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

## TL;DR

This paper reports a search for the isotropic stochastic gravitational-wave background using Advanced LIGO's second observing run data, setting upper limits and discussing implications for astrophysical models and noise sources.

## Contribution

First combined analysis of O1 and O2 LIGO data for stochastic background, providing improved upper limits and insights into noise and polarization models.

## Key findings

- No evidence for stochastic background was detected.
- Upper limits on gravitational wave energy density were established.
- Correlated magnetic noise was found to be below sensitivity levels.

## Abstract

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