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Solar-like oscillations have been observed by Kepler and CoRoT in manysolar-type stars, thereby providing a way to probe the stars usingasteroseismology. We provide the mode linewidths and mode heights of theoscillations of various stars as a function of frequency and of effectivetemperature. We used a time series of nearly two years of data for each star.The 23 stars observed belong to the simple or F-like category. The powerspectra of the 23 main-sequence stars were analysed using both maximumlikelihood estimators and Bayesian estimators, providing individual modecharacteristics such as frequencies, linewidths, and mode heights. We study thesource of systematic errors in the mode linewidths and mode heights, and wepresent a way to correct these errors with respect to a common reference fit.Using the correction, we could explain all sources of systematic errors, whichcould be reduced to less than $\pm$15% for mode linewidths and heights, andless than $\pm$5% for amplitude, when compared to the reference fit. The effectof a different estimated stellar background and a different estimated splittingwill provide frequency-dependent systematic errors that might affect thecomparison with theoretical mode linewidth and mode height, therefore affectingthe understanding of the physical nature of these parameters. All other sourcesof relative systematic errors are less dependent upon frequency. We alsoprovide the dependence of the so-called linewidth dip, in the middle of theobserved frequency range, as a function of effective temperature. We show thatthe depth of the dip decreases with increasing effective temperature. Thedependence of the dip on effective temperature may imply that the mixing lengthparameter $\alpha$ or the convective flux may increase with effectivetemperature.

Oscillation mode linewidths and heights of 23 main-sequence stars observed by Kepler