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We employ gravitational-wave radiometry to map the gravitational wavesstochastic background expected from a variety of contributing mechanisms andtest the assumption of isotropy using data from Advanced LIGO's first observingrun. We also search for persistent gravitational waves from point sources withonly minimal assumptions over the 20 - 1726 Hz frequency band. Finding noevidence of gravitational waves from either point sources or a stochasticbackground, we set limits at 90% confidence. For broadband point sources, wereport upper limits on the gravitational wave energy flux per unit frequency inthe range $F_{\alpha,\Theta}(f) < (0.1 - 56) \times 10^{-8}$ erg cm$^{-2}$s$^{-1}$ Hz$^{-1}$ (f/25 Hz)$^{\alpha-1}$ depending on the sky location$\Theta$ and the spectral power index $\alpha$. For extended sources, we reportupper limits on the fractional gravitational wave energy density required toclose the Universe of $\Omega(f,\Theta) < (0.39-7.6) \times 10^{-8}$ sr$^{-1}$(f/25 Hz)$^\alpha$ depending on $\Theta$ and $\alpha$. Directed searches fornarrowband gravitational waves from astrophysically interesting objects(Scorpius X-1, Supernova 1987 A, and the Galactic Center) yield medianfrequency-dependent limits on strain amplitude of $h_0 <$ (6.7, 5.5, and 7.0)$\times 10^{-25}$ respectively, at the most sensitive detector frequenciesbetween 130 - 175 Hz. This represents a mean improvement of a factor of 2across the band compared to previous searches of this kind for these skylocations, considering the different quantities of strain constrained in eachcase.

Directional limits on persistent gravitational waves from Advanced LIGO's first observing run