We present the asteroseismic analysis of 1948 F- , G- and K-type main-sequence and subgiant stars observed by the NASA Kepler Mission .
We detect and characterise solar-like oscillations in 642 of these stars .
This represents the largest cohort of main-sequence and subgiant solar-like oscillators observed to date .
The photometric observations are analysed using the methods developed by nine independent research teams .
The results are combined to validate the determined global asteroseismic parameters and calculate the relative precision by which the parameters can be obtained .
We correlate the relative number of detected solar-like oscillators with stellar parameters from the Kepler Input Catalog and find a deficiency for stars with effective temperatures in the range 5300 \lesssim T _ { \mathrm { eff } } \lesssim 5700 K and a drop-off in detected oscillations in stars approaching the red edge of the classical instability strip .
We compare the power-law relationships between the frequency of peak power , \nu _ { \mathrm { max } } , the mean large frequency separation , \Delta \nu , and the maximum mode amplitude , A _ { \mathrm { max } } , and show that there are significant method-dependent differences in the results obtained .
This illustrates the need for multiple complementary analysis methods to be used to assess the robustness and reproducibility of results derived from global asteroseismic parameters .