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The stochastic gravitational-wave background is a superposition of sourcesthat are either too weak or too numerous to detect individually. In this studywe present the results from a cross-correlation analysis on data from AdvancedLIGO's second observing run (O2), which we combine with the results of thefirst observing run (O1). We do not find evidence for a stochastic background,so we place upper limits on the normalized energy density in gravitationalwaves at the 95% credible level of $\Omega_{\rm GW}<6.0\times 10^{-8}$ for afrequency-independent (flat) background and $\Omega_{\rm GW}<4.8\times 10^{-8}$at 25 Hz for a background of compact binary coalescences. The upper limitimproves over the O1 result by a factor of 2.8. Additionally, we place upperlimits on the energy density in an isotropic background of scalar- andvector-polarized gravitational waves, and we discuss the implication of theseresults for models of compact binaries and cosmic string backgrounds. Finally,we present a conservative estimate of the correlated broadband noise due to themagnetic Schumann resonances in O2, based on magnetometer measurements at boththe LIGO Hanford and LIGO Livingston observatories. We find that correlatednoise is well below the O2 sensitivity.

Search for the isotropic stochastic background using data from Advanced LIGO's second observing run