All Tables

Table 1: Results for all objects. We list all observed objects grouped by membership (MBM12, in-cloud (in TA), off-cloud Taurus-Auriga (off TA), or Orion) and sorted in order of ascending right ascension. The object name is the most common one used in literature - in one case the Guide Star Catalog number was used. The second column gives the observing run in which the object was observed. The calculated period together with the 1 $\sigma$ error is given in the next column followed by periods as determined by other groups. In the next five columns, $v \sin i$ values from literature, the spectral type, the classification of the object (w: wTTS,c: cTTS,Z: ZAMS, MS: main sequence, ?: unknown) together with the relevant quantities for the lithium-test ( $W_{\lambda }({\rm Li})$ , $W_{\lambda }({\rm H}\alpha )$ ) are given. Negative values stand for emission, f means the absorption lines are partially filled by emission. The last columns give comments on the nature of the object where relevant (SB1/2: single/double-lined spectroscopic binary). For all values, the sources are given as footnotes at the bottom of the table.
Table 2: Results of the two-sample tests. The tested hypothesis was H₀: F₁ (t) = F₂ (t): both samples are equal. The probability p of H₀ being true is given for the three tests. This shows that the two samples must be considered equal.
Table A.1: Measured periods, variability amplitudes, and errors of all objects in Run I. In this table all measurements in the filters VRI are given. The first column gives the total time span covered by the observations followed by the total airmass range of the observations. The next columns describe the noise in each band. For each filter X, the amplitude of variation $\Delta m_{\rm X}$ , the standard deviation of the object $\sigma _{\rm X}$ , the standard deviation of the averaged comparison star $\sigma _{\rm X}^{{\rm av.}}$ , as well as the number of data points are listed. Hence, the variation of the object can be compared to the noise level of the reference stars. The last column gives the determined period together with the 1 $\sigma$ -error. The numbers in parentheses refer to some comments in the footnotes.
Table A.2: Measured periods, variability amplitudes, and errors of all objects in Run II. In this table, the results in the filters V and B are given. The information is the same as for Run I in Table A.1.
Table A.3: Measured periods and variability amplitudes in Run III. The second column lists the determined periods with estimated error interval, the last column gives the amplitude of the unfiltered brightness variation in magnitudes. All results are consistent with Run I and II measurements.
Table A.4: Stellar parameters relevant for the Hertzsprung-Russell Diagram of all objects. The objects are grouped by type and sorted by right ascension. For the objects in Taurus, a distance of $140~{\rm pc}$ is assumed, for MBM12 $90~{\rm pc}$ . The color excess that was used to calculate the extinction A_V is given in the neighboring column. To get the real colors of the objects we used the spectral type - color conversion from Kenyon & Hartmann (1995) for early spectral types and Leggett (1992) for type M0 and later. The masses and ages are interpolated from pre main sequence models by D'Antona & Mazzitelli (1994). The apparent magnitudes in V for objects observed in Run I was determined by absolute photometry ourselves. For Run II objects we had to rely on VizieR (Ochsenbein et al. 2000) values - we averaged all available values. For more details see text.
Table A.5: All wTTS in the comparison sample. They have been known prior to the ROSAT All-Sky Survey. The table lists the rotational period together with the classification of the object. All objects are weak-line TTS, wb stands for binarity, wt for triple system, wsb is a double-lined spectroscopic binary. The last column states if the object was detected with the Einstein observatory (marked with X) and is therefore X-ray selected like the stars found by ROSAT.