaxy stellar mass function, the SMBH--host galaxy relation($M_\mathrm{BH}$--$M_\mathrm{bulge}$), and the binary evolution prescriptionimpact the expected detections. The CW occurrence rate is greatest for fewtotal binaries, high SMBHB masses, large scatter in$M_\mathrm{BH}$--$M_\mathrm{bulge}$, and long hardening times. The occurrencerate depends most on the binary evolution parameters, implying that CWs offer anovel avenue to probe binary evolution. The most detectable CW sources are inthe lowest frequency bin for a 16.03-year PTA, have masses from$\sim\!\!10^9-10^{10}\mathrm{M}_\odot$, and are $\sim\!\!1$ Gpc away. The levelof anisotropy increases with frequency, with the angular power spectrum overmultipole modes $\ell$ varying in low-frequency $C_{\ell>0}/C_0$ from$\sim\!\!5\times 10^{-3}$ to $\sim\!\!2\times10^{-1}$, depending on the model;typical values are near current upper limits. Observing this anisotropy wouldsupport SMBHB models for the GWB over cosmological models, which tend to beisotropic.

Beyond the Background: Gravitational Wave Anisotropy and Continuous Waves from Supermassive Black Hole Binaries