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Figure 1: The central   region of the XMM-Newton image of the Serpens cloud. The image is the sum of the MOS1+MOS2+PN exposures of the three merged data sets (summed exposure time of 46.1 ks for the PN camera and 52.4 ks for each of the two MOS cameras) in the  [0.2-10] keV energy band, binned to   pixels, and is displayed with a linear intensity scale ( , ). The infrared positions of the class I protostars in this area (Kaas et al. 2004) are marked by circles and labeled.

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In the text

	Figure 2: XMM-Newton-EPIC-PN lightcurves of the class I protostars PS 1, EC 53, EC 80, and EC 89, the class II object EC 74, and the flat spectrum source EC 95. The histograms show the number of counts per 20 min time bin after correction for background. In the plot for EC 95, the asterisks show the counts in the background region, scaled to the area of each source extraction region.
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In the text

	Figure 3: XMM-Newton-EPIC-PN spectra of the class I protostars PS 1 and EC 89, and the class II object EC 74. The solid dots with error bars show the observed spectrum, the histogram shows the best fit model.
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In the text

	Figure 4: K-band magnitude versus spectral index between m and m,  for the class I protostars in Serpens from the study of Kaas et al. (2004). The four X-ray detected objects are marked by  X signs and labeled.
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In the text