A&A 377, 538-556 (2001)
DOI: 10.1051/0004-6361:20011093

X-ray emission from young stars in Taurus-Auriga-Perseus: Luminosity functions and the rotation - activity - age - relation

B. Stelzer - R. Neuhäuser

Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, 85741 Garching, Germany

Received 4 September 2000 / Accepted 26 July 2001

Abstract
We report on a systematic search for X-ray emission from pre-main sequence and young main sequence stars in the Taurus-Auriga-Perseus region. Our stellar sample consists of all T Tauri stars from the Taurus-Auriga region, and all late-type stars from the Pleiades and Hyades clusters which have been observed by the ROSAT PSPC in pointed observations. We present the X-ray parameters for all observed stars in tables. Next to the basic results of the data analysis (such as count rates, exposure time, and off-axis angle) we give X-ray luminosities and hardness ratios for all detected stars. Upper limits are given for non-detections. Detection rates for different spectral types are compiled. We use these results to study the connection between coronal X-ray activity and stellar parameters for different subgroups of our sample. In particular we compile X-ray luminosity functions (XLF), and discuss the relations between X-ray emission and spectral type, age, and rotation, which have been disputed extensively in the past. Here, we study these questions with the largest sample so far. The XLF for classical and weak-line T Tauri stars are different, with weak-lines being the stronger X-ray emitters. Proceeding towards the main-sequence (Pleiades, Hyades) the X-ray luminosity declines for all spectral types examined (G, K, and M stars). Within an age group $L_{\rm x}$ decreases towards later spectral types, while $L_{\rm x}/L_{\rm bol}$ remains constant or even increases, reflecting the opposed influence of stellar radius, i.e. emitting area, and convection zone depth. For a given spectral type the fastest rotators show the highest X-ray luminosity. Rotation rate and X-ray emission are clearly correlated for all groups of stars with power law indices for ${\log{(L_{\rm x}/L_{\rm bol})}}$ versus $\log{P_{\rm rot}}$ of $\sim$-0.7 to -1.5. The study of XLF for binary stars shows that the known unresolved secondaries likely contribute a significant amount to the X-ray emission.

Key words: X-rays: stars - stars: late-type, pre-main sequence, coronae, activity

  
1 Introduction

Late-type stars are known to sustain a dynamo which is powered by the combination of convective motions and rotation. The resulting magnetic field is thought to be responsible for various observational phenomena commonly referred to as "activity''. Stellar activity indicators are pervasive in all layers of the atmospheres of late-type stars. The best-studied magnetic field tracers include chromospheric H$\alpha$ and Ca II emission lines and coronal X-rays.

Strong and variable X-ray emission is observed from the early pre-main sequence (PMS) T Tauri stage to main sequence flare stars. Comparative studies of the emission levels of young stars at different ages may shed light on the origin and evolution of magnetic activity, which may be linked to angular momentum evolution.

T Tauri Stars (TTS) are divided into two subclasses according to the strength of their H$\alpha$ emission. Classical TTS (cTTS) are characterized by strong H$\alpha$ emission, while in weak-line TTS (wTTS) the equivalent width of H$\alpha$ is smaller than $10~{\rm\AA}$. In contrast to cTTS, wTTS do not show obvious signs of accretion and optically thick disks, and therefore are thought to represent a later evolutionary stage at which the circumstellar disk has become optically thin or dispersed. Nevertheless, some wTTS occupy the same region in the Hertzsprung-Russell diagram as the cTTS (see e.g. Walter et al. 1988; Alcalá et al. 1997), i.e. there seems to be no preferred disk lifetime between several 10⁵ and $10^7~{\rm yrs}$.

During the PMS contraction stars gain angular momentum and should spin up. However, cTTS show much slower rotation rates than wTTS (Bouvier et al. 1993) despite their high accretion rates. This can be explained by magnetic coupling between the star and the disk in cTTS which allows to regulate angular momentum transport without spinning up the star (Koenigl 1991; Edwards et al. 1993; Bouvier et al. 1997a).

The strength of activity is thought to decline with increasing stellar age. Skumanich et al. (1972) have proposed a $1/\sqrt{t}$-law for the decay of stellar activity in young stellar clusters based on CaII line observations. The power-law relation was confirmed by Feigelson & Kriss (1989) for a sample including PMS objects in Chamaeleon. However, the study of Walter et al. (1988) seemed to indicate that during the PMS phase the X-ray emission remains nearly constant, while for ages $\geq$ $10^8~{\rm yrs}$ it decays exponentially. Walter & Barry (1991) have argued that a power-law decay may be an artefact that occurs when the X-ray luminosity is used as activity indicator in a sample composed of stars with different stellar radii. Using the surface flux Walter & Barry (1991) have shown that the decay of various activity diagnostics probing the lower chromosphere, transition region, and corona can be described by an exponential.

An evolutionary decay of the X-ray emission is favored also by studies of the Einstein Observatory (EO) which have shown that the X-ray luminosity functions (XLF) of stellar clusters with different ages are displaced from each other (see e.g. Feigelson & Kriss 1989; Damiani et al. 1995). However, rather than being a pure age effect, the decreasing activity (i.e. the decay of the dynamo efficiency) might be explained by the slowing down of the rotation with increasing age on the main sequence (MS). A connection between the dynamo efficiency and the rotation rate is also supported by correlations between the X-ray activity and the rotational velocity (see Pallavicini et al. 1981; Bouvier 1990; Neuhäuser et al. 1995 = N95) found to hold for all kinds of active stars, featuring such different objects like dMe stars, RS CVn binaries, and TTS. For the fastest rotators among the Pleiads (Stauffer et al. 1994) and among the wTTS (Damiani & Micela 1995) the relation flattens out suggesting "saturation'' of the X-ray emission at very high rotation speeds. Stauffer et al. (1994) have proposed that the large spread observed in the X-ray luminosities of slower rotators are caused when more and more stars leave the saturation level thus increasing the dispersion. A later study by Micela et al. (1996) showed no significant correlation between $L_{\rm x}$ and ${v \sin{i}}$ for Pleiades stars, indicating that rotation can not be the only parameter governing the X-ray emission level of young stars. To date, no solution has been found to the question whether age or rotation determines the level of stellar activity.

If rotation does determine the activity, then cTTS should show lower X-ray luminosities than wTTS. XLF provide a statistical tool to compare the X-ray properties of different stellar samples. But so far, studies of the XLF of cTTS and wTTS have not led to a conclusive result concerning the evolution of X-ray activity during the PMS. N95 have shown that X-ray emission increases with age from cTTS to wTTS, but decreases after the wTTS phase. While N95 found that wTTS in Taurus-Auriga emit significantly more X-rays as compared to cTTS from the same region, Feigelson et al. (1993) found little evidence for systematic differences in the XLF of wTTS and cTTS in Chamaeleon, and argued that the differences in the X-ray luminosity between wTTS and cTTS in Taurus-Auriga might be attributed to as yet undicovered wTTS at the low-luminosity end of the distribution.

In this paper we examine the connection between X-ray activity, age, and rotation comparing different samples of young stars. The Taurus-Auriga-Perseus region is well suited for a study of the evolution of stellar activity because it hosts a large number of young stars at different ages: the molecular clouds of Taurus-Auriga are sites of ongoing star formation and have produced many TTS with ages between several 10⁵ to $10^7~{\rm yrs}$. Besides this star forming region, two young star clusters are located in the area, the Pleiades and the Hyades, at ages of $10^8~{\rm yrs}$ and $6 \times 10^8~{\rm yrs}$ respectively.

Our sample is larger and the sensitivity improved compared to all previous studies of this issue. The paper presented here is connected to an earlier analysis of archived ROSAT observations (Stelzer et al. 2000). Here we present a list of X-ray parameters for all known TTS in Taurus-Auriga, the Pleiades, and the Hyades as observed by ROSAT during pointed PSPC observations. Both detected and undetected sources are considered, i.e. for non-detections upper limits are given. In Sect. 2 we describe the data base and data reduction and give the results from source detection. In Sect. 3 the Hertzsprung-Russell diagrams (H-R diagrams) for cTTS and wTTS in Taurus-Auriga are presented. Our special interest (Sect. 4) is to compare the XLF of the different stellar groups with respect to the following issues: (i) Are the luminosity functions of cTTS and wTTS different, (ii) how does the X-ray luminosity evolve with stellar age, (iii) how does it depend on the spectral types of the stars and their binary character. Furthermore, we will explore the relation between X-ray emission and rotation rate for the largest sample studied so far (Sect. 5). In Sect. 6 we discuss and summarize our results.

  
2 Observations

  
2.1 Data base

The sky region examined is confined to the Taurus-Auriga-Perseus area. A detailed description of this region is given in Stelzer et al. (2000) (hereafter SNH00) where we have also presented a sky map showing the ROSAT PSPC observations subject to this and the previous study. The stellar sample investigated in this paper is identical to the one described in SNH00. However, we omit stars from the Perseus clouds IC348 (Preibisch et al. 1996) and NGC1333 (Preibisch 1997), since due to their larger distance the PSPC images are dominated by source confusion. We analyse the X-ray emission of young, late-type stars, represented by TTS and members from the Pleiades and Hyades clusters. The selection of the Pleiades and Hyades as examples of young clusters was motivated by their spatial vicinity to the Taurus-Auriga molecular clouds when projected to the sky. For this reason many Pleiads and Hyads lie in the same ROSAT PSPC fields. Most of the X-ray detected Pleiads and Hyads are zero-age main-sequence (ZAMS) stars. There are also some (higher-mass) post-MS stars which are not studied here, and many PMS brown dwarfs. The sample examined extends down to the latest M-type objects and includes brown dwarf candidates. Most of these are below the detection limit. However, we have detected an M9-type object in Taurus-Auriga, the latest type PMS dwarf seen to emit X-rays so far (see Sect. 2.5). The coolest object detected in the Pleiades has spectral type M5. In the Hyades we detect objects down to M9 (spectral types determined from measurements of B-V). With their different ages the three groups of stars (TTS, Pleiads, and Hyads) allow to examine the evolution of the X-ray luminosity.

We have selected all pointed PSPC observations from the ROSAT Public Data Archive available in October 1998 which contain any TTS in the Taurus-Auriga region, any Pleiad, or any Hyad in the field of view. The TTS in that area of the sky are part of the Taurus-Auriga molecular clouds located at $140~{\rm pc}$ (Elias 1978; Wichmann et al. 1998a). For the distance to the Pleiades cluster we have adopted $116~{\rm pc}$, the value given by Mermilliod et al. (1997). Those Hyades stars for which no individual Hipparcos parallaxes are available are assumed to be at a distance of $46~{\rm pc}$ (Perryman et al. 1998).

A detailed description of the membership lists for TTS, Pleiads, and Hyads is given in SNH00. SNH00 also have presented a complete list of the pointed ROSAT PSPC observations analysed here. In the earlier paper we were dealing with the same observations but have concentrated on large X-ray flares observed on detected stars. Now we discuss the X-ray characteristics of the whole sample, including non-flaring stars and non-detections. Therefore, we also analyse the short exposures and observations with unstable background marked with an asterisk in Table 1 of SNH00, and not considered in that earlier investigation.

  
2.2 Source detection

Source detection is performed based on a maximum likelihood method which combines local and map source detection algorithm (see Cruddace et al. 1988). Sources with a $ML \geq 7.4$ (corresponding to $\sim$3.5 Gaussian $\sigma$and shown to be the best choice by N95) are considered to be a detection. The probability for existence of a source of given ML is given by $P = 1 - \exp{(-ML)}$. For ML = 7.4 the probability is 0.9994, and among the $\sim$800 detected young stars we would expect to find less than one spurious source.

Observations whose center positions are less than $15^{\prime\prime}$apart have been merged to increase the sensitivity for faint detections. The photon extraction radius of the X-ray sources is not well defined if the off-axis positions in individual observations that are merged differ strongly from each other. Therefore, we have analysed observations with less overlap, i.e. more than $15^{\prime\prime}$ separation, separately. The center of the merged image is the center from all individual observations that are added up. The off-axis positions of X-ray sources in merged pointings are computed with respect to this averaged pointing position.

As the positional accuracy of the ROSAT PSPC declines towards the edge of the detector, the identification radius between optical and X-ray position depends on the off-axis angle of the source. We have computed the normalized cumulative number of identifications as a function of the offset between optical and X-ray position, $\Delta_{\rm ox}$, for different ranges of off-axis angles. Following N95, for each of these distributions we have determined the turnover point, $\Delta _{\rm ox,max}$, which corresponds to the value of $\Delta_{\rm ox}$ where wrong identifications begin to contribute significantly to the detected sources. We have then performed a linear fit to the mean off-axis angle as a function of this critical offset $\Delta _{\rm ox,max}$. The fit values of $\Delta _{\rm ox,max}$ for all examined off-axis ranges are listed in Table 1.

 

 

Table 1: Maximum offset allowed between optical and X-ray position $\Delta _{\rm ox,max}$ for different off-axis angles $\Omega$. $\Delta _{\rm ox,max}$ is the best-fit value of a linear distribution of offsets found from normalized cumulative numbers of identifications (see text).

Off-axis angle					$\Delta _{\rm ox,max}$
[arcmin]					[arcsec]
		$\Omega$	$\leq$	27.5	40.0
27.5	<	$\Omega$	$\leq$	30	42.4
30	<	$\Omega$	$\leq$	32.5	49.5
32.5	<	$\Omega$	$\leq$	35	56.7
35	<	$\Omega$	$\leq$	37.5	63.8
37.5	<	$\Omega$	$\leq$	40	70.9
40	<	$\Omega$	$\leq$	42.5	78.1
42.5	<	$\Omega$	$\leq$	45	85.2
45	<	$\Omega$	$\leq$	47.5	92.3
47.5	<	$\Omega$	$\leq$	50	99.5

These values are used as identification radii for the cross-correlation of membership lists and X-ray observations. For off-axis angles below $27.5^\prime$ a maximum offset between optical and X-ray position of $40^{\prime\prime}$ is appropriate. Note, that this value agrees with the value found by N95 for the ROSAT All-Sky Survey (RASS). Sources which are located further than $50^\prime$ from the detector center are ignored in the analysis presented here, because at large off-axis angles the point spread function deviates from a Gaussian and can not be adequately modeled by the available software.

We have computed the count rates of detected and undetected sources by integrating all events within a circular region around the source position, i.e. the X-ray position for detections and the optical position for non-detections. We use the 99% quantile of the point spread function at 1 keV as photon extraction radius, except for those few cases where the broad band X-ray image shows that the source obviously exceeds this radius probably due to the energy being different from 1 keV. For these special cases we determine the optimum radius individually by visual inspection of the X-ray image.

The measured counts are background subtracted and divided by the exposure time obtained from the exposure map to determine the count rates. For the background subtraction we have used the information from the background maps. This method is useful in crowded fields where a background annulus around the source may easily be contaminated by adjacent sources.

In the crowded Pleiades region occasionally two or more X-ray sources show significant overlap. In order to separate the contributions from each star we were forced to decrease the photon extraction radius of these sources. This leads to an underestimation of the true count rate, but should not effect our results due to the low number of confused stars (15 versus >200 detections among the Pleiades).

  
2.3 Results of source detection

The result of source detection and identification is summarized in six tables: Tables 2, 3, and 4 contain the X-ray parameters of all detected TTS, Pleiads, and Hyads, and in Tables 5, 6, and 7 the X-ray characteristics of undetected TTS, Pleiads, and Hyads are listed.

In Tables 2-7 the first column contains a number for the observation referring to the numbering in Table 1 in SNH00. (See SNH00 for the ROSAT observation request numbers.) For merged observations we give the numbers of all pointings that have been added up. Column 2 is the designation of the stars. Column 3 contains two flags, one that gives the type of TTS ("W'' - wTTS, "C'' - cTTS) and another one for the multiplicity of the stellar system ("S'' - single, "B'' - binary, "T'' - triple, and "Q'' - quadruple). The distinction between cTTS and wTTS is based mainly on the standard H$\alpha$ equivalent width boundary of 10 Å together with the spectral type of the star (i.e. the H$\alpha$ flux), which is similar to the suggestion by Martín (1997) to use different $W_{\rm H\alpha}$boundaries for different spectral types (GKM). Furthermore, we make use of indications for circumstellar material as revealed from IR and mm observations. SUAur, e.g., is of spectral type G2 and $W_{\rm H\alpha}$ is between 3.5 and 5 Å, but it also has a massive disk and, therefore, clearly is a cTTS. The H$\alpha$ equivalent widths are taken from N95, Kenyon & Hartmann (1995), and Wichmann et al. (1996). The spectral types are shown in Col. 4. The spectral types of Pleiades and Hyades stars were derived from the B-V measurements given in the Open Cluster Data Base compiled by C. Prosser and colleagues (and available at ftp://cfa-ftp.harvard.edu/pub/stauffer/clusters) using the conversion of Schmidt-Kaler (1982). For TTS in Taurus-Auriga we have adopted the spectral types compiled by N95 and König et al. (2001).

For all detected stars (Tables 2-4) we list the X-ray position (Cols. 5 and 6), the offset $\Delta$ between optical and X-ray position (Col. 7), the off-axis angle (Col. 8), and the maximum likelihood (Col. 9) of existence. We give the X-ray hardness ratios HR1 and HR2 in Cols. 10 and 11. The PSPC hardness ratio HR1 is defined as follows:

$$HR1 = \frac{H - S}{H + S}$$ (1)

where H is the hard band count rate between 0.5-2.0 keV, and S is the count rate in the soft band (between 0.1-0.4 keV). HR2 is given by:

$$HR2 = \frac{H2 - H1}{H2 + H1}$$ (2)

where H2 and H1 are the count rates in the upper and lower part of the hard band between 0.5-0.9 keV (H1) and 0.9-2.0 keV (H2), respectively. In cases where no counts are observed in any one energy band, and therefore HR1 or HR2 are either +1.0 (no soft counts) or -1.0 (no hard counts) we have computed upper limits to the hardness from the counts in the background. Column 12 gives the exposure time and Col. 13 the X-ray luminosity.

In order to determine the count-to-energy-conversion-factor CECF for the compilation of luminosities we have used the hardness criterion given by Fleming et al. (1995): $CECF = (8.31 + 5.30 \cdot HR1) \times 10^{-12}~{\rm erg\,cm^{-2}\,cts^{-1}}$. Since the soft band in HR1 is sensitive to A_V, this way we implicitly take account of the extinction. It should be noted that HR1 "saturates'' for extinctions ${A_{V} >} \sim$0.5. High extinctions are however rare in the Taurus region, and do not play a role for the Pleiades and Hyades. But to ensure that no systematic errors are introduced by this method of count-to-energy conversion we have compared the resulting distribution of X-ray luminosities with those directly derived from the available A_V measurements (see Sect. 4.1).

The values of the luminosity given in Tables 2-4 have been derived dividing the count rate by the multiplicity of the stellar system. This means we assume that each of the components in the system contributes the same level of X-ray emission (see König et al. 2001 and Sect. 4.3). The mean value of the CECF is $1.00 \pm 0.25 \times 10^{-11}~{\rm erg\,cm^{-2}\,cts^{-1}}$. This value was used to obtain the luminosity in cases where HR1 is a upper/lower limit, and therefore Fleming's relation cannot be applied. Uncertainties in $\log{L_{\rm x}}$ are derived from the statistical errors without taking account of systematic uncertainties in the distance estimate.

X-ray parameters for non-detections are summarized in Tables 5-7. The meaning of Cols. 1 to 4 in Tables 5-7 is the same as in Tables 2-4. In Cols. 5 and 6 we list the optical position. The off-axis angle of the undetected stars is given in Col. 7. Column 8 contains the upper limits to the source counts, Col. 9 the exposure time, and Col. 10 the X-ray luminosity. We have used the mean value of the CECF for the compilation of an upper limit to $L_{\rm x}$ in the case of non-detections. The X-ray luminosity was divided by the number of stellar components.

Multiple stellar systems are represented by a single entry in Tables 2-7, but the designations and if known the spectral types of all components are given. Whenever more than one star lies in the X-ray-to-optical identification radius we list the designations of all possible counterparts.

If a star was detected in both unmerged and merged observations we list only the result from the merged observations. The same applies to stars which are detected neither in the merged nor in the unmerged observations. Here, we list only the upper limit from the merged observation. In a few cases a star was detected in a single but not in the merged observations. This can occur if the source is not within the inner $50^\prime$ of the merged observation due to the shift in pointing centers during the merging process, or if the source or background is variable.

Stars which have shown an X-ray flare (discussed by SNH00) are represented by their quiescent emission, i.e. the flare has been removed from the data. We have marked the flare observations in Tables 2-7 by a label after the observation ID.

  
2.4 Detection rates

The aim of this study is to examine the X-ray emission from magnetically active stars. Stars of spectral types earlier than $\sim$F5 are not expected to show dynamo activity because they have no or only shallow convection zones (Walter 1983). We are not interested in the X-ray emission of these stars because they obey a different emission mechanism. Therefore, we restrict the following analysis to stars with spectral types G and later.

An overview over the detection rates for stars from the different stellar groups is given in Table 8.

 

 

Table 8: X-ray statistics of TTS, Pleiads, and Hyads observed and detected in pointed ROSAT PSPC observations. $N_{\rm D}$ - Number of detections, $N_{\rm N}$ - Number of non-detections, $N_{\rm stars}$ - Number of different stars observed, $N_{\rm mult. FOV}$ - Number of stars in the FOV of more than one observation, $N_{\rm mult. D}$ - Number of stars detected in more than one observation.

Sp.Type	$N_{\rm D}$	$N_{\rm N}$	$N_{\rm stars}$	$N_{\rm mult. FOV}$	$N_{\rm mult. D}$
Taurus-Auriga TTS
G	28	19	17	12	11
K	66	30	59	23	19
M	74	88	98	44	33
Pleiades
G	41	82	41	31	20
K	118	231	112	87	59
M	52	139	65	47	31
Hyades
G	29	2	22	8	8
K	71	20	54	29	26
M	84	69	99	46	33

We have split up each sample according to the spectral types of its members. The column labeled "$N_{\rm D}$'' gives the sum of all detections, and "$N_{\rm N}$'' is the number of non-detections. The number of observed stars (column $N_{\rm stars}$) is smaller than $N_{\rm D} + N_{\rm N}$ due to multiple observations of a given sky position. The columns labeled " $N_{\rm mult. FOV}$'' and " $N_{\rm mult. D}$'' denote the total number of stars observed/detected in more than one observation. Note, that for most multiple stars only the spectral type of the primary is known, and therefore the stellar system has only one entry in Table 8.

Histograms of the distribution of spectral types in the different stellar samples are displayed in Fig. 1.

Figure 1: Spectral type distribution of the observed late-type stars: a) single stars, b) multiple stellar systems. For multiples the spectral type of the primary is plotted, and the secondary is not taken into account. Solid lines denote the total number of stellar systems in any field of the ROSAT PSPC observations from Table 1 in SNH00. The hatched areas represent the number of detected systems. The numbers given in each panel represent the total number of observed systems (" $N_{\rm FOV}$'') and detected systems ("$N_{\rm D}$''). Note, that individual stellar systems may have been detected in more than one observation. The fraction of detected stars depends on distance, integration time, possible flaring activity, line-of-sight absorption, and stellar parameters such as age, mass, and rotation.

Open with DEXTER

We show separate histograms for single and multiple star systems. In the latter sample only the primary is considered. (For most secondaries the spectral type is unknown). The empty histogram bins give the number of stars in the ROSAT PSPC field of any observation and the hatched histograms the subgroup of detected stars. The total number of stars displayed in the figure is also given and labeled " $N_{\rm FOV}$'' (all observed stars) and "$N_{\rm D}$'' (all detected stars) respectively.

As seen in Fig. 1, the detection rate is higher for the Hyades than for the Pleiades or TTS, although the Hyades are older. This is probably due to their shorter distance. The relative number of detections is larger for TTS than for the Pleiades presumably because TTS are young and more active. Throughout all spectral types the detection rate is higher for unresolved binaries as compared to single stars. This could indicate that all stars in multiple systems contribute to the X-ray emission. The actual detection rate is a complicated function of many influencing factors, such as distance, integration time, absorption, age and mass. A detailed analysis of the X-ray emission levels of the different groups of stars is given in the following sections.

  
2.5 X-ray detection of very-late type dwarfs

A number of very low-mass dwarfs with spectral types between M5 and M9 have been detected. In particular, we report on the detection of LH0429+17, to date the latest PMS dwarf with X-ray emission. This object was listed as a candidate member of the Hyades in a photometric study by Leggett & Hawkins (1989). In the course of a spectroscopic survey for brown dwarfs in the Hyades Reid & Hawley (1999) have detected strong H$\alpha$ emission but weak absorption in the gravity sensitive Na I line, which is an indication for young age. Taking into account its location on the sky, LH0429+17 can, therefore, be considered as member of the Taurus star forming region.

X-rays from young brown dwarfs and brown dwarf candidates in the Chamaeleon, Taurus-Auriga and $\rho$Ophiuchus star forming regions have first been observed by Neuhäuser & Comerón (1998) and Neuhäuser et al. (1999). These objects have spectral types between M6 and M8. Note, that we confirm here the detection of all brown dwarfs and brown dwarf candidates in the Taurus region which have been listed in Neuhäuser et al. (1999).

  
3 H-R diagrams

In order to visualize the age and mass distribution of our stars we have placed the subset of TTS observed with the PSPC and with known bolometric luminosity $L_{\rm bol}$ and effective temperature $T_{\rm eff}$ in the Hertzsprung-Russell diagram (H-R diagram). We dispense with H-R diagrams for Pleiades and Hyades stars because most of the stars in these two clusters are well known to lie on the MS (see previous discussion). The H-R diagram for the TTS in Taurus-Auriga is shown in Fig. 2.

Figure 2: H-R diagram of TTS observed with the ROSAT PSPC during pointed observations. Note, that the stars on display represent only a fraction of all X-ray observed TTS because $L_{\rm bol}$ and $T_{\rm eff}$ are not known in all cases. The data are compared to three different theoretical calculations for the PMS evolution: top - D'Antona & Mazzitelli (1994), middle - Baraffe et al. (1998), and bottom - Palla & Stahler (1999). The masses are given in solar units and the isochrones represent $\log{\rm age}$ except for Palla & Stahler (1999) where the ages are given in Myrs.

Open with DEXTER

We have used the $L_{\rm bol}$ values given by Kenyon & Hartmann (1995), and $T_{\rm eff}$ was obtained from the spectral types using the conversion by Schmidt-Kaler (1982). The location of the stars is compared to different models of evolutionary PMS tracks: D'Antona & Mazzitelli (1994), Baraffe et al. (1998), and Palla & Stahler (1999). All diagrams are drawn with the same scale to facilitate the perception of differences between the model calculations. The computation by Baraffe et al. (1998) does not represent a useful description of the complete TTS sample due to its restriction to masses below $\sim$ $1~{M_\odot}$. Furthermore, the lines of equal mass show significant deviations from the other calculations. A closer look reveals that there are also significant differences between the models of D'Antona & Mazzitelli (1994) and Palla & Stahler (1999).

It would be highly desirable to use the theoretical calculations to assign ages and masses to the individual TTS. However, from the comparison provided in Fig. 2 it is obvious that the calibration of the models is uncertain, i.e. tracks computed by different groups would lead to controversial results on the masses and ages of the stars.

Despite such uncertainties the H-R diagram can be used to demonstrate the average distribution of the cTTS and wTTS. Although the stars closest to the birthline tend to be cTTS, and those nearest to the MS are wTTS, the overall distribution of cTTS and wTTS is mixed. This indicates that individual wTTS are not always older than cTTS despite the fact that they represent a later evolutionary stage. This is known since the discovery of many wTTS by the EO (Walter et al. 1988), and the situation is similar in other star forming regions.

  
4 X-ray luminosity functions

The statistical analysis was performed with the ASURV package version 1.2 (see Feigelson et al. 1985; Isobe et al. 1986; LaValley et al. 1992). The ASURV software is particularly well suited for the study of data sets with censored points, i.e. non-detections. We exclude photons observed during the large X-ray flares presented by SNH00, i.e. for flaring stars only their quiescent radiation is taken into account.

XLF are frequently employed to characterize a stellar population. Our special interest here is to compare the XLF of the different stellar groups with respect to the following issues: (i) Are the luminosity functions of cTTS and wTTS different, (ii) how does the X-ray luminosity evolve with stellar age, (iii) how does it depend on the spectral types of the stars and their binary character.

A substantial number of stars are in the field of more than one pointed PSPC observation (see Table 8). However, every star should appear only once in the XLF. Therefore, we represent each star by its error weighted mean luminosity from all observations in which it was detected. If a star was observed in more than one observation, but not detected in any of them, we use the mean upper limit of all non-detections of this star as an estimate for its luminosity limit.

In Sect. 4.3 we will justify our assumption that the X-ray luminosity can be distributed equally among all stars in unresolved multiple systems. Therefore, if not specified otherwise, we have divided the mean X-ray luminosity by the number of components in the stellar system.

  
4.1 cTTS and wTTS in RASS and pointed PSPC data

When studying the X-ray emission of TTS in Taurus-Auriga observed during the RASS, N95 found that the wTTS are X-ray brighter than the cTTS. This is in contrast to findings in various other star forming regions (see e.g. Feigelson et al. 1993; Casanova et al. 1995; Grosso et al. 2000). This discrepancy is not yet understood. A possible explanation is that the XLF of the wTTS in Taurus-Auriga is uncomplete towards the low-luminosity end, because wTTS are not easily identified due to the lack of pronounced spectral features. In particular, many wTTS have been discovered with the EO. Therefore, even the pre-ROSAT sample studied in N95 could be biased towards X-ray bright wTTS.

Our analysis of a large set of pointed ROSAT observations allows to extend the sensitivity limit substantially with respect to the RASS. In Fig. 3 we compare the XLF of TTS derived from the pointed observations described in this paper to the results from the RASS.

	Figure 3: XLF of TTS in Taurus-Auriga derived from the RASS and from pointed ROSAT PSPC observations. Shown are all cTTS and wTTS in Taurus-Auriga. The inset in the lower left shows the typical error bar.
Open with DEXTER

The XLF of the RASS have been newly compiled with respect to the analysis by N95 to include all TTS discovered since then, i.e. the sample consists of all TTS from N95 plus those listed in König et al. (2001) (including both EO and ROSAT discovered TTS). N95 did include EO discovered but no ROSAT discovered TTS.

The comparison with the RASS data clearly demonstrates the better sensitivity of the pointed observations. The XLF computed from the PSPC pointings extends by $\sim$1-2 orders of magnitude further into the low luminosity regime. We reproduce the result first found by N95: in Taurus-Auriga the wTTS are clearly X-ray brighter than the cTTS.

It was noted by Feigelson et al. (1993) that the XLF can change, if the stars included in the sample were found by different methods, e.g. H$\alpha$ versus X-ray surveys. In order to overcome this bias we have computed XLF where we exclude all X-ray discovered TTS. Figure 4 shows the Kaplan-Meier Estimator (KME) for three subsets of wTTS in Taurus-Auriga: ROSAT discovered wTTS, EO discovered wTTS, and all other wTTS.

Figure 4: XLF of wTTS in Taurus-Auriga derived from pointed ROSAT PSPC observations. The three different distributions are ROSAT discovered wTTS (solid line), EO discovered wTTS (dashed line), and wTTS discovered by other means (dotted line). The inset in the lower left shows the typical error bar. All distributions are similar indicating that the inclusion of X-ray discovered TTS does not introduce a selection bias into the sample of wTTS.

Open with DEXTER

The XLF of these groups do not differ significantly from each other. Therefore, we are led to conclude that the difference in the distributions of cTTS and wTTS is not due to an X-ray selection bias.

The differences to the $\rho$Oph and ChaI star forming regions (Feigelson et al. 1993; Casanova et al. 1995; Grosso et al. 2000) could also be caused by the difference in spatial extension between these two young clusters and the Taurus-Auriga region: The latter is widely dispersed, and, hence, its members may constitute a larger spread in age as compared to the more complex $\rho$Oph and ChaI regions in which the stars are probably more coeval. We can check this by selecting TTS from the central parts of the star forming region, and comparing the resulting XLF with that of the total sample. We have chosen the PSPC observations ROR 200001-0p and 200001-1p pointed on the L1495E cloud. These pointings are centered on the largest concentration of molecular material corresponding to a particular young part of the Taurus complex. In Fig. 5 we show the XLF for wTTS and cTTS in that region.

Figure 5: XLF of wTTS and cTTS in L1495E derived from a $\sim$30 ksec pointed ROSAT PSPC observation: dotted line - cTTS; dashed line - all wTTS; solid line - wTTS except those discovered by ROSAT. The inset in the lower left shows the typical error bar. The distributions of cTTS and wTTS are again different indicating that the discrepancy between the X-ray luminosities of cTTS and wTTS in Taurus-Auriga is not due to the spatial extension of the sample.

Open with DEXTER

A third distribution consists of all wTTS in L1495E which have not been discovered by ROSAT. The general shape of the XLF in L1495E is the same as that for the complete Taurus-Auriga area: wTTS are X-ray brighter than cTTS. This is also evident from the data in Strom & Strom (1994), an earlier analysis of these pointings in L1495E. We conclude that the X-ray luminosity does not depend on the spatial location within the Taurus region.

The difference in the XLF of wTTS and cTTS does also not depend on our choice of roughly 10 Å as boundary between cTTS and wTTS. It is clear that one should use the H$\alpha$ flux instead of the equivalent width as boundary (hence, we classify SUAur as cTTS) because the equivalent width depends on the underlying continuum which varies with spectral type. Martín (1997) suggested three different equivalent width boundaries for three spectral type regimes chosen such as to exclude that the H$\alpha$emission is due to chromospheric activity. Adopting these criteria only a few TTS change classification, but the difference in the XLF remains.

In Sect. 2.3 the conversion from count rates to luminosities by use of hardness ratios was explained. Using hardness ratios allows to indirectly take account of the extinction in the absence of actual A_V measurements. However, HR1 is only sensitive to comparatively low extinctions. The extinction should generally be higher for the cTTS than for the wTTS due to the denser circumstellar environment of the former ones, and if not treated properly may lead to wrong estimates for the luminosities.

We have, therefore, applied an alternative way of deriving X-ray luminosities for the TTS in Taurus-Auriga making use of the available A_V data. In this approach the X-ray flux was computed with standard EXSAS tools assuming a 1 keV RS-model with absorbing column density $N_{\rm H}$ derived from A_V according to Paresce (1984). Similar values for $N_{\rm H}$ are obtained when using the conversion given by Ryter (1996). Stars for which A_V is $\leq$0.05 mag have been assigned a standard value of $N_{\rm H} = 10^{18}~{\rm cm}^{-2}$.

While for individual stars the $L_{\rm x}$ derived by the two methods show typical deviations of $\sim$50%, the statistical distribution of X-ray luminosities is unaffected by the specific choice of CECF, and the previously discussed differences between the XLF of cTTS and wTTS remain.

  
4.2 Dependence on spectral type

In the previous subsection, no distinction was drawn between stars of different spectral type, mass or other stellar parameters. This is justified for young, very low-mass stars which follow fully convective tracks. It is believed that for stars on the MS activity is governed by the relative size of radiative core and convective envelope. This should also apply to TTS once they have reached the radiative part of their PMS evolution. Therefore, to obtain homogeneous samples, stars with different interior structure, i.e. different mass, should be treated separately. As argued in Sect. 3 it is not possible to obtain reliable values for the individual masses and ages of the stars. As an approximation we distinguish the stars by their spectral type. But note, that while for stars on their Hayashi tracks this description is acceptable, for stars on radiative tracks a given spectral type represents a mass range rather than a single value for the mass.

Each subsample is subdivided in three spectral type bins: G, K, and M stars. The mean X-ray luminosities for the different stellar groups and spectral types are listed in Table 9.

 

 

Table 9: Mean X-ray luminosities $\langle \log{L_{\rm x}} \rangle$for cTTS, wTTS, and Pleiades and Hyades. The columns labeled "N'' and " $N_{\rm lim}$'' give the number of stars and number of upper limits within the sample. The second column provides a description of the sample: "C'' - cTTS, "W'' - wTTS, "s'' - single star, "b1'' - binary star assuming that all X-ray emission comes from one component, "b2'' - binary star assuming equal X-ray emission from both components.

Region		Spectral Type G			Spectral Type K			Spectral Type M
		N	$N_{\rm lim}$	$\log{L_{\rm x}}$	N	$N_{\rm lim}$	$\log{L_{\rm x}}$	N	$N_{\rm lim}$	$\log{L_{\rm x}}$
TTS	C	2	(1)	$29.60 \pm 0.66$	22	(9)	$28.93 \pm 0.16$	61	(30)	$28.54 \pm 0.14$
TTS	W	15	(0)	$30.02 \pm 0.17$	36	(5)	$29.78 \pm 0.10$	34	(9)	$29.20 \pm 0.10$
Pleiades		41	(18)	$28.98 \pm 0.12$	112	(41)	$28.94 \pm 0.06$	65	(29)	$28.80 \pm 0.07$
Hyades		22	(2)	$28.97 \pm 0.05$	54	(6)	$28.52 \pm 0.11$	99	(38)	$27.99 \pm 0.10$
TTS	s	-	-	-	34	(11)	$29.44 \pm 0.14$	60	(28)	$28.70 \pm 0.14$
TTS	b2	-	-	-	17	(3)	$29.47 \pm 0.18$	29	(20)	$28.85 \pm 0.18$
TTS	b1	-	-	-	17	(3)	$29.77 \pm 0.18$	29	(10)	$29.15 \pm 0.18$
Pleiades	s	25	(13)	$28.98 \pm 0.15$	84	(38)	$28.83 \pm 0.09$	60	(29)	$28.78 \pm 0.08$
Pleiades	b2	16	(5)	$29.03 \pm 0.16$	27	(3)	$29.00 \pm 0.08$	5	(0)	$28.93 \pm 0.08$
Pleiades	b1	16	(5)	$29.33 \pm 0.16$	27	(3)	$29.30 \pm 0.08$	5	(0)	$29.23 \pm 0.08$
Hyades	s	12	(1)	$28.97 \pm 0.06$	36	(5)	$28.41 \pm 0.15$	89	(35)	$27.95 \pm 0.10$
Hyades	b2	10	(1)	$28.96 \pm 0.07$	18	(1)	$28.75 \pm 0.14$	9	(3)	$28.47 \pm 0.19$
Hyades	b1	10	(1)	$29.26 \pm 0.07$	18	(1)	$29.05 \pm 0.14$	9	(3)	$28.77 \pm 0.19$

For all spectral types the wTTS distribution shows the largest values of $\langle \log{L_{\rm x}} \rangle$, and the Hyades have the lowest $\langle \log{L_{\rm x}} \rangle$. Note, that the group of cTTS of spectral type G is represented by only two stars. But for the other subsamples the statistics are significant. Since in most cases the spectral type (or B-V) is known only for the primary in multiples, we exclude the secondaries from this part of the analysis, except the few cases where the spectral types of all components are known (see Tables 2-7).

In Fig. 6 we provide a comparison of the XLF of TTS, Pleiads, and Hyads.

	Figure 6: XLF for TTS in Taurus-Auriga, for the Pleiades, and the Hyades. The distributions are shown for different spectral types, corresponding to different values of B-V or effective temperature or mass for the MS stars. a) G stars, b) K stars, and c) M stars.
Open with DEXTER

Throughout all examined spectral types the wTTS clearly represent the brightest class among the X-ray objects studied here, and Hyads show the weakest X-ray emission. For the M stars, where the mass range is comparatively small, the decline of $L_{\rm x}$ from TTS over Pleiades to the Hyades can be interpreted as an age effect. G and K type stars represent a larger spread in the mass distribution such that the influences of mass and age may not easily be disentangled. However, the difference between $\langle L_{\rm x} \rangle$ of Pleiades and Hyades decreases towards earlier types indicating that age and not mass is the dominant effect.

The distributions of cTTS and Pleiads intersect each other because of the much shallower slope of the XLF of cTTS, i.e. larger spread in luminosities. This effect may be caused by our assumption of uniform distance for all stars in a given sample: in contrast to the strongly clustered Pleiades region the TTS in Taurus-Auriga may be subject to a larger distance spread that translates to an apparent spread in $L_{\rm x}$.

Luminosity differences between various stars may generally be due to differences in emitting area. In order to eliminate this effect the X-ray to bolometric luminosity ratio, ${\log{(L_{\rm x}/L_{\rm bol})}}$, is often used to characterize the X-ray emission. We have examined the relation between the effective temperature and ${\log{(L_{\rm x}/L_{\rm bol})}}$. $L_{\rm bol}$ of Pleiads and Hyads was computed from the V magnitude and B-V (needed to determine the bolometric correction) given in the Open Cluster Data Base. The effective temperatures of Pleiades and Hyades stars were obtained from B - V. We have assumed negligible absorption to both star clusters. In Fig. 7 all late-type stars (spectral type later than F or ${\log{T_{\rm eff}}}$ < 3.78) are plotted.

	Figure 7: Relation between X-ray to bolometric luminosity ratio, ${\log{(L_{\rm x}/L_{\rm bol})}}$, and effective temperature, ${\log{T_{\rm eff}}}$. From top to bottom: TTS, Pleiades, and Hyades. Only stars with spectral type later than F are considered. The plotting symbols have been scaled to the projected rotational velocity of the stars. Upper limits to $L_{\rm x}$ are indicated by arrows.
Open with DEXTER

Figure 7 shows that within the TTS sample, which is characterized by a decline of $\log{L_{\rm x}}$ with spectral type, ${\log{(L_{\rm x}/L_{\rm bol})}}$ does not depend on effective temperature. Pleiades and Hyades, however, demonstrate a clear anticorrelation between ${\log{(L_{\rm x}/L_{\rm bol})}}$ and ${\log{T_{\rm eff}}}$ (see also e.g. Micela et al. 1999). The fact that we do not see such a trend in the TTS sample may be due to the large age spread among the TTS. Note, that in Fig. 7 only stars with known projected rotational velocity are shown. The plotting symbols have been scaled to ${v \sin{i}}$. With few exceptions the fastest rotators are situated close to the upper envelope, indicating a connection between the activity level and the rotation rate (see also Sect. 5).

  
4.3 Single and binary stars

All XLF presented above may rely to some degree on our assumption that all components in multiple systems emit X-rays (at the same level). In order to check this hypothesis we have studied the XLF of single and binary stars separately. Again we have constructed separate XLF for G, K, and M type stars. In Fig. 8 we show these XLF for TTS, Pleiades and Hyades stars. For comparison we display also the XLF for binaries derived without taking account of the binary character, i.e. XLF in which each binary has been regarded as a single star with the observed X-ray luminosity (dashed in Fig. 8). Henceforth, these distributions are termed "b1'', in contrast to the distributions "b2'' for which equal partition of $L_{\rm x}$ onto the components was assumed (dotted in Fig. 8). As before, binary components with unknown spectral type are not considered.

The mean and median of $\log{L_{\rm x}}$ for all compiled distributions are listed in Table 9. Obviously, throughout all examined groups of stars the distributions "b1'' are shifted towards higher luminosities with respect to the distributions "b2''. We have performed two-sample tests within ASURV to quantify the differences. The results are summarized in Table 10.

 

 

Table 10: Results of two-sample tests performed with ASURV to distinguish between the XLF of single and binary stars. For each group (TTS, Pleiads, and Hyads) and each spectral type we have compared three distributions: s - single stars, b1 - binary stars with only one X-ray emitter, b2 - binary stars assuming that both components emit equal amounts of X-rays. The probabilities given are for the null-hypothesis that the compared pair of XLF is drawn from the same parent distribution. We have applied Gehan's generalized Wilcoxon test (GW), the logrank test, and the Peto & Prentice generalized Wilcoxon test.

Sample	size (ul.)	Prob	Prob	Prob
		GW HV	log rank	P & Pren.
TTS K stars
s-b2	34 (11)-17 (3)	0.948	0.852	0.948
s-b1	34 (11)-17 (3)	0.073	0.165	0.084
TTS M stars
s-b2	60 (28)-29 (10)	0.238	0.471	0.275
s-b1	60 (28)-29 (10)	0.006	0.051	0.010
Pleiads G stars
s-b2	25 (13)-16 (5)	0.844	0.953	0.789
s-b1	25 (13)-16 (5)	0.085	0.103	0.089
Pleiads K stars
s-b2	84 (38)-27 (3)	0.825	0.286	0.688
s-b1	84 (38)-27 (3)	0.002	0.001	0.004
Pleiads M stars
s-b2	60 (29)-5 (0)	0.710	0.294	0.665
s-b1	60 (29)-5 (0)	0.002	0.001	0.009
Hyads G stars
s-b2	12 (1)-10 (1)	0.657	0.711	0.620
s-b1	12 (1)-10 (1)	0.003	0.005	0.005
Hyads K stars
s-b2	36 (5)-18 (1)	0.134	0.095	0.150
s-b1	36 (5)-18 (1)	0.000	0.000	0.001
Hyads M stars
s-b2	89 (35)-9 (3)	0.059	0.217	0.083
s-b1	89 (35)-9 (3)	0.002	0.022	0.005

The comparison between "s'' and "b2'' shows in most cases a high probability that the distributions are similar. Only for the Hyades K and M stars the probability that the distributions of singles and "b2'' are different is $\sim$90%. All samples "s'' and "b1'', on the contrary, have high probability for different underlying parent distributions.

The XLF of Hyades stars have first been examined by Pye et al. (1994) on the basis of ROSAT observations. Their finding that Hyades dK binaries are X-ray brighter than single Hyads of the same spectral type were confirmed by Stern et al. (1995) on a larger sample. Our analysis shows that the comparison depends sensitively on the way in which binary stars are treated. The effect is strongly reduced if it is assumed that both components in binaries emit X-rays ("b2'') with respect to distributions of type "b1'' examined by Pye et al. (1994) and Stern et al. (1995).

  
5 Rotation-activity relations

The rotation-activity connection has been extensively studied by Walter (1981),

Figure 8: XLF of single and binary stars of spectral type G, K and M. a) TTS, b) Pleiades, and c) Hyades. solid lines - single stars (s), dotted lines - binary stars assuming equal $L_{\rm x}$ from both components (b2), dashed lines - binary stars assuming only one X-ray emitting component (b1). See text for a more detailed description of these samples. All G type TTS in Taurus-Auriga are single stars, and therefore not displayed in this figure.

Open with DEXTER

Walter & Bowyer (1981), Walter (1982), Bouvier (1990), Damiani et al. (1991), Grankin (1993), N95, Bouvier et al. (1997b), and Wichmann et al. (1998a).

In this section we study the subsample of the stars from Tables 2 to 7 with measured rotation periods $P_{\rm rot}$ or projected rotational velocity ${v \sin{i}}$. The choice of the best parameters describing the activity-rotation relation is not undisputed. We have, therefore, examined different parameter combinations. On the X-ray side we use the luminosity $L_{\rm x}$, the surface flux $F_{\rm s}$, and the ratio between X-ray and bolometric luminosity $L_{\rm x}/L_{\rm bol}$ to characterize the stars. Each star is represented by its mean X-ray luminosity or upper limit to $L_{\rm x}$ as described in Sect. 4. For binaries only one component is considered, because spectral types and rotation rates are in most cases known only for the primary. The stellar radii used to compute $F_{\rm s}$were determined from the Stefan-Boltzmann law. The rotation is described by the projected rotational velocity, ${v \sin{i}}$, or the rotation period, $P_{\rm rot}$. $P_{\rm rot}$ and ${v \sin{i}}$ of Pleiades and Hyades stars are listed in the Open Cluster Data Base. Values for the rotation rates of TTS are taken from N95, Bouvier et al. (1997b), and Wichmann et al. (1998a).

For the statistical analysis cTTS and wTTS have been combined to yield a larger sample, although generally wTTS are faster rotators than cTTS, and they are more X-ray luminous. A linear regression has been fitted to all pairs of rotation-activity combinations using the ASURV EM algorithm or the method by Schmitt (1985) for doubly censored data. In Table 11 we summarize the results of all correlation tests,

 

 

Table 11: Results of statistical tests with ASURV for the relation between X-ray emission and stellar rotation for TTS, Pleiads, and Hyads. The first two columns are the names of the two parameters to be compared. Next is the size of the sample, N, and in brackets the number of upper limits, $N_{\rm lim}$, to the rotation and X-ray parameter. Columns 5 and 6 give the probability that there is no correlation between the two parameters according to Kendall's and Spearman's test. The slope of a linear regression to the pair of parameters is given in Col. 7. For doubly censored data we have used the linear regression method of Schmitt (1985). All samples where $P_{\rm rot}$ is the rotation parameter have upper limits only in the X-ray parameters, and the EM algorithm is used.

Par 1	Par 2	N	$N_{\rm lim}$	Kendall	Spearman	slope
TTS
${\log{(v \sin{i})}}$	$\log{L_{\rm x}}$	65	(0/17)	0.0031	0.0047	$1.08 \pm 0.36$
${\log{(v \sin{i})}}$	$\log{F_{\rm s}}$	52	(0/14)	0.0009	0.0011	$1.57 \pm 0.46$
${\log{(v \sin{i})}}$	${\log{(L_{\rm x}/L_{\rm bol})}}$	52	(0/14)	0.0053	0.0040	$1.22 \pm 0.44$
$\log{P_{\rm rot}}$	$\log{L_{\rm x}}$	39	(0/7)	0.0000	0.0001	$-1.52 \pm 0.39$
$\log{P_{\rm rot}}$	$\log{F_{\rm s}}$	38	(0/6)	0.0000	0.0000	$-1.93 \pm 0.39$
$\log{P_{\rm rot}}$	${\log{(L_{\rm x}/L_{\rm bol})}}$	38	(0/6)	0.0001	0.0002	$-1.49 \pm 0.42$
Pleiades
${\log{(v \sin{i})}}$	$\log{L_{\rm x}}$	164	(6/53)	0.0000	0.0000	0.61
${\log{(v \sin{i})}}$	$\log{F_{\rm s}}$	164	(6/53)	0.0000	0.0000	0.67
${\log{(v \sin{i})}}$	${\log{(L_{\rm x}/L_{\rm bol})}}$	164	(6/53)	0.0000	0.0000	0.88
$\log{P_{\rm rot}}$	$\log{L_{\rm x}}$	46	(0/13)	0.0008	0.0005	$-0.42 \pm 0.11$
$\log{P_{\rm rot}}$	$\log{F_{\rm s}}$	46	(0/13)	0.0000	0.0001	$-0.52 \pm 0.11$
$\log{P_{\rm rot}}$	${\log{(L_{\rm x}/L_{\rm bol})}}$	46	(0/13)	0.0000	0.0000	$-0.66 \pm 0.12$
Hyades
${\log{(v \sin{i})}}$	$\log{L_{\rm x}}$	67	(41/2)	0.0008	0.0000	1.58
${\log{(v \sin{i})}}$	$\log{F_{\rm s}}$	67	(41/2)	0.0000	0.0001	1.56
${\log{(v \sin{i})}}$	${\log{(L_{\rm x}/L_{\rm bol})}}$	67	(41/2)	0.0003	0.0089	1.64
$\log{P_{\rm rot}}$	$\log{L_{\rm x}}$	21	(0/2)	0.0003	0.0004	$-1.13 \pm 0.32$
$\log{P_{\rm rot}}$	$\log{F_{\rm s}}$	21	(0/2)	0.0016	0.0016	$-0.94 \pm 0.28$
$\log{P_{\rm rot}}$	${\log{(L_{\rm x}/L_{\rm bol})}}$	21	(0/2)	0.3515	0.3489	$-1.51 \pm 0.32$

and also give the slopes of the linear regression. According to the statistical tests X-ray emission and rotation are clearly correlated for most of the examined stellar samples. For a given X-ray parameter the probability for a correlation with $P_{\rm rot}$ is in most cases larger than the probability for a correlation with ${v \sin{i}}$. This is probably due to the unknown inclination angle in ${v \sin{i}}$ whose arbitrary orientation tends to destroy any intrinsic correlation between the rotation and X-ray emission. Using $P_{\rm rot}$ should therefore be more meaningful. However, measurements of the actual periods (by spot modulation) are much sparser than spectroscopic observations of ${v \sin{i}}$, leading to a smaller data set.

We show correlations of all possible combinations of the above mentioned X-ray parameters with $P_{\rm rot}$ in Figs. 9 to 11 for TTS,

Figure 9: Relation between the rotation period and different X-ray parameters for TTS from the Taurus-Auriga region: top - X-ray luminosity, middle - X-ray surface flux, and bottom - Ratio between X-ray luminosity and bolometric luminosity. cTTS are represented by filled symbols and wTTS by open symbols. TTS of unknown nature are displayed as asterisks. Multiple stars are marked by boxes. The solid lines are linear regressions computed with the EM algorithm implemented in ASURV. The size of the errors bars varies a lot due to very different ROSAT exposure times, and they are sometimes smaller than the plotting symbol.

Open with DEXTER

	Figure 10: Same as Fig. 9 for the Pleiades.
Open with DEXTER

	Figure 11: Same as Fig. 9 for the Hyades.
Open with DEXTER

Pleiads, and Hyads. Overlaid are the linear regressions corresponding to the power law relation from Table 11. The lowest significance is found in the Hyades. This may however be due to the limited range in rotation period (only two stars with $P_{\rm rot} < 4~{\rm d}$), and because the Hyades with known period have a small range of spectral types.

  
6 Discussion

  
6.1 The XLF of cTTS and wTTS

We have reanalysed the XLF for cTTS and wTTS in Taurus-Auriga, first presented by N95, increasing the sensitivity with respect to the RASS by $\sim$2 orders of magnitude. Our pointed PSPC observations confirm that in Taurus-Auriga wTTS are on average more X-ray luminous than cTTS. This is in contrast to studies of Cha I and $\rho$ Oph (Feigelson et al. 1993; Casanova et al. 1995; Grosso et al. 2000), where no difference was found between the two sub-classes of TTS concerning their X-ray emission level. In a study of the Orion Nebula region with the ROSAT HRI Gagné & Caillault (1995) found slightly lower median $L_{\rm x}$ and $L_{\rm x}/L_{\rm bol}$ values for stars with massive accretion disks, i.e. cTTS. Alcalá et al. (1997) have found higher X-ray luminosities for ROSAT discovered wTTS in the outer parts of the Cha I and Cha II regions. This seems to indicate that samples of wTTS may be biased towards strong X-ray emitters, and that discrepancies can arise from the different spatial distribution of the cTTS and wTTS sample.

We have ruled out such an X-ray selection bias for our sample, by comparing the XLF for wTTS discovered by means of their X-ray emission to those which have been identified in other ways. XLF constructed for a coeval subgroup of cTTS and wTTS located in a central portion of the Taurus-Auriga complex, the L1495E cloud, show the same disagreement. Therefore, the difference does not seem to be related to the wide spatial extension (hence large age spread) of the Taurus star forming region. In addition this test shows that the disagreement is not caused by the different sensitivities (due to different exposure times) of the various combined PSPC observations.

Further effects, like different spectral type distribution, the specific choice of the $W_{\rm H\alpha}$ boundary between cTTS and wTTS, or our way of splitting the X-ray emission on all components in multiples, can not explain the observed discrepancies between the cTTS and wTTS XLF. To investigate whether the high number of upper limits in the cTTS sample affects the shape of the XLF we have also computed XLF neglecting all upper limits. (Grosso et al. 2000 have not included upper limits in their XLF of $\rho$ Oph.) The structure of the XLF, however, remains unaffected.

We conclude that there is an intrinsic difference in X-ray emission from cTTS and wTTS in Taurus. Besides the extinction effect discussed above the different evolutionary state of TTS in different star forming regions may contribute to the observed discrepancies. It should be noted that the subsamples of cTTS and wTTS in Taurus with known $T_{\rm eff}$ and $L_{\rm bol}$ occupy the same region in the H-R diagram, i.e. the difference in $L_{\rm x}$ seems not to be a direct age effect.

The correlation between the X-ray luminosity and $P_{\rm rot}$ we found for all examined samples suggests that the X-ray emission level may be governed by rotation. To check this hypothesis we have computed separate XLF for fast rotating wTTS ( $v \sin{i} > 22~{\rm km\,s^{-1}}$, the mean ${v \sin{i}}$ for wTTS), and slowly rotating wTTS ( $v \sin{i} < 12~{\rm km\,s^{-1}}$). Indeed, the slow rotators are characterized by lower X-ray luminosity ( $\log{L_{\rm x,mean}} = 29.54 \pm 0.13$versus $30.00 \pm 0.11$ for the fast group). This explains some but not all of the discrepancy between the XLF of Fig. 3. From the mean rotation rate of cTTS and wTTS and the mean $\log{L_{\rm x}}$ values derived from the KME analysis the slope in Fig. 9 would be expected to be much steeper. But note, that only a small fraction of TTS has measured rotation periods, and the large spread in the observed rotation-activity relation may be due to mixing of stars with different mass.

If, indeed, rotation is the major parameter that determines the amount of X-rays emitted by a given star then cTTS and wTTS in Taurus-Auriga are expected to have different $L_{\rm x}$ because the wTTS are on average faster rotators (see Bouvier et al. 1993 and our Fig. 9). Different distributions of rotation periods are also found in other star forming regions, e.g. Lupus (Wichmann et al. 1998b). Only in Orion cTTS and wTTS are found to rotate at the same speed (Stassun et al. 1999). The rotational state of the PMS stars in Cha I and $\rho$ Oph has not yet been investigated in detail. We suspect that most of the wTTS in Taurus-Auriga (including those in L1495E) have spent a longer time than those in Cha I and $\rho$ Oph since they have dispersed their disks, and therefore have had more time to spin up, and consequently should drive a more powerful dynamo. This implies that the disk lifetimes depend on the local condition in the star forming region. We remark that this hypothesis can only be tested after more measurements of rotational velocities in these different regions are available. In a later paper we will compare the XLF in different star forming regions in more detail.

  
6.2 Spectral type and age dependence of the X-ray emission

We have compared the XLF of TTS in Taurus-Auriga, the Pleiades, and the Hyades. Following early studies by the EO the XLF of Pleiades and Hyades had been examined with the improved sensitivity of ROSAT (see e.g. Hodgkin et al. 1995; Micela et al. 1996; Pye et al. 1994; Stern et al. 1995). However, all studies of X-ray luminosity on these young clusters were based on smaller data sets than the one presented here.

In lack of the knowledge about individual masses we take account of the known mass dependence of the X-ray luminosity by regarding G, K, and M stars separately. For all spectral type groups wTTS are found to be the strongest X-ray emitters, and the Hyades show the lowest level of X-ray emission. The difference between $\langle L_{\rm x} \rangle$ of the Pleiades and the Hyades is small for G stars where the spread in the mass distribution is largest, but large for M stars which have more uniform masses. This suggests that the decline in the X-ray emission is mostly an age effect. The XLF of cTTS and the Pleiades intersect each other, because the Pleiades are characterized by a much steeper distribution indicating less spread in $L_{\rm x}$. This difference may be a result of the uniform distance assumed for all stars in a given group (except the Hyades for which individual Hipparcos parallaxes were used). If the extension in the direction along the line-of-sight is comparable to the observed spatial dispersion, the TTS in Taurus-Auriga should be subject to a distance spread of $\sim$50 pc. Consequently the luminosities of some stars are underestimated while others are overestimated, thus leading to a larger spread in $L_{\rm x}$ and a flattening of the XLF. For the more compact Pleiades region instead the assumption of uniform distance may be adequate.

The XLF of Hyades K stars show a substructure appearing as an edge at $\log{L_{\rm x}} \sim 28.7$. In order to explain this feature we have divided the K star Hyades into two subgroups of $\log{L_{\rm x}}$ larger/smaller than 28.7. No differences between these two samples were found concerning the distribution of effective temperature, distances, and location on the sky. Only few of the Hyades K stars have measured ${v \sin{i}}$ or rotation period. Therefore, the hypothesis that the high-luminosity tail is composed of the fast rotators can not be tested. Note, that the edge in the slope is seen in both single and binary stars (see Fig. 8), but seems to be more pronounced for single stars. We suggest, that the effect is due to as yet undiscovered multiples among the K type Hyades.

We have extended our investigation of the dependence of the X-ray emission on spectral type by direct examination of correlations between these parameters (see Fig. 7). This investigation reveals differences between TTS, Pleiades, and Hyades which we suppose are related to the different ages of these groups. For stars on the MS $T_{\rm eff}$ corresponds to mass, and mass is related to the depth of the convection zone. The observed anti-correlation between ${\log{(L_{\rm x}/L_{\rm bol})}}$ and ${\log{T_{\rm eff}}}$ from Fig. 7 therefore demonstrates the importance of convection for X-ray activity. Although there is a tendency of ${\log{(L_{\rm x}/L_{\rm bol})}}$ being larger for cooler stars, the absolute amount of X-rays emitted is smaller (see Figs. 6 and 7). In the Pleiades $L_{\rm x}$ does not strongly depend on spectral type, although ${\log{(L_{\rm x}/L_{\rm bol})}}$ decreases with increasing $T_{\rm eff}$. This is most likely due to the shorter time the latest type stars in the Pleiades have spent on the MS. Most of the late K and M type Pleiads did not spin down to loose their high initial activity level, yet. The PMS TTS show no correlation between ${\log{(L_{\rm x}/L_{\rm bol})}}$ and ${\log{T_{\rm eff}}}$. This may be due to the large age spread in the TTS sample (10^5..7 yrs).

The most active stars of all groups are characterized by ${\log{(L_{\rm x}/L_{\rm bol})}}$ $\sim -3$, the canonical value for late-type stars. This behavior is been referred to as "saturation'', and has been described in the literature; see e.g. Fleming et al. (1989), Feigelson et al. (1993), Micela et al. (1996), Randich et al. (1996), Stauffer et al. (1997), Micela et al. (1999). A common explanation is that all saturated stars have reached their highest possible level of X-ray activity, e.g. by coverage of the full surface with active regions. The stellar radius rather than rotation would then determine the X-ray emission level (see Fleming et al. 1989). The correlation between $L_{\rm x}$ and spectral type in TTS may be understood in terms of such a saturation effect: Fig. 7 suggests that many TTS regardless of their spectral type have reached the saturation level. However, the more luminous the stars, the larger they are, and the higher the saturation level for $L_{\rm x}$. Therefore, for given $L_{\rm bol}$ the X-ray luminosity is limited by a value that corresponds to saturation, and which is lower for later spectral types.

The dispersion of $\log{L_{\rm x}}$ for given spectral type can be regarded from two points of view: (a) all stars of given spectral type show intrinsically similar amounts of X-ray emission, and the spread in $L_{\rm x}$is caused by variability of individual stars, or (b) the dispersion reflects different activity levels of the stars. Our analysis of the longterm X-ray behavior of these stars (to be presented in a subsequent paper; Stelzer et al. in prep.) suggests little variability on long timescales making the former hypothesis improbable. The distribution of $L_{\rm x}$ within stars of homogeneous spectral type thus more likely reflects the variety of X-ray emission from individual stars.

  
6.3 Are Hyades binaries overluminous?

Pye et al. (1994) have examined the XLF of Hyades stars combining 11 ROSAT PSPC observations. In their sample they found that Hyades dK binaries are overluminous in X-rays: all binary dK stars analysed by Pye et al. (1994) were brighter than any of the single dK stars. This result was confirmed by Stern et al. (1995) on a larger sample of Hyades drawn from the RASS.

In our analysis of the XLF in the Hyades we have treated binary stars in two ways: (A) in the same way as singles, i.e. without taking account of the multiplicity (sample "b1''), and (B) dividing the observed luminosity by two to account for X-rays from both components (sample "b2''). We find a probability of $\sim$10-15% for the null-hypothesis that the distributions of singles ("s'') and "b2'' among the Hyades K stars are drawn from the same parent distribution. For Hyades M stars (not examined by Pye et al. 1994 due to lack of statistics but found to display a similar though less pronounced divergence between single and binary XLF in the study of Stern et al. 1995) we find a similar probability for the rejection of the null-hypothesis that "s'' and "b2'' are drawn from the same parent distribution. However, the sample of M star binaries in the Hyades is very small (9 stellar systems). For all other pairs of "s'' - "b2'' distributions, i.e. those of Hyades G stars, Pleiades, and TTS, there is no statistical evidence for differences. The agreement between the XLF of single ("s'') and binary ("b2'') stars is expected if the components in binaries have no mutual influence on their activity, and if indeed the distribution of the observed X-ray emission equally on all components conforms with the real situation. This seems likely because binaries with very high mass ratio, i.e. largely different $L_{\rm x}$, are more difficult to detect than equal mass ratio binaries.

When compared to the distributions "b1'', singles are fainter in all cases (probability for the distributions being similar <10%). This is in agreement with the study of Pye et al. (1994) and Stern et al. (1995) who have examined samples of type "b1''.

This results emphasize that it is important to consider the binary character when analysing XLF of double stars. Splitting the X-ray emission onto the components significantly decreases the difference between single and binary XLF. However, some discrepancy for the Hyades K and M stars remains unexplained. A proper treatment of binary stars is also important in correlation studies, as it decreases the spread.

  
6.4 The age-activity-rotation connection

We have shown that the rotation period and various measures for the X-ray activity (i.e. luminosity, surface flux, and $L_{\rm x}/L_{\rm bol}$-ratio) are correlated for all examined age groups. The steepness of the activity-rotation relation is very different for TTS, Pleiades, and Hyades, with the largest slope for the TTS, e.g. slow rotators in the Pleiades have much higher surface flux than TTS with similar periods (see Figs. 9 to 11). We think that these differences can be explained by the particular distribution of spectral types: In Fig. 12 we show the $\log{F_{\rm s}} - \log{P_{\rm rot}}$diagrams with plotting symbols scaled according to $T_{\rm eff}$.

	Figure 12: X-ray surface flux versus rotation period for TTS, Pleiades, and Hyades indicating the distribution of effective temperatures (plotting symbols are scaled to $T_{\rm eff}$). Note, that most of the slow rotators in the TTS sample are cool objects. Open circles are upper limits for undetected objects.
Open with DEXTER

In the TTS sample we observe a clear clustering of cooler stars at slow rotation periods. For given $L_{\rm bol}$ and $L_{\rm x}$ cooler stars have larger radius and therefore smaller surface flux. This results in a steeper slope for the TTS sample.

Fast rotators are found at all spectral types in the Pleiades and among the TTS. Indeed, the fastest rotators form the upper envelope to the ${\log{(L_{\rm x}/L_{\rm bol})}}$- ${\log{T_{\rm eff}}}$ diagram (Fig. 7). At the age of the Hyades most stars (regardless of spectral type) have slowed down their rotation, such that the range of measured periods is limited, and definitive statements about the activity-rotation connection for the Hyades are difficult.

We have examined the mean level of X-ray surface flux for each age group in order to infer a decay law. In Fig. 13 the mean $F_{\rm s}$ is plotted for cTTS,

Figure 13: Time evolution of the X-ray surface flux for TTS, Pleiades, and Hyades for three spectral type groups (plotting symbols for G and M stars for clarity with a small offset on the age-scale). The thick solid line represents a fit to the mean of $F_{\rm s}$ obtained by combining G, K, and M stars from the wTTS, Pleiades, and Hyades sample. The slope of this exponential decay is $-2.0 \pm 0.1$ in agreement with earlier estimates for smaller samples of stars from the same region (see text).

Open with DEXTER

wTTS, Pleiades, and Hyades, each being split into G, K, and M type stars. The X-ray flux increases from cTTS to wTTS as mentioned by N95. (Only one cTTS has spectral type of G.) An exponential fit to the combined G + K + M sample from the wTTS to the Hyades age is overlaid, and provides a slope of $-2.01 \pm 0.09$. This compares well with the result by Walter & Barry (1991) who found a decrease of $F_{\rm s}$ with $-2.20 \pm 0.21$ for a sample composed of Einstein detected naked TTS, Pleiades and Hyades.

Acknowledgements

We made use of the Open Cluster Database, compiled by C. F. Prosser and J. R. Stauffer. R.N. wishes to acknowledge financial support from the Bundesministerium für Bildung und Forschung through the Deutsche Zentrum für Luft- und Raumfahrt e.V. (DLR) under grant number 50 OR 0003. The ROSAT project is supported by the Max-Planck-Gesellschaft and Germany's federal government (BMBF/DLR). We would like to thank the referee T. Montmerle for helpful comments and stimulating discussions.

References

 
• Alcalá, J. M., Krautter, J., Covino, E., et al. 1997, A&A, 319, 184 In the text NASA ADS  
• Baraffe, I., Chabrier, G., Allard, F., & Hauschildt, P. H. 1998, A&A, 337, 403 In the text NASA ADS  
• Bouvier, J. 1990, AJ, 99, 946 In the text NASA ADS  
• Bouvier, J., Cabrit, S., Fernández, M., Martín, E. L., & Matthews, J. M. 1993, A&A, 272, 176 In the text NASA ADS  
• Bouvier, J., Forestini, M., & Allain, S. 1997a, A&A, 326, 1023 In the text NASA ADS  
• Bouvier, J., Wichmann, R., Grankin, K., et al. 1997b, A&A, 318, 495 In the text NASA ADS  
• Casanova, S., Montmerle, T., Feigelson, E. D., & André, P. 1995, ApJ, 439, 752 In the text NASA ADS  
• Cernicharo, J., Bachiller, R., & Duvert, G. 1985, A&A, 149, 273 NASA ADS  
• Cruddace, R. G., Hasinger, G. R., & Schmitt, J. H. M. M. 1988, in Astronomy from large databases, ed. F. Murtagh, A. Heck (ESO, Garching), 177  
• Damiani, F., Micela, G., & Vaiana, G. S. 1991, in Angular Momentum Evolution of Young Stars, NATO Adv. Research Workshop held in Noto, Sicily, Italy, ed. S. Catalano, & J. R. Stauffer (Kluwer, Dordrecht), 89 In the text  
• Damiani, F., & Micela, G. 1995, ApJ, 446, 341 In the text NASA ADS  
• Damiani, F., Micela, G., Sciortino, S., & Harnden, Jr. F. R. 1995, ApJ, 446, 331 In the text NASA ADS  
• D'Antona, F., & Mazzitelli, I. 1994, ApJS, 90, 467 In the text NASA ADS  
• Edwards, S., Strom, S. E., Hartigan, P., et al. 1993, AJ, 106, 372 In the text NASA ADS  
• Elias, J. H. 1978, ApJ, 224, 857 In the text NASA ADS  
• Feigelson, E. D., & Nelson, P. I. 1985, ApJ, 293, 192 In the text NASA ADS  
• Feigelson, E. D., & Kriss, G. A. 1989, ApJ, 338, 262 In the text NASA ADS  
• Feigelson, E. D., Casanova, S., Montmerle, T., et al. 1993, ApJ, 416, 623 In the text NASA ADS  
• Fleming, T. A., Gioia, I. M., & Maccacaro, T. 1989, ApJ, 340, 1011 In the text NASA ADS  
• Fleming, T. A., Molendi, S., Maccacaro, T., et al. 1995, ApJS, 99, 701 In the text NASA ADS  
• Gagné, M., & Caillault, J.-P. 1995, ApJ, 445, 280 In the text NASA ADS  
• Grankin, K. N. 1993, IBVS, 3823 In the text  
• Grosso, N., Montmerle, T., Bontemps, S., et al. 2000, A&A, 359, 113 In the text NASA ADS  
• Hearty, T. J., Neuhäuser, R., Stelzer, B., et al. 2000, A&A, 353, 1044 NASA ADS  
• Herbig, G. H., & Bell, K. R. 1988, Lick Observatory Bulletin, No. 1111  
• Hodgkin, S. T., Jameson, R. F., & Steele, I. A. 1995, MNRAS, 274, 869 In the text NASA ADS  
• Isobe, T., Feigelson, E. D., & Nelson, P. I. 1986, ApJ, 306, 490 In the text NASA ADS  
• Kenyon, S. J., & Hartmann, L. 1995, ApJS, 101, 117 In the text NASA ADS  
• König, B., Neuhäuser, R., & Stelzer, B. 2001, A&A, 369, 971 In the text NASA ADS  
• Koenigl, A. 1991, ApJ, 370, L39 In the text NASA ADS  
• LaValley, M., Isobe, T., & Feigelson, E. 1992, in Astronomical Data Analysis Software and Systems I, ed. D. M. Worrall et al., ASP Conf. Ser. 25, 245 In the text  
• Leggett, S. K., & Hawkins, M. R. S. 1989, MNRAS, 238, 145 In the text NASA ADS  
• Luhman, K. L. 2000, ApJ, 544, 1044 NASA ADS  
• Martín, E. L. 1997, A&A, 321, 492 In the text NASA ADS  
• Martín, E. L., Montmerle, T., Gregorio-Hetem, J., & Casanova, S. 1998, MNRAS, 300, 733 NASA ADS  
• Mermilliod, J. C., Turon, C., Robichon, N., et al. 1997, in ESA Symposium Hipparcos Venice 98, Venice, Italy, ed. B. Battrick, ESA SP-402, 643 In the text  
• Micela, G., Sciortino, S., Kashyap, V., et al. 1996, ApJS, 102, 75 In the text NASA ADS  
• Micela, G., Sciortino, S., Harnden, Jr. F. R., et al. 1999, A&A, 341, 751 In the text NASA ADS  
• Montmerle, T., Koch-Miramond, L., Falgarone, E., & Grindlay, J. E. 1983, ApJ, 269, 182 NASA ADS  
• Neuhäuser, R., Sterzik, M. F., Schmitt, J. H. M. M., et al. 1995, A&A, 297, 391 (N95) In the text NASA ADS  
• Neuhäuser, R., & Comerón, F. 1998, Science, 282, 83 In the text NASA ADS  
• Neuhäuser, R., Briceño, C., Comerón, F., et al. 1999, A&A, 343, 883 In the text NASA ADS  
• Palla, F., & Stahler, S. W. 1999, ApJ, 525, 772 In the text NASA ADS  
• Pallavicini, R., Golub, L., Rosner, R., et al. 1981, ApJ, 248, 279 In the text NASA ADS  
• Paresce, F. 1984, AJ, 89, 1022 In the text NASA ADS  
• Perryman, M. A. C., Brown, A. G. A., Lebreton, Y., et al. 1998, A&A, 331, 81 In the text NASA ADS  
• Preibisch, T. 1997, A&A, 324, 690 In the text NASA ADS  
• Preibisch, T., Zinnecker, H., & Herbig, G. H. 1996, A&A, 310, 456 In the text NASA ADS  
• Pye, J. P., Hodgkin, S. T., Stern, R. A., et al. 1994, MNRAS, 266, 798 In the text NASA ADS  
• Randich, S., Schmitt, J. H. M. M., Prosser, C. F., & Stauffer, J. R. 1996, A&A, 305, 785 In the text NASA ADS  
• Reid, I. N., & Hawley, S. L. 1999, AJ, 117, 343 In the text NASA ADS  
• Ryter, C. E. 1996, Ap&SS, 236, 285 In the text NASA ADS  
• Schmidt-Kaler, T. H. 1982, Physical Parameters of Stars, in Landolt-Börnstein New Ser., Vol 2b, Astronomy and Astrophysics Stars and Star Clusters, ed. K. Shaifers, & H. H. Voigt (New York, Springer) In the text  
• Schmitt, J. H. M. M. 1985, ApJ, 293, 178 In the text NASA ADS  
• Skumanich, A. 1972, ApJ, 171, 565 In the text NASA ADS  
• Stassun, K. G., Mathieu, R. D., Mazeh, T., & Vrba, F. J. 1999, AJ, 117, 2941 In the text NASA ADS  
• Stauffer, J. R., Caillault, J.-P., Gagné, M., Prosser, C. F., & Hartmann, L. W. 1994, ApJS, 91, 625 In the text NASA ADS  
• Stauffer, J. R., Hartmann, L. W., Prosser, C. F., et al. 1997, ApJ, 479, 776 In the text NASA ADS  
• Stelzer, B., Neuhäuser, R., & Hambaryan, V. 2000, A&A, 356, 949 (SNH00) In the text NASA ADS  
• Strom, K. M., & Strom, S. E. 1994, ApJ, 424, 237 In the text NASA ADS  
• Stern, R. A., Schmitt, J. H. M. M., Pye, J. P., et al. 1994, ApJ, 427, 808 NASA ADS  
• Stern, R. A., Schmitt, J. H. M. M., & Kahabka, P. T. 1995, ApJ, 448, 683 In the text NASA ADS  
• Walter, F. M. 1981, ApJ, 245, 677 In the text NASA ADS  
• Walter, F. M., & Bowyer, S. 1981, ApJ, 245, 671 In the text NASA ADS  
• Walter, F. M. 1982, ApJ, 253, 745 In the text NASA ADS  
• Walter, F. M. 1983, ApJ, 274, 794 In the text NASA ADS  
• Walter, F. M., Brown, A., Mathieu, R. D., Myers, P. C., & Vrba, F. J. 1988, AJ, 96, 297 In the text NASA ADS  
• Walter, F. M., & Barry, D. C. 1991, in The sun in time, ed. C. P. Sonnett et al. (Tucson, Univ. Arizona Press), 663 In the text  
• Wichmann, R., Krautter, J., Schmitt, J. H. M. M., Neuhäuser, R., Alcalá, J. M., et al. 1996, A&A, 312, 439 In the text NASA ADS  
• Wichmann, R., Bastian, U., Krautter, J., et al. 1998a, MNRAS, 301, L39 In the text NASA ADS  
• Wichmann, R., Bouvier, J., Allain, S., & Krautter, J. 1998b, A&A, 330, 521 In the text NASA ADS

 

Online Material

   

Table 2: X-ray data for TTS in Taurus-Auriga detected in PSPC observations.

Obs. No.	Designation	Type/	SpT.	X-ray position		$\Delta$	Offax	ML	HR1	HR2	Expos	$\log{L_{\rm X}}$
		Mult.		$\alpha_{2000}$	$\delta_{2000}$	[ $^{\prime\prime}$]	[$^\prime$]				[s]	[erg/s]
3	${\rm CZTau +/c }$	WB	M2	04 18 31.6	+28 16 59	1	11	139	>0.82	$0.24 \pm 0.16$	4173	29.07 $\pm$0.15
	${\rm DDTau +/c }$	CB	M1	04 18 31.6	+28 16 59	29						$\pm$
3F	${\rm V410x-ray7 }$	W	M1	04 18 42.0	+28 19 03	12	0	1616	>0.97	$0.84 \pm 0.05$	4180	30.16 $\pm$0.13
3F	${\rm BPTau }$	C	K7	04 19 16.4	+29 06 27	8	0	598	$0.92 \pm 0.12$	$0.27 \pm 0.14$	3020	30.06 $\pm$0.06
3	${\rm HD283572 }$	W	G5	04 21 58.5	+28 18 28	19	46	1534	$0.92 \pm 0.03$	$0.26 \pm 0.04$	2792	30.83 $\pm$0.02
4F	${\rm DDTau +/c }$	B	M1	04 18 31.3	+28 16 35	6	10	1274	$0.88 \pm 0.06$	$0.43 \pm 0.06$	22508	28.78 $\pm$0.00
	${\rm CZTau +/c }$	WB	M2			24						$\pm$
4	${\rm V410x-ray7 }$	W	M1	04 18 41.3	+28 19 14	26	8	2285	$0.98 \pm 0.02$	$0.72 \pm 0.03$	25645	29.84 $\pm$0.02
4	${\rm BPTau }$	C	K7	04 19 15.7	+29 06 08	19	40	193	$0.78 \pm 0.10$	$0.27 \pm 0.08$	16412	29.78 $\pm$0.05
4F	${\rm HD283572 }$	W	G5	04 21 57.8	+28 19 44	96	0	2264	$0.90 \pm 0.01$	$0.31 \pm 0.02$	13203	30.96 $\pm$0.12
11	${\rm BD+23^\circ502 }$	W	G5	03 44 18.3	+24 06 00	61	37	58	>0.75	$0.36 \pm 0.16$	894	30.00 $\pm$0.17
19	${\rm RXJ0453.1+3311 +B + C}$	WT	G8	04 53 10.6	+33 12 54	57	48	17	$0.14 \pm 0.61$	$-0.01 \pm 0.57$	5624	28.44 $\pm$0.56
21	${\rm NTTS041559+1716 }$	W	K7	04 18 52.0	+17 23 18	7	35	664	$0.15 \pm 0.05$	$0.08 \pm 0.06$	13460	30.05 $\pm$0.02
21	${\rm J2-157 }$	C	M6	04 20 53.0	+17 46 40	6	15	128	$0.09 \pm 0.10$	$0.09 \pm 0.13$	18121	29.18 $\pm$0.06
22	${\rm RXJ0431.4+1800 +B}$	CB	M5	04 31 22.9	+18 00 07	21	32	13	$0.54 \pm 0.39$	$-0.39 \pm 0.26$	15229	28.61 $\pm$0.20
22F	${\rm L1551-51 }$	W	K7	04 32 09.2	+17 57 26	3	0	2259	$0.92 \pm 0.03$	$0.07 \pm 0.04$	12191	29.98 $\pm$0.29
22	${\rm V827Tau }$	W	K7	04 32 13.5	+18 20 14	13	48	713	$0.82 \pm 0.05$	$0.06 \pm 0.04$	12033	30.29 $\pm$0.02
22	${\rm V826Tau }$	WSB	K7	04 32 16.0	+18 01 35	4	29	2592	$0.89 \pm 0.02$	$0.16 \pm 0.03$	14170	30.13 $\pm$0.01
22	${\rm GGTau +/c }$	CQ	K7/M5/	04 32 30.3	+17 31 45	3/13/	2	342	>0.81	$0.16 \pm 0.09$	19724	28.61 $\pm$0.13
	${\rm +/c2 +/c3 }$		M1/M7			16/14						$\pm$
22	${\rm L1551-55 }$	W	K7	04 32 44.1	+18 02 57	4	31	140	$0.76 \pm 0.12$	$0.26 \pm 0.09$	15357	29.54 $\pm$0.06
22	${\rm LH0429+17 }$	C	M9	04 32 50.4	+17 30 10	10	4	7	$-0.24 \pm 0.35$	$0.58 \pm 0.57$	20190	28.18 $\pm$0.26
22	${\rm RXJ0432.9+1735 }$	W	M2	04 32 53.2	+17 35 37	3	6	1375	$0.95 \pm 0.03$	$0.13 \pm 0.05$	19526	29.82 $\pm$0.02
22	${\rm NTTS043230+1746 +B}$	WB	M2	04 35 24.8	+17 51 58	20	45	345	$0.45 \pm 0.06$	$0.13 \pm 0.06$	12828	29.80 $\pm$0.03
26	${\rm RXJ0348.8+2359 }$	W	G7	03 48 49.1	+23 58 35	17	29	167	$0.65 \pm 0.09$	$-0.09 \pm 0.09$	14869	29.63 $\pm$0.04
26	${\rm Melotte22-2147 }$	W	G7	03 49 06.6	+23 46 46	12	37	2922	$0.51 \pm 0.02$	$0.20 \pm 0.03$	16019	30.55 $\pm$0.01
26	${\rm Melotte22-2881 }$	W	G7	03 50 54.4	+23 50 07	11	33	501	$0.57 \pm 0.05$	$-0.03 \pm 0.06$	15339	29.94 $\pm$0.03
26	${\rm NTTS034903+2431 +B}$	WB	K5	03 52 01.4	+24 39 48	11	32	1452	$0.57 \pm 0.03$	$0.04 \pm 0.04$	16137	29.89 $\pm$0.02
27	${\rm Mellote22Pels56 }$	W	G2	03 43 26.7	+25 23 02	29	38	1164	$0.74 \pm 0.04$	$0.09 \pm 0.04$	15442	30.16 $\pm$0.02
27	${\rm Mellote22\,253 }$	W	G0	03 44 03.4	+24 30 11	6	17	10288	$0.80 \pm 0.01$	$0.18 \pm 0.02$	25915	30.50 $\pm$0.01
27	${\rm BD+23^\circ501B }$	W	K0	03 44 12.1	+24 02 15	15	44	54	$0.59 \pm 0.04$	$0.14 \pm 0.04$	17258	30.19 $\pm$0.02
27	${\rm BD+23^\circ502 }$	W	G5	03 44 17.4	+24 05 48	56	41	2449	$0.90 \pm 0.02$	$0.15 \pm 0.03$	18262	30.35 $\pm$0.01
27	${\rm RXJ0344.3+2447 }$	W	G0	03 44 20.0	+24 47 38	21	2	9163	$0.46 \pm 0.02$	$0.08 \pm 0.02$	26570	30.31 $\pm$0.01
27	${\rm Melotte22-345 }$	W	G7	03 44 26.2	+24 35 16	8	11	5657	$0.46 \pm 0.02$	$0.09 \pm 0.03$	25805	30.19 $\pm$0.01
27	${\rm RXJ0345.6+2454 }$	W	G5	03 45 41.9	+24 54 17	8	19	3756	$0.62 \pm 0.02$	$0.07 \pm 0.03$	14062	30.41 $\pm$0.01
29	${\rm CoKuHPTau/G2 +/G3}$	WT	G0/K7	04 35 54.0	+22 54 21	7/13/	2	297	>0.98	$0.40 \pm 0.12$	740	29.83 $\pm$0.14
	${\rm + HPTau }$		K2			16						$\pm$
31	${\rm DNTau }$	C	M0	04 35 27.7	+24 14 06	54	47	219	$0.81 \pm 0.11$	$0.19 \pm 0.10$	2978	30.08 $\pm$0.06
39	${\rm NTTS041529+1652 }$	W	K5	04 18 18.1	+16 58 15	55	43	9	>-0.76	$0.25 \pm 0.15$	15647	29.06 $\pm$0.20
40F	${\rm RXJ0437.5+1851B +B}$	WB	M1	04 37 26.7	+18 51 20	5	0	7979	$0.02 \pm 0.02$	$0.10 \pm 0.03$	15420	30.01 $\pm$0.13
45	${\rm LkCa1 }$	W	M4	04 13 14.3	+28 19 12	2	13	27	$0.76 \pm 0.31$	$0.01 \pm 0.26$	5580	29.06 $\pm$0.15
45	${\rm Anon1 }$	W	M0	04 13 27.5	+28 16 23	5	10	1136	$0.98 \pm 0.02$	$0.39 \pm 0.06$	5864	30.16 $\pm$0.03
45	${\rm V773Tau +/c +/c1}$	WT	K3	04 14 13.2	+28 12 13	4	2	6026	$0.96 \pm 0.01$	$0.31 \pm 0.03$	6330	30.25 $\pm$0.01
	${\rm FMTau }$	C	M0			38						30.72 $\pm$0.01
45	${\rm FNTau }$	C	M5	04 14 14.7	+28 27 54	5	15	101	>0.62	$0.31 \pm 0.14$	5381	29.37 $\pm$0.15
45	${\rm MHO-2 + MHO-1 }$	CB	M3	04 14 26.5	+28 06 01	2/5	7	185	>0.84	$0.61 \pm 0.11$	6093	29.07 $\pm$0.14
45	${\rm MHO-3 }$	C	K7	04 14 30.6	+28 05 13	4	8	69	>0.65	$0.79 \pm 0.13$	6122	29.00 $\pm$0.17
45	${\rm LkCa3 +/c }$	W	M1	04 14 48.2	+27 52 40	5	21	432	$0.67 \pm 0.06$	$0.15 \pm 0.08$	4424	29.83 $\pm$0.04
45	${\rm FOTau +/c }$	CB	M2	04 14 49.0	+28 12 28	5/4	8	17	>0.33	$-0.32 \pm 0.31$	5607	28.38 $\pm$0.25
45	${\rm Briceno2 }$	W	M5	04 15 04.7	+28 08 50	6	12	24	>0.28	$0.01 \pm 0.28$	5945	28.85 $\pm$0.21
45	${\rm LkCa4 }$	W	K7	04 16 29.0	+28 07 44	14	31	198	$0.63 \pm 0.10$	$0.09 \pm 0.10$	4481	29.99 $\pm$0.05
48	${\rm NTTS041529+1652 }$	W	K5	04 18 21.4	+16 59 17	31	24	45	$0.98 \pm 0.23$	$0.50 \pm 0.18$	3697	29.43 $\pm$0.13
48	${\rm NTTS041559+1716 }$	W	K7	04 18 48.8	+17 23 35	44	45	42	$0.26 \pm 0.18$	$0.15 \pm 0.20$	2335	29.83 $\pm$0.11
50	${\rm V836Tau }$	W	K7	05 03 06.6	+25 23 20	1	11	930	$0.99 \pm 0.02$	$0.22 \pm 0.07$	6997	30.01 $\pm$0.03
50	${\rm IRAS05023+2527 }$	C	K7M0	05 05 20.5	+25 31 13	37	29	24	>-0.46	$0.52 \pm 0.19$	5661	28.99 $\pm$0.25
53	${\rm RXJ0446.7+2459 }$	C	M4	04 46 42.8	+24 58 59	5	14	51	>0.29	$0.29 \pm 0.20$	9011	28.92 $\pm$0.17
55	${\rm HVTau A + B + C }$	WT	M1	04 38 35.0	+26 10 40	3	21	792	$0.96 \pm 0.04$	$0.33 \pm 0.06$	7083	29.57 $\pm$0.03
55	${\rm Elias18 }$	C		04 39 55.6	+25 45 16	13	20	28	$0.54 \pm 0.35$	$0.89 \pm 0.25$	5689	29.00 $\pm$0.19
55	${\rm JH223 }$	W	M2	04 40 49.7	+25 51 20	3	17	32	>-0.03	$0.51 \pm 0.24$	8739	28.78 $\pm$0.20
55	${\rm CoKuLkH\alpha332/G1/c}$	WTr		04 42 04.1	+25 23 17	43	49	185	$0.88 \pm 0.12$	$0.60 \pm 0.08$	6083	29.48 $\pm$0.06
56	${\rm IWTau +/c }$	WB	K7	04 41 04.9	+24 51 11	6	37	933	$0.95 \pm 0.04$	$0.15 \pm 0.05$	5966	30.05 $\pm$0.03
56	${\rm CoKuLkH\alpha332/G1 +V955Tau~}$	WT	M1/K7	04 42 05.8	+25 22 59	15/29	3	1563	>0.98	$0.46 \pm 0.05$	8100	29.51 $\pm$0.12
	${\rm CoKuLkH\alpha332/G2 }$	W	K7			5						29.98 $\pm$0.12
56	${\rm Briceno7 }$	C	M3	04 42 21.3	+25 20 33	6	5	53	$0.82 \pm 0.25$	$0.32 \pm 0.21$	7816	28.96 $\pm$0.13
56	${\rm GOTau }$	C	M0	04 43 03.4	+25 20 18	5	13	9	>-0.18	$-0.01 \pm 0.43$	7565	28.43 $\pm$0.35
58	${\rm CoKuTau/1 +B }$	CB	M0	04 18 46.8	+28 20 04	66	43	309	$0.80 \pm 0.06$	$0.39 \pm 0.06$	3263	30.10 $\pm$0.03
60	${\rm LkCa19 }$	W	K0	04 55 37.5	+30 17 55	7	15	787	$0.85 \pm 0.04$	$0.21 \pm 0.08$	1249	30.63 $\pm$0.04
61F	${\rm LkCa19 }$	W	K0	04 55 37.2	+30 17 56	2	0	5235	$0.87 \pm 0.02$	$0.27 \pm 0.03$	3549	30.82 $\pm$0.02
64	${\rm NTTS043230+1746 +/c}$	WB	M2	04 35 20.9	+17 51 48	45	46	20	$0.53 \pm 0.27$	$0.10 \pm 0.20$	2250	29.41 $\pm$0.17
70	${\rm RXJ0416.5+2053A }$	WB	M5	04 16 30.2	+20 53 07	38	23	9	>-0.24	$0.07 \pm 0.42$	3112	28.76 $\pm$0.38
72	${\rm RXJ0451.9+1758 +B}$	WB	M2	04 51 53.1	+17 58 27	15	29	133	$0.98 \pm 0.07$	$0.17 \pm 0.14$	1344	29.82 $\pm$0.07
72	${\rm RXJ0452.5+1730 }$	W	K4	04 52 31.0	+17 30 37	11	16	81	$0.64 \pm 0.15$	$-0.46 \pm 0.18$	1577	29.75 $\pm$0.09
72	${\rm St34 }$	C	M3	04 54 21.5	+17 11 24	93	46	17	$0.83 \pm 0.31$	$0.31 \pm 0.24$	995	29.75 $\pm$0.20
80	${\rm RXJ0416.5+2053A +B}$	WB	M5/M6	04 16 31.5	+20 53 36	51/61	42	20	>-0.69	$0.75 \pm 0.22$	5075	28.69 $\pm$0.35
81	${\rm Lick6 }$	W	M0	04 30 01.4	+35 17 24	4	2	85	$0.67 \pm 0.17$	$0.79 \pm 0.12$	5716	29.19 $\pm$0.10
81	${\rm Lick3 }$	W	K7	04 30 19.5	+35 17 47	5	3	598	>0.96	$0.71 \pm 0.06$	5715	29.71 $\pm$0.13
82	${\rm DKTau +/c }$	CB	K7	04 30 43.6	+26 01 26	8	27	190	$0.88 \pm 0.09$	$0.25 \pm 0.10$	8288	29.32 $\pm$0.06
82	${\rm UZTauw +w/c +e }$	CT	M3/-/M1	04 32 43.1	+25 52 33	3	2	254	$0.89 \pm 0.10$	$0.25 \pm 0.12$	10320	28.85 $\pm$0.06
82	${\rm ISTau +/c }$	CB	K7	04 33 36.5	+26 10 03	13	21	57	>0.32	$0.39 \pm 0.17$	5598	28.72 $\pm$0.19
82	${\rm ITTau +/c }$	WB	K2	04 33 54.5	+26 13 20	7/6	26	147	$0.96 \pm 0.13$	$0.49 \pm 0.11$	6639	29.23 $\pm$0.07
83	${\rm J4872 A + B }$	WB	K7	04 25 19.5	+26 17 48	32/30	35	527	$0.96 \pm 0.06$	$0.42 \pm 0.06$	7291	29.73 $\pm$0.04
83	${\rm DFTau +/c }$	CB	M3	04 27 03.3	+25 42 19	9	24	81	$0.70 \pm 0.14$	$0.17 \pm 0.15$	5773	29.14 $\pm$0.08
85	${\rm Hubble4 }$	W	K7	04 18 48.0	+28 20 19	17	46	1436	$0.99 \pm 0.02$	$0.50 \pm 0.04$	3408	30.73 $\pm$0.02
	${\rm CoKuTau/1 +B }$	CB	M0			47						30.43 $\pm$0.02
89	${\rm Kim3-76 }$	W		04 17 51.0	+28 28 32	67	41	23	>-0.41	$0.89 \pm 0.14$	3677	29.08 $\pm$0.35
96	${\rm IRAS04187+1927 }$	C	M0	04 21 43.8	+19 34 11	12	18	26	>0.41	$0.67 \pm 0.22$	3433	28.95 $\pm$0.24
96F	${\rm TTau N + S }$	CB	K0	04 22 00.0	+19 32 09	9	0	1614	$0.91 \pm 0.04$	$0.35 \pm 0.07$	2420	29.71 $\pm$0.12
96F	${\rm RXJ0422.1+1934 +B}$	CB	M5	04 22 05.1	+19 34 49	3	0	1881	$0.93 \pm 0.04$	$0.54 \pm 0.08$	4162	29.98 $\pm$0.13
106	${\rm RXJ0338.3+1020 }$	W	G9	03 38 18.0	+10 20 14	4	22	22	$0.70 \pm 0.23$	$-0.12 \pm 0.28$	913	29.74 $\pm$0.15
107	${\rm RXJ0338.3+1020 }$	W	G9	03 38 18.2	+10 20 19	2	22	57	$0.65 \pm 0.17$	$0.36 \pm 0.18$	1457	29.85 $\pm$0.10
108	${\rm RXJ0338.3+1020 }$	W	G9	03 38 17.8	+10 20 14	7	22	66	$0.86 \pm 0.14$	$0.06 \pm 0.18$	1949	29.77 $\pm$0.09
109	${\rm RXJ0338.3+1020 }$	W	G9	03 38 17.5	+10 20 16	10	22	92	$0.94 \pm 0.12$	$-0.01 \pm 0.13$	6025	29.63 $\pm$0.07
110	${\rm RXJ0304.6+1438 }$	W	G5	03 04 45.1	+14 37 36	27	47	391	$0.66 \pm 0.06$	$0.17 \pm 0.06$	3622	30.45 $\pm$0.03
112	${\rm RXJ0255.4+2005 }$	W	K6	02 55 26.6	+20 05 04	16	26	2250	$0.49 \pm 0.03$	$0.08 \pm 0.03$	18182	29.61 $\pm$0.01
112	${\rm LkHa262 }$	C	M0	02 56 08.3	+20 03 28	6	18	768	$0.88 \pm 0.04$	$0.11 \pm 0.06$	21135	29.02 $\pm$0.03
	${\rm LkHa263 }$	C	M4			11						$\pm$
112	${\rm LkHa264 }$	C	K5	02 56 37.8	+20 05 34	6	16	137	>0.31	$0.31 \pm 0.11$	20567	28.34 $\pm$0.14
112	${\rm 1E0255.3+2018 }$	WSB	K3	02 58 09.3	+20 29 54	26	42	495	$0.83 \pm 0.06$	$0.19 \pm 0.05$	16263	29.71 $\pm$0.03
112	${\rm RXJ0258.3+1947 }$	C	M5	02 58 15.9	+19 47 17	0	17	333	$0.99 \pm 0.06$	$0.17 \pm 0.08$	22808	28.73 $\pm$0.04
116	${\rm RXJ0459.8+1430 }$	W	K4	04 59 47.4	+14 30 28	33	48	160	$0.61 \pm 0.11$	$0.17 \pm 0.10$	2429	30.29 $\pm$0.05
3,4	${\rm Briceno2 }$	W	M5	04 15 06.9	+28 08 32	28	48	65	>-0.70	$0.14 \pm 0.09$	17826	29.49 $\pm$0.15
3,4	${\rm LkCa4 }$	W	K7	04 16 28.2	+28 07 44	7	33	626	$0.73 \pm 0.06$	$0.18 \pm 0.05$	21460	29.93 $\pm$0.03
3,4	${\rm CYTau }$	C	M1	04 17 33.8	+28 20 45	3	13	127	$0.87 \pm 0.16$	$0.07 \pm 0.12$	25972	29.09 $\pm$0.06
3,4	${\rm LkCa5 }$	W	M2	04 17 39.2	+28 32 57	5	12	584	$0.65 \pm 0.06$	$0.05 \pm 0.07$	30559	29.46 $\pm$0.03
3,4	${\rm Kim3-76 }$	W		04 17 49.7	+28 29 34	2	9	538	$0.99 \pm 0.06$	$0.31 \pm 0.07$	27114	29.42 $\pm$0.04
3,4	${\rm V410x-ray3 }$	C	M7	04 18 08.4	+28 26 00	7	4	74	>0.33	$0.02 \pm 0.16$	28184	28.69 $\pm$0.15
3,4	${\rm StromAnon13 }$	C	M5	04 18 18.1	+28 28 41	12	3	13	>-0.41	$0.81 \pm 0.39$	30759	27.86 $\pm$0.54
3,4	${\rm V410Tau +/c }$	WB	K3	04 18 31.3	+28 27 15	4	1	27166	$0.65 \pm 0.01$	$0.16 \pm 0.01$	28147	30.59 $\pm$0.01
3,4	${\rm V410x-ray2 }$		M0	04 18 34.6	+28 30 28	4	3	449	$0.99 \pm 0.09$	$0.73 \pm 0.07$	31813	29.22 $\pm$0.04
3,4	${\rm V410x-ray4 }$		M4	04 18 40.3	+28 24 27	1	3	82	>0.21	$0.79 \pm 0.15$	36351	28.45 $\pm$0.17
3,4	${\rm Hubble4 }$	W	K7	04 18 47.1	+28 20 08	1	8	7424	$0.96 \pm 0.01$	$0.30 \pm 0.02$	32312	30.21 $\pm$0.01
3,4	${\rm Kim3-89 }$	W	M5	04 19 01.5	+28 19 44	4	10	62	$0.92 \pm 0.26$	$0.23 \pm 0.17$	27928	28.78 $\pm$0.10
3,4	${\rm V410x-ray5a }$	C	M5	04 19 01.7	+28 22 33	4	8	141	>0.46	$0.35 \pm 0.12$	26268	28.89 $\pm$0.14
3,4	${\rm FQTau +/c }$	CB	M2	04 19 12.5	+28 29 35	3/2	9	45	>-0.04	$0.56 \pm 0.20$	27097	28.19 $\pm$0.18
3,4	${\rm V819Tau +/c }$	WB	K7	04 19 26.3	+28 26 14	1/10	12	7058	$0.97 \pm 0.01$	$0.24 \pm 0.02$	27198	30.01 $\pm$0.01
3,4	${\rm LkCa7 +/c }$	WB	K7	04 19 36.8	+27 50 12	63/62	39	1147	$0.60 \pm 0.04$	$0.18 \pm 0.04$	21144	29.90 $\pm$0.02
3,4	${\rm LkCa21 }$	W	M3	04 21 56.9	+28 25 08	86	45	1543	$0.99 \pm 0.02$	$0.64 \pm 0.02$	17254	30.46 $\pm$0.02
8,9	${\rm BD+23^\circ501B }$	W	K0	03 44 15.3	+24 01 50	45	36	31	$0.51 \pm 0.07$	$0.13 \pm 0.08$	8562	29.96 $\pm$0.04
8,9	${\rm Melotte22-345 }$	W	G7	03 44 25.2	+24 34 57	31	43	24	$0.53 \pm 0.07$	$0.09 \pm 0.07$	7179	30.14 $\pm$0.03
8,9	${\rm RXJ0345.6+2454 }$	W	G5	03 45 40.7	+24 53 54	36	48	738	$0.67 \pm 0.05$	$0.09 \pm 0.05$	7642	30.37 $\pm$0.02
8,9	${\rm RXJ0348.8+2359 }$	W	G7	03 48 49.3	+23 58 32	16	28	112	$0.67 \pm 0.12$	$-0.07 \pm 0.11$	9895	29.56 $\pm$0.06
8,9	${\rm Melotte22-2147 }$	W	G7	03 49 07.4	+23 47 14	28	37	3131	$0.50 \pm 0.02$	$0.19 \pm 0.03$	7816	30.75 $\pm$0.01
11-13	${\rm BD+23^\circ501B }$	W	K0	03 44 12.1	+24 01 03	57	35	460	$0.30 \pm 0.04$	$0.07 \pm 0.04$	28694	29.98 $\pm$0.02
11-13	${\rm RXJ0348.8+2359 }$	W	G7	03 48 49.4	+23 58 17	29	29	512	$0.57 \pm 0.05$	$0.16 \pm 0.05$	22939	29.82 $\pm$0.03
11-13	${\rm Melotte22-2147 }$	W	G7	03 49 06.1	+23 46 45	8	33	5098	$0.54 \pm 0.02$	$0.12 \pm 0.02$	30582	30.50 $\pm$0.01
30,31	${\rm FXTau +/c }$	WB	M1	04 30 30.8	+24 26 50	18/17	23	44	$0.58 \pm 0.22$	$-0.01 \pm 0.21$	3966	29.02 $\pm$0.12
30,31	${\rm V927Tau +/c }$	WB	M6	04 31 23.6	+24 10 56	2	21	62	$0.61 \pm 0.19$	$-0.19 \pm 0.20$	2640	29.21 $\pm$0.11
30,31	${\rm Haro6-13 }$	C	cont	04 32 15.7	+24 28 59	6	2	10	>0.23	$0.24 \pm 0.49$	7461	28.14 $\pm$0.47
30,31	${\rm V928Tau +/c }$	WB	M1	04 32 19.1	+24 22 28	4	7	466	>0.94	$0.19 \pm 0.10$	6900	29.24 $\pm$0.13
30,31	${\rm FZTau }$	C	M0	04 32 31.0	+24 20 03	8	10	418	>0.92	$0.53 \pm 0.09$	6861	29.52 $\pm$0.13
	${\rm FYTau }$	C	K7			9						$\pm$
30,31	${\rm V807Tau +/c }$	CB	K7	04 33 06.8	+24 09 53	4	22	299	$0.96 \pm 0.08$	$0.14 \pm 0.10$	5001	29.55 $\pm$0.05
	${\rm GHTau }$	CB	M2			20						$\pm$
30,31	${\rm V830Tau }$	W	K7	04 33 10.3	+24 33 49	5	14	1885	$0.81 \pm 0.03$	$0.17 \pm 0.05$	6694	30.28 $\pm$0.02
30,31	${\rm GKTau +/c }$	CT	K7/-/	04 33 34.7	+24 21 11	4/6/	20	735	$0.98 \pm 0.03$	$0.49 \pm 0.06$	5413	29.61 $\pm$0.03
	${\rm + GITau }$		K6			11						$\pm$
30,31	${\rm AATau }$	C	K7	04 34 55.6	+24 29 06	13	37	55	>-0.25	$0.50 \pm 0.15$	4846	29.34 $\pm$0.17
51,52	${\rm V836Tau }$	W	K7	05 03 06.2	+25 23 10	10	40	141	>-0.23	$0.31 \pm 0.09$	6253	29.65 $\pm$0.14
51,52	${\rm Briceno10 }$	W	M4	05 06 18.3	+24 45 48	33	31	19	>-0.51	$-0.18 \pm 0.23$	5706	28.96 $\pm$0.30
51,52	${\rm RXJ057.2 }$	W	K6	05 07 11.4	+24 37 05	14	44	142	>-0.28	$0.08 \pm 0.10$	5750	29.83 $\pm$0.14
60,61	${\rm GMAur }$	C	K3	04 55 11.4	+30 21 58	7	13	504	>0.92	$0.06 \pm 0.09$	4706	29.84 $\pm$0.13
60,61	${\rm SUAur }$	C	G2	04 55 59.5	+30 34 02	2	3	3405	$0.98 \pm 0.01$	$0.34 \pm 0.04$	5222	30.53 $\pm$0.02
60,61	${\rm NTTS045251+3016 }$	WSB	K7	04 56 02.0	+30 21 05	2	12	1031	$0.73 \pm 0.05$	$0.04 \pm 0.07$	4994	29.89 $\pm$0.03
67-69	${\rm IRAS04187+1927 }$	C	M0	04 21 43.4	+19 34 12	6	4	40	>0.72	$0.85 \pm 0.16$	4261	28.86 $\pm$0.21
67-69	${\rm TTau N + S }$	CB	K0	04 21 59.3	+19 32 07	0	1	1986	$0.96 \pm 0.02$	$0.40 \pm 0.05$	4283	30.10 $\pm$0.02
67-69	${\rm RXJ0422.1+1934 +B}$	CB	M5	04 22 05.0	+19 34 51	1	3	841	$0.92 \pm 0.04$	$0.23 \pm 0.08$	4886	29.73 $\pm$0.04
75,76	${\rm J2-157 }$	C	M6	04 20 54.3	+17 46 06	42	40	13	$0.16 \pm 0.25$	$0.26 \pm 0.25$	12648	29.14 $\pm$0.13
58,63	${\rm V410Tau +/c }$	WB	K3	04 18 31.4	+28 27 04	13	43	935	$0.66 \pm 0.04$	$0.27 \pm 0.05$	5026	30.24 $\pm$0.02
58,63	${\rm Hubble4 }$	W	K7	04 18 45.6	+28 20 07	18	39	709	$0.91 \pm 0.05$	$0.42 \pm 0.05$	5441	30.35 $\pm$0.03
58,63	${\rm V819Tau +/c }$	WB	K7	04 19 26.6	+28 26 14	5/11	31	492	$0.84 \pm 0.06$	$0.28 \pm 0.06$	5545	29.87 $\pm$0.03
58,63	${\rm LkCa7 +/c }$	WB	K7	04 19 40.5	+27 50 00	14/13	39	394	$0.66 \pm 0.07$	$0.04 \pm 0.07$	5099	29.94 $\pm$0.04
58,63	${\rm HD283572 }$	W	G5	04 21 58.7	+28 18 06	2	5	17128	$0.86 \pm 0.01$	$0.16 \pm 0.02$	7746	31.07 $\pm$0.01
58,63	${\rm LkCa21 }$	W	M3	04 22 03.2	+28 25 38	2	10	595	$0.91 \pm 0.05$	$0.23 \pm 0.07$	7403	29.89 $\pm$0.04
85-89	${\rm LkCa5 }$	W	M2	04 17 40.3	+28 32 35	32	39	259	$0.94 \pm 0.11$	$0.30 \pm 0.07$	17880	29.59 $\pm$0.05
85-89	${\rm V410Tau +/c }$	WB	K3	04 18 32.2	+28 27 20	15	40	3496	$0.69 \pm 0.02$	$0.22 \pm 0.02$	19880	30.23 $\pm$0.01
85-89	${\rm V410x-ray4 }$		M4	04 18 37.7	+28 24 46	39	42	5210	$0.81 \pm 0.02$	$0.35 \pm 0.03$	19109	30.33 $\pm$0.02
85-89	${\rm BPTau }$	C	K7	04 19 16.1	+29 06 29	4	2	4100	$0.91 \pm 0.02$	$0.14 \pm 0.03$	29310	29.98 $\pm$0.01
85-89	${\rm V819Tau +/c }$	WB	K7	04 19 25.4	+28 26 16	10/15	40	1346	$0.87 \pm 0.04$	$0.26 \pm 0.04$	16836	29.79 $\pm$0.02
64,115	${\rm UXTau A + B + C }$	WT	K2/M1/M6	04 30 03.9	+18 13 52	1/6/4	28	1820	$0.92 \pm 0.03$	$0.21 \pm 0.04$	8244	29.92 $\pm$0.02
64,115	${\rm RXJ0431.4+1800 +B}$	CB	M5	04 31 24.2	+18 00 24	3	6	82	>0.66	$0.09 \pm 0.17$	11520	28.62 $\pm$0.15
64,115	${\rm XZTau N + S }$	CB	-/M3	04 31 39.9	+18 13 57	0/1	16	532	$0.95 \pm 0.05$	$0.06 \pm 0.08$	11097	29.43 $\pm$0.04
	${\rm HLTau }$	C	K7			21						29.73 $\pm$0.04
64,115	${\rm L1551-51 }$	W	K7	04 32 09.3	+17 57 25	2	8	2476	$0.90 \pm 0.02$	$0.10 \pm 0.04$	11351	30.18 $\pm$0.02
64,115	${\rm V827Tau }$	W	K7	04 32 14.5	+18 20 18	2	23	1897	$0.92 \pm 0.02$	$0.21 \pm 0.04$	8420	30.34 $\pm$0.02
64,115	${\rm MHO-5 }$	C	M6	04 32 15.1	+18 12 48	13	16	14	>-0.30	$-0.08 \pm 0.34$	9895	28.48 $\pm$0.28
64,115	${\rm V826Tau }$	WSB	K7	04 32 15.8	+18 01 41	1	8	7153	$0.89 \pm 0.01$	$0.14 \pm 0.03$	11141	30.29 $\pm$0.01
64,115	${\rm GGTau +/c1 }$	CQ	K7/M5/	04 32 30.1	+17 31 57	15/25/	29	80	>-0.21	$0.16 \pm 0.14$	8918	28.64 $\pm$0.15
	${\rm +/c2 +/c3 }$		M1 /M7			28/10						$\pm$
64,115	${\rm RXJ0432.7+1809 }$	W	M5	04 32 40.6	+18 09 23	5	17	25	$0.96 \pm 0.49$	>0.66	7114	28.89 $\pm$0.20
64,115	${\rm L1551-55 }$	W	K7	04 32 43.5	+18 02 59	4	15	740	$0.95 \pm 0.04$	$0.18 \pm 0.07$	9089	29.89 $\pm$0.03
64,115	${\rm RXJ0432.9+1735 }$	W	M2	04 32 53.7	+17 35 35	6	29	131	$0.87 \pm 0.14$	$0.20 \pm 0.11$	9113	29.59 $\pm$0.06
64,115	${\rm NTTS043124+1824 }$	W	G8	04 34 13.8	+18 29 45	65	47	23	>-0.80	$0.29 \pm 0.20$	6623	28.70 $\pm$0.00

   

Table 3: X-ray data for Pleiads detected in PSPC observations.

Obs. No.	Designation	Mult.	SpT.	X-ray position		$\Delta$	Offax	ML	HR1	HR2	Expos	$\log{L_{\rm X}}$
				$\alpha_{2000}$	$\delta_{2000}$	[ $^{\prime\prime}$]	[$^\prime$]				[s]	[erg/s]
5	${\rm sk630 }$			03 43 32.6	+23 38 33	60	41	10	>-0.33	$-0.46 \pm 0.32$	457	29.45 $\pm$0.58
5	${\rm hii980 }$		B9	03 46 26.4	+23 57 16	97	48	12	$0.39 \pm 0.36$	<-0.70	385	29.97 $\pm$0.21
7	${\rm hii1103 }$		M2	03 46 41.1	+23 25 11	86	45	48	>-0.34	$0.55 \pm 0.30$	393	29.42 $\pm$0.56
8	${\rm hii193 }$		G9	03 43 55.0	+24 15 24	45	42	39	>-0.47	$-0.06 \pm 0.17$	3615	29.61 $\pm$0.15
	${\rm hii263 }$	SB	K1			40	40	63				29.31 $\pm$0.15
8	${\rm hii357 +B }$	VB	K6	03 44 24.9	+24 09 02	7	33	21	$0.68 \pm 0.09$	$0.24 \pm 0.09$	3780	29.62 $\pm$0.05
	${\rm hii338 }$		F6			21	34	195				29.92 $\pm$0.05
8	${\rm hii625 }$		K5	03 45 21.0	+23 44 07	26	31	19	>-0.10	$0.23 \pm 0.22$	3844	28.90 $\pm$0.27
8	${\rm hii673 }$			03 45 30.7	+24 18 58	13	22	18	$0.60 \pm 0.17$	$0.27 \pm 0.17$	3780	29.39 $\pm$0.09
8	${\rm hii817 }$		B9	03 45 54.3	+24 33 26	7	30	27	>-0.16	$0.26 \pm 0.20$	3990	29.16 $\pm$0.18
8	${\rm hii916 }$	SB	K1	03 46 11.9	+24 36 55	27	31	13	$0.29 \pm 0.27$	$-0.20 \pm 0.28$	4657	28.81 $\pm$0.14
8	${\rm hii1094 }$		M0	03 46 36.8	+23 58 04	13	10	25	$0.62 \pm 0.31$	$-0.20 \pm 0.27$	5194	28.87 $\pm$0.15
8	${\rm hcg246 }$			03 46 58.6	+24 27 42	2	21	100	$0.63 \pm 0.13$	$0.15 \pm 0.15$	4849	29.40 $\pm$0.07
8	${\rm hii1384 }$		A7	03 47 24.5	+24 35 25	9	29	507	$0.39 \pm 0.06$	$0.06 \pm 0.07$	4553	30.07 $\pm$0.03
8	${\rm hii2147 }$	SB2	G9	03 49 06.7	+23 46 59	11	36	339	$0.49 \pm 0.06$	$0.23 \pm 0.07$	3046	29.91 $\pm$0.03
8	${\rm hcg355 }$			03 49 08.9	+24 21 20	39	34	9	$0.77 \pm 0.54$	$0.02 \pm 0.35$	4422	28.98 $\pm$0.28
8	${\rm hii2193 +B }$	VB	K9	03 49 09.1	+23 33 43	36	45	10	$0.95 \pm 0.56$	$-0.09 \pm 0.28$	3594	28.98 $\pm$0.24
8	${\rm hii2407 }$	SB1	K3	03 49 40.3	+24 28 28	46	44	8	$0.55 \pm 0.45$	$-0.88 \pm 0.39$	3866	28.77 $\pm$0.29
8	${\rm hii2462 }$		K1	03 49 52.1	+23 42 33	28	48	10	$0.36 \pm 0.30$	$-0.26 \pm 0.26$	3232	29.30 $\pm$0.18
	${\rm sk293 }$					84						$\pm$
8	${\rm hii2602 }$		M5	03 50 18.5	+23 59 36	87	47	32	$0.00 \pm 0.23$	$0.35 \pm 0.30$	3664	29.33 $\pm$0.14
9	${\rm hii263 }$	SB	K1	03 44 01.3	+24 16 22	47	40	129	$0.85 \pm 0.11$	$-0.02 \pm 0.11$	4789	29.46 $\pm$0.06
9	${\rm hii338 }$		F6	03 44 22.1	+24 08 02	18	34	95	>0.41	$-0.12 \pm 0.09$	3967	29.80 $\pm$0.13
9	${\rm hcg149 }$		M4	03 44 22.9	+24 47 02	59	50	303	$0.60 \pm 0.06$	$0.02 \pm 0.06$	3849	30.34 $\pm$0.03
9	${\rm hii625 }$		K5	03 45 21.0	+23 43 52	11	33	122	$0.95 \pm 0.11$	$0.28 \pm 0.11$	4271	29.64 $\pm$0.07
9	${\rm hii659 }$		K3	03 45 27.8	+23 26 21	41	47	47	$0.77 \pm 0.30$	$0.33 \pm 0.20$	4303	29.34 $\pm$0.17
9	${\rm hii799 }$		K7	03 45 49.7	+23 51 58	30	23	12	>-0.19	$-0.22 \pm 0.31$	4535	28.71 $\pm$0.29
9	${\rm hii996 }$		G2	03 46 21.9	+24 34 11	9	25	30	$0.42 \pm 0.18$	$0.06 \pm 0.20$	5635	29.19 $\pm$0.10
9F	${\rm hii1384 }$		A7	03 47 24.2	+24 35 16	6	0	1118	$0.52 \pm 0.05$	$0.08 \pm 0.07$	5439	30.05 $\pm$0.08
9F	${\rm hii2147a }$	SB2	G9	03 49 07.5	+23 47 20	33	0	2829	$0.47 \pm 0.05$	$0.11 \pm 0.06$	4555	30.05 $\pm$0.06
9	${\rm hcg355 }$			03 49 08.6	+24 21 34	53	32	14	$0.45 \pm 0.30$	$-0.06 \pm 0.26$	4919	29.12 $\pm$0.16
9	${\rm hii2193 +B }$	VB	K9	03 49 13.9	+23 33 07	40	48	48	>-0.86	$0.61 \pm 0.51$	4082	28.54 $\pm$0.72
9	${\rm hii2548 }$		K7	03 50 06.6	+24 07 22	23	43	13	$-0.31 \pm 0.20$	$-0.53 \pm 0.35$	4013	29.18 $\pm$0.14
9	${\rm hii2601 +B }$	VB	M4	03 50 10.8	+24 20 48	34	46	10	$-0.41 \pm 0.16$	$-0.62 \pm 0.34$	3924	28.99 $\pm$0.11
11	${\rm hii298 +B }$	VB	K1	03 44 11.1	+24 02 19	32	37	10	$0.16 \pm 0.26$	$-0.40 \pm 0.36$	897	29.31 $\pm$0.17
11	${\rm hii303 +B }$	VB	K1	03 44 18.3	+24 06 00	52	37	58	>0.75	$0.36 \pm 0.16$	894	29.54 $\pm$0.17
11	${\rm hii817 }$		B9	03 45 52.7	+24 32 48	37	45	32	>-0.42	$0.78 \pm 0.63$	686	29.56 $\pm$0.26
11	${\rm hii1827 }$		M3	03 48 24.8	+23 58 31	30	26	18	$0.65 \pm 0.36$	$0.79 \pm 0.30$	614	29.53 $\pm$0.22
12	${\rm hii164 }$	SB1	F7	03 43 46.1	+23 34 49	71	43	111	$0.76 \pm 0.14$	$0.08 \pm 0.11$	7656	29.27 $\pm$0.07
12	${\rm hii298 +B }$	VB	K1	03 44 13.0	+24 01 40	15	34	29	$0.41 \pm 0.08$	$0.00 \pm 0.09$	8888	29.37 $\pm$0.04
12	${\rm hii303 +B }$	VB	K1	03 44 17.4	+24 05 27	57	35	426	$0.85 \pm 0.05$	$0.17 \pm 0.06$	8742	29.64 $\pm$0.03
12	${\rm hii762 }$		M0	03 45 44.4	+24 04 32	7	17	17	$0.73 \pm 0.35$	$0.06 \pm 0.28$	9664	28.65 $\pm$0.18
12	${\rm hcg219 }$		K4	03 46 26.7	+24 09 31	20	17	20	$0.54 \pm 0.26$	$-0.41 \pm 0.24$	10780	28.73 $\pm$0.14
12	${\rm hii1061 +B }$	VB	K9	03 46 31.8	+24 07 00	10	14	190	$0.72 \pm 0.10$	$0.08 \pm 0.11$	11800	28.93 $\pm$0.05
12	${\rm hii1094 }$		M0	03 46 36.4	+23 58 02	8	6	176	$0.71 \pm 0.11$	$0.22 \pm 0.13$	12671	29.12 $\pm$0.06
12	${\rm hii1100 +B }$	VB	K5	03 46 37.2	+24 20 34	3	27	124	$0.72 \pm 0.11$	$0.14 \pm 0.11$	8076	29.19 $\pm$0.06
12	${\rm hii1332 }$		K4	03 47 13.5	+23 43 08	15	12	18	$0.45 \pm 0.12$	$0.15 \pm 0.13$	11525	29.14 $\pm$0.06
12	${\rm hii1338 }$	SB2	F6	03 47 17.2	+24 07 38	11	17	41	$0.41 \pm 0.20$	$-0.43 \pm 0.18$	9570	28.60 $\pm$0.10
12	${\rm hcg273 }$			03 47 32.6	+24 22 26	31	32	11	$0.42 \pm 0.16$	$0.04 \pm 0.16$	8997	29.23 $\pm$0.08
12	${\rm hcg307 }$			03 48 07.8	+23 44 11	12	22	15	$0.61 \pm 0.39$	$0.39 \pm 0.29$	8641	28.76 $\pm$0.18
12	${\rm hii1827 }$		M3	03 48 21.2	+23 58 37	24	23	39	>-0.02	$0.10 \pm 0.22$	6068	28.92 $\pm$0.19
12	${\rm hcg324 }$		M5	03 48 32.3	+24 17 13	26	35	11	>-0.61	$-0.11 \pm 0.23$	9037	28.81 $\pm$0.24
12	${\rm hii2345 }$		F5	03 49 30.6	+23 23 32	49	49	16	$0.48 \pm 0.42$	$-0.45 \pm 0.33$	6425	29.15 $\pm$0.22
13	${\rm hii164 }$	SB1	F7	03 43 44.2	+23 35 21	29	45	104	$0.97 \pm 0.10$	$0.21 \pm 0.07$	17489	29.37 $\pm$0.04
13F	${\rm hii298 +B }$	VB	K1	03 44 12.7	+24 01 17	37	0	552	$0.31 \pm 0.05$	$0.14 \pm 0.06$	19693	29.62 $\pm$0.27
13F	${\rm hcg144 }$			03 44 16.8	+23 36 49	17	0	555	$0.70 \pm 0.16$	$0.19 \pm 0.13$	20293	29.54 $\pm$0.96
13F	${\rm hii303 +B }$	VB	K1	03 44 16.9	+24 05 21	57	0	2068	$0.94 \pm 0.03$	$0.29 \pm 0.04$	19678	29.96 $\pm$0.17
13	${\rm hcg194 }$			03 45 38.9	+24 37 34	97	46	108	$0.61 \pm 0.06$	$0.13 \pm 0.07$	16011	29.80 $\pm$0.03
13	${\rm hii762 }$		M0	03 45 43.9	+24 04 11	17	17	92	$0.96 \pm 0.12$	$0.05 \pm 0.11$	23294	29.00 $\pm$0.06
13	${\rm hcg219 }$		K4	03 46 25.5	+24 09 24	14	16	50	>1.00	$-0.19 \pm 0.14$	23511	28.82 $\pm$0.08
13	${\rm hii1061 +B }$	VB	K9	03 46 31.7	+24 06 55	11	13	163	$0.55 \pm 0.09$	$0.18 \pm 0.10$	25091	28.75 $\pm$0.05
13	${\rm hii1094 }$		M0	03 46 36.4	+23 57 54	11	5	181	$0.87 \pm 0.09$	$-0.07 \pm 0.11$	25292	28.99 $\pm$0.05
13F	${\rm hii1100 +B }$	VB	K5	03 46 37.6	+24 20 33	7	0	443	$0.68 \pm 0.07$	$0.10 \pm 0.08$	20380	29.26 $\pm$0.28
13	${\rm sk465 }$			03 46 38.9	+23 04 48	50	48	11	$0.35 \pm 0.23$	$0.41 \pm 0.24$	15611	29.14 $\pm$0.12
13	${\rm hcg247 }$			03 46 57.9	+23 14 24	42	39	41	$0.30 \pm 0.13$	$0.13 \pm 0.14$	17991	29.22 $\pm$0.07
13	${\rm hii1234 }$		A1	03 46 58.2	+24 30 43	34	37	13	$0.64 \pm 0.24$	$0.29 \pm 0.20$	18365	29.03 $\pm$0.12
13	${\rm hii1332 }$		K4	03 47 13.3	+23 43 14	21	11	78	$-0.33 \pm 0.14$	$0.76 \pm 0.21$	25997	28.54 $\pm$0.09
13	${\rm hii1338 }$	SB2	F6	03 47 16.3	+24 07 36	7	15	97	$0.41 \pm 0.11$	$-0.13 \pm 0.12$	24492	28.64 $\pm$0.06
13	${\rm hii1514 }$		G4	03 47 39.3	+24 22 02	15	31	14	$0.44 \pm 0.09$	$-0.07 \pm 0.10$	19344	29.36 $\pm$0.05
13F	${\rm hcg307 }$			03 48 08.8	+23 44 15	15	0	223	$0.65 \pm 0.25$	$0.08 \pm 0.21$	11533	28.88 $\pm$0.00
13	${\rm hii1762 }$		F2	03 48 14.4	+24 19 21	18	32	263	$0.69 \pm 0.06$	$0.07 \pm 0.07$	19757	29.58 $\pm$0.03
13	${\rm hii1883 }$		K4	03 48 30.3	+23 18 06	33	42	79	$0.61 \pm 0.10$	$0.17 \pm 0.09$	17357	29.56 $\pm$0.05
26	${\rm hii1032 }$		G8	03 46 29.3	+24 26 22	22	49	547	$0.95 \pm 0.06$	$0.31 \pm 0.05$	13207	30.02 $\pm$0.03
26	${\rm hii1355 +B }$	VB	M0	03 47 15.5	+24 02 08	34	43	50	$0.76 \pm 0.12$	$0.25 \pm 0.11$	14687	29.18 $\pm$0.06
26	${\rm hii1384 }$		A7	03 47 24.3	+24 35 12	9	39	1564	$0.57 \pm 0.03$	$0.12 \pm 0.03$	15268	30.21 $\pm$0.01
26	${\rm hcg261 }$			03 47 30.0	+24 50 47	97	46	11	$0.73 \pm 0.13$	$0.13 \pm 0.08$	13181	29.13 $\pm$0.12
26F	${\rm hii1516 }$		K7	03 47 40.6	+24 18 19	11	0	792	$0.64 \pm 0.06$	$0.19 \pm 0.06$	17021	29.72 $\pm$0.49
26	${\rm hii1653 }$		K6	03 47 58.9	+24 43 33	23	36	111	$0.63 \pm 0.09$	$0.11 \pm 0.08$	15586	29.40 $\pm$0.05
26	${\rm hii1726 +B }$	VB	F9	03 48 07.0	+24 08 08	25	30	119	$0.84 \pm 0.11$	$-0.29 \pm 0.10$	17223	29.00 $\pm$0.05
26	${\rm hii1762 }$		F2	03 48 12.4	+24 18 47	25	26	405	$0.69 \pm 0.06$	$0.05 \pm 0.07$	16644	29.58 $\pm$0.03
26	${\rm hii1785 }$		M5	03 48 16.4	+24 29 53	26	26	23	$0.43 \pm 0.23$	$-0.13 \pm 0.21$	18684	28.73 $\pm$0.12
26	${\rm hii1794 }$		G2	03 48 18.1	+23 53 22	16	37	67	$0.77 \pm 0.12$	$0.20 \pm 0.10$	15769	29.39 $\pm$0.06
26	${\rm hii1856 }$		F9	03 48 27.1	+24 02 45	17	29	44	$0.39 \pm 0.15$	$-0.46 \pm 0.15$	17939	29.05 $\pm$0.07
26	${\rm hii1912 +B }$	VB	F7	03 48 35.1	+24 10 53	6	23	277	$0.66 \pm 0.07$	$0.05 \pm 0.08$	17218	29.12 $\pm$0.04
26	${\rm hii2027 }$	SB1	K1	03 48 48.6	+24 15 58	7	18	279	$0.58 \pm 0.08$	$0.05 \pm 0.09$	16812	29.03 $\pm$0.04
26	${\rm hii2034 }$		K3	03 48 49.1	+23 58 35	5	29	167	$0.65 \pm 0.09$	$-0.09 \pm 0.09$	14869	29.47 $\pm$0.04
26	${\rm hcg349 }$			03 48 57.3	+24 19 32	13	16	150	$0.49 \pm 0.11$	$-0.10 \pm 0.12$	20606	29.02 $\pm$0.05
26	${\rm hcg351 }$			03 49 03.3	+24 53 49	40	35	9	>-0.77	$-0.40 \pm 0.32$	15597	28.23 $\pm$0.86
26	${\rm hii2147 }$	SB2	G9	03 49 06.6	+23 46 46	11	37	2922	$0.51 \pm 0.02$	$0.20 \pm 0.03$	16019	30.08 $\pm$0.01
26	${\rm hii2172 }$	SB1	G2	03 49 11.1	+24 38 14	7	21	134	$0.59 \pm 0.11$	$-0.04 \pm 0.11$	15806	28.85 $\pm$0.06
26	${\rm hcg355 }$			03 49 11.2	+24 20 45	7	12	58	$0.66 \pm 0.21$	$0.23 \pm 0.17$	20470	28.68 $\pm$0.09
26	${\rm hii2181 }$		B9	03 49 11.4	+24 08 08	7	18	613	$0.42 \pm 0.05$	$0.01 \pm 0.06$	19361	29.54 $\pm$0.03
26	${\rm hii2208 }$		K8	03 49 15.3	+24 33 56	7	17	250	$0.51 \pm 0.08$	$0.03 \pm 0.09$	16667	29.24 $\pm$0.04
26F	${\rm hii2244 }$		K3	03 49 20.2	+24 46 25	12	0	1091	$0.00 \pm 0.00$	$0.13 \pm 0.06$	15924	29.59 $\pm$0.26
26	${\rm hii2289 }$		A6	03 49 26.4	+24 14 48	9	11	16	$0.51 \pm 0.31$	$-0.27 \pm 0.26$	21013	28.35 $\pm$0.16
26	${\rm hcg370 }$			03 49 27.4	+24 31 45	10	13	95	$0.64 \pm 0.15$	$0.01 \pm 0.14$	19701	28.84 $\pm$0.07
26	${\rm hii2278 +B }$	VB	K1	03 49 29.5	+24 55 45	62	35	175	$0.57 \pm 0.09$	$0.05 \pm 0.09$	11515	29.20 $\pm$0.05
26	${\rm hcg372 }$		M3	03 49 31.1	+24 31 53	27	13	112	$0.34 \pm 0.14$	$-0.03 \pm 0.15$	19679	28.83 $\pm$0.07
26	${\rm hii2366 }$		K0	03 49 36.6	+24 17 55	7	8	361	$0.30 \pm 0.08$	$0.03 \pm 0.09$	21306	29.16 $\pm$0.04
	${\rm hcg375 }$					16						$\pm$
26	${\rm hii2407 }$	SB1	K3	03 49 42.2	+24 27 37	10	8	292	$0.59 \pm 0.09$	$0.07 \pm 0.10$	21480	28.79 $\pm$0.04
26	${\rm hcg380 }$		M2	03 49 55.7	+24 44 52	19	23	28	$0.20 \pm 0.29$	$-0.22 \pm 0.30$	15733	28.53 $\pm$0.17
26	${\rm hii2500 }$	SB		03 49 57.5	+23 50 44	6	30	2702	$0.51 \pm 0.02$	$0.06 \pm 0.03$	17130	29.93 $\pm$0.01
26	${\rm hii2548 }$		K7	03 50 05.3	+24 07 17	8	14	60	$0.54 \pm 0.16$	$0.09 \pm 0.16$	20920	28.77 $\pm$0.08
26	${\rm hii2588 }$		K5	03 50 12.1	+24 31 51	9	10	265	$0.57 \pm 0.09$	$0.21 \pm 0.10$	21098	29.07 $\pm$0.05
26	${\rm hii2602 }$		M5	03 50 12.4	+23 59 33	13	22	174	$0.57 \pm 0.09$	$-0.06 \pm 0.10$	13043	29.36 $\pm$0.05
26	${\rm hii2601 +B }$	VB	M4	03 50 12.8	+24 20 59	9	2	450	$0.53 \pm 0.07$	$-0.03 \pm 0.08$	23140	28.89 $\pm$0.04
26	${\rm hcg394 }$		M9	03 50 15.5	+24 13 26	12	8	50	$0.37 \pm 0.19$	$0.09 \pm 0.19$	22302	28.59 $\pm$0.09
26	${\rm hii2644 }$		G9	03 50 20.6	+24 27 50	12	7	130	$0.43 \pm 0.13$	$0.14 \pm 0.14$	21957	28.83 $\pm$0.06
26	${\rm hii2741 }$		K4	03 50 34.1	+24 30 19	11	11	557	$0.79 \pm 0.06$	$0.07 \pm 0.08$	20242	29.32 $\pm$0.04
26	${\rm hii2866 }$		A3	03 50 50.7	+23 57 39	24	25	149	$0.69 \pm 0.10$	$-0.11 \pm 0.10$	17670	29.23 $\pm$0.05
26	${\rm hii2881 +B }$	VB	K3	03 50 54.4	+23 50 07	3	33	501	$0.57 \pm 0.05$	$-0.03 \pm 0.06$	15339	29.48 $\pm$0.03
26	${\rm hii2880 }$		K1	03 50 54.7	+24 11 41	11	14	69	$0.35 \pm 0.15$	$-0.22 \pm 0.16$	20262	28.76 $\pm$0.08
26	${\rm hcg415 }$			03 50 57.0	+24 06 30	5	18	31	$0.49 \pm 0.23$	$-0.20 \pm 0.21$	16583	28.66 $\pm$0.11
26	${\rm hii2927 }$		K6	03 51 05.9	+24 44 04	11	26	107	$0.44 \pm 0.11$	$-0.16 \pm 0.11$	14275	29.23 $\pm$0.06
26F	${\rm hcg422 }$			03 51 11.2	+24 23 05	9	0	267	$0.52 \pm 0.07$	$0.11 \pm 0.08$	19673	28.73 $\pm$0.00
26	${\rm hcg424 }$			03 51 18.8	+24 10 05	9	20	91	$0.52 \pm 0.14$	$-0.02 \pm 0.14$	12620	29.10 $\pm$0.07
26	${\rm hii3019 }$		K6	03 51 24.6	+24 05 03	14	24	97	$0.34 \pm 0.12$	$-0.10 \pm 0.13$	15254	29.15 $\pm$0.06
26	${\rm hcg428 }$			03 51 26.4	+24 47 32	11	31	99	$0.45 \pm 0.11$	$-0.02 \pm 0.11$	13568	29.30 $\pm$0.06
26	${\rm hii3063 }$		K5	03 51 28.8	+23 53 35	27	33	279	$0.59 \pm 0.07$	$0.09 \pm 0.07$	16064	29.60 $\pm$0.03
26	${\rm hii3097 }$	SB1	G8	03 51 37.9	+24 59 33	46	43	62	$0.48 \pm 0.14$	$0.01 \pm 0.12$	11327	29.13 $\pm$0.07
26	${\rm hii3096 }$		K2	03 51 39.3	+24 32 58	1	24	508	$0.62 \pm 0.06$	$-0.01 \pm 0.06$	18235	29.56 $\pm$0.03
26	${\rm hii3163 }$		K4	03 51 53.2	+24 23 04	10	24	602	$0.64 \pm 0.05$	$-0.03 \pm 0.06$	15439	29.65 $\pm$0.03
26	${\rm hcg441 }$			03 51 54.1	+24 03 07	14	30	70	$0.63 \pm 0.15$	$0.08 \pm 0.12$	16166	29.18 $\pm$0.07
	${\rm B201 }$		M6			40						$\pm$0
26	${\rm hii3197 + B + C }$	T	K4	03 52 01.4	+24 39 48	9	32	1452	$0.57 \pm 0.03$	$0.04 \pm 0.04$	16137	29.55 $\pm$0.02
27F	${\rm sk702 }$			03 42 00.5	+25 01 40	11	0	94	$0.87 \pm 0.35$	$0.11 \pm 0.21$	19055	29.32 $\pm$1.05
27	${\rm hcg58 }$		M1	03 42 00.5	+25 18 23	85	45	153	$0.78 \pm 0.14$	$-0.04 \pm 0.10$	16858	29.36 $\pm$0.07
27	${\rm hcg65 }$		K8	03 42 03.6	+24 42 44	2	31	237	$0.68 \pm 0.08$	$0.12 \pm 0.08$	19775	29.42 $\pm$0.04
27	${\rm sk671 }$		M1	03 42 42.7	+24 11 43	21	42	56	$0.83 \pm 0.23$	$0.03 \pm 0.15$	14662	29.14 $\pm$0.11
27F	${\rm hcg97 }$			03 43 05.6	+24 49 21	8	0	617	$0.75 \pm 0.07$	$0.23 \pm 0.08$	20945	28.77 $\pm$0.00
27	${\rm hcg100 }$		M5	03 43 09.0	+24 41 29	10	17	15	$0.42 \pm 0.13$	$-0.14 \pm 0.14$	24149	28.83 $\pm$0.07
27	${\rm AK1B121 }$		K0	03 43 26.7	+25 23 02	15	38	1164	$0.74 \pm 0.04$	$0.09 \pm 0.04$	15442	30.00 $\pm$0.02
27	${\rm hii97 +B }$	VB	K4	03 43 26.8	+24 59 33	8	17	428	$0.58 \pm 0.07$	$0.05 \pm 0.08$	19886	29.02 $\pm$0.04
27	${\rm hcg109 }$			03 43 28.4	+24 53 21	11	13	71	$0.51 \pm 0.17$	$0.05 \pm 0.16$	24894	28.67 $\pm$0.08
27	${\rm hii134 +B }$	VB	M1	03 43 34.6	+24 14 21	35	34	135	$0.88 \pm 0.12$	$0.20 \pm 0.09$	20110	28.98 $\pm$0.06
27	${\rm hii153 }$		A5	03 43 41.7	+25 04 50	19	20	446	$0.81 \pm 0.06$	$0.33 \pm 0.07$	18916	29.37 $\pm$0.04
27	${\rm hcg123 }$		M4	03 43 42.3	+24 34 21	5	15	276	$0.37 \pm 0.08$	$0.03 \pm 0.09$	25263	29.13 $\pm$0.04
27	${\rm hii173 }$	SB2	K1	03 43 47.6	+25 11 20	11	25	81	$0.75 \pm 0.16$	$-0.12 \pm 0.13$	15627	28.76 $\pm$0.07
27F	${\rm hii174 }$		K1	03 43 48.1	+25 00 09	8	0	6083	$0.74 \pm 0.02$	$0.14 \pm 0.03$	25495	29.87 $\pm$0.20
27	${\rm sk609 }$			03 43 48.5	+25 02 40	33	17	63	$0.92 \pm 0.19$	$-0.03 \pm 0.16$	20143	28.74 $\pm$0.09
27F	${\rm hii191 }$		K8	03 43 51.8	+24 50 22	9	0	759	$0.84 \pm 0.07$	$0.04 \pm 0.10$	28138	28.91 $\pm$0.00
27	${\rm hii193 }$		G9	03 43 54.2	+24 14 32	53	33	28	$0.47 \pm 0.08$	$-0.09 \pm 0.08$	20594	29.41 $\pm$0.04
27F	${\rm hii212 }$		K9	03 43 55.5	+24 25 20	16	0	259	$0.28 \pm 0.11$	$-0.02 \pm 0.13$	17776	28.90 $\pm$0.00
27	${\rm hii232 }$	SB?	A7	03 44 02.0	+24 33 25	24	14	33	$0.85 \pm 0.58$	$0.31 \pm 0.34$	25174	27.77 $\pm$0.31
27	${\rm hii263 }$	SB	K1	03 44 02.3	+24 16 05	43	31	762	$0.87 \pm 0.05$	$0.10 \pm 0.05$	20875	29.37 $\pm$0.03
27	${\rm hcg134 }$		M3	03 44 02.3	+25 03 54	1	17	195	$0.58 \pm 0.09$	$0.11 \pm 0.10$	20073	29.10 $\pm$0.05
27F	${\rm hii253 }$		G5	03 44 03.4	+24 30 11	6	0	10288	$0.80 \pm 0.01$	$0.16 \pm 0.02$	25915	30.34 $\pm$0.12
27	${\rm hii250 }$	SB?	G4	03 44 04.2	+24 59 17	8	13	505	$0.30 \pm 0.07$	$-0.15 \pm 0.08$	24161	28.93 $\pm$0.03
27	${\rm sk586 }$			03 44 09.5	+24 35 20	3	12	205	$0.63 \pm 0.10$	$0.01 \pm 0.11$	26410	28.92 $\pm$0.05
27	${\rm hii298 +B }$	VB	K1	03 44 12.1	+24 02 15	21	44	54	$0.59 \pm 0.04$	$0.14 \pm 0.04$	17258	29.72 $\pm$0.02
27	${\rm hii293 }$		G6	03 44 13.9	+24 46 39	8	2	379	$0.69 \pm 0.08$	$-0.19 \pm 0.09$	27319	29.05 $\pm$0.04
27	${\rm hii303 +B }$	VB	K1	03 44 17.4	+24 05 48	44	41	2449	$0.90 \pm 0.02$	$0.15 \pm 0.03$	18262	29.89 $\pm$0.01
27	${\rm hcg145 }$			03 44 18.5	+24 26 44	12	20	59	$0.75 \pm 0.18$	$0.09 \pm 0.16$	17056	28.82 $\pm$0.09
27	${\rm hcg146 }$		M4	03 44 18.9	+24 35 13	6	12	136	$0.83 \pm 0.12$	$0.30 \pm 0.12$	26152	28.77 $\pm$0.07
27	${\rm hii314 }$	SB1	G3	03 44 20.0	+24 47 38	9	2	9163	$0.46 \pm 0.02$	$0.08 \pm 0.02$	26570	29.85 $\pm$0.01
27	${\rm hii324 }$		K4	03 44 21.0	+24 46 09	10	2	6750	$0.65 \pm 0.02$	$0.05 \pm 0.03$	28738	30.06 $\pm$0.01
	${\rm hii320 }$	SB	K1			17						29.76 $\pm$0.01
27F	${\rm hcg143 }$		M5	03 44 23.3	+25 21 34	2	0	124	$0.59 \pm 0.38$	$-0.59 \pm 0.37$	19404	29.31 $\pm$0.79
27	${\rm hcg149 }$		M4	03 44 24.8	+24 45 42	25	2	43	$0.51 \pm 0.05$	$0.09 \pm 0.06$	28318	29.37 $\pm$0.03
27	${\rm hcg148 }$			03 44 24.9	+24 51 45	11	5	88	$0.48 \pm 0.16$	$0.17 \pm 0.16$	27125	28.63 $\pm$0.08
27	${\rm hcg150 }$		M3	03 44 25.4	+24 40 47	7	6	322	$0.42 \pm 0.08$	$-0.03 \pm 0.09$	27645	29.02 $\pm$0.04
27F	${\rm hii345 }$		K1	03 44 26.2	+24 35 16	8	0	5657	$0.45 \pm 0.03$	$0.06 \pm 0.03$	25805	29.98 $\pm$0.12
27	${\rm hii347 +B }$	VB	M0	03 44 27.1	+24 50 30	9	4	924	$0.50 \pm 0.05$	$-0.02 \pm 0.06$	27685	29.04 $\pm$0.03
27	${\rm hii380 }$		K6	03 44 36.7	+25 08 22	8	21	35	$0.54 \pm 0.21$	$-0.04 \pm 0.19$	16093	28.80 $\pm$0.10
27	${\rm hcg160 }$			03 44 38.6	+24 31 48	12	15	135	$0.61 \pm 0.11$	$0.10 \pm 0.12$	26501	28.89 $\pm$0.06
27	${\rm hii405 }$		F9	03 44 40.5	+24 48 57	11	5	1435	$0.50 \pm 0.04$	$-0.10 \pm 0.05$	26678	29.51 $\pm$0.02
27	${\rm hii451 }$		K6	03 44 49.8	+24 54 33	9	10	357	$0.44 \pm 0.08$	$-0.05 \pm 0.09$	25141	29.11 $\pm$0.04
27	${\rm hcg172 }$			03 45 00.7	+24 46 34	9	8	122	$0.61 \pm 0.14$	$-0.01 \pm 0.14$	26449	28.73 $\pm$0.07
27	${\rm hhj48 }$			03 45 05.9	+24 40 33	12	11	69	$0.23 \pm 0.16$	$0.14 \pm 0.17$	26015	28.59 $\pm$0.08
27	${\rm hii541 }$	SB?	B9	03 45 08.2	+24 50 23	19	11	20	$-0.30 \pm 0.21$	$0.53 \pm 0.36$	25514	27.84 $\pm$0.15
27	${\rm hii531 }$		F2	03 45 09.2	+24 16 12	44	32	39	>-0.57	$0.32 \pm 0.21$	18824	28.70 $\pm$0.20
27	${\rm hii563 }$	SB1	B8	03 45 13.2	+24 27 55	14	22	882	$0.61 \pm 0.04$	$-0.07 \pm 0.05$	19738	29.36 $\pm$0.02
27	${\rm hii566 }$			03 45 15.4	+25 05 28	19	22	331	$0.57 \pm 0.06$	$-0.03 \pm 0.08$	16139	29.47 $\pm$0.04
	${\rm hii559 }$		K5			29						$\pm$
27F	${\rm hcg181 }$		M4	03 45 15.8	+24 34 34	10	0	471	$0.51 \pm 0.12$	$0.10 \pm 0.15$	20582	29.20 $\pm$0.66
27	${\rm hcg178 }$		M5	03 45 16.8	+25 16 31	42	32	146	$0.84 \pm 0.12$	$-0.14 \pm 0.11$	18651	29.20 $\pm$0.06
	${\rm hii571 }$	SB1	G9			56						28.90 $\pm$0.06
27	${\rm hii605 }$	SB1	F5	03 45 20.8	+24 55 07	13	15	45	$0.17 \pm 0.17$	$-0.17 \pm 0.19$	23690	28.30 $\pm$0.09
27	${\rm hii624 }$		M4	03 45 23.2	+24 50 56	7	14	186	$0.60 \pm 0.10$	$-0.06 \pm 0.11$	23213	29.01 $\pm$0.05
27	${\rm hii627 }$	SB?	F7	03 45 23.8	+24 53 04	6	15	660	$0.76 \pm 0.05$	$-0.17 \pm 0.06$	24594	29.10 $\pm$0.03
27	${\rm hii686 }$		M6	03 45 34.9	+24 17 55	34	33	539	$0.55 \pm 0.05$	$-0.06 \pm 0.06$	20489	29.68 $\pm$0.03
27	${\rm hii708 }$		G2	03 45 35.6	+24 05 05	5	45	96	$0.96 \pm 0.10$	$0.11 \pm 0.08$	16939	29.58 $\pm$0.05
27	${\rm hii727 }$		F9	03 45 39.3	+24 37 49	13	19	1279	$0.54 \pm 0.04$	$-0.12 \pm 0.05$	16083	29.81 $\pm$0.02
27	${\rm hii739 }$	PHB	G2	03 45 41.9	+24 54 17	6	19	3756	$0.62 \pm 0.02$	$0.07 \pm 0.03$	14062	29.95 $\pm$0.01
27	${\rm hii761 }$	SB1	G4	03 45 44.3	+24 13 25	10	38	255	$0.30 \pm 0.07$	$-0.01 \pm 0.08$	19067	29.26 $\pm$0.03
27	${\rm hii890 +B }$	VB	K7	03 46 06.7	+24 22 31	9	34	74	$0.78 \pm 0.27$	$-0.24 \pm 0.22$	20115	28.58 $\pm$0.13
27	${\rm hii885 +B }$	VB	K4	03 46 08.3	+24 51 39	24	24	38	$0.62 \pm 0.17$	$-0.04 \pm 0.16$	15159	28.66 $\pm$0.08
27	${\rm hii956 +B }$	VB	F1	03 46 15.6	+24 11 12	13	44	89	$0.65 \pm 0.11$	$0.12 \pm 0.10$	17027	29.17 $\pm$0.05
27	${\rm hii1032 }$		G8	03 46 27.0	+24 25 59	18	35	1603	$0.72 \pm 0.03$	$0.15 \pm 0.04$	18548	30.00 $\pm$0.02
27	${\rm hii1015 }$		G3	03 46 28.1	+25 07 48	24	35	84	$0.37 \pm 0.12$	$-0.09 \pm 0.12$	18506	29.18 $\pm$0.06
27	${\rm hii1100 +B }$	VB	K5	03 46 36.4	+24 20 36	10	40	213	$0.74 \pm 0.15$	$-0.13 \pm 0.12$	18095	29.00 $\pm$0.07
27	${\rm hii1101 }$	SB2	G1	03 46 40.0	+24 57 04	36	32	139	$0.66 \pm 0.09$	$-0.09 \pm 0.09$	15210	29.13 $\pm$0.04
27	${\rm hcg241 }$		M5	03 46 49.6	+25 13 59	74	43	8	$-0.78 \pm 0.65$	<0.79	17002	27.85 $\pm$0.00
27	${\rm hii1309 }$		F6	03 47 09.3	+24 17 04	27	48	115	$0.31 \pm 0.14$	$-0.14 \pm 0.16$	15911	29.34 $\pm$0.07
27	${\rm sk432 }$			03 47 13.4	+25 07 08	26	43	63	$0.84 \pm 0.18$	$0.10 \pm 0.12$	16091	29.25 $\pm$0.08
27	${\rm Teide1 }$			03 47 20.3	+24 21 36	63	47	561	$-0.42 \pm 0.65$	$-0.49 \pm 1.31$	9911	28.53 $\pm$0.76
27	${\rm hii1384 }$		A7	03 47 23.6	+24 35 27	7	42	1653	$0.49 \pm 0.03$	$0.07 \pm 0.03$	16583	30.18 $\pm$0.01
27F	${\rm hii1653 }$		K6	03 47 57.6	+24 43 39	31	0	101	$0.36 \pm 0.20$	$0.08 \pm 0.21$	14583	29.75 $\pm$0.36
8,9	${\rm hii233 }$	SB	F8	03 43 58.2	+23 54 03	63	42	24	>-0.80	>-0.32	7967	28.40 $\pm$0.47
8,9	${\rm hii298 +B }$	VB	K1	03 44 15.3	+24 01 50	37	36	31	$0.51 \pm 0.07$	$0.14 \pm 0.08$	8709	29.50 $\pm$0.04
8,9	${\rm hii345 }$		K1	03 44 25.2	+24 34 57	30	43	24	$0.53 \pm 0.07$	$0.09 \pm 0.07$	7179	29.98 $\pm$0.03
8,9	${\rm hii476 }$	SB	G9	03 44 55.5	+23 55 30	27	30	30	$0.90 \pm 0.28$	$0.27 \pm 0.18$	8940	28.78 $\pm$0.13
8,9	${\rm hii531 }$		F2	03 45 07.3	+24 15 48	12	25	51	>-0.04	$-0.04 \pm 0.16$	9597	29.01 $\pm$0.16
8,9	${\rm hii563 }$	SB1	B8	03 45 13.1	+24 27 27	38	30	128	$0.56 \pm 0.10$	$0.05 \pm 0.11$	7647	29.24 $\pm$0.05
8,9	${\rm hcg181 }$		M4	03 45 13.6	+24 34 33	39	34	43	$0.50 \pm 0.18$	$0.23 \pm 0.16$	8955	29.25 $\pm$0.09
	${\rm hii554 }$		K7			45						$\pm$
8,9	${\rm hii686 }$		M6	03 45 32.8	+24 18 25	12	21	177	$0.50 \pm 0.09$	$0.02 \pm 0.10$	9015	29.50 $\pm$0.05
8,9	${\rm hii708 }$		G2	03 45 35.8	+24 04 59	7	18	327	$0.87 \pm 0.06$	$-0.03 \pm 0.09$	9127	29.55 $\pm$0.04
8,9	${\rm hii738 +B }$	VB	K5	03 45 38.9	+23 45 23	8	28	430	$0.99 \pm 0.05$	$0.28 \pm 0.06$	7729	29.56 $\pm$0.03
8,9	${\rm hii727 }$		F9	03 45 39.6	+24 37 43	6	33	311	$0.46 \pm 0.07$	$-0.04 \pm 0.07$	8814	29.79 $\pm$0.03
8,9	${\rm hii739 }$	PHB	G2	03 45 40.7	+24 53 54	33	48	738	$0.67 \pm 0.05$	$0.09 \pm 0.05$	7642	29.90 $\pm$0.02
8,9	${\rm hii745 }$		F8	03 45 40.8	+24 17 17	6	19	62	$0.68 \pm 0.10$	$0.15 \pm 0.12$	9568	29.32 $\pm$0.06
8,9	${\rm hii746 }$	SB?	G9	03 45 43.8	+24 25 35	34	23	15	$0.56 \pm 0.35$	$-0.31 \pm 0.29$	7999	28.47 $\pm$0.18
8,9	${\rm hii761 }$	SB1	G4	03 45 44.7	+24 13 11	6	16	418	$0.34 \pm 0.07$	$-0.03 \pm 0.08$	10827	29.27 $\pm$0.04
8,9	${\rm hii890 +B }$	VB	K7	03 46 07.8	+24 22 22	8	17	21	>-0.04	$-0.16 \pm 0.27$	9596	28.30 $\pm$0.20
8,9	${\rm hii930 }$		K6	03 46 13.3	+24 03 15	7	11	83	$0.67 \pm 0.16$	$0.05 \pm 0.16$	11799	28.92 $\pm$0.08
8,9	${\rm hii956 +B }$	VB	F1	03 46 16.3	+24 11 20	7	9	657	$0.63 \pm 0.06$	$-0.01 \pm 0.07$	12492	29.25 $\pm$0.03
8,9	${\rm hii974 }$		K7	03 46 18.6	+24 46 37	39	39	12	$0.69 \pm 0.43$	$-0.47 \pm 0.27$	8465	29.01 $\pm$0.20
8,9	${\rm hii980 }$		B9	03 46 19.9	+23 56 53	6	14	774	$0.88 \pm 0.04$	$-0.08 \pm 0.06$	11632	29.70 $\pm$0.03
8,9	${\rm hcg219 }$		K4	03 46 25.8	+24 09 31	9	7	91	$0.51 \pm 0.16$	$0.14 \pm 0.16$	12387	28.92 $\pm$0.08
8,9	${\rm hii1032 }$		G8	03 46 28.5	+24 25 59	5	18	1265	$0.78 \pm 0.04$	$0.01 \pm 0.05$	9957	29.97 $\pm$0.02
8,9	${\rm hii1039 }$		K7	03 46 28.5	+23 35 57	24	33	71	>-0.13	$0.32 \pm 0.11$	9438	29.22 $\pm$0.14
8,9	${\rm hii1061 +B }$	VB	K9	03 46 31.4	+24 07 03	4	6	265	$0.74 \pm 0.09$	$0.17 \pm 0.11$	12755	28.91 $\pm$0.05
8,9	${\rm hii1100 +B }$	VB	K5	03 46 37.6	+24 20 35	6	13	565	$0.73 \pm 0.06$	$0.04 \pm 0.08$	12232	29.25 $\pm$0.03
8,9	${\rm hii1117 }$	SB2	G8	03 46 39.2	+23 47 10	23	21	45	$0.28 \pm 0.16$	$-0.09 \pm 0.18$	9470	28.77 $\pm$0.08
8,9	${\rm hii1122 }$	SB2	F6	03 46 39.4	+24 06 10	4	5	383	$0.54 \pm 0.08$	$-0.14 \pm 0.09$	12602	29.04 $\pm$0.04
8,9	${\rm hii1124 }$		K3	03 46 39.7	+24 01 47	5	8	312	$0.66 \pm 0.08$	$0.08 \pm 0.10$	12772	29.30 $\pm$0.04
8,9	${\rm hii1136 }$		K3	03 46 39.7	+23 29 55	7	38	276	$0.88 \pm 0.07$	$0.37 \pm 0.06$	8797	29.83 $\pm$0.04
8,9	${\rm hii1101 }$	SB2	G1	03 46 45.7	+24 57 08	99	48	10	$0.70 \pm 0.32$	$-0.26 \pm 0.23$	6640	29.00 $\pm$0.15
8,9	${\rm hcg244 }$			03 46 53.9	+24 17 15	6	9	81	$0.64 \pm 0.17$	$-0.23 \pm 0.17$	12466	28.91 $\pm$0.08
8,9	${\rm hii1234 }$		A1	03 46 59.8	+24 31 17	7	23	71	$0.69 \pm 0.16$	$0.03 \pm 0.16$	6490	29.26 $\pm$0.08
8,9	${\rm hii1280 }$		K5	03 47 03.6	+24 09 33	3	4	216	$0.75 \pm 0.11$	$-0.07 \pm 0.12$	12552	29.17 $\pm$0.06
8,9	${\rm hii1266 +B }$	VB	F2	03 47 03.9	+24 48 56	17	40	66	$0.68 \pm 0.14$	$-0.28 \pm 0.12$	8396	29.19 $\pm$0.07
8,9	${\rm hii1306 }$		K8	03 47 09.3	+23 43 03	25	25	145	$0.51 \pm 0.09$	$0.03 \pm 0.11$	7293	29.56 $\pm$0.05
	${\rm hii1298 +B }$	VB	K3			37						29.26 $\pm$0.05
8,9	${\rm hii1309 }$		F6	03 47 10.1	+24 16 32	6	9	416	$0.65 \pm 0.07$	$-0.22 \pm 0.09$	12374	29.40 $\pm$0.04
8,9	${\rm hcg258 }$		K8	03 47 13.4	+23 49 44	10	19	78	$0.17 \pm 0.14$	$0.02 \pm 0.16$	8551	29.16 $\pm$0.07
8,9	${\rm hii1338 }$	SB2	F6	03 47 16.5	+24 07 42	2	6	99	$0.47 \pm 0.15$	$-0.16 \pm 0.16$	12550	28.64 $\pm$0.07
8,9	${\rm hii1348 A + B }$	VB	K5	03 47 18.1	+24 23 22	6	16	75	$0.33 \pm 0.16$	$0.12 \pm 0.17$	10807	28.69 $\pm$0.08
8,9	${\rm NPL22 }$	VB		03 47 18.1	+24 23 22	38	16	75	$0.33 \pm 0.16$	$0.12 \pm 0.17$	10807	28.69 $\pm$0.08
8,9	${\rm hii1355 +B }$	VB	M0	03 47 18.3	+24 02 09	5	9	319	$0.45 \pm 0.08$	$-0.01 \pm 0.10$	12513	29.02 $\pm$0.04
8,9	${\rm hii1397 +B }$	VB	A2	03 47 24.2	+23 54 53	1	15	174	$0.50 \pm 0.10$	$-0.10 \pm 0.11$	11624	28.98 $\pm$0.05
	${\rm hii1392 +B }$	VB				7						$\pm$
8,9	${\rm hii1432 }$		B9	03 47 28.9	+24 06 26	5	8	9	$-0.14 \pm 0.36$	$0.04 \pm 0.48$	11956	28.20 $\pm$0.25
8,9	${\rm hcg273 }$			03 47 30.8	+24 22 13	3	16	34	$0.16 \pm 0.21$	$0.33 \pm 0.23$	11418	28.72 $\pm$0.11
8,9	${\rm hii1514 }$		G4	03 47 37.9	+24 21 35	38	16	97	$0.78 \pm 0.14$	$-0.14 \pm 0.16$	11586	29.00 $\pm$0.08
8,9	${\rm hii1516 }$		K7	03 47 40.5	+24 18 09	2	14	341	$0.53 \pm 0.07$	$0.05 \pm 0.09$	11104	29.46 $\pm$0.04
8,9	${\rm hii1532 }$		K6	03 47 40.8	+23 44 15	11	26	55	$0.47 \pm 0.14$	$-0.06 \pm 0.15$	10237	29.16 $\pm$0.08
8,9	${\rm hii1531 }$		K6	03 47 41.7	+23 58 17	5	15	287	$0.49 \pm 0.08$	$0.00 \pm 0.10$	11481	29.41 $\pm$0.04
8,9	${\rm ALR929 }$		M4	03 47 48.6	+24 30 08	16	25	16	$0.64 \pm 0.38$	$0.42 \pm 0.25$	9100	28.76 $\pm$0.18
	${\rm hcg295 }$					32						$\pm$
8,9	${\rm hii1613 }$		F9	03 47 52.4	+23 56 27	3	18	62	$0.54 \pm 0.17$	$-0.37 \pm 0.16$	9163	29.07 $\pm$0.08
8,9	${\rm hii1653 }$		K6	03 47 59.9	+24 43 53	3	38	32	$0.30 \pm 0.17$	$-0.10 \pm 0.17$	8662	29.27 $\pm$0.09
8,9	${\rm hii1726 +B }$	VB	F9	03 48 07.2	+24 08 33	1	17	291	$0.86 \pm 0.07$	$-0.18 \pm 0.09$	10291	29.15 $\pm$0.04
8,9	${\rm hcg310 }$			03 48 12.2	+23 39 16	43	33	16	$0.27 \pm 0.23$	$0.26 \pm 0.26$	9213	28.87 $\pm$0.17
	${\rm hcg315 }$					25	35	12				$\pm$
	${\rm hii1797 }$		F9			21	35	12				$\pm$
8,9	${\rm hii1762 }$		F2	03 48 14.0	+24 19 10	8	21	193	$0.66 \pm 0.09$	$-0.23 \pm 0.10$	7859	29.51 $\pm$0.05
8,9	${\rm hii1827 }$		M3	03 48 21.7	+23 58 24	13	22	10	$0.42 \pm 0.12$	$-0.09 \pm 0.14$	8872	29.27 $\pm$0.07
8,9	${\rm hii1856 }$		F9	03 48 26.2	+24 02 58	3	22	47	>0.08	$0.01 \pm 0.18$	9047	28.86 $\pm$0.17
8,9	${\rm hii1912 +B }$	VB	F7	03 48 33.4	+24 10 55	17	23	23	$0.66 \pm 0.26$	$-0.18 \pm 0.24$	6403	28.72 $\pm$0.13
8,9	${\rm hii2034 }$		K3	03 48 49.3	+23 58 32	7	28	112	$0.67 \pm 0.12$	$-0.07 \pm 0.11$	9895	29.40 $\pm$0.06
8,9	${\rm hii2027 }$	SB1	K1	03 48 49.4	+24 16 08	8	27	66	$0.60 \pm 0.14$	$-0.10 \pm 0.14$	9587	28.94 $\pm$0.07
8,9	${\rm hii2181 }$		B9	03 49 10.6	+24 08 16	6	31	50	$0.37 \pm 0.15$	$0.14 \pm 0.15$	8904	29.27 $\pm$0.08
8,9	${\rm hii2208 }$		K8	03 49 15.4	+24 33 42	21	41	25	$0.24 \pm 0.16$	$0.26 \pm 0.20$	8352	29.27 $\pm$0.09
8,9	${\rm hii2500 }$	SB		03 49 57.4	+23 51 02	11	45	558	$0.54 \pm 0.05$	$0.01 \pm 0.06$	7622	29.83 $\pm$0.03
11-13	${\rm hii157 }$		F2	03 43 38.9	+23 39 17	39	44	8	$0.56 \pm 0.14$	$0.23 \pm 0.12$	24716	29.26 $\pm$0.07
	${\rm sk630 }$					50						$\pm$
11-13	${\rm hii193 }$		G9	03 43 52.0	+24 14 37	24	44	55	$0.58 \pm 0.09$	$0.08 \pm 0.08$	22771	29.53 $\pm$0.04
11-13	${\rm hcg135 }$		K4	03 43 57.0	+23 57 42	34	38	22	$0.89 \pm 0.36$	$0.46 \pm 0.23$	29214	28.76 $\pm$0.18
11-13	${\rm hii296 }$	SB1	K1	03 44 12.5	+23 22 39	22	46	209	$0.56 \pm 0.08$	$0.14 \pm 0.07$	24483	29.29 $\pm$0.04
11-13	${\rm hii357 +B }$	VB	K6	03 44 28.1	+24 09 56	23	35	61	$0.49 \pm 0.06$	$0.25 \pm 0.06$	27954	29.33 $\pm$0.03
11-13	${\rm hii370 }$		M1	03 44 31.2	+23 52 18	17	30	38	>-0.55	$-0.03 \pm 0.15$	29912	28.56 $\pm$0.19
11-13	${\rm hii476 }$	SB	G9	03 44 55.2	+23 55 15	21	25	237	$0.92 \pm 0.08$	$-0.08 \pm 0.07$	32084	28.91 $\pm$0.04
11-13	${\rm hii513 }$		K7	03 45 01.4	+23 23 52	46	37	56	$0.82 \pm 0.21$	$0.09 \pm 0.13$	26727	29.06 $\pm$0.09
11-13	${\rm hii522 }$	SB1	K2	03 45 04.0	+23 50 18	12	23	12	$0.66 \pm 0.39$	$-0.52 \pm 0.23$	30274	28.20 $\pm$0.16
11-13	${\rm hii531 }$		F2	03 45 06.0	+24 15 40	11	31	14	$0.83 \pm 0.54$	$0.10 \pm 0.33$	29064	28.60 $\pm$0.22
11-13	${\rm hii563 }$	SB1	B8	03 45 11.1	+24 28 09	17	41	500	$0.36 \pm 0.05$	$-0.01 \pm 0.06$	26434	29.40 $\pm$0.03
11-13	${\rm hii625 }$		K5	03 45 21.2	+23 43 35	5	21	1240	$0.98 \pm 0.02$	$0.35 \pm 0.04$	21754	29.72 $\pm$0.02
11-13	${\rm hii659 }$		K3	03 45 23.3	+23 26 56	23	32	154	$0.91 \pm 0.12$	$0.17 \pm 0.09$	26220	29.11 $\pm$0.07
	${\rm hii636 }$		K4			35	31	34				$\pm$
11-13	${\rm hii676 }$		K7	03 45 31.4	+23 45 38	26	18	36	>0.09	$0.14 \pm 0.12$	32275	28.61 $\pm$0.14
11-13	${\rm hii686 }$		M6	03 45 35.6	+24 18 03	40	29	615	$0.47 \pm 0.04$	$0.03 \pm 0.05$	30959	29.63 $\pm$0.02
11-13	${\rm hii708 }$		G2	03 45 36.1	+24 04 52	14	19	727	$0.92 \pm 0.04$	$0.00 \pm 0.06$	21938	29.57 $\pm$0.03
11-13	${\rm hii727 }$		F9	03 45 39.0	+24 37 23	21	46	278	$0.56 \pm 0.06$	$0.08 \pm 0.06$	24003	29.78 $\pm$0.03
11-13	${\rm hii738 +B }$	VB	K5	03 45 39.6	+23 45 12	6	16	2868	$0.97 \pm 0.02$	$0.27 \pm 0.03$	35081	29.50 $\pm$0.01
11-13	${\rm hii746 }$	SB?	G9	03 45 44.0	+24 25 29	40	35	81	$0.79 \pm 0.18$	$-0.15 \pm 0.13$	27517	28.77 $\pm$0.08
11-13	${\rm hii761 }$	SB1	G4	03 45 44.6	+24 13 10	6	24	1106	$0.44 \pm 0.03$	$-0.09 \pm 0.04$	33918	29.37 $\pm$0.02
11-13	${\rm hii801 +B }$	VB	A2	03 45 47.6	+23 08 28	28	46	19	>-0.82	$-0.54 \pm 0.18$	25127	28.49 $\pm$0.22
11-13	${\rm hii793 }$		M1	03 45 49.5	+23 51 09	9	12	28	$0.63 \pm 0.30$	$-0.06 \pm 0.21$	36741	28.36 $\pm$0.13
11-13	${\rm hii799 }$		K7	03 45 50.9	+23 52 22	8	12	89	>0.34	$-0.08 \pm 0.13$	37970	28.50 $\pm$0.14
11-13	${\rm hii870 +B }$	VB	K6	03 46 03.2	+23 44 15	7	13	109	$0.94 \pm 0.15$	$0.05 \pm 0.12$	36638	28.42 $\pm$0.07
11-13	${\rm hii890 +B }$	VB	K7	03 46 05.5	+24 21 56	42	30	29	$0.41 \pm 0.21$	$0.17 \pm 0.19$	29085	28.48 $\pm$0.11
11-13	${\rm hii915 +B }$	VB	K6	03 46 09.0	+23 20 53	9	33	483	$0.39 \pm 0.05$	$0.00 \pm 0.06$	30194	29.25 $\pm$0.03
	${\rm hii923 }$		G1			30						29.55 $\pm$0.03
11-13	${\rm hii930 }$		K6	03 46 13.3	+24 03 08	11	12	354	$0.69 \pm 0.07$	$-0.01 \pm 0.08$	37503	29.07 $\pm$0.04
11-13	${\rm hii956 +B }$	VB	F1	03 46 16.2	+24 11 17	9	19	1355	$0.63 \pm 0.03$	$-0.04 \pm 0.04$	27733	29.41 $\pm$0.02
11-13	${\rm hii975 }$	PHB	K1	03 46 18.0	+23 29 09	5	24	149	>-0.05	$0.27 \pm 0.09$	32869	28.58 $\pm$0.13
11-13	${\rm hii980 }$		B9	03 46 19.8	+23 56 47	10	7	3636	$0.84 \pm 0.02$	$-0.04 \pm 0.03$	38142	29.75 $\pm$0.01
11-13	${\rm hii1039 }$		K7	03 46 27.9	+23 35 30	6	18	604	>0.62	$0.13 \pm 0.06$	33638	29.18 $\pm$0.12
11-13	${\rm hii1032 }$		G8	03 46 28.4	+24 26 02	2	33	2011	$0.80 \pm 0.02$	$0.17 \pm 0.03$	30336	30.03 $\pm$0.01
11-13	${\rm hii1081 }$		M0	03 46 34.2	+23 18 02	27	35	17	$0.22 \pm 0.25$	$0.00 \pm 0.25$	28982	28.65 $\pm$0.15
11-13	${\rm hii1084 }$		F2	03 46 34.5	+23 37 20	10	16	69	$0.90 \pm 0.18$	$0.13 \pm 0.14$	36685	28.63 $\pm$0.09
11-13	${\rm hii1103 }$		M2	03 46 36.3	+23 24 28	21	28	125	>-0.22	$0.29 \pm 0.10$	34629	28.85 $\pm$0.14
11-13	${\rm hii1117 }$	SB2	G8	03 46 38.4	+23 47 08	15	6	536	$0.32 \pm 0.06$	$-0.11 \pm 0.07$	40018	28.82 $\pm$0.03
11-13	${\rm hii1122 }$	SB2	F6	03 46 39.6	+24 06 06	9	13	897	$0.61 \pm 0.05$	$-0.10 \pm 0.06$	37905	29.05 $\pm$0.02
11-13	${\rm hii1124 }$		K3	03 46 39.7	+24 01 42	8	8	1189	$0.62 \pm 0.04$	$0.07 \pm 0.05$	39961	29.38 $\pm$0.02
11-13	${\rm hii1136 }$		K3	03 46 40.7	+23 29 47	9	23	2317	$0.95 \pm 0.02$	$0.17 \pm 0.03$	32112	29.81 $\pm$0.02
11-13	${\rm hii1215 }$		G2	03 46 54.0	+23 34 56	8	18	245	$0.64 \pm 0.07$	$-0.19 \pm 0.08$	35106	29.08 $\pm$0.04
11-13	${\rm hcg244 }$			03 46 54.2	+24 17 11	10	24	110	$0.84 \pm 0.12$	$0.16 \pm 0.10$	34727	29.00 $\pm$0.06
11-13	${\rm hii1275 }$		K0	03 47 01.0	+23 29 47	5	23	31	$0.30 \pm 0.18$	$-0.03 \pm 0.19$	27335	28.66 $\pm$0.10
11-13	${\rm hii1286 }$	SB2	M5	03 47 03.8	+23 36 55	5	17	230	>0.43	$0.08 \pm 0.09$	35506	28.61 $\pm$0.13
11-13	${\rm hii1280 }$		K5	03 47 03.9	+24 09 28	9	17	329	$0.56 \pm 0.07$	$0.07 \pm 0.08$	34157	29.16 $\pm$0.04
11-13	${\rm hii1284 }$		F0	03 47 06.6	+23 59 39	35	8	8	>-0.31	$-0.30 \pm 0.35$	38557	27.83 $\pm$0.29
11-13	${\rm hii1306 }$		K8	03 47 08.7	+23 42 37	4	12	1416	$0.67 \pm 0.03$	$0.05 \pm 0.05$	41597	29.48 $\pm$0.02
	${\rm hii1298 +B }$	VB	K3			32						29.18 $\pm$0.02
11-13	${\rm hii1309 }$		F6	03 47 08.9	+24 17 03	28	24	556	$0.65 \pm 0.05$	$-0.08 \pm 0.05$	32639	29.51 $\pm$0.03
11-13	${\rm hii1321 }$		M1	03 47 09.5	+23 44 28	6	10	472	$0.29 \pm 0.06$	$0.01 \pm 0.08$	38922	29.10 $\pm$0.03
11-13	${\rm hcg258 }$		K8	03 47 13.8	+23 49 50	6	7	368	$0.43 \pm 0.08$	$-0.06 \pm 0.08$	39375	29.02 $\pm$0.04
11-13	${\rm hii1355 +B }$	VB	M0	03 47 18.3	+24 02 06	7	12	1113	$0.64 \pm 0.04$	$0.03 \pm 0.05$	38946	29.10 $\pm$0.02
11-13	${\rm hii1397 +B }$	VB	A2	03 47 24.3	+23 54 48	6	9	1321	$0.60 \pm 0.04$	$-0.11 \pm 0.05$	39501	29.13 $\pm$0.02
	${\rm hii1392 +B }$	VB				11						$\pm$
29.13	0.02
11-13	${\rm hii1384 }$		A7	03 47 24.6	+24 35 10	14	43	1076	$0.52 \pm 0.03$	$0.13 \pm 0.03$	26187	30.14 $\pm$0.01
11-13	${\rm hcg269 }$			03 47 26.5	+23 38 02	1	18	71	$0.77 \pm 0.15$	$0.24 \pm 0.13$	35248	28.71 $\pm$0.07
11-13	${\rm hii1432 }$		B9	03 47 29.6	+24 06 17	9	16	20	$0.12 \pm 0.23$	$0.16 \pm 0.25$	32335	28.37 $\pm$0.13
11-13	${\rm hcg277 }$		M1	03 47 33.7	+23 41 31	5	16	221	$0.38 \pm 0.08$	$-0.10 \pm 0.09$	37837	29.00 $\pm$0.04
11-13	${\rm hii1512 }$		K6	03 47 38.4	+23 27 39	27	28	33	$0.33 \pm 0.16$	$-0.11 \pm 0.16$	32535	28.78 $\pm$0.09
11-13	${\rm hii1532 }$		K6	03 47 41.2	+23 44 19	8	15	765	$0.36 \pm 0.05$	$0.08 \pm 0.06$	34856	29.38 $\pm$0.02
11-13	${\rm hii1531 }$		K6	03 47 41.6	+23 58 14	7	14	713	$0.48 \pm 0.05$	$0.07 \pm 0.06$	36768	29.32 $\pm$0.03
11-13	${\rm ALR929 }$		M4	03 47 48.3	+24 29 30	30	39	13	$0.45 \pm 0.26$	$-0.01 \pm 0.22$	27751	28.86 $\pm$0.13
	${\rm hcg295 }$					60						$\pm$
11-13	${\rm hii1613 }$		F9	03 47 52.6	+23 56 23	7	16	390	$0.46 \pm 0.07$	$-0.04 \pm 0.07$	33868	29.20 $\pm$0.03
11-13	${\rm hii1726 +B }$	VB	F9	03 48 07.8	+24 08 32	11	24	276	$0.58 \pm 0.07$	$-0.23 \pm 0.07$	32533	28.99 $\pm$0.03
11-13	${\rm hii1785 }$		M5	03 48 14.9	+24 29 52	40	42	8	$-0.26 \pm 0.30$	<0.70	22872	28.63 $\pm$0.20
11-13	${\rm hcg315 }$			03 48 15.2	+23 37 56	21	25	384	$0.49 \pm 0.06$	$0.06 \pm 0.06$	26959	29.49 $\pm$0.03
	${\rm hii1797 }$		F9			28						$\pm$
11-13	${\rm hii1794 }$		G2	03 48 19.3	+23 53 15	33	21	201	$0.54 \pm 0.08$	$0.08 \pm 0.09$	21618	29.27 $\pm$0.04
11-13	${\rm hii1856 }$		F9	03 48 27.4	+24 02 52	18	25	134	$0.36 \pm 0.09$	$-0.11 \pm 0.09$	33401	29.13 $\pm$0.04
11-13	${\rm hii1924 }$		G1	03 48 33.9	+23 25 43	24	37	60	$0.30 \pm 0.11$	$-0.22 \pm 0.12$	28445	29.16 $\pm$0.06
11-13	${\rm hii1912 +B }$	VB	F7	03 48 36.4	+24 11 19	34	31	170	$0.59 \pm 0.08$	$0.03 \pm 0.08$	30996	29.00 $\pm$0.04
11-13	${\rm hii2034 }$		K3	03 48 49.4	+23 58 17	23	29	512	$0.57 \pm 0.05$	$0.16 \pm 0.05$	22939	29.66 $\pm$0.03
11-13	${\rm hcg349 }$			03 48 56.9	+24 19 29	17	40	8	$0.54 \pm 0.13$	$0.21 \pm 0.11$	26891	29.24 $\pm$0.06
11-13	${\rm hii2147 }$	SB2	G9	03 49 06.1	+23 46 45	8	33	5098	$0.54 \pm 0.02$	$0.12 \pm 0.02$	30582	30.04 $\pm$0.01
11-13	${\rm hii2181 }$		B9	03 49 11.2	+24 08 14	1	36	205	$0.59 \pm 0.06$	$0.15 \pm 0.06$	28773	29.52 $\pm$0.03
11-13	${\rm hii2368 }$		M3	03 49 32.8	+23 26 28	56	47	53	$0.54 \pm 0.16$	$-0.21 \pm 0.13$	19648	29.29 $\pm$0.08
11-13	${\rm hii2366 }$		K0	03 49 42.8	+24 17 53	87	47	371	$-0.03 \pm 0.03$	$0.12 \pm 0.04$	23316	30.03 $\pm$0.02
	${\rm hcg375 }$					88						$\pm$
11-13	${\rm hii2500 }$	SB		03 49 57.2	+23 50 46	5	44	1747	$0.60 \pm 0.02$	$0.16 \pm 0.02$	25260	29.98 $\pm$0.01
11-13	${\rm hii2548 }$		K7	03 50 06.8	+24 08 29	69	48	32	>-0.59	$0.30 \pm 0.06$	22238	29.19 $\pm$0.15

   

Table 4: X-ray data for Hyads detected in PSPC observations.

Obs. No.	Designation	Mult.	SpT.	X-ray position		$\Delta$	Offax	ML	HR1	HR2	Expos	$\log{L_{\rm X}}$
				$\alpha_{2000}$	$\delta_{2000}$	[ $^{\prime\prime}$]	[$^\prime$]				[s]	[erg/s]
10	${\rm VB40}$	SB	F9	04 22 43.8	+15 03 30	10	30	6659	$-0.22 \pm 0.01$	$-0.10 \pm 0.02$	20214	29.36 $\pm$0.01
10	${\rm VA260}$		M5	04 23 02.1	+15 13 59	21	27	43	$-0.42 \pm 0.12$	$-0.01 \pm 0.25$	31740	27.84 $\pm$0.08
10	${\rm VA275}$		M5	04 23 24.4	+14 25 35	13	45	219	$-0.23 \pm 0.05$	$-0.33 \pm 0.08$	24794	28.75 $\pm$0.03
10	${\rm VB46}$		K1	04 23 32.5	+14 40 12	2	31	432	$-0.45 \pm 0.05$	$-0.24 \pm 0.10$	23619	28.58 $\pm$0.03
10	${\rm VA288}$	SB2	M4	04 23 50.4	+14 55 20	3	17	9143	$-0.23 \pm 0.02$	$-0.04 \pm 0.03$	32137	28.99 $\pm$0.01
10	${\rm VB50}$	SB?	G1	04 24 12.3	+14 45 25	5	22	12852	$-0.15 \pm 0.01$	$0.00 \pm 0.02$	29019	29.52 $\pm$0.01
10	${\rm VA334}$		M0	04 24 50.2	+15 52 21	36	46	937	$-0.13 \pm 0.02$	$-0.11 \pm 0.04$	22583	29.24 $\pm$0.01
10	${\rm VA368}$		M4	04 25 50.4	+15 00 13	4	15	172	$-0.47 \pm 0.08$	$0.12 \pm 0.17$	35439	27.89 $\pm$0.05
10	${\rm VA383}$		M1	04 26 04.7	+15 02 33	5	18	1382	$-0.17 \pm 0.04$	$0.04 \pm 0.06$	31263	28.70 $\pm$0.02
10	${\rm VB59}$	SB	F9	04 26 05.9	+15 32 09	41	32	3489	$-0.23 \pm 0.02$	$-0.01 \pm 0.03$	24946	29.15 $\pm$0.01
10	${\rm VB141}$	var	A8	04 26 19.9	+15 37 09	12	38	10838	$-0.13 \pm 0.01$	$0.05 \pm 0.01$	24307	30.22 $\pm$0.00
14	${\rm VB93}$		K2	04 33 36.1	+16 45 33	27	36	36	$-0.22 \pm 0.18$	$0.73 \pm 0.22$	1626	28.74 $\pm$0.12
14	${\rm VB184}$	SB	K6	04 35 59.6	+16 32 29	7	2	129	$-0.38 \pm 0.13$	$0.55 \pm 0.22$	2321	28.28 $\pm$0.09
14	${\rm VB101}$	SB1	F5	04 36 40.3	+15 52 11	6	40	128	$-0.20 \pm 0.10$	$0.04 \pm 0.16$	1219	28.93 $\pm$0.06
14	${\rm LP415-266}$			04 37 31.5	+16 45 48	17	27	33	$-0.52 \pm 0.18$	$0.52 \pm 0.37$	1896	28.45 $\pm$0.13
14	${\rm LP415-171}$			04 38 30.3	+17 02 32	17	48	12	$-0.41 \pm 0.23$	$0.36 \pm 0.57$	1425	28.66 $\pm$0.16
16	${\rm VA382}$		M3	04 26 04.5	+17 07 11	7	37	68	$0.01 \pm 0.12$	$-0.03 \pm 0.16$	1845	29.07 $\pm$0.07
16	${\rm VB63}$	SB	G2	04 26 24.7	+16 51 14	2	31	441	$-0.22 \pm 0.06$	$-0.18 \pm 0.10$	2029	29.11 $\pm$0.04
16	${\rm VB64}$		G4	04 26 40.1	+16 44 50	1	30	187	$-0.43 \pm 0.08$	$-0.21 \pm 0.16$	2133	29.06 $\pm$0.05
16	${\rm RE240 A + B}$	VB		04 27 10.6	+16 26 01	62	37	9	$-0.49 \pm 0.29$	$-0.11 \pm 0.64$	1960	27.97 $\pm$0.22
16	${\rm VB189}$		K9	04 28 12.1	+16 28 26	23	30	8	$-0.58 \pm 0.45$	<0.03	1841	27.96 $\pm$0.45
16	${\rm VA486 +B}$	VB	M2	04 28 27.8	+17 41 33	16	43	297	$-0.26 \pm 0.07$	$0.27 \pm 0.11$	1756	29.14 $\pm$0.04
16	${\rm VA490}$		A3	04 28 39.5	+16 58 13	4	2	357	$-0.98 \pm 0.02$	<-0.42	2760	28.49 $\pm$0.05
16	${\rm VB73}$		G1	04 28 48.5	+17 17 04	4	19	224	$-0.34 \pm 0.09$	$-0.42 \pm 0.16$	2019	29.02 $\pm$0.06
16	${\rm VB75}$	SB	F8	04 28 59.3	+16 09 53	21	48	61	$-0.25 \pm 0.10$	$-0.06 \pm 0.17$	1628	29.02 $\pm$0.06
16	${\rm VB77}$	SB1	F7	04 29 21.0	+17 32 32	11	36	433	$-0.36 \pm 0.06$	$-0.05 \pm 0.11$	1985	29.07 $\pm$0.04
16	${\rm VA559}$		M2	04 29 55.8	+16 54 59	9	19	135	$0.06 \pm 0.12$	$-0.26 \pm 0.16$	1863	28.98 $\pm$0.07
16	${\rm VB180}$		K1	04 29 58.6	+16 40 29	14	26	120	$-0.47 \pm 0.10$	$-0.46 \pm 0.19$	2193	28.71 $\pm$0.07
16	${\rm VA575}$		M4	04 30 25.0	+17 30 21	27	41	24	$-0.35 \pm 0.21$	$-0.39 \pm 0.38$	1905	28.70 $\pm$0.13
17	${\rm V471Tau}$		K1	03 50 25.4	+17 14 41	16	40	14370	$-0.78 \pm 0.00$	$0.11 \pm 0.02$	18824	30.38 $\pm$0.00
17	${\rm VB6}$		F2	03 53 09.8	+17 19 50	11	19	1607	$-0.19 \pm 0.03$	$-0.25 \pm 0.05$	20683	28.83 $\pm$0.02
18F	${\rm V471Tau}$		K1	03 50 24.4	+17 15 02	14	0	22707	$-0.70 \pm 0.01$	$0.03 \pm 0.04$	3733	29.98 $\pm$0.04
18	${\rm VB6}$		F2	03 53 09.0	+17 19 40	10	39	68	$-0.18 \pm 0.12$	$-0.09 \pm 0.18$	2737	28.79 $\pm$0.07
20	${\rm VA122}$		M5	04 17 58.3	+14 33 00	44	48	17	$0.04 \pm 0.21$	$0.05 \pm 0.24$	5961	28.49 $\pm$0.13
20	${\rm VB30}$	SB1	A9	04 19 58.1	+14 02 33	28	43	432	$-0.34 \pm 0.05$	$-0.05 \pm 0.09$	7038	28.78 $\pm$0.03
20	${\rm VA203}$		M5	04 20 56.3	+14 51 39	8	10	46	$-0.03 \pm 0.18$	$-0.35 \pm 0.23$	10766	27.91 $\pm$0.10
20	${\rm VB37}$		F4	04 21 34.8	+14 24 36	1	18	2134	$-0.17 \pm 0.04$	$-0.32 \pm 0.05$	7608	29.37 $\pm$0.02
20	${\rm VA216}$		K3	04 21 35.1	+14 41 46	4	5	120	$-0.33 \pm 0.12$	$-0.18 \pm 0.20$	10651	28.07 $\pm$0.07
20	${\rm VB38}$	SB1	F1	04 22 03.9	+14 04 38	8	39	185	$-0.52 \pm 0.07$	$-0.07 \pm 0.16$	7192	28.44 $\pm$0.04
20	${\rm VB40}$	SB	F9	04 22 44.1	+15 03 23	1	30	3988	$-0.25 \pm 0.02$	$-0.03 \pm 0.04$	7257	29.35 $\pm$0.01
20	${\rm VA275}$		M5	04 23 23.8	+14 25 30	12	35	123	$-0.37 \pm 0.09$	$-0.05 \pm 0.17$	7952	28.59 $\pm$0.06
20	${\rm VB46}$		K1	04 23 31.4	+14 39 47	30	33	76	$-0.59 \pm 0.10$	$0.16 \pm 0.28$	6714	28.43 $\pm$0.07
20	${\rm VA288}$	SB2	M4	04 23 49.8	+14 55 21	6	39	1009	$-0.27 \pm 0.04$	$0.07 \pm 0.06$	7704	29.02 $\pm$0.02
20F	${\rm VB50}$	SB?	G1	04 24 12.3	+14 45 48	18	0	4852	$-0.23 \pm 0.02$	$-0.01 \pm 0.04$	6550	29.51 $\pm$0.11
21	${\rm VA135}$		K5	04 18 22.0	+17 25 02	17	41	1090	$-0.30 \pm 0.03$	$-0.06 \pm 0.05$	11667	29.39 $\pm$0.02
21	${\rm VB27}$		G7	04 19 07.3	+17 31 58	30	30	570	$-0.42 \pm 0.05$	$-0.25 \pm 0.10$	9717	28.91 $\pm$0.03
21	${\rm VA213}$		M4	04 21 37.5	+16 53 55	35	38	108	$-0.28 \pm 0.09$	$-0.06 \pm 0.15$	12031	28.59 $\pm$0.05
21	${\rm VB39}$	SB1	G5	04 22 45.7	+16 47 40	21	49	349	$-0.38 \pm 0.04$	$-0.11 \pm 0.09$	11161	28.61 $\pm$0.03
21	${\rm VB41}$	SB	K3	04 22 56.9	+17 32 36	11	24	173	$-0.40 \pm 0.08$	$0.07 \pm 0.16$	9432	28.27 $\pm$0.05
22	${\rm VB77}$	SB1	F7	04 29 21.3	+17 32 52	14	45	1320	$-0.24 \pm 0.02$	$-0.15 \pm 0.04$	11436	29.16 $\pm$0.01
22	${\rm VB78}$		F5	04 29 28.9	+17 51 59	23	48	400	$-0.49 \pm 0.04$	$-0.12 \pm 0.09$	11821	29.08 $\pm$0.02
22	${\rm VA575}$		M4	04 30 24.1	+17 30 06	7	30	316	$-0.19 \pm 0.06$	$-0.13 \pm 0.09$	14379	28.76 $\pm$0.03
22	${\rm VA622}$		M1	04 31 28.6	+17 42 59	9	18	51	$-0.63 \pm 0.12$	$0.45 \pm 0.37$	12939	27.81 $\pm$0.10
22	${\rm VA627}$	SB1	K4	04 31 37.2	+17 42 37	4	16	1949	$-0.33 \pm 0.03$	$-0.01 \pm 0.06$	15652	28.61 $\pm$0.02
22	${\rm VA657}$		M4	04 32 07.9	+17 39 55	2	9	203	$-0.17 \pm 0.09$	$0.07 \pm 0.13$	19352	28.18 $\pm$0.05
22	${\rm VA673}$	SB	F0	04 32 23.6	+17 45 06	2	13	1808	$-0.23 \pm 0.04$	$-0.05 \pm 0.06$	18386	28.59 $\pm$0.02
22	${\rm VA674}$		M4	04 32 29.0	+17 54 20	4	22	344	$-0.21 \pm 0.06$	$0.09 \pm 0.10$	12205	28.67 $\pm$0.04
22	${\rm LH992}$			04 32 50.4	+17 30 10	15	4	7	$-0.24 \pm 0.35$	$0.58 \pm 0.57$	20190	27.22 $\pm$0.26
22	${\rm VB93}$		K2	04 33 41.1	+16 47 02	89	48	16	$-0.05 \pm 0.13$	$0.17 \pm 0.17$	10783	28.67 $\pm$0.07
23	${\rm H495}$		M4	04 30 42.5	+14 39 18	24	27	13	$-0.86 \pm 0.22$	$0.76 \pm 1.97$	11190	27.63 $\pm$0.23
23	${\rm VB96}$	SB	K1	04 33 58.9	+15 09 55	10	34	604	$-0.33 \pm 0.04$	$-0.15 \pm 0.08$	10947	28.64 $\pm$0.03
25F	${\rm VA677}$	SB2	K5	04 32 25.6	+13 06 46	1	0	2690	$-0.11 \pm 0.02$	$0.05 \pm 0.04$	7028	29.70 $\pm$0.10
26F	${\rm LP357-4}$		M5	03 49 43.1	+24 18 57	13	0	16804	$0.52 \pm 0.07$	$0.11 \pm 0.08$	23027	29.64 $\pm$0.09
26	${\rm VB170}$		K5	03 51 02.5	+23 54 10	8	30	178	$-0.37 \pm 0.08$	$-0.28 \pm 0.15$	17806	28.30 $\pm$0.04
28	${\rm L40}$		M2	04 25 13.1	+18 59 43	80	49	32	$0.23 \pm 0.19$	$-0.10 \pm 0.20$	807	29.22 $\pm$0.10
28	${\rm VB58}$	SB	G5	04 25 52.7	+18 51 44	14	43	117	$-0.36 \pm 0.10$	$-0.43 \pm 0.19$	922	28.93 $\pm$0.06
28	${\rm LP415-108}$			04 27 36.2	+19 26 42	3	21	46	$-0.28 \pm 0.20$	$-0.45 \pm 0.31$	1018	28.67 $\pm$0.13
28	${\rm L57}$	SB1	K4	04 27 58.1	+18 30 18	20	41	38	$-0.28 \pm 0.17$	$-0.30 \pm 0.27$	983	28.63 $\pm$0.11
28	${\rm L72}$	SB?	M4	04 27 59.7	+18 45 39	10	26	95	$-0.21 \pm 0.13$	$-0.06 \pm 0.22$	1207	28.69 $\pm$0.08
28	${\rm VB70}$		K4	04 28 37.2	+19 10 50	2	2	29	$-0.16 \pm 0.28$	$-0.44 \pm 0.41$	1665	28.24 $\pm$0.18
28	${\rm VB69}$	SB1	G8	04 28 37.8	+19 44 18	11	33	55	$0.03 \pm 0.16$	$-0.22 \pm 0.21$	1030	28.82 $\pm$0.09
28	${\rm L71}$	SB	M3	04 29 03.1	+18 40 27	30	30	68	$0.12 \pm 0.16$	$-0.22 \pm 0.19$	874	28.86 $\pm$0.08
28	${\rm VB81}$		F6	04 30 17.8	+19 50 19	7	46	104	$-0.08 \pm 0.11$	$0.05 \pm 0.18$	944	29.44 $\pm$0.06
29	${\rm LP358-739}$			04 35 13.3	+22 59 30	11	10	18	$0.22 \pm 0.35$	$0.02 \pm 0.44$	605	28.68 $\pm$0.20
29	${\rm VB100}$		F3	04 36 26.8	+23 20 07	37	27	25	$-0.97 \pm 0.12$	>-0.53	487	28.45 $\pm$0.18
29	${\rm VB105}$		G0	04 38 55.2	+23 09 40	72	44	18	$-0.70 \pm 0.21$	>-0.26	331	29.06 $\pm$0.17
32	${\rm VB25}$		K3	04 18 17.5	+16 05 36	28	35	41	$-0.53 \pm 0.14$	$0.11 \pm 0.33$	2971	28.56 $\pm$0.10
32	${\rm VB28}$	SB1	K3	04 19 47.5	+15 37 41	5	2	8648	$0.13 \pm 0.03$	$-0.25 \pm 0.03$	4163	29.63 $\pm$0.01
33	${\rm VA115}$		M1	04 17 45.0	+13 40 25	56	46	20	$-0.09 \pm 0.16$	$-0.06 \pm 0.19$	14857	28.29 $\pm$0.10
33	${\rm VA146}$		M0	04 18 49.0	+13 22 01	31	42	16	$0.12 \pm 0.12$	$0.62 \pm 0.11$	12793	28.54 $\pm$0.07
33	${\rm VB30}$	SB1	A9	04 19 57.6	+14 02 33	26	16	5381	$-0.26 \pm 0.02$	$0.06 \pm 0.04$	18728	28.92 $\pm$0.01
33	${\rm VB34}$	SB2	F6	04 20 52.8	+13 51 50	4	2	8279	$-0.47 \pm 0.02$	$-0.31 \pm 0.04$	23520	28.85 $\pm$0.01
33	${\rm VB37}$		F4	04 21 34.7	+14 24 37	2	34	2748	$-0.18 \pm 0.02$	$-0.20 \pm 0.04$	16278	29.44 $\pm$0.01
33	${\rm VB38}$	SB1	F1	04 22 04.5	+14 04 48	20	22	549	$-0.45 \pm 0.05$	$-0.31 \pm 0.09$	14273	28.35 $\pm$0.03
33	${\rm VA294}$		K7	04 23 52.0	+14 03 36	42	45	32	$-0.56 \pm 0.11$	$0.27 \pm 0.28$	13151	28.22 $\pm$0.09
34	${\rm VA282}$		M5	04 23 42.1	+15 52 45	11	28	15	$-0.15 \pm 0.22$	$0.01 \pm 0.30$	9876	28.01 $\pm$0.14
34	${\rm VB49}$		G0	04 24 12.8	+16 23 01	16	33	1040	$-0.22 \pm 0.04$	$-0.11 \pm 0.06$	11647	29.16 $\pm$0.02
34	${\rm VA321}$		M4	04 24 29.1	+15 52 51	19	17	34	$-0.38 \pm 0.15$	$0.00 \pm 0.28$	14596	27.81 $\pm$0.11
34F	${\rm VA334}$		M0	04 24 48.0	+15 52 27	3	0	9289	$-0.17 \pm 0.02$	$0.08 \pm 0.03$	15105	29.31 $\pm$0.07
34	${\rm VA352}$		M5	04 25 16.2	+16 18 12	2	21	107	$-0.18 \pm 0.10$	$-0.09 \pm 0.16$	10450	28.39 $\pm$0.06
34	${\rm VB57}$	SB	F7	04 25 37.2	+15 56 28	2	2	14895	$-0.16 \pm 0.02$	$-0.22 \pm 0.03$	17384	29.29 $\pm$0.01
34	${\rm VB59}$	SB	F9	04 26 05.8	+15 31 27	1	26	5027	$-0.18 \pm 0.02$	$-0.06 \pm 0.03$	13005	29.23 $\pm$0.01
34F	${\rm VB141}$	var	A8	04 26 20.6	+15 37 08	3	0	18333	$-0.09 \pm 0.01$	$0.01 \pm 0.02$	11477	30.21 $\pm$0.03
34	${\rm RE240 A + B}$	VB		04 27 02.8	+16 25 33	53	35	37	$0.28 \pm 0.25$	$0.00 \pm 0.20$	9027	27.99 $\pm$0.13
34	${\rm VB65}$		F9	04 27 37.5	+15 36 01	46	35	368	$-0.48 \pm 0.04$	$-0.17 \pm 0.09$	10045	28.92 $\pm$0.03
34	${\rm VB189}$		K9	04 28 13.9	+16 28 25	47	49	9	<0.41	$0.00 \pm 0.00$	8655	28.34 $\pm$0.22
34	${\rm VB71}$	SB	K3	04 28 34.0	+15 57 30	17	42	10940	$0.05 \pm 0.01$	$-0.08 \pm 0.02$	8792	30.04 $\pm$0.01
35	${\rm VB190}$	SB	K8	04 28 50.5	+16 17 23	2	43	158	$-0.14 \pm 0.09$	$-0.04 \pm 0.15$	1226	29.06 $\pm$0.05
35	${\rm VB85}$	var	F5	04 30 46.7	+16 09 01	5	32	545	$-0.24 \pm 0.06$	$-0.12 \pm 0.11$	1424	29.42 $\pm$0.04
36F	${\rm VA677}$	SB2	K5	04 32 25.4	+13 06 37	10	0	1782	$-0.14 \pm 0.03$	$-0.03 \pm 0.04$	10820	29.62 $\pm$0.10
37	${\rm VA677}$	SB2	K5	04 32 25.5	+13 06 48	0	45	2975	$-0.09 \pm 0.02$	$-0.06 \pm 0.04$	8945	29.55 $\pm$0.01
40	${\rm LP415-157}$			04 35 50.3	+19 47 18	35	47	95	$-0.22 \pm 0.08$	$0.04 \pm 0.13$	15416	28.61 $\pm$0.05
40	${\rm L86}$		M3	04 36 03.7	+18 53 16	5	34	1156	$-0.18 \pm 0.03$	$0.00 \pm 0.05$	17699	29.06 $\pm$0.02
40	${\rm RE355}$		M6	04 36 29.5	+19 05 23	17	23	135	$-0.15 \pm 0.09$	$0.02 \pm 0.14$	12730	28.39 $\pm$0.05
40	${\rm L87}$		M3	04 36 39.1	+18 36 43	14	40	20	$-0.50 \pm 0.19$	$-0.62 \pm 0.46$	13712	27.93 $\pm$0.15
40	${\rm LP415-292}$		M3	04 38 54.5	+19 10 56	2	11	2667	$-0.11 \pm 0.03$	$-0.10 \pm 0.05$	23238	28.92 $\pm$0.02
40	${\rm RE391}$		M8	04 39 52.9	+19 39 28	20	37	102	$-0.36 \pm 0.08$	$0.31 \pm 0.15$	17756	28.38 $\pm$0.05
40	${\rm J310}$		M1	04 40 13.9	+19 16 54	23	30	35	$-0.39 \pm 0.14$	$0.23 \pm 0.26$	15839	28.01 $\pm$0.10
41	${\rm BD22^\circ669}$		K3	04 18 10.6	+23 17 05	19	2	15615	$-0.09 \pm 0.02$	$-0.01 \pm 0.03$	4193	30.10 $\pm$0.01
42	${\rm L18}$		K2	04 08 38.6	+23 45 39	45	46	26	$-0.34 \pm 0.19$	$-0.97 \pm 0.39$	1965	28.68 $\pm$0.12
42	${\rm L20}$		K4	04 11 56.0	+23 38 12	3	2	12822	$-0.04 \pm 0.02$	$-0.04 \pm 0.03$	3584	29.88 $\pm$0.01
43	${\rm VA404}$	SB	K8	04 26 41.7	+12 41 20	16	37	323	$-0.10 \pm 0.06$	$-0.03 \pm 0.08$	5425	28.67 $\pm$0.03
43	${\rm VA407}$		K5	04 26 55.4	+13 08 39	28	27	24	$-0.31 \pm 0.18$	$-0.70 \pm 0.27$	5749	28.28 $\pm$0.12
43	${\rm H430}$		M1	04 28 17.8	+13 49 49	71	47	28	$-0.35 \pm 0.22$	$-0.81 \pm 0.40$	3657	28.54 $\pm$0.16
43	${\rm VB84}$		A8	04 30 34.2	+13 43 44	44	48	140	$-0.08 \pm 0.08$	$0.19 \pm 0.11$	3510	29.24 $\pm$0.04
44	${\rm VB178}$	SB?	K1	04 28 07.7	+13 51 29	59	36	11	$0.46 \pm 0.37$	$-0.33 \pm 0.27$	3050	28.35 $\pm$0.19
44	${\rm VB84}$		A8	04 30 37.3	+13 43 34	9	2	784	$-0.21 \pm 0.06$	$-0.11 \pm 0.09$	4200	29.13 $\pm$0.03
44	${\rm VB88}$		F9	04 31 29.5	+13 54 17	5	17	570	$-0.05 \pm 0.06$	$-0.23 \pm 0.09$	3471	29.36 $\pm$0.03
44F	${\rm VA677}$	SB2	K5	04 32 24.9	+13 07 03	18	0	372	$-0.12 \pm 0.07$	$-0.12 \pm 0.11$	2502	29.55 $\pm$0.07
46	${\rm RE367}$		K9	04 37 14.9	+12 05 42	84	47	15	$0.60 \pm 0.64$	$-0.62 \pm 0.31$	5156	28.24 $\pm$0.40
47	${\rm RE367}$		K9	04 37 06.9	+12 06 14	43	48	35	$-0.13 \pm 0.16$	$-0.04 \pm 0.24$	2439	28.74 $\pm$0.10
48	${\rm VA83}$		M1	04 16 01.8	+16 59 00	8	14	705	$-0.01 \pm 0.07$	$0.17 \pm 0.09$	4102	29.13 $\pm$0.04
48	${\rm RE126}$		M9	04 16 13.1	+16 47 44	5	8	17	$-0.02 \pm 0.33$	$-0.11 \pm 0.40$	4067	27.90 $\pm$0.20
48	${\rm VA94}$		M3	04 16 43.2	+16 49 20	2	2	117	$-0.09 \pm 0.15$	$-0.08 \pm 0.21$	4622	28.40 $\pm$0.08
48	${\rm VA119}$		M3	04 17 55.0	+16 32 38	4	23	189	$-0.12 \pm 0.10$	$-0.22 \pm 0.14$	2849	28.94 $\pm$0.05
48	${\rm VB25}$		K3	04 18 18.8	+16 06 05	46	48	33	$-0.28 \pm 0.15$	$0.15 \pm 0.23$	2595	28.80 $\pm$0.10
	${\rm VA131}$		M5			87						28.74 $\pm$0.10
48	${\rm VA135}$		K5	04 18 23.2	+17 25 15	21	42	293	$-0.21 \pm 0.07$	$0.12 \pm 0.12$	3081	29.33 $\pm$0.04
48	${\rm VB29}$	VB	F9	04 19 54.5	+16 31 13	9	48	324	$-0.35 \pm 0.06$	$0.02 \pm 0.11$	2731	28.98 $\pm$0.04
49	${\rm VA407}$		K5	04 26 57.5	+13 08 40	52	46	9	$-0.09 \pm 0.27$	$0.07 \pm 0.31$	4015	28.42 $\pm$0.17
49	${\rm VA432}$		M4	04 27 23.5	+14 07 06	6	23	36	$-0.10 \pm 0.17$	$0.03 \pm 0.24$	5420	28.29 $\pm$0.10
49	${\rm VB177}$	SB	K4	04 27 23.9	+14 15 47	20	30	101	$-0.17 \pm 0.10$	$-0.24 \pm 0.16$	6201	28.32 $\pm$0.06
49	${\rm VB179}$		K2	04 27 49.1	+14 25 01	32	36	59	$-0.51 \pm 0.11$	$-0.16 \pm 0.26$	4871	28.72 $\pm$0.08
49	${\rm VB178}$	SB?	K1	04 28 04.5	+13 52 08	3	6	547	$-0.29 \pm 0.07$	$-0.46 \pm 0.11$	7561	28.39 $\pm$0.04
49	${\rm H430}$		M1	04 28 22.2	+13 49 21	1	2	201	$0.01 \pm 0.11$	$-0.04 \pm 0.15$	8036	28.43 $\pm$0.06
49	${\rm RE287}$		K3	04 30 27.3	+13 36 56	30	31	11	$0.75 \pm 0.54$	$0.78 \pm 0.25$	4683	28.13 $\pm$0.27
49	${\rm VB84}$		A8	04 30 36.7	+13 43 28	5	32	961	$-0.21 \pm 0.04$	$-0.03 \pm 0.07$	5878	29.28 $\pm$0.02
49	${\rm VB88}$		F9	04 31 29.1	+13 54 10	4	44	209	$-0.23 \pm 0.07$	$-0.11 \pm 0.11$	4692	29.16 $\pm$0.04
53	${\rm VB117}$	SB	K4	04 49 13.4	+24 48 08	16	22	4743	$-0.12 \pm 0.03$	$0.03 \pm 0.04$	6703	29.50 $\pm$0.01
54	${\rm VB117}$	SB	K4	04 49 12.4	+24 48 28	14	47	1392	$-0.12 \pm 0.03$	$-0.03 \pm 0.05$	6032	29.46 $\pm$0.02
59F	${\rm VB169}$		A7	06 02 23.2	+09 38 52	4	0	5348	$-0.12 \pm 0.03$	$-0.10 \pm 0.05$	10630	29.34 $\pm$0.11
64	${\rm VB79}$		K0	04 29 31.5	+17 52 44	52	39	133	$-0.49 \pm 0.08$	$-0.16 \pm 0.18$	2827	28.95 $\pm$0.05
64F	${\rm VA673}$	SB	F0	04 32 23.5	+17 45 10	6	0	9268	$-0.13 \pm 0.04$	$0.09 \pm 0.06$	3212	29.60 $\pm$0.03
65	${\rm RE202}$		M8	04 24 32.1	+18 59 05	25	37	8	$-0.18 \pm 0.35$	$-0.02 \pm 0.51$	1888	28.26 $\pm$0.26
70	${\rm VB162}$	SB2	G7	04 15 41.8	+20 49 08	9	29	489	$-0.41 \pm 0.06$	$0.24 \pm 0.11$	3227	28.92 $\pm$0.04
70	${\rm VB26}$		G8	04 18 57.5	+19 54 39	16	44	47	$-0.37 \pm 0.13$	$0.04 \pm 0.25$	2548	28.68 $\pm$0.09
71	${\rm LP357-309}$			04 12 51.8	+22 24 21	79	46	12	$0.26 \pm 0.41$	$-0.88 \pm 0.38$	1050	28.55 $\pm$0.27
72	${\rm VB119}$	SB1	F9	04 50 24.0	+17 12 07	2	23	493	$-0.19 \pm 0.08$	$-0.14 \pm 0.13$	716	29.23 $\pm$0.05
72	${\rm LP416-94}$	SB	K6	04 51 49.0	+17 16 41	18	14	13	$-0.57 \pm 0.29$	<-0.75	1796	27.62 $\pm$0.26
73F	${\rm VB190}$	SB	K8	04 28 50.2	+16 17 11	11	0	918	$-0.09 \pm 0.03$	$0.07 \pm 0.04$	10382	29.22 $\pm$0.20
73F	${\rm VB85}$	var	F5	04 30 46.5	+16 08 55	4	0	3507	$-0.15 \pm 0.03$	$-0.08 \pm 0.04$	11914	29.50 $\pm$0.06
74F	${\rm VB45}$	SB1	F0	04 23 26.1	+16 46 53	23	0	187	$0.04 \pm 0.17$	$-0.02 \pm 0.22$	8337	28.59 $\pm$0.40
74	${\rm VB47}$		A5	04 24 06.4	+17 25 18	81	48	30	$0.90 \pm 0.24$	$0.48 \pm 0.12$	9152	28.57 $\pm$0.10
74	${\rm VB49}$		G0	04 24 14.0	+16 23 13	33	42	883	$-0.21 \pm 0.04$	$-0.16 \pm 0.07$	9553	29.17 $\pm$0.02
74	${\rm VB51}$		F5	04 24 22.3	+17 04 40	4	33	505	$-0.45 \pm 0.05$	$-0.45 \pm 0.10$	11405	28.92 $\pm$0.03
74	${\rm VB52}$	SB?	G1	04 24 28.1	+16 53 14	4	29	1902	$-0.21 \pm 0.03$	$-0.18 \pm 0.05$	11501	28.94 $\pm$0.02
74	${\rm VB175}$		K4	04 25 00.3	+16 59 01	7	22	127	$-0.23 \pm 0.10$	$-0.13 \pm 0.17$	11438	28.29 $\pm$0.06
74	${\rm VA351}$	SB3	M4	04 25 13.8	+17 16 11	7	30	3790	$-0.14 \pm 0.02$	$0.02 \pm 0.04$	11683	29.00 $\pm$0.01
74	${\rm VA352}$		M5	04 25 18.2	+16 17 27	51	37	45	$-0.20 \pm 0.17$	$0.12 \pm 0.25$	9877	28.22 $\pm$0.10
74	${\rm LH994}$			04 25 25.1	+17 34 04	74	45	15	$0.58 \pm 0.38$	$0.22 \pm 0.23$	9549	28.23 $\pm$0.20
74	${\rm VA382}$		M3	04 26 04.2	+17 07 11	5	17	628	$-0.09 \pm 0.06$	$0.11 \pm 0.09$	12637	28.70 $\pm$0.03
74	${\rm RE230}$		M9	04 26 18.4	+17 02 59	8	12	18	$-0.09 \pm 0.26$	$-0.20 \pm 0.34$	14627	27.54 $\pm$0.16
74	${\rm VB63}$	SB	G2	04 26 24.5	+16 51 13	1	2	8156	$-0.15 \pm 0.02$	$-0.18 \pm 0.03$	16104	29.04 $\pm$0.01
74	${\rm VB64}$		G4	04 26 40.0	+16 44 50	1	6	4023	$-0.20 \pm 0.03$	$-0.12 \pm 0.05$	14345	29.14 $\pm$0.02
74	${\rm RE240 A + B}$	VB		04 27 07.5	+16 26 18	35	26	17	$-0.15 \pm 0.24$	$-0.33 \pm 0.33$	11244	27.55 $\pm$0.15
74	${\rm VA420}$		M2	04 27 16.7	+17 14 46	14	26	13	$-0.67 \pm 0.20$	$-0.27 \pm 0.64$	11502	27.62 $\pm$0.17
74	${\rm VB189}$		K9	04 28 10.3	+16 28 50	34	32	24	$-0.20 \pm 0.17$	$-0.42 \pm 0.25$	11240	28.10 $\pm$0.11
74	${\rm VA490}$		A3	04 28 40.0	+16 58 20	13	32	541	<-0.84	$0.00 \pm 0.00$	8789	29.08 $\pm$0.12
74	${\rm VB73}$		G1	04 28 48.5	+17 17 09	2	42	1373	$-0.15 \pm 0.03$	$0.01 \pm 0.05$	10227	29.35 $\pm$0.02
74	${\rm VB190}$	SB	K8	04 28 52.3	+16 17 36	28	48	1244	$-0.16 \pm 0.03$	$0.00 \pm 0.05$	9073	29.14 $\pm$0.02
74	${\rm VA559}$		M2	04 29 54.5	+16 54 28	27	49	100	$-0.37 \pm 0.09$	$0.15 \pm 0.17$	9274	28.71 $\pm$0.05
75	${\rm VB23}$	SB2	G6	04 18 02.4	+18 14 50	35	49	164	$-0.45 \pm 0.08$	$-0.08 \pm 0.16$	2597	28.89 $\pm$0.05
80	${\rm VB24}$	SB	A9	04 18 23.6	+21 34 52	14	29	1335	$-0.23 \pm 0.04$	$-0.17 \pm 0.07$	5613	29.15 $\pm$0.02
80	${\rm L44}$		M3	04 19 32.6	+21 45 45	46	37	1411	$-0.07 \pm 0.04$	$0.06 \pm 0.06$	5252	29.49 $\pm$0.02
80	${\rm LP414-167}$		M6	04 20 31.4	+21 22 55	27	21	51	$-0.03 \pm 0.17$	$-0.24 \pm 0.22$	4053	28.42 $\pm$0.09
80	${\rm VB35}$		F5	04 21 31.8	+21 02 19	4	31	882	$-0.27 \pm 0.05$	$-0.28 \pm 0.08$	5563	29.26 $\pm$0.03
82	${\rm LP358-352}$			04 30 17.0	+26 23 36	70	44	74	$-0.57 \pm 0.27$	$0.20 \pm 0.66$	4157	28.04 $\pm$0.24
84	${\rm LP358-134}$			04 21 48.6	+24 13 57	68	47	13	$-0.54 \pm 0.20$	$0.19 \pm 0.42$	3555	28.37 $\pm$0.14
84	${\rm LP358-534}$		M4	04 21 56.0	+23 25 00	6	15	212	$0.01 \pm 0.11$	$-0.13 \pm 0.15$	5452	28.60 $\pm$0.06
84	${\rm LP358-724}$		M4	04 25 19.2	+23 03 57	24	40	12	$-0.35 \pm 0.23$	$-0.68 \pm 0.52$	4063	28.26 $\pm$0.16
90	${\rm VA638 + LP415-175}$	VB	M1	04 31 46.8	+15 38 01	35	40	35	$-0.15 \pm 0.14$	$-0.32 \pm 0.20$	13356	27.98 $\pm$0.08
90	${\rm VB89}$	SB1	F2	04 31 52.1	+15 51 59	53	44	193	$-0.70 \pm 0.06$	$-0.65 \pm 0.26$	12334	28.16 $\pm$0.05
90	${\rm VB91 +B}$	VB	K1	04 32 51.7	+16 00 54	40	38	279	$-0.46 \pm 0.05$	$-0.25 \pm 0.12$	13142	28.39 $\pm$0.04
90	${\rm VB92}$		G8	04 32 59.4	+15 49 05	3	29	505	$-0.40 \pm 0.05$	$-0.35 \pm 0.09$	15171	28.71 $\pm$0.03
90	${\rm VB95}$	SB	A8	04 33 54.0	+14 50 59	55	40	25	$-0.25 \pm 0.13$	$0.51 \pm 0.17$	12852	27.96 $\pm$0.09
90	${\rm VB96}$	SB	K1	04 33 59.2	+15 09 50	11	22	1249	$-0.28 \pm 0.04$	$-0.14 \pm 0.07$	11092	28.60 $\pm$0.02
90	${\rm VB183}$		K2	04 34 33.1	+15 49 50	16	19	428	$-0.31 \pm 0.06$	$-0.13 \pm 0.11$	13466	28.55 $\pm$0.04
90	${\rm VB97}$		G2	04 34 35.7	+15 30 15	6	2	3491	$-0.25 \pm 0.03$	$-0.28 \pm 0.05$	19540	28.89 $\pm$0.02
90	${\rm VA763}$		M5	04 35 28.5	+15 23 51	7	15	243	$-0.20 \pm 0.08$	$0.05 \pm 0.13$	17162	28.25 $\pm$0.05
90	${\rm VB99}$		K1	04 36 05.2	+15 41 03	1	25	455	$-0.27 \pm 0.05$	$-0.10 \pm 0.09$	15732	28.63 $\pm$0.03
90	${\rm VB101}$	SB1	F5	04 36 41.3	+15 52 02	10	38	1794	$-0.23 \pm 0.03$	$-0.21 \pm 0.05$	12180	28.95 $\pm$0.02
90	${\rm VB102}$	SB	G2	04 37 31.6	+15 08 55	10	48	1151	$-0.18 \pm 0.03$	$-0.13 \pm 0.05$	10582	28.98 $\pm$0.02
91	${\rm VB18}$		G3	04 14 27.6	+12 26 10	5	2	3897	$-0.16 \pm 0.03$	$-0.34 \pm 0.04$	17523	29.02 $\pm$0.02
91	${\rm VA68}$		K6	04 14 51.1	+13 03 24	11	37	102	$-0.29 \pm 0.09$	$0.02 \pm 0.15$	12057	28.43 $\pm$0.05
95	${\rm LP301-63}$			03 53 37.4	+31 12 53	32	24	94	$-0.19 \pm 0.11$	$-0.29 \pm 0.17$	5958	28.55 $\pm$0.06
96	${\rm VB26}$		G8	04 19 00.5	+19 54 59	49	47	39	$-0.40 \pm 0.13$	$0.27 \pm 0.28$	2458	28.73 $\pm$0.09
96	${\rm VB31}$		F9	04 20 14.0	+19 13 59	15	47	592	$-0.11 \pm 0.06$	$0.09 \pm 0.09$	2618	29.43 $\pm$0.03
96	${\rm RE162}$		M7	04 21 39.2	+20 18 13	14	28	26	$0.01 \pm 0.20$	$0.04 \pm 0.27$	3674	28.39 $\pm$0.12
96	${\rm LP415-30}$		M5	04 22 40.2	+20 33 57	39	43	19	$-0.49 \pm 0.21$	$0.04 \pm 0.57$	2866	28.38 $\pm$0.16
96	${\rm VB43}$	SB1	K2	04 23 22.9	+19 39 37	7	18	163	$-0.32 \pm 0.10$	$-0.39 \pm 0.17$	3509	28.66 $\pm$0.06
97	${\rm VB90}$		F4	04 32 05.3	+05 24 34	8	16	303	$-0.40 \pm 0.08$	$-0.21 \pm 0.16$	1669	29.08 $\pm$0.05
100	${\rm VB90}$		F4	04 32 04.8	+05 24 37	1	15	416	$-0.10 \pm 0.09$	$-0.30 \pm 0.12$	1849	29.13 $\pm$0.05
101	${\rm VB90}$		F4	04 32 04.8	+05 24 44	7	15	614	$-0.29 \pm 0.07$	$-0.22 \pm 0.11$	2800	29.06 $\pm$0.04
102	${\rm VB90}$		F4	04 32 04.7	+05 24 37	2	16	352	$-0.38 \pm 0.08$	$-0.69 \pm 0.13$	1767	29.02 $\pm$0.05
103	${\rm VB90}$		F4	04 32 05.1	+05 24 38	4	17	416	$-0.13 \pm 0.08$	$-0.48 \pm 0.12$	1842	29.17 $\pm$0.05
111	${\rm VB19 +B}$	VB	F8	04 14 34.9	+10 42 16	14	22	6772	$-0.18 \pm 0.02$	$-0.17 \pm 0.03$	17520	29.16 $\pm$0.01
111	${\rm RE131}$		M5	04 16 35.0	+10 22 57	18	47	42	$0.07 \pm 0.15$	$0.01 \pm 0.16$	11934	28.48 $\pm$0.08
115	${\rm VA622}$		M1	04 31 29.0	+17 43 06	2	14	30	$-0.29 \pm 0.16$	$0.05 \pm 0.27$	7132	28.07 $\pm$0.10
115	${\rm VA673}$	SB	F0	04 32 23.7	+17 45 01	3	18	438	$-0.24 \pm 0.07$	$0.17 \pm 0.12$	5865	28.48 $\pm$0.04
8,9	${\rm LP357-4}$		M5	03 49 42.6	+24 19 13	10	40	386	$-0.27 \pm 0.05$	$-0.06 \pm 0.10$	8223	29.02 $\pm$0.03
11-13	${\rm LP357-4}$		M5	03 49 42.8	+24 17 53	70	47	371	$-0.03 \pm 0.03$	$0.12 \pm 0.04$	23316	29.23 $\pm$0.02
30,31	${\rm LP358-371}$			04 30 55.8	+24 50 07	11	27	23	$-0.30 \pm 0.19$	$-0.91 \pm 0.30$	5801	28.10 $\pm$0.13
30,31	${\rm L74}$	SB	M3	04 33 23.8	+23 59 38	12	33	845	$-0.17 \pm 0.05$	$-0.12 \pm 0.07$	5237	28.98 $\pm$0.03
38,39	${\rm VA83}$		M1	04 16 01.3	+16 58 54	6	20	195	$-0.25 \pm 0.08$	$-0.04 \pm 0.13$	15173	28.34 $\pm$0.05
38,39	${\rm RE126}$		M9	04 16 13.3	+16 47 49	2	12	117	$-0.20 \pm 0.11$	$-0.30 \pm 0.16$	23838	27.94 $\pm$0.07
38,39	${\rm VA94}$		M3	04 16 43.1	+16 49 20	1	19	224	$-0.41 \pm 0.07$	$-0.17 \pm 0.14$	16985	28.29 $\pm$0.05
38,39	${\rm VA96}$		M4	04 16 53.5	+16 21 04	24	27	10	$-0.96 \pm 0.17$	$-0.93 \pm 4.19$	19755	27.28 $\pm$0.22
38,39	${\rm VA119}$		M3	04 17 55.6	+16 32 44	12	35	896	$-0.17 \pm 0.04$	$-0.09 \pm 0.06$	18599	28.97 $\pm$0.02
46,47	${\rm LP475-141}$			04 37 14.8	+11 19 24	5	7	292	$0.11 \pm 0.09$	$0.02 \pm 0.11$	13838	28.39 $\pm$0.05
46,47	${\rm LP475-214}$			04 38 09.2	+11 19 03	4	6	169	$-0.36 \pm 0.10$	$-0.05 \pm 0.18$	13868	28.11 $\pm$0.06
25,36,37	${\rm VA537}$		M5	04 29 16.2	+12 21 30	7	31	249	$-0.34 \pm 0.06$	$-0.05 \pm 0.10$	26712	28.48 $\pm$0.04
25,36,37	${\rm LH81}$			04 30 10.0	+13 00 30	55	40	8	$-0.07 \pm 0.29$	$-0.11 \pm 0.32$	27933	27.85 $\pm$0.19
25,36,37	${\rm VA607}$		M3	04 30 57.5	+12 18 15	3	8	7029	$-0.14 \pm 0.02$	$-0.01 \pm 0.03$	40932	29.05 $\pm$0.01
25,36,37	${\rm RE297}$		K6	04 31 12.8	+12 28 42	5	5	130	$0.05 \pm 0.11$	$-0.14 \pm 0.13$	42338	27.86 $\pm$0.06
25,36,37	${\rm VA683}$		M8	04 32 45.7	+12 04 04	6	28	222	$-0.05 \pm 0.07$	$-0.17 \pm 0.09$	25937	28.50 $\pm$0.04
25,36,37	${\rm VA709}$		M4	04 33 26.2	+13 02 41	10	49	123	$-0.28 \pm 0.06$	$-0.27 \pm 0.11$	22782	28.74 $\pm$0.04
25,36,37	${\rm VA722}$		A3	04 33 46.0	+12 42 46	17	39	21	<0.34	>-0.99	28694	28.13 $\pm$0.17
65,66	${\rm VB53}$		F3	04 24 56.6	+19 02 34	7	34	324	$-0.32 \pm 0.07$	$-0.30 \pm 0.12$	2918	29.21 $\pm$0.04
65,66	${\rm L40}$		M2	04 25 14.5	+18 58 20	5	28	128	$-0.15 \pm 0.11$	$-0.16 \pm 0.16$	3261	28.81 $\pm$0.06
65,66	${\rm VB176}$		K3	04 25 42.1	+18 00 03	96	51	44	$0.10 \pm 0.12$	$-0.26 \pm 0.17$	2355	29.08 $\pm$0.07
65,66	${\rm VB58}$	SB	G5	04 25 51.6	+18 51 54	4	18	1106	$-0.25 \pm 0.05$	$-0.34 \pm 0.08$	2940	28.98 $\pm$0.03
65,66	${\rm LP415-875}$			04 26 23.6	+18 01 34	97	46	11	$0.34 \pm 0.25$	$0.05 \pm 0.25$	2495	28.72 $\pm$0.13
65,66	${\rm LP415-108}$			04 27 37.3	+19 27 25	42	41	23	$-0.20 \pm 0.18$	$-0.11 \pm 0.28$	2667	28.60 $\pm$0.11
65,66	${\rm L57}$	SB1	K4	04 27 58.5	+18 29 58	5	21	273	$-0.15 \pm 0.09$	$-0.14 \pm 0.14$	2903	28.65 $\pm$0.05
65,66	${\rm L72}$	SB?	M4	04 27 59.5	+18 45 38	8	12	431	$-0.16 \pm 0.08$	$0.14 \pm 0.13$	3583	28.60 $\pm$0.05
65,66	${\rm VB70}$		K4	04 28 37.3	+19 10 56	5	32	29	$-0.19 \pm 0.18$	$-0.13 \pm 0.27$	2705	28.52 $\pm$0.12
65,66	${\rm L71}$	SB	M3	04 29 01.5	+18 40 24	9	28	616	$-0.23 \pm 0.06$	$0.08 \pm 0.10$	3204	28.95 $\pm$0.03
67-69	${\rm VB26}$		G8	04 18 59.2	+19 54 36	21	48	28	$-0.22 \pm 0.18$	$-0.91 \pm 0.29$	2515	28.60 $\pm$0.11
67-69	${\rm GH7-163}$			04 19 04.7	+19 33 02	27	41	8	$-0.02 \pm 0.20$	$-0.11 \pm 0.26$	2831	28.57 $\pm$0.12
67-69	${\rm VB31}$		F9	04 20 13.0	+19 14 05	5	31	667	$-0.18 \pm 0.06$	$-0.14 \pm 0.09$	3292	29.29 $\pm$0.03
67-69	${\rm Bry262}$			04 21 48.2	+19 28 37	35	4	10	<-0.85	$0.00 \pm 0.00$	4428	27.46 $\pm$0.47
67-69	${\rm VB43}$	SB1	K2	04 23 22.6	+19 39 30	1	20	81	$-0.20 \pm 0.15$	$0.07 \pm 0.24$	2430	28.57 $\pm$0.09
75,76	${\rm VB32}$		F3	04 20 24.9	+18 44 30	4	25	2276	$-0.27 \pm 0.03$	$-0.13 \pm 0.05$	13940	29.19 $\pm$0.02
75,76	${\rm LP415-543}$			04 20 27.3	+18 54 10	20	33	50	$-0.15 \pm 0.13$	$0.36 \pm 0.18$	13764	28.26 $\pm$0.07
75,76	${\rm VB36}$		F5	04 21 32.1	+18 25 06	3	2	3026	$-0.25 \pm 0.03$	$-0.42 \pm 0.05$	19404	29.02 $\pm$0.02
75,76	${\rm VA242}$		M3	04 22 39.4	+18 16 14	5	17	17	$-0.65 \pm 0.20$	$0.03 \pm 0.62$	13427	27.53 $\pm$0.17
75,76	${\rm VB174}$		K4	04 24 16.7	+18 00 55	43	45	40	$-0.42 \pm 0.13$	$0.13 \pm 0.26$	11467	28.43 $\pm$0.09
92,93	${\rm VB10}$		G1	04 06 16.4	+15 41 54	4	1	573	$-0.09 \pm 0.08$	$-0.20 \pm 0.12$	2348	29.13 $\pm$0.04
92,93	${\rm L15}$		K5	04 07 03.6	+15 20 10	37	24	11	$-0.21 \pm 0.30$	$0.11 \pm 0.43$	1915	28.11 $\pm$0.21
92,93	${\rm VB11 +B}$	VB	F4	04 07 42.0	+15 09 44	1	38	113	$-0.40 \pm 0.10$	$-0.49 \pm 0.19$	1681	28.74 $\pm$0.07
35,73	${\rm VB65}$		F9	04 27 35.9	+15 35 22	1	36	669	$-0.33 \pm 0.04$	$-0.35 \pm 0.07$	13261	29.05 $\pm$0.02
35,73	${\rm VB71}$	SB	K3	04 28 34.1	+15 57 44	6	29	12304	$0.04 \pm 0.01$	$-0.15 \pm 0.01$	14275	29.90 $\pm$0.01
35,73	${\rm VB72}$	SB1	A6	04 28 39.3	+15 52 32	17	25	141	$-0.28 \pm 0.08$	$0.00 \pm 0.14$	12270	28.19 $\pm$0.05
35,73	${\rm VB75}$	SB	F8	04 28 59.1	+16 09 38	10	35	1436	$-0.23 \pm 0.03$	$-0.11 \pm 0.05$	12815	29.06 $\pm$0.02
35,73	${\rm VB181}$		K5	04 29 31.0	+16 14 54	12	37	70	$-0.25 \pm 0.11$	$-0.17 \pm 0.17$	10270	28.58 $\pm$0.06
35,73	${\rm RE281}$		M9	04 30 02.5	+16 03 54	27	25	14	<0.13	$0.00 \pm 0.00$	15026	27.96 $\pm$0.19
35,73	${\rm VB182}$	SB	K1	04 30 34.6	+15 44 02	3	9	1336	$-0.27 \pm 0.04$	$-0.27 \pm 0.07$	17040	28.50 $\pm$0.02
35,73	${\rm VA610}$		M4	04 31 07.4	+16 23 23	55	47	48	$-0.33 \pm 0.10$	$-0.17 \pm 0.18$	11016	28.67 $\pm$0.06
35,73	${\rm VA638 + LP415-175}$	VB	M1	04 31 46.0	+15 37 50	20	24	66	$-0.12 \pm 0.12$	$-0.26 \pm 0.16$	13406	28.00 $\pm$0.07
35,73	${\rm VB89}$	SB1	F2	04 31 51.6	+15 51 11	5	28	219	$-0.32 \pm 0.06$	$-0.08 \pm 0.11$	13632	28.32 $\pm$0.04
35,73	${\rm VB191}$		K7	04 31 52.3	+15 29 50	8	27	27	$-0.31 \pm 0.16$	$-0.49 \pm 0.26$	15351	28.34 $\pm$0.10
35,73	${\rm VB91 +B}$	VB	K1	04 32 50.3	+16 00 11	10	45	78	$-0.45 \pm 0.08$	$0.00 \pm 0.17$	10714	28.39 $\pm$0.06
35,73	${\rm VB92}$		G8	04 32 59.5	+15 49 10	2	43	71	$-0.49 \pm 0.10$	$0.40 \pm 0.22$	8477	28.64 $\pm$0.07
98,99	${\rm L14}$		K7	04 08 26.7	+12 11 32	2	15	94	$-0.45 \pm 0.11$	$0.03 \pm 0.22$	14852	27.88 $\pm$0.07
64,115	${\rm VA486 +B}$	VB	M2	04 28 30.2	+17 41 48	24	49	1521	$-0.15 \pm 0.03$	$-0.01 \pm 0.05$	5706	29.30 $\pm$0.02
64,115	${\rm VB77}$	SB1	F7	04 29 20.6	+17 32 45	3	42	1916	$-0.20 \pm 0.03$	$-0.17 \pm 0.05$	7427	29.19 $\pm$0.02
64,115	${\rm VB78}$		F5	04 29 30.3	+17 52 29	42	32	531	$-0.43 \pm 0.05$	$-0.14 \pm 0.10$	7159	29.00 $\pm$0.03
64,115	${\rm VA575}$		M4	04 30 24.1	+17 30 02	4	34	332	$-0.06 \pm 0.06$	$-0.17 \pm 0.09$	7347	29.02 $\pm$0.03
64,115	${\rm VA627}$	SB1	K4	04 31 37.1	+17 42 35	3	17	1214	$-0.17 \pm 0.05$	$-0.09 \pm 0.07$	9238	28.65 $\pm$0.03
64,115	${\rm VA657}$		M4	04 32 09.9	+17 40 02	31	20	39	$-0.03 \pm 0.19$	$0.10 \pm 0.24$	7467	28.16 $\pm$0.10
64,115	${\rm VA674}$		M4	04 32 29.1	+17 54 18	3	12	237	$-0.15 \pm 0.09$	$0.01 \pm 0.13$	10814	28.40 $\pm$0.05
116,117	${\rm L104}$		K8	05 01 36.2	+13 55 58	3	6	102	$-0.15 \pm 0.14$	$0.35 \pm 0.19$	11236	28.05 $\pm$0.08
116,117	${\rm VB187}$		G9	05 03 08.0	+13 43 50	5	18	318	$-0.27 \pm 0.07$	$-0.46 \pm 0.12$	8551	28.75 $\pm$0.04

 

Table 5: X-ray data for TTS in Taurus-Auriga below the detection limit of the ROSAT PSPC.

Obs. No.	Designation	Type/	SpT	X-ray position		Offax	Cts	Expos	$\log{L_{\rm X}}$
		Mult		$\alpha_{2000}$	$\delta_{2000}$	[arcmin]		[s]	[erg/s]
2	${\rm FPTau }$	C	M4	04 14 47.2	+26 46 28	35.0	22.6	1105	<29.70
2	${\rm CXTau }$	C	M3	04 14 47.8	+26 48 12	36.6	25.9	1063	<29.77
5	${\rm Mellote22\,253 }$	W	G0	03 44 03.8	+24 30 13	15.6	2.9	663	<29.03
5	${\rm BD+23^\circ501B }$	W	K0	03 44 12.1	+24 02 00	22.1	5.5	457	<29.47
5	${\rm BD+23^\circ502 }$	W	G5	03 44 14.1	+24 06 23	18.9	0.2	520	<27.94
5	${\rm RXJ0344.3+2447 }$	W	G0	03 44 20.7	+24 47 19	31.2	19.0	515	<29.95
5	${\rm Melotte22-345 }$	W	G7	03 44 26.3	+24 35 25	22.5	1.4	358	<28.96
5	${\rm RXJ0345.6+2454 }$	W	G5	03 45 42.4	+24 54 21	47.8	60.0	422	<30.54
6	${\rm Mellote22\,253 }$	W	G0	03 44 03.8	+24 30 13	43.4	7.3	79	<30.35
6	${\rm BD+23^\circ501B }$	W	K0	03 44 12.1	+24 02 00	20.4	0.6	90	<29.19
6	${\rm BD+23^\circ502 }$	W	G5	03 44 14.1	+24 06 23	22.8	1.0	93	<29.40
6	${\rm Melotte22-345 }$	W	G7	03 44 26.3	+24 35 25	46.3	1.3	75	<29.64
6	${\rm RXJ0348.8+2359 }$	W	G7	03 48 50.1	+23 58 45	47.4	1.6	64	<26.82
7	${\rm HHJ339 }$	C	M5	03 48 26.5	+23 11 30	22.7	2.8	360	<29.27
7	${\rm RXJ0348.8+2359 }$	W	G7	03 48 50.1	+23 58 45	42.7	0.6	478	<28.48
7	${\rm Melotte22-2147 }$	W	G7	03 49 05.9	+23 46 54	30.4	7.7	480	<29.59
7	${\rm Melotte22-2881 }$	W	G7	03 50 55.0	+23 50 16	34.8	2.9	522	<29.14
10	${\rm LH0419+15 }$	C	M7	04 22 30.7	+15 26 31	39.4	21.4	25551	<28.31
10	${\rm HD285751 }$	W	K2	04 23 42.0	+15 37 36	35.9	3149.9	28110	<30.43
12	${\rm BD+23^\circ502 }$	W	G5	03 44 14.1	+24 06 23	36.1	348.0	8147	<30.01
13	${\rm BD+23^\circ502 }$	W	G5	03 44 14.1	+24 06 23	37.1	1448.6	19614	<30.25
14	${\rm 2MWJ0438 }$	C	M8	04 38 35.2	+16 34 35	38.4	67.9	1658	<30.00
20	${\rm LH0416+14 }$	C	M8	04 19 36.9	+14 33 33	25.2	75.1	8867	<29.31
20	${\rm LH0418+15 }$	C	M7	04 21 17.5	+15 30 03	48.0	26.8	5068	<29.11
20	${\rm LH0419+15 }$	C	M7	04 22 30.7	+15 26 31	48.2	3.1	6607	<28.06
22	${\rm CoKuTau/2 }$	C	M6	04 31 35.0	+18 13 42	43.8	852.4	10545	<30.29
22	${\rm HLTau }$	C	K7	04 31 38.4	+18 13 59	43.8	732.0	9969	<30.25
22	${\rm XZTau N + S }$	CB	-/M3	04 31 40.0	+18 13 58	43.7	640.2	9709	<29.90
22	${\rm MHO-5 }$	C	M6	04 32 16.0	+18 12 46	40.9	41.9	13097	<28.89
22	${\rm RXJ0432.7+1809 }$	W	M5	04 32 41.0	+18 09 24	37.4	12.3	14308	<28.32
22	${\rm HNTau +/c }$	CB	M4	04 33 39.4	+17 51 50	25.4	6.0	14385	<27.71
22	${\rm DMTau }$	C	M0	04 33 48.6	+18 10 11	42.2	135.9	11769	<29.45
23	${\rm LH0429+15 }$	C	M7	04 32 38.1	+15 08 55	26.6	138.9	8887	<29.58
24	${\rm RXJ0453.1+3311 +B + C}$	WT	G8	04 53 08.7	+33 12 02	48.0	93.4	17248	<28.64
29	${\rm JH112 }$	C	K6	04 32 48.9	+22 53 03	42.4	44.9	392	<30.44
29	${\rm IRAS04303+2240 }$	C		04 33 18.7	+22 46 34	36.4	26.8	402	<30.21
29	${\rm CITau }$	C	K7	04 33 51.9	+22 50 31	28.2	14.3	500	<29.84
29	${\rm JH108 }$	W	M1	04 34 10.9	+22 51 45	23.7	3.1	460	<29.21
29	${\rm HOTau }$	C	M0	04 35 20.2	+22 32 14	23.1	5.3	412	<29.49
29	${\rm FFTau +/c }$	WB	K7	04 35 20.8	+22 54 25	7.5	5.0	593	<29.01
29	${\rm Haro6-28 +/c }$	CB	M5	04 35 56.7	+22 54 37	2.6	7.2	680	<29.11
29	${\rm RXJ0438.3+2302 +/c}$	WB	M1	04 38 15.6	+23 02 28	33.9	16.6	378	<29.73
29	${\rm VYTau +/c }$	WB	M0	04 39 17.3	+22 47 54	47.4	4.6	397	<29.15
30	${\rm CoKuTau3 +/c }$	WB	M1	04 35 41.1	+24 11 08	49.4	23.9	1147	<29.40
32	${\rm LH0418+15 }$	C	M7	04 21 17.5	+15 30 03	22.2	9.6	2023	<29.06
32	${\rm LH0419+15 }$	C	M7	04 22 30.7	+15 26 31	40.1	86.6	2683	<29.89
33	${\rm LH0416+14 }$	C	M8	04 19 36.9	+14 33 33	45.4	15.0	14010	<28.41
34	${\rm HD285751 }$	W	K2	04 23 42.0	+15 37 36	33.9	1643.2	12054	<30.52
38	${\rm NTTS041529+1652 }$	W	K5	04 18 21.4	+16 58 46	45.9	2.3	941	<28.77
45	${\rm CWTau }$	C	K3	04 14 16.9	+28 10 59	2.8	7.2	6221	<28.45
45	${\rm Briceno1 }$	C	cont	04 14 17.5	+28 06 11	6.8	3.7	5870	<28.19
45	${\rm CYTau }$	C	M1	04 17 33.7	+28 20 48	45.7	3.4	2794	<28.47
48	${\rm 2MWJ0417 }$	W	M8	04 17 24.8	+16 34 36	17.1	0.9	3391	<27.80
50	${\rm Briceno8 }$	C	M4	05 04 41.4	+25 09 57	32.0	108.2	5396	<29.69
52	${\rm IRAS05023+2527 }$	C	K7M0	05 05 22.7	+25 31 34	49.9	251.2	2743	<30.35
53	${\rm IRAS04414+2506 }$	C		04 44 27.3	+25 11 31	47.5	450.2	5601	<30.29
54	${\rm RXJ0446.7+2459 }$	C	M4	04 46 42.7	+24 59 04	44.4	533.0	6283	<30.31
55	${\rm GMTau }$	C	cont	04 38 21.2	+26 09 14	24.5	60.0	7561	<29.28
55	${\rm DOTau }$	C	M0	04 38 28.5	+26 10 50	23.2	78.5	7047	<29.43
55	${\rm GNTau +/c }$	CB	cont	04 39 20.8	+25 45 03	23.4	10.5	6953	<28.26
55	${\rm Kim1-44 }$	C		04 40 04.3	+26 04 49	2.7	7.0	10073	<28.23
55	${\rm IRAS04385+2550 }$	C		04 41 34.1	+25 55 43	21.5	38.8	7219	<29.11
56	${\rm GNTau +/c }$	CB	cont	04 39 20.8	+25 45 03	42.6	18.9	5161	<28.65
56	${\rm Elias18 }$	C		04 39 55.6	+25 45 02	35.9	146.1	5737	<29.79
56	${\rm Kim1-44 }$	C		04 40 04.3	+26 04 49	48.4	324.4	4858	<30.21
56	${\rm JH223 }$	W	M2	04 40 49.4	+25 51 20	31.5	4.3	6059	<28.24
56	${\rm IRAS04385+2550 }$	C		04 41 34.1	+25 55 43	31.4	97.1	6474	<29.56
56	${\rm CoKuLkH\alpha332/G1/c}$	WTr		04 42 06.8	+25 23 40	2.8	31.4	7930	<28.98
56	${\rm DPTau }$	C	M1	04 42 37.6	+25 15 38	11.7	8.2	7723	<28.41
56	${\rm IRAS04414+2506 }$	C		04 44 27.3	+25 11 31	34.3	4.6	6267	<28.25
62	${\rm LkH\alpha329 }$	C	K3	03 45 36.8	+32 25 59	21.5	61.8	9967	<29.18
62	${\rm LkH\alpha330 }$	C	G3	03 45 48.2	+32 24 13	21.9	12.1	11775	<28.40
63	${\rm CYTau }$	C	M1	04 17 33.7	+28 20 48	46.1	268.6	1747	<30.57
63	${\rm LkCa5 }$	W	M2	04 17 38.9	+28 33 01	47.5	268.0	1661	<30.59
63	${\rm Kim3-76 }$	W		04 17 49.6	+28 29 37	44.2	14.6	1765	<29.30
63	${\rm CoKuTau/1 +B }$	CB	M0	04 18 51.5	+28 20 28	29.0	113.4	2248	<29.79
64	${\rm J2-2041 }$	W	M4	04 33 55.4	+18 38 39	44.3	274.1	2507	<30.42
64	${\rm NTTS043220+1815 }$	W	F8	04 35 14.0	+18 21 37	47.6	1.2	2225	<28.10
70	${\rm RXJ0416.5+2053B }$	WB	M6	04 16 27.2	+20 53 28	24.1	5.7	3095	<28.65
77	${\rm LkH\alpha329 }$	C	K3	03 45 36.8	+32 25 59	34.1	24.2	4982	<29.07
77	${\rm LkH\alpha330 }$	C	G3	03 45 48.2	+32 24 13	33.8	13.3	4697	<28.84
82	${\rm FWTau +/c }$	CB	M4	04 29 29.6	+26 16 54	48.8	14.7	5935	<28.48
82	${\rm IQTau }$	C	M1	04 29 51.4	+26 06 47	40.1	221.0	7129	<29.88
82	${\rm J665 }$	W	M5	04 31 58.4	+25 43 30	13.2	9.2	9516	<28.37
82	${\rm IRAS04301+2608 }$	C		04 33 10.1	+26 14 17	22.8	29.1	7338	<28.98
82	${\rm DLTau }$		K7	04 33 39.0	+25 20 39	34.9	16.0	7259	<28.73
83	${\rm IRAS04216+2603 }$	C	M1	04 24 39.5	+26 09 51	28.4	71.8	8045	<29.34
83	${\rm FVTau +/c }$	CQ	K5/M4/	04 26 53.5	+26 06 55	33.0	16.1	6434	<28.18
	${\rm +/c1 +/c2 }$		-/-	04 26 54.4	+26 06 52	33.1	16.5	6433	<28.19
83	${\rm FVTau/c }$	CQu	M4	04 26 54.4	+26 06 52	33.1	16.5	6433	<28.19
83	${\rm DGTauB }$	C		04 27 02.6	+26 05 31	33.4	11.9	6505	<28.65
83	${\rm DGTau }$	C	K7M0	04 27 04.6	+26 06 17	34.3	11.4	6411	<28.63
84	${\rm RXJ0423.0+2310 }$	W	K1	04 23 01.2	+23 10 47	18.7	3.4	5498	<28.17
85	${\rm Kim3-76 }$	W		04 17 49.6	+28 29 37	41.4	16.2	3843	<29.01
86	${\rm Kim3-76 }$	W		04 17 49.6	+28 29 37	41.3	12.8	4207	<28.87
86	${\rm Hubble4 }$	W	K7	04 18 47.0	+28 20 08	47.1	199.3	3720	<30.11
86	${\rm CoKuTau/1 +B }$	CB	M0	04 18 51.5	+28 20 28	46.6	182.5	3750	<29.77
87	${\rm Kim3-76 }$	W		04 17 49.6	+28 29 37	41.0	203.2	3487	<30.15
87	${\rm Hubble4 }$	W	K7	04 18 47.0	+28 20 08	46.7	227.1	3516	<30.19
87	${\rm CoKuTau/1 +B }$	CB	M0	04 18 51.5	+28 20 28	46.3	207.6	3514	<29.85
88	${\rm Kim3-76 }$	W		04 17 49.6	+28 29 37	41.0	28.9	3720	<29.27
88	${\rm Hubble4 }$	W	K7	04 18 47.0	+28 20 08	46.7	168.3	3490	<30.07
88	${\rm CoKuTau/1 +B }$	CB	M0	04 18 51.5	+28 20 28	46.3	157.5	3574	<29.73
89	${\rm Hubble4 }$	W	K7	04 18 47.0	+28 20 08	46.7	207.7	3351	<30.18
89	${\rm CoKuTau/1 +B }$	CB	M0	04 18 51.5	+28 20 28	46.2	178.1	3414	<29.80
90	${\rm LH0429+15 }$	C	M7	04 32 38.1	+15 08 55	34.8	9.2	11779	<28.28
94	${\rm V836Tau }$	W	K7	05 03 06.5	+25 23 20	36.3	1.4	476	<28.84
94	${\rm Briceno8 }$	C	M4	05 04 41.4	+25 09 57	11.7	0.5	674	<28.28
94	${\rm IRAS05023+2527 }$	C	K7M0	05 05 22.7	+25 31 34	31.4	0.4	404	<28.36
94	${\rm Briceno10 }$	W	M4	05 06 16.6	+24 46 13	20.6	0.9	393	<28.73
94	${\rm Briceno11 }$	C	M4	05 06 23.2	+24 32 24	32.4	6.4	500	<29.49
94	${\rm RXJ057.2 }$	W	K6	05 07 12.1	+24 37 16	35.9	1.4	481	<28.84
94	${\rm Briceno12 }$	C	M4	05 07 55.9	+25 00 19	37.5	6.4	344	<29.65
3,4	${\rm IRAS04154+2823 }$	C		04 18 31.5	+28 31 12	4.2	8.6	27679	<27.88
3,4	${\rm V410x-ray7 }$	W	M1	04 18 42.4	+28 18 52	8.9	604.9	30389	<29.68
3,4	${\rm CoKuTau/1 +B }$	CB	M0	04 18 51.5	+28 20 28	8.4	27.3	28863	<28.06
3,4	${\rm V410x-ray8d }$	W	K0	04 19 21.6	+28 14 04	17.5	33.8	25224	<28.51
3,4	${\rm V410x-ray8b }$	W	K-M	04 19 27.3	+28 12 48	19.3	1.6	17289	<27.35
3,4	${\rm IRAS04171+2756 }$	C		04 20 11.8	+28 03 09	33.0	34.6	22202	<28.58
8,9	${\rm Mellote22\,253 }$	W	G0	03 44 03.8	+24 30 13	44.5	402.5	7922	<30.09
8,9	${\rm BD+23^\circ502 }$	W	G5	03 44 14.1	+24 06 23	36.6	287.9	6854	<30.01
11-13	${\rm HHJ339 }$	C	M5	03 48 26.5	+23 11 30	47.8	105.1	23764	<29.03
30,31	${\rm GVTau N + S }$	CB	K4/K3	04 29 23.6	+24 33 02	38.8	4.7	5046	<28.05
30,31	${\rm IRAS04264+2433 }$	C	M5	04 29 29.9	+24 39 55	38.6	16.1	5062	<26.96
30,31	${\rm ZZTauA +/c }$	CB	M3	04 30 51.3	+24 42 23	22.8	4.4	2483	<28.33
30,31	${\rm HKTau +/c }$	CB	M1	04 31 50.5	+24 24 18	7.6	0.8	6960	<27.16
30,31	${\rm MHO-8 }$	C	M6	04 33 01.1	+24 21 11	13.6	7.9	6760	<28.45
38,39	${\rm 2MWJ0417 }$	W	M8	04 17 24.8	+16 34 36	27.8	26.5	20730	<28.49
51,52	${\rm Briceno8 }$	C	M4	05 04 41.4	+25 09 57	26.7	82.7	7410	<29.43
51,52	${\rm Briceno11 }$	C	M4	05 06 23.2	+24 32 24	34.8	196.5	6636	<29.86
58,63	${\rm V410x-ray3 }$	C	M7	04 18 08.0	+28 26 05	48.1	38.2	4526	<29.31
58,63	${\rm StromAnon13 }$	C	M5	04 18 17.2	+28 28 43	46.7	179.4	4860	<29.95
58,63	${\rm DDTau +/c }$	CB	M1	04 18 31.1	+28 16 30	42.4	36.4	5143	<28.93
58,63	${\rm CZTau +/c }$	WB	M2	04 18 31.5	+28 16 59	42.3	46.7	5140	<29.04
58,63	${\rm IRAS04154+2823 }$	C		04 18 31.5	+28 31 12	44.3	151.8	4973	<29.87
58,63	${\rm V410x-ray2 }$		M0	04 18 34.5	+28 30 32	43.5	215.9	5006	<30.02
58,63	${\rm V410x-ray4 }$		M4	04 18 40.2	+28 24 26	40.9	208.7	5278	<29.98
58,63	${\rm V410x-ray7 }$	W	M1	04 18 42.4	+28 18 52	39.9	307.9	5302	<30.15
58,63	${\rm Kim3-89 }$	W	M5	04 19 01.2	+28 19 43	35.8	42.2	5779	<29.25
58,63	${\rm V410x-ray5a }$	C	M5	04 19 02.0	+28 22 34	35.8	16.0	5708	<28.83
58,63	${\rm FQTau +/c }$	CB	M2	04 19 12.7	+28 29 34	35.2	208.0	5447	<29.66
58,63	${\rm V410x-ray8d }$	W	K0	04 19 21.6	+28 14 04	31.5	144.7	5230	<29.83
58,63	${\rm V410x-ray8b }$	W	K-M	04 19 27.3	+28 12 48	30.5	127.0	5259	<29.77
58,63	${\rm IRAS04171+2756 }$	C		04 20 11.8	+28 03 09	25.4	93.1	6372	<29.55
58,63	${\rm DETau }$	C	M2	04 21 55.6	+27 55 07	24.0	74.5	6603	<29.44
58,63	${\rm IRAS04200+2759 }$	C		04 23 06.0	+28 05 57	22.2	51.8	6269	<29.30
85-89	${\rm V410x-ray3 }$	C	M7	04 18 08.0	+28 26 05	42.9	99.1	19432	<29.09
85-89	${\rm StromAnon13 }$	C	M5	04 18 17.2	+28 28 43	39.8	821.3	20085	<30.00
85-89	${\rm IRAS04154+2823 }$	C		04 18 31.5	+28 31 12	36.6	332.7	20779	<29.59
85-89	${\rm V410x-ray2 }$		M0	04 18 34.5	+28 30 32	37.0	709.0	20452	<29.92
85-89	${\rm V410x-ray7 }$	W	M1	04 18 42.4	+28 18 52	48.2	1306.6	17253	<30.26
85-89	${\rm Kim3-89 }$	W	M5	04 19 01.2	+28 19 43	47.0	894.5	17422	<30.09
85-89	${\rm V410x-ray5a }$	C	M5	04 19 02.0	+28 22 34	44.2	484.4	18220	<29.81
85-89	${\rm FQTau +/c }$	CB	M2	04 19 12.7	+28 29 34	37.1	61.6	18584	<28.60
35,73	${\rm LH0429+15 }$	C	M7	04 32 38.1	+15 08 55	47.2	1462.9	10872	<30.51
64,115	${\rm MHO-9 }$	W	M4	04 31 15.7	+18 20 08	23.0	14.7	5449	<28.81
64,115	${\rm CoKuTau/2 }$	C	M6	04 31 35.0	+18 13 42	16.0	21.2	10780	<28.68
64,115	${\rm V710Tau N }$	CB	M1	04 31 57.7	+18 21 37	23.6	187.3	8900	<29.41
	${\rm V710Tau S }$		M3	04 31 57.7	+18 21 34	23.6	186.4	8900	<29.40
64,115	${\rm MHO-6 }$	C	M5	04 32 22.0	+18 27 42	30.7	3.3	8088	<28.00
64,115	${\rm MHO-7 }$	W	M5	04 32 26.2	+18 27 52	31.1	6.5	8238	<28.28
64,115	${\rm LH0429+17 }$	C	M9	04 32 51.1	+17 30 11	33.3	11.0	8366	<28.50
64,115	${\rm HNTau +/c }$	CB	M4	04 33 39.4	+17 51 50	28.7	19.1	8632	<28.43
64,115	${\rm DMTau }$	C	M1	04 33 48.6	+18 10 11	32.0	38.2	8875	<29.02

 

Table 6: X-ray data for Pleiads below the detection limit of the ROSAT PSPC.

Obs. No.	Designation	Mult	SpT	X-ray position		Offax	Cts	Expos	$\log{L_{\rm X}}$
				$\alpha_{2000}$	$\delta_{2000}$	[arcmin]		[s]	[erg/s]
5	${\rm hcg27 }$			03 40 03.6	+24 30 03	45.4	4.8	389	<29.31
5	${\rm hcg34 }$			03 40 24.1	+24 35 05	42.3	0.6	422	<28.38
5	${\rm sk778 }$			03 40 26.3	+24 05 25	42.1	1.3	404	<28.74
5	${\rm AK1B031 }$			03 40 30.5	+24 29 16	39.2	31.3	418	<30.09
5	${\rm hcg40 }$			03 40 39.9	+24 44 10	43.2	45.1	445	<30.23
5	${\rm hcg45 }$			03 41 02.9	+23 43 23	48.3	16.2	382	<29.85
5	${\rm sk729 }$			03 41 26.8	+24 01 04	32.2	16.1	497	<29.73
5	${\rm AK1B055 }$		G9	03 41 27.6	+23 42 32	45.6	39.3	403	<30.21
5	${\rm sk724 }$			03 41 39.5	+23 45 48	41.4	5.3	447	<29.29
5	${\rm sk709 }$		M2	03 41 58.6	+23 42 28	42.1	36.8	433	<30.15
5	${\rm sk702 }$			03 41 59.9	+25 01 49	45.3	8.0	450	<29.47
5	${\rm hcg64 }$			03 42 02.8	+23 55 55	30.2	0.6	517	<28.28
5	${\rm hcg63 }$			03 42 02.8	+24 12 38	19.4	4.1	519	<29.12
5	${\rm sk701 }$			03 42 03.2	+24 32 14	20.8	2.7	552	<28.91
5	${\rm hcg65 }$		K8	03 42 03.7	+24 42 46	28.2	1.4	448	<28.72
5	${\rm sk699 }$			03 42 08.7	+23 35 18	47.8	2.3	351	<29.04
5	${\rm hcg68 }$		M3	03 42 10.8	+24 05 10	22.1	5.2	438	<29.30
5	${\rm hcg71 }$		M0	03 42 21.5	+24 39 54	23.6	7.5	436	<29.46
5	${\rm hcg73 }$			03 42 26.2	+24 14 09	14.2	0.1	598	<27.39
5	${\rm AK1B078 }$		K4	03 42 27.5	+25 02 51	44.3	48.1	461	<30.24
5	${\rm sk676 }$			03 42 28.5	+25 01 02	42.5	43.0	460	<30.19
5	${\rm hcg80 }$		K8	03 42 40.1	+23 59 23	23.1	5.9	434	<29.36
5	${\rm hcg82 }$			03 42 41.1	+24 01 44	20.9	4.0	363	<29.26
5	${\rm sk671 }$		M1	03 42 41.8	+24 11 59	12.8	1.9	620	<28.70
5	${\rm sk663 }$			03 42 49.0	+24 10 17	13.1	1.9	597	<28.73
5	${\rm hii25 }$		F7	03 42 55.0	+24 29 36	11.1	2.3	591	<28.81
5	${\rm hcg93 }$			03 42 56.4	+24 05 00	16.7	3.0	553	<28.95
5	${\rm hii34 }$		K2	03 43 02.8	+24 40 12	20.6	6.2	606	<29.23
5	${\rm hcg97 }$			03 43 05.4	+24 49 30	29.7	3.4	547	<29.01
5	${\rm hcg100 }$		M5	03 43 09.6	+24 41 34	21.8	6.8	555	<29.31
5	${\rm hcg103 }$			03 43 13.0	+24 39 21	19.6	2.8	579	<28.91
5	${\rm hii97 +B }$	VB	K4	03 43 26.5	+24 59 41	39.8	5.9	463	<29.03
5	${\rm sk638 }$			03 43 26.8	+24 27 11	8.8	1.3	675	<28.49
5	${\rm hcg109 }$			03 43 28.1	+24 53 33	33.8	24.7	458	<29.95
5	${\rm hii120 }$	SB1	G6	03 43 31.8	+23 40 28	40.0	4.9	460	<28.95
5	${\rm hii129 }$		K1	03 43 34.3	+23 45 44	34.8	0.5	510	<28.25
5	${\rm hii134 +B }$	VB	M1	03 43 36.5	+24 13 58	8.2	1.1	651	<28.15
5	${\rm hii133 }$		K8	03 43 36.8	+24 23 40	7.7	1.1	716	<28.42
5	${\rm hii152 }$		G6	03 43 37.6	+23 32 11	48.3	3.3	405	<29.13
5	${\rm hcg124 }$			03 43 38.9	+23 44 07	36.6	1.7	493	<28.76
5	${\rm hii157 }$		F2	03 43 41.4	+23 38 58	41.7	7.6	450	<29.45
5	${\rm hcg123 }$		M4	03 43 42.0	+24 34 25	16.1	3.1	540	<28.97
5	${\rm hii164 }$	SB1	F7	03 43 42.8	+23 35 42	45.0	3.8	432	<28.87
5	${\rm hii153 }$		A5	03 43 43.1	+25 04 52	45.3	5.2