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<jats:title>ABSTRACT</jats:title> <jats:p>Extreme ultraviolet (EUV) coronal dimmings are often observed in response to solar eruptive events. These phenomena can be generated via several different physical processes. For space weather, the most important of these is the temporary void left behind by a coronal mass ejection (CME). Massive, fast CMEs tend to leave behind a darker void that also usually corresponds to minimum irradiance for the cooler coronal emissions. If the dimming is associated with a solar flare, as is often the case, the flare component of the irradiance light curve in the cooler coronal emission can be isolated and removed using simultaneous measurements of warmer coronal lines. We apply this technique to 37 dimming events identified during two separate two-week periods in 2011 plus an event on 2010 August 7, analyzed in a previous paper to parameterize dimming in terms of depth and slope. We provide statistics on which combination of wavelengths worked best for the flare-removal method, describe the fitting methods applied to the dimming light curves, and compare the dimming parameters with corresponding CME parameters of mass and speed. The best linear relationships found are</jats:p> <jats:p> <jats:inline-formula> <jats:tex-math> <?CDATA \begin{eqnarray*}{v}_{\mathrm{CME}}\ \left[\displaystyle \frac{\mathrm{km}}{{\rm{s}}}\right] & \approx & 2.36\times {10}^{6}\ \left[\displaystyle \frac{\mathrm{km}}{ \% }\right]\times {s}_{\dim }\ \left[\displaystyle \frac{ \% }{{\rm{s}}}\right]\\ {m}_{\mathrm{CME}}\ [{\rm{g}}] & \approx & 2.59\times {10}^{15}\left[\displaystyle \frac{g}{ \% }\right]\times \sqrt{{d}_{\dim }}\ [ \% ].\end{eqnarray*}?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa34a8ueqn1.gif" xlink:type="simple" /> </jats:inline-formula> </jats:p> <jats:p>These relationships could be used for space weather operations of estimating CME mass and speed using near-real-time irradiance dimming measurements.</jats:p>