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The two pulsating pre-main sequence (PMS) stars V 588 Mon and V 589 Mon wereobserved by CoRoT for 23.4 days in March 2008 during the Short Run SRa01 and in2004 and 2006 by MOST for a total of ~70 days. We present their photometricvariability up to 1000 $\mu$ Hz and down to residual amplitude noise levels of23 and 10 ppm of the CoRoT data for V 588 Mon and V 589 Mon, respectively. TheCoRoT imagette data as well as the two MOST data sets allowed for detailedfrequency analyses using Period04 and SigSpec. We confirm all previouslyidentified frequencies, improve the known pulsation spectra to a total of 21frequencies for V 588 Mon and 37 for V 589 Mon and compare them to our PMSmodel predictions. No model oscillation spectrum with l = 0, 1, 2, and 3p-modes matches all the observed frequencies. When rotation is included we findthat the rotationally split modes of the slower rotating star, V 589 Mon, areaddressable via perturbative methods while for the more rapidly rotating star,V 588 Mon, they are not and, consequently, will require more sophisticatedmodeling. The high precision of the CoRoT data allowed us to investigate thelarge density of frequencies found in the region from 0 to 300 $\mu$Hz. Thepresence of granulation appears to be a more attractive explanation than theexcitation of high-degree modes. Granulation was modeled with a superpositionof white noise, a sum of Lorentzian-like functions and a Gaussian. Our analysisclearly illustrates the need for a more sophisticated granulation model.

Pulsational analysis of V 588 Mon and V 589 Mon observed with the MOST and CoRoT satellites