We note that another observation with somewhat shorter exposure time was obtained two days earlier; these data, however, were strongly affected by a high, flaring radiation background and were therefore not used in our analysis.

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According to the XMM-Newton Users' Handbook, photon pile up occurs only for PN count rates exceeding 8 cnts/s.

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... stochastic

Given the flare probability for each source of $p = 8.3\%$ , the probability to observe k flares among the 12 sources is P(k) = ${12 \choose k}~p^k~(1-p)^{12-k}$ .

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... PIMMS

PIMMS is the Portable, Interactive Multi-Mission Simulator provided by the HEASARC Online Service; for further information see http://heasarc.gsfc.nasa.gov/Tools/w3pimms.html

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... tracer

We note that we detect X-ray emission from the YSO EC 105, which seems to be associated with a molecular hydrogen outflow (Herbst et al. 1997). The characteristics of the observed X-ray emission, however, is fully consistent with the assumption of coronal emission from the young star EC 105, and there is no indication for any contribution from the outflow. Also, it is not clear whether the source of the outflow actually is EC 105 or a nearby deeply embedded object (SMM-3; see Herbst et al. 1997).

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... source

We note that the previous analysis of the ROSAT data could not fully exclude the possibility that the faint X-ray emission ( ${\sim} 20$ source counts) might come from EC 92, 5'' to the north, rather than from EC 95. In our XMM-Newton image, this source has more than 1000 counts and we could achieve a much better astrometric calibration due to the larger number of detected sources. Our analysis clearly shows that the X-ray source is identified with EC 95, and not with EC 92.

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... probability

The statistical acceptance Q gives the probability that the deviations between the observed spectrum and the model spectrum are only due to statistical measurement errors (see e.g. Press et al. 1986).

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... temperature

The observed plasma temperature of ${\sim} 30$ MK would require wind velocities of the order of ${\ga} 1000$ km s^-1, much larger than typical for low-luminosity YSOs.

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... SVS 16

SVS 16 was recently confirmed to be a flat-spectrum source by Rebull et al. (2003).

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