A&A 397, 473-486 (2003)
DOI: 10.1051/0004-6361:20021384

Clusters in the inner spiral arms of M 51: The cluster IMF and the formation history^,

A. Bik ^1,2 - H. J. G. L. M. Lamers ^1,3 - N. Bastian ¹ - N. Panagia ^4,5 - M. Romaniello ⁶

1 - Astronomical Institute, Utrecht University, Princetonplein 5, 3584 CC Utrecht, The Netherlands
2 - Astronomical Institute Anton Pannekoek, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
3 - SRON Laboratory for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands
4 - Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD21218, USA
5 - On assignment from the Space Science Department of ESA
6 - European Southern Observatory, Karl-Schwarzschild Strasse 2, Garching-bei-Muenchen 85748, Germany

Received 19 June 2002 / Accepted 16 September 2002

Abstract
We present the results of an analysis of the HST-WFPC2 observations of the interacting galaxy M 51. From the observations in 5 broadband filters (UBVRI) and two narrowband filters (H$\alpha$ and [OIII]) we study the cluster population in a region of 3.2 $\times 3.2$ kpc² in the inner spiral arms of M 51, at a distance of about 1 to 3 kpc from the nucleus. We found 877 cluster candidates and we derived their ages, initial masses and extinctions by means of a comparison between the observed spectral energy distribution and the predictions from cluster synthesis models for instantaneous star formation and solar metallicity. The lack of [OIII] emission in even the youngest clusters with strong H$\alpha$ emission, indicates the absence of the most massive stars and suggests a mass upper limit of about 25 to 30 $M_{\odot }$. The mass versus age distribution of the clusters shows a drastic decrease in the number of clusters with age, much more severe than can be expected on the basis of evolutionary fading of the clusters. This indicates that cluster dispersion is occurring on a timescale of 10 Myr or longer. The cluster initial mass function has been derived from clusters younger than 10 Myr by a linear regression fit of the cumulative mass distribution. This results in an exponent $\alpha = -{\rm d} \log~ N(M) /{\rm d} \log~(M) = 2.1 \pm 0.3$ in the range of $2.5\times 10^3 < M < 5\times 10^4~\mbox{$M_{\odot}$ }$ but with an overabundance of clusters with $M > 2\times 10^4$ $M_{\odot }$. In the restricted range of $2.5\times 10^3 < M < 2\times 10^4$ $M_{\odot }$ we find $\alpha = 2.0 \pm 0.05$. This exponent is very similar to the value derived for clusters in the interacting Antennae galaxies, and to the exponent of the mass distribution of the giant molecular clouds in our Galaxy. To study the possible effects of the interaction of M 51 with its companion NGC 5195 about 400 Myr ago, which triggered a huge starburst in the nucleus, we determined the cluster formation rate as a function of time for clusters with an initial mass larger than 10⁴ $M_{\odot }$. There is no evidence for a peak in the cluster formation rate at around 200 to 400 Myr ago within 2 $\sigma$ accuracy, i.e. within a factor two. The formation rate of the detected clusters decreases strongly with age by about a factor 10² between 10 Myr and 1 Gyr. For clusters older than about 150 Myr this is due to the evolutionary fading of the clusters below the detection limit. For clusters younger than 100 Myr this is due to the dispersion of the clusters, unless one assumes that the cluster formation rate has been steadily increasing with time from 1 Gyr ago to the present time.

Key words: galaxies: individual: M 51 - galaxies: interactions - galaxies: spiral - galaxies: starburst - galaxies: star clusters

   
1 Introduction

The interaction of galaxies triggers star formation as clearly seen in the young starbursts in interacting galaxies (for reviews see Kennicutt 1998; Schweizer 1998). One of the best examples is the Antennae system where the interaction is presently going on and star formation and cluster formation occurs on a very large scale in the region between the two merging nuclei (Whitmore et al. 1999).

The way the triggered star formation progresses through an interacting galaxy is best studied from a slightly older interacting system, where the close passage of the companion is over. In such a system one can hope to derive the age distribution of clusters as a function of location in the galaxy and thus measure the time sequence of the induced star and cluster formation as a function of location in the galaxy.

One of the best systems for this purpose is the interacting sytem of the Whirlpool galaxy (M 51) at a distance of $8.4 \pm 0.6$ Mpc (Feldmeier et al. 1997). The M 51 system consists of a grand design spiral galaxy (NGC 5194) interacting with its dwarf companion (NGC 5195). The almost face-on orientation of M 51 allows the observation of its structure in great detail with minimum obscuration by interstellar dust. The interaction of these two galaxies has been modelled by various authors, starting from the fundamental paper by Toomre & Toomre (1972). These authors derived an age of the closest passage to be $2 \times 10^8$ years ago. Later refined models, e.g. by Hernquist (1990), and reviewed by Barnes (1998), have improved this time estimate. The closest approach is now believed to have occurred about 250-400 Myrs ago. The best model is found for a distance of the pericenter of 17 to 20 kpc, for a mass ratio of $M/m \approx 2$ and a relative orbit which crosses the plane of M 51 under an angle of about 15 degrees. (For a discussion of the problems with this model and possible improvements, see Barnes 1998). Recently Salo & Laurikainen (2000) suggested that on the basis of N-body simulations that the M 51 system had multiple passages, with the two last at 50-100 Myrs and 400-500 Myrs ago.

Because of its relatively small distance from us, and the fact that we see the M 51 system face one, the system is ideally suited for the study of the progression of cluster formation due to galaxy - galaxy interaction. For this reason we started a series of studies of different aspects of the M 51 system based on HST-WFPC2 observations in six broad band and two narrow band filters.

The nucleus of M 51 was studied by Scuderi et al. (2002). They found that the core contains a starburst with an age of $410 \pm 140$ Myrs and a total stellar mass of about $2 \times 10^7 ~M_{\odot}$ within the central 17 pc. This age agrees with the estimated time of closest passage of the companion, so the starburst in the core is most likely due to the interaction with the passing companion. M 51 contains an unresolved nucleus with a diameter smaller than 2 pc and a luminosity of $2\times 10^6~ L_{\odot}$ (Scuderi et al. 2002).

The bulge, i.e. the reddish region with a size of $11 \times$ 16 arcsec $^2 = 460 \times 680$ pc², between the nucleus and the inner spiral arms, was studied by Scuderi et al. (2002) and by Lamers et al. (2002). The bulge is dominated by an old stellar population with an age in excess of 5 Gyrs. The HST-WFPC2 images of the bulge show the presence of dust lanes. The total amount of dust in the bulge is about $2.3 \times 10^3$ $M_{\odot }$ and the dust has about the same extinction law and approximately the same gas to dust ratio as our Galaxy (Lamers et al. 2002). This suggests a metallicity close to that in the solar neighbourhood. The HST-WFPC2 images of the bulge of M 51 show clearly that the dust is concentrated in structures in the forms of spiral-like dust lanes and a bar that reaches all the way down into the core. Most intriguingly is the discovery of about 30 bright and mainly blue point-like sources in the bulge that are aligned more or less along the spiral-like dust lanes. Lamers et al. (2002) have shown that these are most likely very young massive stars $20 < M_* < 150~\mbox{$M_{\odot}$ }$ with little evidence of associated clusters. This mode of star formation is the result of the peculiar conditions, in particular the destruction of CO molecules, of the interstellar clouds in the bulge of M 51.

In this study we focus on the clusters at a distance of about 1 to 3 kpc from the nucleus, i.e. near the inner spiral arms. The purpose of the paper is two-fold:
- (a) to determine the cluster intitial mass function, and
- (b) to determine the presence or absence of a starburst period that can be linked to triggering by the passage of the companion. This is not an easy task, because our data will show that the age distribution of the clusters is strongly affected by the disruption of clusters older than about 40 Myrs.

We study the clusters and their properties by identifying point-like sources in the HST-WFPC2 images and measuring their UBVRI magnitudes to obtain their energy distributions. The magnitudes indicate that the sources are clusters instead of single stars. Their energy distributions are compared to cluster evolutionary synthesis models to determine the age, mass and E(B-V) of these clusters.

In Sect. 2 we describe the observations and the data reduction. In Sect. 3 the selection of cluster candidates is discussed. In Sect. 4 we describe the cluster evolutionary synthesis models and in Sect. 5 the fitting procedure for the derivation of the cluster parameters is explained. The mass versus age distribution of the clusters is derived in Sect. 6. In Sect. 7 the initial mass function of the clusters is derived from the sample of clusters younger than 10 Myrs. The cluster formation history is studied in Sect. 8. The summary and conclusions are given in Sect. 9.

   
2 Observations and reduction

M 51 was observed with HST-WFPC2 as part of the HST Supernova INtensive Study (SINS) program (Millard et al. 1999). For this study we use the images taken in the broad band filters F336W (U), F439W (B), F555W (V), F675W (R) and F814W (I) from the SINS program and in the narrow band filters F502N $(\mbox{[OIII]})$ and F656N ( $\mbox{H$\alpha$ }$) from the GO-program of H. C. Ford. The image in U was taken on 1994 May 12, the BVRI images were taken on Jan. 15 1995 and the [OIII] and H$\alpha$ images on Jan. 25 1995. The U and B images were split into three and two exposures of 400 s and 700 s respectively. The [OIII] and H$\alpha$ images are split into two exposures of 1200 s and 500 s ( $\mbox{[OIII]}$), and 1400 s and 400 s ( $\mbox{H$\alpha$ }$). In the remaining bands one single exposure of 600 s was taken. The data was processed through the PODPS (Post Observing Data Processing System) for bias removal, flat fielding and dark frame correction.

To remove the cosmic rays from the U, B [OIII] and H$\alpha$ images, we used the STSDAS task crrej for combining the available exposures. For the VRI images, where only one exposure is available, we used a procedure called "Cosmic Eraser''. This procedure combines the IRAF tasks cosmicrays and imedit to reject as carefully as possible the cosmic rays. The automatic detection of cosmic rays with the task cosmicrays is based upon two parameters, a detection threshold and a flux ratio. The first parameter enables the detection of all the pixels with a value larger than the average value of the surrounding pixels. The flux ratio is defined as the percentage of the average value of the four neighboring pixels (excluding the second brightest pixel) to the flux of the brightest pixel. This parameter allows a classification of the detected objects: cosmic ray or star. Training objects are used to determine the flux ratio carefully. These training objects are labeled by the user to be a cosmic ray or a star. With imedit the detected cosmic rays signals are replaced by an interpolation of a third order surface fit to the surrounding pixels.

After the correction for the cosmic rays, the images were corrected for bad pixels using the hot pixel list from the STScI WFPC2 website in combination with the task warmpix. Corrections for non-optimal charge transfer efficiency on the CCD's of the WFPC2 camera were applied using the formulae by Whitmore & Heyer (1997).

With the task daofind from the DAOPHOT package Stetson (1987), we identified the point sources on the image. We performed aperture photometry on these sources, also with the DAOPHOT package. We used an aperture radius of 3 pixels. The sky background was calculated in an annulus with internal and external radius of 10 and 14 pixels respectively. We only selected the point sources with an uncertainty smaller than 0.2 in the magnitude. Photometric zeropoints were obtained from table 28.2 of the HST Data Handbook (Voit 1997), using the VEGAMAG photometric system (Holtzman et al. 1995).

The aperture correction was measured for a number of isolated, high S/N point sources on each WFPC2-chip. This output was adopted for all the other point sources on the chip. Following Holtzman et al. (1995) we have normalized the aperture correction to 1 $^{\prime\prime}$ (10 WF pixels). The aperture corrections we found are between -0.24 and -0.37 mag. This is larger than the aperture corrections for stars ${\approx}{-}0.17$ mag (Holtzman et al. 1995), which means that the detected point sources are fairly well resolved.

We adopt a distance of $d = 8.4 \pm 0.6$ Mpc (Feldmeier et al. 1997), which corresponds to a distance modulus of 29.62. At this distance, 1 $^{\prime\prime}$ corresponds to a linear distance of 40.7 pc, which means that an HST-WFC pixel of 0.1 $^{\prime\prime}$ corresponds to 4.1 pc.

   
3 Selection of the clusters

The U-band images were taken in 1994, 8 months earlier than the images in the other passbands. The orientation of HST-WFPC2 was not the same at the two epochs. In the 1995 BVRI-images the nucleus of M 51 was in the center of the PC-image. The U-image was centered on SN1994I (that was 15'' off from the nucleus) so that the nucleus was near the edge of the PC-image. The orientation of the WFPC2-images is shown in Fig. 1.

Figure 1: The location of the WFPC2 camera when the BVRI images were taken, superimposed on an optical image of M 51. Right: the orientation of the WFPC2 camera when the BVRI and the U images were taken. The grey area indicates the location of the WF2 chip, covering an area of $3.25 \times 3.25$ kpc (for an adopted distance of 8.4 Mpc), that was used in this analysis. Its exact location and orientation are given in Fig. 2. The dark grey region shows the overlap of the BVRI and U images.

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For our analysis only the part of WF4-chip of the U image that overlap with the WF2-chip of the BVRI images is used (see Fig. 1). To identify the various sources, we obtained a position of the sources in U and transformed these positions to the coordinate frame of the BVRI images. The orientation of the [OIII] and H$\alpha$ images is very similar to those of the BVRI images. We transformed these narrow band images to the same orientation as the BVRI images. We applied our analysis of the cluster energy distributions to the sources that were detected in the images of at least three of the BVRI broad-band filters with a magnitude uncertainty smaller than 0.2 in each band. To this purpose we compared the positions of all detected sources in the BVRI images. If objects occur in at least three images within a position tolerance of 2 pixels they are selected for our study. This tolerance was chosen on the basis of tests with clearly identifiable sources that were observed in most bands. For the sources detected in at least three images we then checked for the presence of a source in the U image, in the region where the U image and the BVRI images do overlap (the dark grey region in Fig. 1). If a source was not detected in a particular band, we adopted a conservative lower limit for the magnitude in that band (see below). This was not always possible for the U-magnitude, because many of the sources detected in the BVRI bands are located in an area that was not covered by the U-image. As a consequence, we have no information on the U-magnitude for many of the sources. The location of the sources in the WF2-chip is shown in Fig. 2. The overlay of the sources on the V band image clearly shows that the clusters are concentrated in or near the spiral arms at a distance of about 1.5 kpc from the nucleus of M 51. The number of sources, detected in the various bands, is listed in Table 1. The sample contains a total of 877 sources for which we have reliable photometry ( $\sigma < 0.20$ mag) in at least three bands.

Figure 3 shows the magnitude distribution of the sources in the various bands. All distributions show a slow increase in numbers towards fainter objects, a maximum and a steep decrease towards even fainter sources. The slow increase to fainter sources reflects their luminosity function. The steep decrease to high magnitudes is due to the detection limit. This detection limit is not a single value for each band, because of the variable background in the WF2 field due to the spiral arms. The maximum of the distributions are near $U \simeq 20.0$, $B \simeq 22.0$, $V\simeq 22.0$, $R \simeq 21.5$ and $I \simeq 21.0$. These values will be adopted as conservative lower limits for the magnitudes of sources that were not detected in any given band.

All the objects fall in the visual magnitude range of 16.5 <V < 23.6. For distance modulus of 29.62 this corresponds to an absolute magnitude range of -12.1 < M_V <-6.0 in the case of zero extinction and -12.6 < M_V<-6.5 in case of moderate extinction with $E(B-V) \simeq 0.17$. This means that the faintest objects could be either very bright stars or small clusters. The vast majority of the selected point sources are so bright that they must be clusters. (See Sect. 5.6.)

 

 

Table 1: Numbers of point sources detected in the different WFPC2-HST-images.

F336W	F439W	F555W	F675W	F814W	number
(U)	(B)	(V)	(R)	(I)	objects
d	d	d	d	d	76
l	d	d	d	d	366
n	d	d	d	d	109
d	l	d	d	d	30
l	l	d	d	d	144
n	l	d	d	d	39
d	d	d	d	l	21
l	d	d	d	l	78
n	d	d	d	l	14
					877

d means "detected", l means "lower magnitude limit" (i.e. the object is fainter than the detection limit) and n means "not observed".

Figure 2: Left: the location of all the detected point sources in the WF2 chip superimposed on the V-band image. This image is rotated 90 degrees clockwise compared to Fig. 1. The coordinates of the lower-left and upper-right corners of the image are: pixel (1, 1): $\rm RA(2000)=13^h29^m55\hbox{$.\!\!^{\rm s}$ }90$, $\rm Dec(2000)=47^011'27\hbox{$.\!\!^{\prime\prime}$ }2.$ and pixel 800, 800: $\rm RA(2000)=13^h29^m57\hbox{$.\!\!^{\rm s}$ }94$, $\rm Dec(2000)=47^013'16\hbox{$.\!\!^{\prime\prime}$ }6$.

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	Figure 3: The histogram of the magnitudes in the different bands. The slow increase at bright magnitudes is due to the luminosity function and the steep decrease at fainter magnitudes is due to the detection limit.
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3.1 The $\mathsfsl{H{\alpha}}$ and [OIII] magnitudes

The magnitudes in the narrow-band images of filters F656N ( $m({\rm H}\alpha )$) and F502N ( $m{\rm [OIII]}$) can be compared with those of the wide-band filters F675W (R) and F555W (V) respectively to derive a measure of the equivalent width of the H$\alpha$ and [OIII] lines. When the magnitudes are expressed in the HST-system, the magnitude differences $R-\mbox{$m({\rm H}\alpha)$ }$ and $V-\mbox{$m{\rm [OIII]}$ }$ are by definition equal to 0.0 if the spectrum of a source is a featureless, flat continuum (i.e. the spectrum of the source is a continuum $F_\lambda=\rm const.$ without a photospheric H$\alpha$ absorption, and there is no HII region around the star). The differences $R-\mbox{$m({\rm H}\alpha)$ }$ and $V-\mbox{$m{\rm [OIII]}$ }$ are either positive or negative if the source spectrum has an emission or an absorption line, respectively, falling in the narrow band filter, independently of the interstellar extinction. With the Vega-system magnitudes one has to fold in both the non-zero spectral slope and the discrete features present in $\alpha$ Lyrae's spectrum. Therefore, a featureless flat continuum would correspond to $R-\mbox{$m({\rm H}\alpha)$ }\simeq +0.08$ and $V-\mbox{$m{\rm [OIII]}$ }\simeq -0.26$ colors in the Vega-system.

Figure 4a shows the $m({\rm H}\alpha )$ versus R and Fig. 4b shows $m{\rm [OIII]}$ versus V for the subset of sources for which we could measure these magnitudes with an accuracy better than 0.2. The figure shows that many sources have H$\alpha$ emission ( $\mbox{$m({\rm H}\alpha)$ } < R$) but none (!) of the sources has [OIII] emission (note that $m{\rm [OIII]}$ is slightly fainter than the V magnitude as appropriate for complete absence of an emission line). The lack of [OIII] emission indicates that the far-UV flux, at $\lambda < 350$ Å  i.e. at energies higher than the second ionization potential of oxygen, is quite low. For main sequence stars with $L>2.5 \times 10^5~ \mbox{$L_{\odot}$ }$ (i.e. with $M > 30~\mbox{$M_{\odot}$ }$ and $\mbox{$T_{\rm eff}$ }> 33~000$ K), surrounded by an HII region with approximately solar abundances, we would expect $V - \mbox{$m{\rm [OIII]}$ }> R - \mbox{$m({\rm H}\alpha)$ }$. We will show later, on the basis of the study of the energy distributions, that many of the objects are very young clusters with ages less than a 10 Myr. The lack of [OIII] emission shows that these clusters do not contain stars with $T_{\rm eff}$ above about 30 000 K, which corresponds to about 25 to 30 $M_{\odot }$ (e.g. Chiosi & Maeder 1986). We can exclude the possibility that the lack of [OIII] emission be due to just a high metallicity, which could reduce the electron temperature in an HII region and weaken optical forbidden lines considerably, without requiring a lower effective temperature, or, equivalently, a low upper mass cutoff. This is because in many HII regions in M 51 and in other metal-rich spiral galaxies not only are the [OIII] lines faint or absent but also the HeI lines are unusually faint relative to Balmer lines (Panagia 2000; Lenzuni & Panagia, in preparation). This result indicates that He is only partially ionized and, therefore, that the ionizing radiation field is indeed produced exclusively by stars with effective temperatures much lower than 33 000 K . So we conclude that the upper mass limit for clusters in the inner spiral arms of M 51 is about 25 to 30 $M_{\odot }$.

	Figure 4: The top figure shows $m({\rm H}\alpha )$ versus R and the lower figure shows $m{\rm [OIII]}$ versus V for objects were these magnitudes could be determined with an accuracy better than 0.2 mag. Notice that many objects have H$\alpha$ emission, but no object has detectable [OIII] emission.
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4 Cluster evolution models

To determine the age, initial mass and E(B-V) of the clusters, we compare the observed energy distributions with energy distributions derived from theoretical cluster evolutionary synthesis models. We used two sets of models: the Starburst99 models for ages up to 1 Gyr, and the Frascati models for ages of 10 Myr to 5 Gyr. In this section the models are described.

4.1 Starburst99 cluster evolution models

To determine the age, initial mass and E(B-V) of the clusters, we compare the observed energy distributions with energy distributions derived from theoretical cluster evolutionary synthesis models. We used two sets of models: the Starburst99 models for ages up to 1 Gyr, and the Frascati models for ages of 10 Myr to 5 Gyr. In this section the models are described.

   
4.2 Starburst99 cluster evolution models

We compared the observed spectral energy distributions (SED) of our objects with the cluster evolutionary synthesis models of Leitherer et al. (1999), i.e. the Starburst99 models for instantaneous star formation. In these models, the stellar atmosphere models of Lejeune et al. (1997) are included. For stars with a strong mass loss the Schmutz et al. (1992) extended model atmospheres are used. The stellar evolution models of the Geneva group are included in these models. For our analysis we used the models of the Spectral Energy Distributions (SEDs).

In the cluster models the stars are assumed to be formed with a classical Salpeter IMF-slope of ${\rm d} \log (N) /{\rm d}\log (M) =-2.35$. The lower cut-off mass is $M_{\rm low} = 1~M_{\odot}$. We adopt two values for the upper cut-off mass: the standard value of $M_{\rm up} = 100~M_{\odot}$, and the value of $\mbox{$M_{\rm up}$ }= 30~ \mbox{$M_{\odot}$ }$. This last value is adopted because it is suggested by the lack of [OIII] emission (see Sect. 3.1). The total initial mass of all models is 10⁶ $M_{\odot }$. Leitherer et al. (1999) present models for 5 different metallicities, from Z= 0.001 to $Z=0.040 = 2 \times Z_{\odot}$. Observations of HII-regions have shown that the metallicity of the inner region of M 51 is approximately $2 ~ Z_\odot$ or slightly higher (e.g. Diaz et al. 1991; Hill et al. 1997). Therefore we adopt the models with Z=0.020 and 0.040. The almost solar metallicity agrees with the study of Lamers et al. (2002), who found that the extinction properties and the gas to dust-ratio in the bulge of M 51 is very similar to that in the Milky Way. So we use four sets of models, denoted by the pair $(Z,\mbox{$M_{\rm up}$ })$ of (0.02, 100), (0.02, 30), (0.04, 100) and (0.04, 30). For these combinations we calculated the SEDs of the cluster models, taking into account the nebular continuum emission.

To obtain the absolute magnitudes from the theoretical spectral energy distributions in the five broad-band filters and the two narrow-band filters we convolved the predicted spectra of the Starburst99 models with the WFPC2 filter profiles. The spectrum of Vega was also convolved with the filter functions in order to find the zero-points of the magnitudes in the VEGAMAG system. For each combination of Z and $\mbox{$M_{\rm up}$ }$ we calculated the SED of 195 models in the range of 0.1 Myr to 1 Gyr, with time steps increasing from 0.5 Myr for the youngest models to 10 Myr for the oldest models.

The adopted lower mass limit of 1 $M_{\odot }$ for the cluster stars has consequences for the derived masses of the clusters. If the IMF with a slope of -2.35 has a lower mass limit of 0.2 $M_{\odot }$, as for the Orion Nebula Cluster (Hillenbrand 1997), the derived masses of the clusters would be a factor 2.09 higher for an upper limit of 30 $M_{\odot }$. If the lower limit is 0.6 $M_{\odot }$, the mass of the clusters will be a factor 1.28 higher than those of the Starburst99 models for $M_{\rm up}=30$ $M_{\odot }$. We will take this effect into account in the determination of the cluster masses.

Some of the theoretical energy distributions in the WFPC2 wide-band filters used in this study are shown in Fig. 5, for clusters with an initial mass of 10⁶ $M_{\odot }$ at the distance of M 51. During the first 5 Myrs the UV flux remains high because most of the O-type stars have main sequence ages longer than 5 Myr. Between 5 and 10 Myr the O-type stars disappear. This results in a general decrease at all magnitudes, except in the I band where the red supergiants start to dominate. At later ages the flux decreases at all wavelengths as stars end their lives. After 900 Myrs only stars of types late-B and later have survived.

	Figure 5: Examples of some characteristics of the theoretical energy distributions, in magnitude versus wavelength (Å) of the UBVRI filters (from left to right), for STARBURST99 clusters with an initial mass of 106 $M_{\odot }$ at the distance of M 51. The age of the cluster in Myrs is indicated. The evolutionary variation is discussed in Sect. 4.1.
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Figure 5 shows that at any wavelength in the observed range the flux decreases with time. This fading of the clusters indicates that the detection limit of the clusters will gradually shift to those of higher mass as the clusters age. This is because the flux of a cluster (for a given stellar initial mass function) at any age and wavelength is proportional to the initial number of stars. The more massive the initial cluster, the brighter the cluster and the longer the flux will remain above the detection limit as the cluster fades due to stellar evolution. For any given detection limit, we can calculate the lower mass limit of the observable cluster as a function of age.

Figure 6 shows the relation between the initial mass of a cluster and its age when it fades below the detection limit, derived from the Starburst99 models. The R-magnitude (R) of a cluster of initial mass M_i without extinction at the adopted distance of 8.4 Mpc of M 51 (dm=29.62) is related to the absolute R-magnitude (M_R) predicted for the Starburst99 models of 10⁶ $M_{\odot }$ by

$$R(t)=M_R(t) + 29.62 - 2.5 \times \log \left(M/10^6\right)\cdot$$ (1)

So, for a given detection limit $R_{\rm lim}$ the critical mass $M_{\rm lim}$ of a cluster that can be detected at age t is given by

$$\log M_{\rm lim}(t)~=~6+0.4 \times(M_R(t)+29.62-R_{\rm lim}).$$ (2)

We have adopted the R magnitudes to calculate the observed lower limits of the distributions for two reasons: (a) all clusters were detected in the R band and (b) the effect of extinction is small in the R band. The resulting relation between $M_{\rm lim}$ and age is shown in Fig. 6 for detection limits of $R_{\rm lim}$= 22.0 and 23.0 mag. We will use these limits later, in Sect. 5, to explain the distribution of clusters in the mass versus age diagram.

Figure 6: The relation between the critical initial mass $M_{\rm lim}$ and age, derived for two values of the R-band magnitude limit; 22.0 and 23.0 mag. It is calculated from the Starburst99 cluster models, for a distance of 8.4 Mpc and no extinction. Only clusters with an initial mass higher than $M_{\rm lim}$ can be detected as faint as $R_{\rm lim}$ at time t. Alternatively, clusters with a mass $M_{\rm lim}$ can only be detected down to a magnitude $R_{\rm lim}$ when they are younger than the age t, indicated by these relations.

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Figure 7 shows the variations of the colours of the Starburst99 models for solar metallicity and with an upper mass limit of 30 $M_{\odot }$. The figure shows that the colours do not change monotonically, but that there are peaks and dips, especially in the age range of $6.5 < \log(t) < 7.3$. These are related to the phases of the appearance of red supergiants that also produced the dips in the limiting magnitude curves of Fig. 6.

   
4.3 The Frascati models

Since the Starburst99 models only cover the age range up to 1 Gyr, we also used synthetic cluster models for older ages from the Frascati group. These "Frascati-models'' were calculated by Romaniello (1998) from the evolutionary tracks of Brocato & Castellani (1993) and Cassisi et al. (1994) using the HST-WFPC2 magnitudes derived from the stellar atmosphere models by Kurucz (1993). These models are for instantaneous formation of a cluster of solar metallicity stars in the mass range of 0.6 to 25 $M_{\odot }$, with a total initial mass of 50 000 $M_{\odot }$, distributed according to Salpeter's IMF. These models cover an age range of 10 to 5000 Myr. There are 48 models with timesteps increasing from 10 Myr for the youngest ones to 500 Myr for the oldest ones. We have increased the magnitudes of the Frascati models by -3.526 mag in order to scale these models to a total mass of 10⁶ $M_{\odot }$ in the mass range of 1.0 to 25 $M_{\odot }$; i.e. -3.25 mag correction for the conversion from $5\times 10^4$ to $1\times 10^6$ $M_{\odot }$, and 0.279 mag correction for the conversion from a lower stellar mass limit of 0.6 $M_{\odot }$ to 1.0 $M_{\odot }$. In this way the masses can be compared directly with those of the Starburst99 models.

The Starburst99 models are expected to be more accurate for the younger clusters, because they are based on the evolutionary tracks of the Geneva-group which include massive stars. The Frascati models are expected to be more accurate for the old clusters, because they include stars with masses down to 0.6 $M_{\odot }$.

	Figure 7: The variations of colours with age of the Starburst99 models of Z=0.02 and an upper mass limit of 30 $M_{\odot }$. Notice the periods of rapid variability near the peaks and dips around $t \simeq 6$ and 16 Myrs, $\log (t) \simeq 6.8$ and 7.2.
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4.4 The extinction curve

To determine the values of E(B-V) of the clusters we assume the mean galactic reddening law. Lamers et al. (2002) and Scuderi et al. (2002) have shown that the extinction law of respectively the bulge and the core of M 51 agree very well with the galactic law. The values of R_i=A_i/E(B-V) for the HST-WFPC2 filters have been calculated by Romaniello (1998). They are respectively 4.97, 4.13, 3.11, 2.41 and 1.91 for the U, B, V, R and I bands.

In the fitting of the energy distributions we did not take into account the disruption of clusters. We assumed that the stars contribute to the total energy distribution of the clusters until the cluster is completely dissolved and is no longer detectable as a point source. This is a reasonable assumption because we measured the magnitudes in a circle of 12 pc radius (see Sect. 2).

Figure 8: Example of some fits. The filled dots represent the observed energy distributions of objects measured in at least four bands, with their error bars in magnitude versus wavelength (in $\mu$m). In several cases the error bars are smaller than the size of the dots. Crosses indicate magnitude lower limits. The parameters of the fits are indicated in an array $(E(B-V),~\log(t),~\log(\mbox{$M_{\rm cl}$ }))$. The second array gives the uncertainties in these parameters. The line is the best fit obtained with the maximum likelihood method. Top figures: fits with $\mbox{$\chi^2_{\nu}$ }< 1$; bottom figures: fits with $\mbox{$\chi^2_{\nu}$ }\simeq 3$. Notice that the uncertainty of the fit parameters depends not only on $\chi _{\nu }^2$ but also strongly on the quality of the data. For instance, the errors in the magnitudes of the last two clusters are very small, so that the fit parameters are accurate, despite the high value of $\chi _{\nu }^2$.

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5 Fitting the observed energy distributions to observed cluster models

   
5.1 The fitting procedure

We have fitted the energy distributions of the clusters with good photometry in four or more filters, viz. UBVRI, BVRI, UVRI and UBVR (see Table 1), with the energy distributions of the cluster evolutionary synthesis models, discussed above, using a three dimensional maximum likelihood method. The three fitting parameters are: the age of the cluster (t), the reddening (E(B-V)) and the initial mass of the cluster (M). For the clusters detected in only three filters we reduce the parameter space and make a two dimensional maximum likelihood fit. For objects not detected in a band, we adopted the magnitude lower limits (described in Sect. 3) to check which fits were acceptable.

   
5.2 Three dimensional maximum likelihood method

This method was applied to sources that are detected in at least four bands. We fitted the observed energy distributions with those predicted for the Starburst99 cluster models and the Frascati models (see Sect. 4.2). For each model-age we have two fitting parameters M and E(B-V). The cluster models are for an initial cluster mass of 10⁶ $M_{\odot }$. For other masses the flux simply scales $M/10^6~\mbox{$M_{\odot}$ }$. We have adopted an uncertainty in the model fluxes of 5 percent (0.05 mag) in all bands.

To reduce the range in masses in the parameter space, we make an initial guess of the cluster mass based on the observed magnitudes, since the distance to M 51 is known. By calculating the average difference in magnitude - weighted by the errors - between the theoretical energy distribution for 10⁶ $M_{\odot }$ and the observed one, we have a good first approximation of the mass of the cluster:

 

$$M_{\rm guess}(E(B-V),\tau) \simeq \frac{\sum_{\lambda} 1/\sigma_{... ...- m_{\lambda}^{\rm mod}(E(B-V),\tau)\right\}}{\sum_{\lambda}1/\sigma_{\lambda}}$$ (3)

with E(B-V) between 0.0 and 2.0 in steps of 0.02, where $\sigma$ is the uncertainty in the magnitude. This is a reasonable range, compared to the average colour excess for the bulge of 0.2 found by Lamers et al. (2002). With this initial guess we then make a three dimensional likelihood analysis, using a mass range from 1/1.5 to 1.5 times the initial mass estimate in steps of 0.004 dex. The extinction was varied between 0.0 and 2.0 in steps of 0.01 and the age was varied between 0.1 Myr and 1 Gyr for the Starburst99 models and between 10 Myr to 5 Gyr for the Frascati models.

For every fit we obtain a value for the reduced $\chi^2$, i.e. $\chi^2_{\nu}$ = $\chi^2$/$\nu$, where $\nu$ is the number of free parameters i.e. the number of the observed data points minus the number of parameters in the theoretical model. For a good fit, $\chi^2_{\nu}$ should be about unity. We checked that the fits were consistent with the faint magnitude limits of the filters in which the object was not detected. If not, the fit was rejected. The fit with the minimum value of $\chi^2_{\nu}$ was adopted as the best fit and the corresponding values of E(B-V), age and M_i were adopted. This method was applied for fits with the four sets of the Starburst99 models and with the Frascati models. Figure 8 shows some examples of the results of the fitting process.

To estimate the uncertainty in the determined parameters we use confidence limits. If $\mbox{$\chi^2_{\nu}$ }< \mbox{$\chi^2_{\nu}$ }(\min)+1$ then the resulting parameters, i.e. $\log (t)$, $\log (M_i)$ and E(B-V), are within the 68.3% probability range. So the accepted ranges in age, mass and extinction are derived from the fits which have $\mbox{$\chi^2_{\nu}$ }(\min) < \mbox{$\chi^2_{\nu}$ }< \mbox{$\chi^2_{\nu}$ }(\min)+1$. With this method we derived the ages, initial masses and extinction with their uncertainties of 602 clusters.

Figure 9 shows a histogram of number of clusters as function of E(B-V). We will use this distribution for the two dimensional maximum likelihood fit of clusters detected in three bands only. The redding is small: 90% of the clusters have a reddening lower than 0.40; 67% of the clusters have a reddening lower than 0.18 and 23% have no detectable reddening.

   
5.3 Two dimensional maximum likelihood method

For the clusters observed in only three bands, it is not possible to make a three dimensional maximum likelihood fit. To reduce the parameter space we adopted the probability distribution of E(B-V) in the range of E(B-V) between 0.0 and 0.4, as shown in Fig. 9. For every value of E(B-V) between 0.0 and 0.40 (in steps of 0.02) and for every age of the model cluster, we first determine the mass of the cluster by means of Eq. (3). The results of the three dimensional fits have shown this is a good approximation. This results in a maximum likelihood age of the cluster for every value of E(B-V).

The $\chi^2_{\nu}$ which comes out from the two dimensional maximum likelihood method is used to distinguish between the accepted and rejected fits. For the parameter $\nu$ we used a value of 3-1=2, because we only fit the age of the cluster. The mass of the cluster comes from the scaling of the magnitudes to the best-fit model. A fit is accepted if it agrees with the lower magnitude limits in the filters where it was not measured. To determine the age of the cluster, we average the ages, weighted by the probability that each particular value of E(B-V) occurs, derived by normalizing the distribution in Fig. 9 in the range of 0.0 < E(B-V)<0.40. The error in the age is determined by calculating the value of the standard deviation $\sigma$ of the age, again weighted with the probability that the value of E(B-V) occurs. The value of E(B-V) is determined by using the one which belongs to the model with the age closest to the average age. The initial mass of the cluster is then calculated by Eq. (3) for the adopted value of E(B-V). With this method we derived the age, initial mass and the extinction of 275 clusters, using both the Starburst99 models and the Frascati models.

   
5.4 Starburst99 or Frascati models?

We have compared the energy distributions of the objects with five sets of models: four sets of Starburst99 models, with $Z=Z_{\odot}$ or $2 ~ Z_\odot$ and $\mbox{$M_{\rm up}$ }=30$ or 100 $M_{\odot }$, and the Frascati models with $Z=Z_{\odot}$ and $\mbox{$M_{\rm up}$ }=25$ $M_{\odot }$. Based on the lack of [OIII] emission we adopt the models with $\mbox{$M_{\rm up}$ }=25$ or 30 $M_{\odot }$. The models with $\mbox{$M_{\rm up}$ }=100$ $M_{\odot }$ are only used later to check the influence of this adopted upper limit on our results.

	Figure 9: Histogram of the values of E(B-V) from the fits with observations in BVRI and UBVRI. The extinction is small: 90% of the clusters have $\mbox{$E(B-V)$ }<0.40$.
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We have compared the ages derived from fitting the observed SEDs with the Starburst99 models and the Frascati models, for objects measured in at least four filters and with fits of $\mbox{$\chi^2_{\nu}$ }< 3.0$. We found that in the age range of 10 to 800 Myr there is a reasonable correlation between the results of the SB99 models and the Frascati models, with the Frascati models giving ages systematically about 0.4 dex smaller than the SB99 models. In this age range we adopt the SB99 models, because they are based on more reliable evolutionary tracks, better stellar atmosphere models and because the nebular continuum is included. We find that in this mass range the fits with the SB99 models have smaller $\mbox{$\chi_{\nu}^2$ }$ than the fits with the Frascati-models. For objects with ages above about 700 Myrs ( $\log (t) > 8.85$) the Frascati-models give the most reliable fits with smaller $\mbox{$\chi_{\nu}^2$ }$ than the SB99 models. This is probably because the lower mass limit of the SB99 models is 1 $M_{\odot }$, and the Frascati models go down to 0.6 $M_{\odot }$. Moreover the SB99 models do not go beyond 1 Gyr. Based on this comparison we adopt the SB99 fits for ages less than 700 Myrs and the results of the Frascati models for older ages.

   
5.5 Uncertainties in the derived parameters

The determination of the cluster parameters, age, mass and extinction, by means of the two or thee dimensional maximum likelihood fitting method, i.e. the 3(2)DEF-method, results not only in the values of $\log(\mbox{$M_{\rm cl}$ })$, $\log (t)$ and E(B-V) but also in their maximum and minimum acceptable values. The best-fit values are not necessarily in the middle of the minimum and the maximum values. If we define the uncertainties in the parameters, $\Delta E(B-V)$, $\Delta \log(\mbox{$M_{\rm cl}$ })$ and $\Delta \log(t)$ as half the difference between the maximum and mimimum values, we find that 30 percent of the clusters have $\Delta E(B-V)<0.08$, 50 percent have $\Delta E(B-V)<0.11$ and 70 percent have $\Delta E(B-V)<0.15$. For the uncertainties in the mass determination we find $\Delta \log(\mbox{$M_{\rm cl}$ })<0.20$, <0.33 and <0.55 for 30, 50 and 70 percent of the clusters respectively. For the uncertainties in the age determination we find $\Delta \log(t)<0.23$, <0.39 and <0.69 for 30, 50 and 70 percent of the clusters respectively. Taking the values for 50 percent of the clusters as representative, we conclude that the uncertainties are $\Delta E(B-V)\simeq 0.11$, $\Delta \log(\mbox{$M_{\rm cl}$ }) \simeq 0.33$ and $\Delta \log(t) \simeq 0.39$.

   
5.6 Contamination of the cluster sample by stars?

To estimate the number of stars that may contaminate our cluster sample we use the stellar population in the solar neighbourhood. From the tabulated stellar densities as a function of spectral type (Allen 1976) we derived the number of stars brighter than a certain value of M_V per pc³. Using the mass density of $0.13~ \mbox{$M_{\odot}$ }$pc^-3, we derived the number of stars per unit stellar mass. The results are listed in Table 2. The total stellar mass of the observed region of M 51 (see Fig. 2) is estimated to be about 1/20 of the total mass of $5\times 10^{10}$ $M_{\odot }$ in the disk of that galaxy (Athanassoula et al. 1987), i.e. about $2.5\times 10^{9}$ $M_{\odot }$. This implies that we can expect the following numbers of stars brighter than M_V<-6.5 per spectral type in the observed region: 4 (O), 13 (B), 6 (A), 6 (F), 6 (G), <1 (K) and <1 (M). So we can expect of the order of 40 bright stars with M_V<-6.5 in the observed region of M 51. However, these are all massive young supergiants of which the vast majority will be in clusters! So the number of bright stars outside clusters, that may contaminate our sample of clusters will be considerable smaller, and we expect it to be smaller than about 20 out of the total sample of 877. Moreover, we have shown above, from the lack of O[III] emission, that the clusters in M 51 have a shortage of massive stars with M>30 $M_{\odot }$. We can expect this effect also to occur for the massive field stars. This would reduce the number of expected contaminating stars even further. Tests have shown that a considerable fraction of possibly remaining stellar sources will be eliminated by the requirement that their energy distribution should fit that of cluster models within a given accuracy. Based on all these considerations, we conclude that contamination of our cluster sample with very massive stars of M_V<-6.5 outside clusters is expected to be negligible.

 

 

Table 2: Numbers of stars above a certain absolute magnitude limit in the solar neighbourhood.

Limit	O	B	A	F	G	K	M	Total
MV < -5.5	-8.3	-7.6	-8.0	-7.4	-7.4	-8.5	-8.5	-6.9
MV < -6.5	-8.8	-8.3	-8.6	-8.6	-8.6	<-9.5	<-9.5	-7.9
MV < -7.5	-9.8	-9.3	-9.6	-9.6	-9.6	<-10.5	<-10.5	-8.9

(1) The data are in log (Number/per $M_{\odot }$).
(2) The number of stars with M_V<-7.5 was estimated to be about 10 times smaller than for M_V<-6.5 because of the small number
of very massive stars formed, and their short evolution time.

   
6 The mass versus age distribution

We discuss the results from the fitting of the observed energy distributions to those of cluster models with solar metallicity and with and upper mass limit of 30 $M_{\odot }$. We have checked that the fits with twice solar metallicity and with an upper limit of 100 $M_{\odot }$ give about the same results.

Figure 10 shows the mass versus age distribution of sources with M_v<-7.5 (to eliminate possible stellar sources) and with energy distributions that could be fitted to that of a cluster models with an accuracy of $\mbox{$\chi^2_{\nu}$ }\le 3.0$. (The distributions for clusters with $\mbox{$\chi^2_{\nu}$ }\le 1$ or 10, not shown here, show the same distribution, but with 294 and 508 clusters respectively.) We see that the lower limit of the mass increases with increasing age, from about 1000 $M_{\odot }$ at $t\simeq 5$ Myrs to about $5\times 10^4$ $M_{\odot }$ at 1 Gyr. This is due to the expected effect of fading of the clusters as they age (see Sect. 4.1). The full line in the figure is the fading line in the R magnitude for clusters which have a limiting magnitude of $R_{\rm lim}=22.0$ at the distance of M 51 for a reddening of E(B-V) = 0. The line in Fig. 10 thus gives the mass of the clusters, that reaches this magnitude detection limit, as a function of age.

Figure 10: The mass versus age relation of the 392 clusters with MV < -7.5, whose energy distribution could be fitted with an accuracy of $\mbox{$\chi^2_{\nu}$ }< 3.0$. The cross shows the characteristic uncertainties (Sect. 5.5). The full line is the predicted fading line due to the evolution of clusters with E(B-V) = 0 and with a limiting magnitude of $R_{\rm lim}=22.0$ at the distance of M 51. This line roughly agrees with the observed lower limit. The distribution is discussed in the text.

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These initial mass versus age distribution of the clusters in Fig. 10 show the following characteristics:
- (i) The lower mass limit increases with age due to the fading of the clusters. The observed lower limit agrees with the predicted ones for the R band. There are even hints of the presence of the predicted dips in the lower limit near $\log(t)=6.8$ and 7.2. This strengthens our confidence in the adopted models.
- (ii) There are clear concentrations in the distribution at $\log(t)=6.70$ and 7.45 and possibly also around $\log(t) \simeq 7.2$. These are due to the properties of the cluster models and the adopted method. In Fig. 7 we have shown that the colours of the models do not change monotonically with time, but that there are phases when the colours change rapidly with time. These phases occur in the range of $6.5 < \log(t) < 7.3$. Large changes in the colours of the models occur just before and after the peaks where the slopes of the curves in Fig. 7 are large. It is more difficult to fit the observed energy distributions with high accuracy to models in the age range when the spectral changes are large, than in the age range when the changes are small. So there is a tendency of the model fits to concentrate in agebins just outside the age-regions of large spectral changes. This explains the concentrations and the voids in the derived age distributions of the clusters between about $6.5 < \log(t) < 7.5$.
- (iii) The density of the points drops at $\log(t) > 7.5$. Since the age scale is logarithmic, we might have expected an increasing density of points towards the higher ages, which is not observed. This is due to the disruption or dispersion of the clusters (see first paragraphs of Sect. 7).

We conclude that the mass versus age distribution agrees with the expected evolutionary fading of the clusters and that the decrease in numbers of clusters with age shows the affect of disruption/dispersion of clusters with time. The concentrations of the clusters at ages around $\log(t)=6.8$, 7.2 and 7.45 are due to statistical effects and do not represent periods of enhanced cluster formation.

   
7 The cluster initial mass function

The data in Fig. 10 and the detailed study of this distribution by Boutloukos & Lamers (2002) show that the clusters in the inner spiral arms of M 51 disrupt on a time scale of about tens of Myrs. In fact, these authors derived the dependence of the disruption time on the initial mass of the clusters in the inner spiral arms of M 51 as

$$\log t_{\rm disr} = \log t_4 ~+~\gamma \times \log (M_{\rm cl}/10^4~\mbox{$M_{\odot}$ })$$ (4)

with $\log t_4 = 7.64 \pm 0.22$ and $\gamma=0.62 \pm 0.06$ for the mass range of $3 \le \log (\mbox{$M_{\rm cl}$ }/ \mbox{$M_{\odot}$ }) \le 5.2$, where $M_{\rm cl}$ is the initial mass of the cluster. We see that clusters with an initial mass larger than 10⁴ $M_{\odot }$ survive $4\times10^7$ years. Clusters with an initial mass of only 10³ $M_{\odot }$ disrupt on a time scale of $1\times10^7$ yrs. This implies that the cluster initial mass function cannot be derived from the total sample of clusters, because the disruption will produce a strong bias towards the more massive clusters. However for the youngest clusters with ages less than about 10 Myr disruption is not yet an important effect and, therefore, these clusters can be used to derive the initial cluster mass function.

Figure 11: Histograms of the mass of clusters (in $\log M_{\rm cl}$) with an age of 10 Myrs or younger. The light shaded area shows the distribution of all 354 clusters. The dark shaded area shows the histogram of clusters with an accurate mass determination of $\Delta \log M_{\rm cl} < 0.25$. The steep part at $\log(M) < 3.0$ is due to the detection limit. The decrease at $\log(M) >3.0$ reflects the slope of the cluster IMF. (All masses have to be increased by a factor 2.1 if the lower limit of the stellar mass is 0.2 $M_{\odot }$ rather than the value of 1 $M_{\odot }$ that was adopted in the Starburst99 models.)

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Figure 11 shows the resulting mass distribution of clusters with an age less or equal to 10 Myr for two samples of clusters. The first sample contains all 354 clusters younger than 10 Myr. The second sample contains 168 clusters in the same age range but with a mass determination of $\Delta \log(\mbox{$M_{\rm cl}$ }) \le 0.25$. Both samples show the same characteristics: a steep increase in number between $2.5 < \log \mbox{$M_{\rm cl}$ }<3.0$ and a slow decrease to higher masses. The steep increase is due to the detection limit or the disruption of the low mass clusters. The slow decrease reflects the cluster initial mass function (CIMF). The decrease indicates that the clusters are formed with an CIMF that has a negative slope of ${\rm d}\log (N)/{\rm d}\log (M)$, as expected.

If the CIMF can be written as a power law of the type

$$N(M)~{\rm d}M~ \sim ~ M^{\alpha}~{\rm d}M~~~~~{\rm for}~~\mbox{$M_{\rm min}$ }<M<\mbox{$M_{\rm max}$ }$$ (5)

then the normalized cumulative distribution will be

 

$$\Sigma (M)=A - B\times M^{-\alpha+1}~~~~~{\rm with}$$

$$A=B \times \mbox{$M_{\rm min}$ }^{-\alpha+1}$$

$$B=\left(M_{\rm min}^{-\alpha+1}~-~M_{\rm max}^{-\alpha+1}\right)^{-1}\cdot$$ (6)

Figure 12 shows the observed and predicted normalized cumulative distribution of the 149 clusters with an age less than 10 Myr and with a mass $\mbox{$M_{\rm cl}$ }>2.5\times 10^3~\mbox{$M_{\odot}$ }$ that are used for the determination of the CIMF. We eliminated the clusters with $\mbox{$M_{\rm cl}$ }<2.5\times 10^3~\mbox{$M_{\odot}$ }$ from the sample because Fig. 11 shows that the sample may not be complete for smaller masses. The cumulative distributions of the 84 clusters of $M>2.5\times 10^3~\mbox{$M_{\odot}$ }$, younger than 10 Myr, which are fitted to the models with an accuracy of $\mbox{$\chi^2_{\nu}$ }\le 3.0$, or of the 66 clusters with $\Delta \log(\mbox{$M_{\rm cl}$ }) \le 0.25$, not shown here, (where $\Delta \log(\mbox{$M_{\rm cl}$ })$ is the uncertainty in the mass determination), have the same shape as the distribution in Fig. 12. For these three samples we have determined the values of $\alpha$ and $M_{\rm min}$ by means of a linear regression under the reasonable assumption that $\mbox{$M_{\rm min}$ }\ll\mbox{$M_{\rm max}$ }$, which implies that $A \simeq 1$. The resulting values of $\alpha$ and $M_{\rm min}$ are listed in Table 3. The table shows that $\alpha \simeq 2.1$ for all three samples.

 

 

Table 3: The CIMF for clusters with t<10 Myr and $\mbox{$M_{\rm cl}$ }<2.5\times 10^3~\mbox{$M_{\odot}$ }$.

Sample	Nr	$\log \mbox{$M_{\rm min}$ }$	$\alpha$
All	149	3.49	2.12 $\pm$ 0.26
$\Delta \log \mbox{$M_{\rm cl}$ }< 0.25$	66	3.48	2.04 $\pm$ 0.41
$\mbox{$\chi^2_{\nu}$ }< 3.0$	82	3.46	2.16 $\pm$ 0.40

	Figure 12: The cumulative mass distribution of 149 clusters with an age less than 10 Myrs and an inital mass of $\log (M) > 3.40$. The full line is the best power-law fits for an IMF with the value of $\alpha$ and $M_{\rm min}$ from Table 3. The dashed line is the fit with $\alpha =2.00$.
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The predicted cumulative distribution with the derived values of $\alpha=2.12$ and $M_{\rm min}$ is shown in Fig. 12 (full line). The figure shows a slight underabundance of clusters in the range of $4.0 < \log (\mbox{$M_{\rm cl}$ }) < 4.3$ and a slight overabundance in the range of $\log (\mbox{$M_{\rm cl}$ })>4.3$. In fact, for the mass range of $3.5 < \log (\mbox{$M_{\rm cl}$ }) < 4.3$ a fit with $\alpha =2.00$, shown by dashed lines, fits the distribution excellently. We conclude that the CIMF of clusters younger than 10 Myr has a slope of $\alpha \simeq 2.1 \pm 0.3$ in the mass range of $3.0 < \log (\mbox{$M_{\rm cl}$ }) < 5.0$ and a slope of $2.00 \pm 0.05$ in the range of $3.0 < \log(\mbox{$M_{\rm cl}$ }) < 4.3~\mbox{$M_{\odot}$ }$.

The derived exponent of the cluster IMF is very similar to the value of $\alpha = 2.0$ of young clusters in the Antennae galaxies, as found by Zhang & Fall (1999). It shows that the IMF of clusters formed in the process of galaxy-galaxy interaction is very similar to the one of clusters formed in the spiral arms of a galaxy, long after the interaction. This mass distribution is also similar to that of giant molecular clouds (e.g. McKee 1999; Myers 1999). This may support the suggestion that the mass distribution of the clusters is determined by the mass distribution of the clouds from which they originate.

   
8 The cluster formation history

One of the goals of this paper is to study the influence of the interaction between M 51 and its companion on the cluster formation in the region of the inner spiral arms. To this purpose we compare the observed age distribution of the clusters with predictions for a constant cluster formation rate. This comparison is hampered by two effects: (a) the disruption of clusters and (b) the fading of clusters below the detection limit. The disruption time of the clusters in the inner spiral arms of M 51 is given by Eq. (4). We see that only clusters with an initial mass larger than about 10⁴ $M_{\odot }$ will survive more than 40 Myrs.

Figure 13 shows the histogram of the formation rates of the detected clusters, in number per Myr, for 140 clusters with $\mbox{$M_{\rm cl}$ }> 10^4$ $M_{\odot }$ and with an energy distribution that is fitted with an accuracy of $\mbox{$\chi^2_{\nu}$ }\le 3.0$. The sample of 111 clusters with $\mbox{$M_{\rm cl}$ }> 10^4$ $M_{\odot }$ and with an age uncertainty of $\Delta \log(t) < 0.25$, and the full sample of 285 clusters with $\mbox{$M_{\rm cl}$ }> 10^4$ $M_{\odot }$, not shown here, have a distribution very similar to the one shown in Fig. 12.

Figure 13: The formation rates of the observed clusters with an initial mass of $M_{\rm i} > 10^4$ $M_{\odot }$  in number per Myr, for clusters with an accuracy of the fit of the energy distribution of $\mbox{$\chi^2_{\nu}$ }\le 3.0$. The $1 \sigma$ uncertainty due to the Poisson statistics in each bin ( $\sigma = 1/\sqrt (N)$) is indicated. The diagram shows that the formation rate of the observed clusters decreases with age. This is due to the disruption of the older clusters.

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All three samples show about the same characteristics.
(a) There is a general trend of a decrease in the cluster formation rate towards increasing age.
(b) There is a steep drop around $\log(t)\simeq 7.5$. This drop is the result of the concentration of clusters at ages $\log(t)=7.45$ that was apparent in the mass versus age diagrams of Fig. 10, and was explained in Sect. 6.
(c) There is no clear evidence for a peak in the cluster formation rate near $\log(t)\simeq 8.6$, which is the time of the interaction of M 51 with its companion, and which is the age of the huge starburst in the nucleus of M 51. There is a hint of a small peak around $\log(t) \simeq 8.1$. However this peak is only $2 \sigma$ high. Its reality has to be verified with a larger sample of clusters.
(d) The peak in the last bin of 5 Gyr contains all the clusters ages older than 3 Gyr, because the cluster models that we used for fitting the energy distributions do not go beyond 5 Gyr.
We have checked that these characteristics are not the result of the binning process: the same features appear for different choices of the binning parameters.

The general decrease in the formation rate of the observed clusters is partly due to the evolutionary fading of the clusters and partly due to the disruption of clusters. In Sect. 6 and in Fig. 10 we have shown that clusters with an initial mass of 10⁴ $M_{\odot }$ fade below the detection limit when they are older than $\log(t)=8.2$. This can explain the decrease in the formation rate of clusters older than about 150 Myrs. However, clusters with $\mbox{$M_{\rm cl}$ }>10^4~\mbox{$M_{\odot}$ }$ and younger than about 100 Myr should still all be detectable. The fact that we see a decrease in the apparent cluster formation rate must thus be due to the disruption of clusters (unless for some unknown reason the cluster formation rate has been steadily increasing from 100 Myrs up to now, which we consider unlikely).

It is interesting that the CFR in the inner spiral arms of M 51, at a distance of about 1 to 3 kpc from the nucleus, does not show any evidence for a peak at the age of the strongest interaction of M 51 with its companion galaxy. The closest approach occurred about 250-400 Myrs ago according to the dynamical models of Barnes (1998) or 400-500 and 50-100 Myrs ago according to Salo & Laurikainen (2000). The only significant peak occurred at $\log(t) \simeq 7.4$. However we attributed this peak to the large changes in the energy distributions of the models in the age range of $6.5 < \log(t) < 7.5$, and not to a real increase in the CFR.

   
9 Summary and conclusions

We have studied images of the inner spiral arms of the interacting galaxy M 51 obtained with the HST-WFPC2 camera in broad-band UBVRI and in the narrow band H$\alpha$ and [OIII] filters. The study can be summarized as follows:

1.

We found a total of 877 point-like objects, which are probably clusters. Many of the clusters are strong H$\alpha$ emitters, but none of the clusters, not even the youngest ones, have an excess of radiation in the [OIII] line at 5007 Å (F502N-filter). This suggests that the upper mass limit of the stars in the clusters is about 25 to 30 $M_{\odot }$.

2.

We have compared their energy distributions with those of Starburst99 cluster models (Leitherer et al. 1999) for instantaneous star formation with a stellar IMF of exponent 2.35, solar metallicity, a lower and upper stellar mass limit of 1 $M_{\odot }$ and 30 $M_{\odot }$ respectively. The energy distributions were also compared with those of the Frascati models (Romaniello 1998). For clusters younger than 700 Myr the results from the fitting with the Starburst99 models were adopted because these models are more accurate for young clusters and the fits of the energy distributions are better than those of the Frascati models. For older clusters the results from the fits with the Frascati models were adopted.

3.

For clusters that were observed in four or five bands a three dimensional maximum likelihood method was used to derive the properties of the clusters from the comparison between the observed and predicted energy distributions. The free parameters are the age t and E(B-V), which together determined the shape of the energy distribution, and the initial cluster mass $M_{\rm cl}$ which determines the absolute magnitude. For clusters that were not observed in all bands, the empirically derived lower magnitudes limits were taken into account.

4.

For clusters that were observed in only three bands the age and mass were derived in a two-dimensional maximum likelihood fitting of the energy distributions, with t and $M_{\rm cl}$ as free parameters. The observed probability distribution of E(B-V) was used as a weighting factor in the fitting procedure.

5.

The histogram of E(B-V) is strongly peaked at very small $E(B-V) \simeq 0$. All cluster have a reddening smaller than E(B-V)<1.0 and 67% of the clusters have E(B-V)<0.18.

6.

We have analysed the observed clusters also with cluster models of higher metallicity, $Z=2\times Z_{\odot}$. These higher metallicity models fit the observations considerably worse than the solar metallicity models. For instance, for solar metallicity models the energy distribution of 294 clusters can be fitted with an accuracy of $\mbox{$\chi^2_{\nu}$ }\le 1.0$ and 392 with $\mbox{$\chi^2_{\nu}$ }\le 3.0$. For models with twice the solar metallicity these numbers are respectively 138 and 217. So the energy distributions of the clusters support the adopted solar metallicity.

7.

The clusters have masses in the range of $2.5 < \log (\mbox{$M_{\rm cl}$ }) < 5.7$ and ages of $\log(t) >5.0$. These masses are the initial masses of the clusters, i.e. the current mass corrected for stellar evolution effects, but not corrected for evaporation or disruption. All derived masses have to be multiplied by a factor 1.3 if the lower mass of the stars is 0.6 $M_{\odot }$, instead of the adopted 1 $M_{\odot }$, and by a factor 2.1 if the lower mass is 0.2 $M_{\odot }$, as found for the Orion Nebula cluster.

8.

The distribution of the clusters in a mass-versus-age diagram shows the predicted lower limit due to the evolutionary fading of the clusters, including the dips at $\log (t) \simeq 6.8$ and 7.1. Three apparent concentrations at $\log(t)=6.7$, 7.2 and 7.45 are not real but due to the properties of the cluster models used.

9.

About 60% of the clusters are younger than 40 Myr. The number of older clusters is much less than expected for a constant cluster formation rate. This is partly due to the evolutionary fading of low mass clusters below the detection limit, and partly due to the disruption of the clusters.

10.

The cluster initial mass function (CIMF) was derived from the cumulative mass distribution of clusters younger than 10 Myr, for which disruption has not occured. The CIMF has a slope of $\alpha = 2.1 \pm 0.3$ in the range of $3.0 < \log (\mbox{$M_{\rm cl}$ }) < 5.0$ and $\alpha= 2.00 \pm 0.05$ in the range of $3.0 < \log (\mbox{$M_{\rm cl}$ }) < 4.5$ $M_{\odot }$, for $N(\mbox{$M_{\rm cl}$ }) \sim \mbox{$M_{\rm cl}$ }^{-\alpha}$. This slope is the same to that found in the interacting Antennae galaxies (Zhang & Fall 1999). Zhang and Fall deived a power law slope of the CIMF of $\alpha=1.95 \pm 0.03$ and $2.00 \pm 0.04$ for two cluster samples of the Antennae galaxies. The good agreement between these slopes and the one found by us suggests that $\alpha$ is about the same for cluster formation triggered by strong galaxy-galaxy interactions, such as presently going on in the Antennae, as for cluster formation that is not dominated by the interactions.

11.

The age distribution of clusters with $\mbox{$M_{\rm cl}$ }> 10^4$ $M_{\odot }$, is used to derive the history of the cluster formation rate (CFR). There is a general trend of a decrease of the formation rate of the observed clusters with age. It is unlikely that the real CFR has been increasing continuously from about 1 Gyr to the present time. The decrease of the CFR with age of clusters younger than about 100 Myr cannot be due to evolutionary fading, but it is due to the disruption of clusters. For clusters older than 200 Myr the decrease of the derived CFR could, at least partly, be due to evolutionary fading.

12.

There is no evidence for a peak in the CFR at about 400 Myr, which is the time of the interaction of M 51 with its companion and the age of the huge starburst in the nucleus.

In a forthcoming paper we describe the cluster formation as a function of location in a large part of M 51, using the same methods as used here (Bastian et al. 2002). The disruption of clusters in M 51, derived from the results of the study presented here, are described by Boutloukos & Lamers (2002).

Acknowledgements

H.J.G.L.M.L. and N.B. are grateful to the Space Telescope Scence Institute for hospitality and financial support during several stays. We thank Claus Leitherer for help and advice in the calculation of the cluster models. Support for the SINS program GO-9114 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. N.B. ackowledges a grant from the Netherlands Organization for Scientific Research. We thank the unknown referee for constructive comments that resulted in an improvement of this paper.

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Online Material

  Table 4: Coordinates and HST-WFPC2 broad-band photometry of 881 clusters in the inner regions of the M51.

Explanation of columns:
(1) : an index number of all point sources
(2) : an old index number
(3) : the x-coordinate of the HST-WF2 chip
(4) : the y coordinate of the HST-WF2 chip
pixel (x=1,y=1) is RA(2000) 13h 29 m 55.90 s,    DEC(2000) = +47 degr 11 min 27.2 sec
pixel (x=800, y=800) is RA(2000) 13h 29 m 57.94 s,    DEC(2000) = +47 degr 13 min 16.6 sec
(5) through (16): magnitudes in the VEGAMAG system (Holtzman et al. 1995 PASP 107, 156)
magn 0.00 means: not observed (ouside the observed field)
magn 99.99 means: source too faint, only lower magn limit
lower magn. limits: F336W=20.0, F439W=22.0, F555W=22.0, F675W=21.5, F814W=21.0 (see paper)
(5) and (6) : magn and uncertainty in F255W filter
(7) and (8) : magn and uncertainty in F336W filter
(9) and (10): magn and uncertainty in F439W filter
(11) and (12): magn and uncertainty in F555W filter
(13) and (14): magn and uncertainty in F675W filter
(15) and (16): magn and uncertainty in F814W filter
(17): 6-digit code that summarizes the observations
first digit refers to F255W filter, last digit to F814W filter
0 = not observed (outside observed HST-field),
1 = observed magnitude
9 = lower magnitude limit only

 

i	i(old)	x	y	mag	$\Delta$mag	mag	$\Delta$mag	mag	$\Delta$mag	mag	$\Delta$mag	mag	$\Delta$mag	mag	$\Delta$mag	icode
				F255W	F255W	F336W	F336W	F439W	F439W	F555W	F555W	F675W	F675W	F814W	F814W
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)	(13)	(14)	(15)	(16)	(17)
1	1001	69.777	36.890	0.00	9.99	0.00	9.99	20.88	0.06	20.77	0.10	20.54	0.12	20.19	0.13	001111
2	1002	97.360	36.866	0.00	9.99	0.00	9.99	21.56	0.12	21.29	0.18	20.89	0.19	20.56	0.21	001111
3	1003	205.844	38.133	0.00	9.99	99.99	-9.99	18.70	0.02	18.72	0.04	18.53	0.04	18.53	0.04	091111
4	1004	303.164	38.382	0.00	9.99	99.99	-9.99	21.49	0.07	20.92	0.09	20.30	0.10	19.88	0.10	091111
5	1005	545.934	38.252	0.00	9.99	0.00	9.99	21.48	0.09	21.21	0.13	22.58	0.15	22.55	0.20	001111
6	1006	572.451	38.762	0.00	9.99	0.00	9.99	21.51	0.07	21.50	0.05	20.38	0.09	20.40	0.03	001111
7	1007	203.947	39.183	0.00	9.99	99.99	-9.99	18.70	0.02	18.72	0.04	18.60	0.04	18.53	0.04	091111
8	1008	525.198	39.474	0.00	9.99	0.00	9.99	21.27	0.08	21.90	0.06	21.80	0.08	20.29	0.14	001111
9	1009	566.688	38.493	0.00	9.99	0.00	9.99	21.66	0.08	22.20	0.06	22.08	0.08	20.58	0.16	001111
10	1010	52.926	39.867	0.00	9.99	0.00	9.99	20.95	0.02	20.60	0.03	20.21	0.02	19.84	0.01	001111
11	1011	76.592	39.070	0.00	9.99	0.00	9.99	20.74	0.06	20.68	0.10	20.43	0.11	20.82	0.06	001111
12	1012	429.070	39.393	0.00	9.99	99.99	-9.99	20.61	0.04	21.60	0.06	21.10	0.06	20.82	0.06	091111
13	1013	574.315	40.026	0.00	9.99	0.00	9.99	21.52	0.07	21.57	0.05	20.38	0.09	20.39	0.03	001111
14	1014	124.414	40.596	0.00	9.99	0.00	9.99	21.65	0.10	21.21	0.13	20.79	0.15	20.45	0.17	001111
15	1015	108.407	42.775	0.00	9.99	0.00	9.99	21.83	0.18	21.23	0.17	20.80	0.17	20.41	0.17	001111
16	1016	61.610	42.668	0.00	9.99	0.00	9.99	21.13	0.07	20.88	0.10	20.66	0.12	20.29	0.13	001111
17	1017	94.948	42.821	0.00	9.99	0.00	9.99	21.39	0.11	21.12	0.14	20.88	0.17	20.56	0.18	001111
18	1018	130.911	44.346	0.00	9.99	0.00	9.99	21.54	0.07	21.11	0.10	20.67	0.12	20.28	0.12	001111
19	1019	161.545	46.265	0.00	9.99	0.00	9.99	21.55	0.08	21.35	0.11	21.02	0.14	20.82	0.17	001111
20	1020	761.764	46.129	0.00	9.99	0.00	9.99	22.26	0.09	22.04	0.14	21.90	0.19	21.62	0.23	001111
21	1021	127.567	46.993	0.00	9.99	0.00	9.99	21.03	0.05	20.88	0.08	20.71	0.10	20.53	0.13	001111
22	1022	174.604	47.935	0.00	9.99	0.00	9.99	21.36	0.09	21.33	0.08	20.96	0.08	21.07	0.10	001111
23	1023	198.918	47.934	0.00	9.99	99.99	-9.99	20.26	0.04	20.21	0.04	19.98	0.03	19.77	0.04	091111
24	1024	285.837	48.290	0.00	9.99	99.99	-9.99	21.95	0.07	21.81	0.10	21.73	0.14	21.34	0.14	091111
25	1025	396.059	47.656	0.00	9.99	99.99	-9.99	21.88	0.15	21.69	0.11	21.31	0.10	20.78	0.09	091111
26	1026	410.019	49.293	0.00	9.99	99.99	-9.99	22.16	0.10	22.28	0.15	22.28	0.23	22.12	0.28	091111
27	1027	750.016	48.923	0.00	9.99	0.00	9.99	23.09	0.10	22.17	0.05	21.83	0.05	21.67	0.06	001111
28	1028	282.445	49.499	0.00	9.99	99.99	-9.99	21.99	0.07	21.75	0.09	21.67	0.12	21.33	0.12	091111
29	1029	321.740	49.780	0.00	9.99	99.99	-9.99	22.43	0.15	21.43	0.08	21.22	0.11	20.99	0.13	091111
30	1030	407.301	49.749	0.00	9.99	99.99	-9.99	22.22	0.11	22.28	0.15	22.28	0.23	22.12	0.28	091111
31	1031	466.216	50.264	0.00	9.99	99.99	-9.99	22.65	0.08	22.47	0.08	22.17	0.12	22.24	0.19	091111
32	1032	396.267	52.842	0.00	9.99	99.99	-9.99	22.54	0.16	21.76	0.10	21.74	0.11	21.42	0.12	091111
33	1033	114.423	53.970	0.00	9.99	0.00	9.99	20.39	0.03	20.36	0.04	20.07	0.04	19.85	0.04	001111
34	1034	121.414	55.540	0.00	9.99	0.00	9.99	20.12	0.03	20.04	0.04	19.82	0.03	19.41	0.02	001111
35	1035	268.249	55.877	0.00	9.99	99.99	-9.99	23.26	0.17	22.59	0.11	21.93	0.09	21.54	0.10	091111
36	1036	331.802	57.324	0.00	9.99	99.99	-9.99	20.74	0.03	20.39	0.04	19.89	0.04	19.96	0.04	091111
37	1037	535.170	56.934	0.00	9.99	0.00	9.99	21.97	0.07	22.04	0.09	21.87	0.09	21.49	0.10	001111
38	1038	116.142	56.934	0.00	9.99	0.00	9.99	20.27	0.03	20.36	0.04	20.07	0.04	19.85	0.04	001111
39	1039	167.955	57.502	0.00	9.99	0.00	9.99	20.44	0.05	20.51	0.06	20.56	0.08	20.33	0.08	001111
40	1040	170.836	58.538	0.00	9.99	0.00	9.99	20.44	0.05	20.52	0.06	20.56	0.08	20.33	0.08	001111
41	1041	525.110	58.058	0.00	9.99	0.00	9.99	21.93	0.06	21.70	0.05	21.48	0.05	21.35	0.06	001111
42	1042	166.230	59.921	0.00	9.99	0.00	9.99	20.44	0.05	20.51	0.06	20.50	0.09	20.33	0.08	001111
43	1043	112.343	60.052	0.00	9.99	0.00	9.99	21.70	0.08	21.72	0.08	21.44	0.08	21.00	0.08	001111
44	1044	305.707	60.538	0.00	9.99	99.99	-9.99	22.24	0.13	21.78	0.10	21.54	0.11	21.37	0.12	091111
45	1045	120.777	61.204	0.00	9.99	0.00	9.99	21.31	0.05	21.31	0.05	21.22	0.06	20.79	0.05	001111
46	1046	236.218	61.127	0.00	9.99	20.58	0.07	21.51	0.08	21.02	0.07	20.76	0.06	20.25	0.04	011111
47	1047	101.849	61.690	0.00	9.99	0.00	9.99	20.64	0.03	20.49	0.04	20.24	0.03	19.85	0.03	001111
48	1048	147.727	61.854	0.00	9.99	0.00	9.99	23.92	0.28	23.17	0.15	22.72	0.19	22.65	0.23	001111
49	1049	239.238	62.420	0.00	9.99	99.99	-9.99	21.32	0.06	21.02	0.07	20.46	0.05	20.25	0.04	091111
50	1050	333.120	61.344	0.00	9.99	99.99	-9.99	20.46	0.03	20.00	0.04	19.51	0.03	19.39	0.03	091111
51	1051	115.436	63.298	0.00	9.99	0.00	9.99	22.21	0.12	22.14	0.11	22.23	0.17	21.56	0.12	001111
52	1052	366.011	63.936	0.00	9.99	0.00	9.99	0.00	9.99	0.00	9.99	0.00	9.99	0.00	9.99	000000
53	1053	180.443	64.247	0.00	9.99	99.99	-9.99	21.19	0.06	21.33	0.07	21.29	0.09	21.10	0.10	091111
54	1054	186.320	65.387	0.00	9.99	99.99	-9.99	21.28	0.07	21.47	0.09	21.43	0.09	21.20	0.09	091111
55	1055	189.263	64.997	0.00	9.99	99.99	-9.99	21.30	0.07	21.47	0.09	21.43	0.09	21.20	0.09	091111
56	1056	295.339	65.924	0.00	9.99	99.99	-9.99	22.09	0.09	21.93	0.09	21.67	0.10	21.55	0.12	091111
57	1057	339.525	66.312	0.00	9.99	99.99	-9.99	20.46	0.03	21.16	0.07	21.28	0.12	20.65	0.09	091111
58	1058	704.435	65.891	0.00	9.99	0.00	9.99	20.96	0.02	19.69	0.03	18.78	0.02	18.27	0.01	001111
59	1059	120.354	66.506	0.00	9.99	0.00	9.99	21.88	0.10	21.91	0.10	21.62	0.09	21.33	0.10	001111
60	1060	205.697	67.172	0.00	9.99	99.99	-9.99	21.68	0.10	21.87	0.12	21.99	0.15	22.14	0.21	091111
61	1061	669.088	67.450	0.00	9.99	0.00	9.99	20.62	0.03	20.63	0.04	20.06	0.03	20.31	0.03	001111
62	1062	176.183	68.228	0.00	9.99	99.99	-9.99	21.54	0.14	21.65	0.18	20.87	0.09	21.02	0.11	091111
63	1063	525.031	69.065	0.00	9.99	0.00	9.99	20.53	0.03	20.47	0.04	20.24	0.04	19.76	0.03	001111
64	1064	346.036	70.244	0.00	9.99	99.99	-9.99	21.62	0.06	21.17	0.06	20.65	0.05	20.53	0.06	091111
65	1065	671.381	70.373	0.00	9.99	0.00	9.99	20.16	0.02	20.17	0.03	20.06	0.03	19.97	0.03	001111
66	1066	785.974	69.852	0.00	9.99	0.00	9.99	22.17	0.05	22.07	0.05	21.95	0.07	21.46	0.05	001111
67	1067	189.981	71.181	0.00	9.99	99.99	-9.99	21.49	0.09	21.62	0.10	21.47	0.09	21.34	0.11	091111
68	1068	346.184	71.762	0.00	9.99	99.99	-9.99	21.62	0.06	21.17	0.06	20.65	0.05	20.53	0.06	091111
69	1069	364.211	72.775	0.00	9.99	99.99	-9.99	22.45	0.13	22.28	0.13	21.46	0.09	22.18	0.23	091111
70	1070	668.342	73.060	0.00	9.99	0.00	9.99	20.16	0.02	20.17	0.03	20.06	0.03	19.97	0.03	001111
71	1071	242.968	73.628	0.00	9.99	99.99	-9.99	21.41	0.07	21.64	0.11	21.71	0.12	21.34	0.10	091111
72	1072	671.147	74.145	0.00	9.99	0.00	9.99	20.75	0.03	20.80	0.04	20.06	0.03	20.35	0.03	001111
73	1073	192.589	74.232	0.00	9.99	99.99	-9.99	21.43	0.09	21.42	0.09	20.94	0.06	21.08	0.09	091111
74	1074	186.513	75.468	0.00	9.99	99.99	-9.99	21.11	0.08	20.98	0.09	20.81	0.09	20.69	0.12	091111
75	1075	348.268	78.906	0.00	9.99	20.76	0.07	21.61	0.07	21.49	0.08	21.39	0.12	21.42	0.19	011111
76	1076	268.008	79.150	0.00	9.99	99.99	-9.99	21.96	0.06	21.47	0.05	21.11	0.05	20.68	0.04	091111
77	1077	386.075	80.239	0.00	9.99	99.99	-9.99	21.84	0.09	21.84	0.11	21.54	0.10	20.68	0.06	091111
78	1078	738.295	78.718	0.00	9.99	0.00	9.99	22.69	0.09	22.43	0.08	22.15	0.09	22.15	0.12	001111
79	1079	123.082	79.714	0.00	9.99	0.00	9.99	21.94	0.10	21.63	0.07	21.22	0.06	20.63	0.05	001111
80	1080	181.086	80.025	0.00	9.99	99.99	-9.99	21.07	0.11	21.04	0.13	20.94	0.14	20.61	0.13	091111
81	1081	346.778	78.771	0.00	9.99	20.76	0.07	21.61	0.07	21.49	0.08	21.39	0.12	21.42	0.19	011111
82	1082	366.021	80.299	0.00	9.99	99.99	-9.99	21.47	0.06	21.23	0.07	21.03	0.08	20.87	0.08	091111
83	1083	192.484	81.165	0.00	9.99	99.99	-9.99	21.35	0.10	21.49	0.12	21.64	0.15	21.34	0.15	091111
84	1084	384.795	80.218	0.00	9.99	99.99	-9.99	21.83	0.09	21.84	0.11	21.54	0.10	20.68	0.06	091111
85	1085	773.664	80.598	0.00	9.99	0.00	9.99	20.79	0.03	20.92	0.04	20.97	0.03	21.15	0.05	001111
86	1086	211.979	82.174	0.00	9.99	99.99	-9.99	20.99	0.05	21.03	0.06	21.15	0.07	20.67	0.06	091111
87	1087	778.906	81.590	0.00	9.99	0.00	9.99	21.71	0.04	21.76	0.05	20.97	0.03	22.12	0.10	001111
88	1088	353.643	82.627	0.00	9.99	99.99	-9.99	22.73	0.20	22.45	0.24	22.47	0.39	21.68	0.24	091111
89	1089	391.806	83.000	0.00	9.99	19.13	0.03	20.39	0.03	20.40	0.04	20.59	0.05	20.48	0.05	011111
90	1090	408.671	82.891	0.00	9.99	18.06	0.02	19.32	0.02	19.36	0.03	19.36	0.03	19.42	0.03	011111
91	1091	82.919	83.349	0.00	9.99	0.00	9.99	22.72	0.18	22.69	0.15	22.55	0.18	22.27	0.20	001111
92	1092	423.812	83.545	0.00	9.99	18.07	0.02	19.15	0.02	19.14	0.03	19.01	0.02	19.00	0.02	011111
93	1093	467.789	83.448	0.00	9.99	20.33	0.06	21.60	0.06	21.37	0.06	21.55	0.09	21.68	0.14	011111
94	1094	476.741	83.902	0.00	9.99	99.99	-9.99	22.85	0.17	22.57	0.16	22.66	0.26	22.12	0.19	091111
95	1095	405.152	84.295	0.00	9.99	99.99	-9.99	19.74	0.03	19.79	0.04	19.71	0.03	19.63	0.03	091111
96	1096	159.250	86.178	0.00	9.99	99.99	-9.99	19.94	0.02	19.05	0.03	18.27	0.02	18.06	0.01	091111
97	1097	212.126	85.818	0.00	9.99	99.99	-9.99	20.55	0.04	20.46	0.04	20.34	0.04	19.89	0.03	091111
98	1098	450.541	85.989	0.00	9.99	18.93	0.03	20.28	0.03	20.42	0.04	20.29	0.04	20.12	0.04	011111
99	1099	409.000	86.757	0.00	9.99	18.88	0.03	20.24	0.04	20.39	0.06	20.16	0.04	20.43	0.07	011111
100	1100	483.035	86.958	0.00	9.99	21.31	0.15	22.24	0.10	22.16	0.10	21.89	0.11	21.33	0.08	011111
101	1101	588.541	86.989	0.00	9.99	0.00	9.99	22.31	0.06	21.89	0.05	21.59	0.05	21.93	0.08	001111
102	1102	597.034	86.759	0.00	9.99	0.00	9.99	21.96	0.05	21.86	0.05	21.61	0.06	21.77	0.09	001111
103	1103	198.197	88.783	0.00	9.99	99.99	-9.99	17.02	0.02	17.46	0.03	17.22	0.02	16.98	0.01	091111
104	1104	458.209	88.552	0.00	9.99	17.94	0.02	19.24	0.02	19.20	0.03	19.04	0.02	18.95	0.01	011111
105	1105	209.861	88.742	0.00	9.99	99.99	-9.99	20.55	0.04	20.46	0.04	20.34	0.04	20.28	0.05	091111
106	1106	388.385	90.800	0.00	9.99	99.99	-9.99	21.84	0.14	21.88	0.16	22.01	0.18	21.84	0.20	091111
107	1107	399.189	88.331	0.00	9.99	17.93	0.02	19.31	0.02	19.45	0.03	19.50	0.03	19.47	0.02	011111
108	1108	729.687	88.669	0.00	9.99	0.00	9.99	22.01	0.05	21.69	0.05	21.87	0.06	21.55	0.06	001111
109	1109	223.098	89.655	0.00	9.99	99.99	-9.99	21.99	0.09	22.01	0.09	21.63	0.07	21.23	0.09	091111
110	1110	390.072	90.244	0.00	9.99	99.99	-9.99	21.84	0.14	21.87	0.16	22.01	0.18	21.84	0.20	091111
111	1111	209.734	91.168	0.00	9.99	99.99	-9.99	22.06	0.26	22.27	0.35	20.34	0.04	20.28	0.05	091111
112	1112	345.903	91.593	0.00	9.99	18.76	0.02	19.35	0.02	18.82	0.03	18.39	0.02	18.17	0.01	011111
113	1113	460.449	90.464	0.00	9.99	17.94	0.02	19.24	0.02	19.20	0.03	19.04	0.02	18.95	0.01	011111
114	1114	597.799	91.626	0.00	9.99	0.00	9.99	21.50	0.04	21.51	0.05	21.21	0.05	21.22	0.05	001111
115	1115	194.085	92.613	0.00	9.99	99.99	-9.99	17.02	0.02	17.46	0.03	17.22	0.02	16.98	0.01	091111
116	1116	209.184	92.871	0.00	9.99	99.99	-9.99	22.06	0.26	22.27	0.35	21.80	0.26	21.28	0.22	091111
117	1117	406.483	93.308	0.00	9.99	99.99	-9.99	20.58	0.06	20.68	0.08	21.30	0.12	20.58	0.06	091111
118	1118	469.206	93.455	0.00	9.99	99.99	-9.99	22.22	0.08	22.17	0.09	22.16	0.12	21.28	0.07	091111
119	1119	582.916	93.807	0.00	9.99	0.00	9.99	19.96	0.02	19.93	0.03	19.67	0.02	19.21	0.01	001111
120	1120	101.782	94.886	0.00	9.99	0.00	9.99	22.65	0.19	22.51	0.18	22.24	0.17	21.78	0.14	001111
121	1121	104.596	94.402	0.00	9.99	0.00	9.99	22.76	0.23	22.51	0.18	22.24	0.17	21.78	0.14	001111
122	1122	139.138	95.660	0.00	9.99	99.99	-9.99	22.30	0.10	22.30	0.11	21.57	0.07	21.39	0.08	091111
123	1123	347.252	95.184	0.00	9.99	18.76	0.02	19.35	0.02	18.82	0.03	18.39	0.02	18.17	0.01	011111
124	1124	493.441	94.515	0.00	9.99	17.48	0.02	18.92	0.02	19.03	0.03	18.70	0.02	19.01	0.02	011111
125	1125	266.074	96.110	0.00	9.99	99.99	-9.99	21.13	0.03	20.68	0.04	20.33	0.03	20.09	0.03	091111
126	1126	216.828	97.205	0.00	9.99	99.99	-9.99	18.40	0.02	18.41	0.03	18.24	0.02	17.85	0.01	091111
127	1127	384.477	96.464	0.00	9.99	20.58	0.12	21.58	0.10	21.51	0.11	21.42	0.11	21.29	0.12	011111
128	1128	406.785	97.398	0.00	9.99	18.51	0.04	19.87	0.04	20.02	0.05	20.08	0.04	20.05	0.05	011111
129	1129	466.305	96.946	0.00	9.99	99.99	-9.99	21.28	0.04	21.16	0.05	21.03	0.05	20.87	0.05	091111
130	1130	767.169	96.728	0.00	9.99	0.00	9.99	21.00	0.03	20.88	0.04	20.68	0.03	20.64	0.03	001111
131	1131	239.069	97.655	0.00	9.99	99.99	-9.99	22.62	0.23	22.22	0.18	21.72	0.13	21.13	0.11	091111
132	1132	390.721	97.974	0.00	9.99	20.34	0.10	21.42	0.10	21.35	0.08	21.06	0.06	21.05	0.08	011111
133	1133	369.027	100.096	0.00	9.99	99.99	-9.99	21.14	0.04	20.86	0.05	20.48	0.06	20.14	0.05	091111
134	1134	405.548	99.396	0.00	9.99	18.51	0.04	19.87	0.04	20.02	0.05	20.08	0.04	20.05	0.05	011111
135	1135	446.458	99.677	0.00	9.99	99.99	-9.99	21.17	0.05	21.23	0.05	21.15	0.06	20.90	0.06	091111
136	1136	281.218	101.232	0.00	9.99	99.99	-9.99	22.50	0.09	22.22	0.08	21.85	0.08	21.96	0.13	091111
137	1137	372.040	100.799	0.00	9.99	99.99	-9.99	21.14	0.04	20.86	0.05	20.48	0.06	20.14	0.05	091111
138	1138	410.868	100.796	0.00	9.99	19.05	0.05	20.21	0.04	20.23	0.05	20.18	0.04	19.85	0.04	011111
139	1139	511.848	101.836	0.00	9.99	99.99	-9.99	21.88	0.07	21.89	0.09	21.76	0.12	21.81	0.13	091111
140	1140	486.576	104.211	0.00	9.99	19.68	0.04	20.97	0.04	21.12	0.05	21.20	0.06	20.98	0.07	011111
141	1141	52.220	105.453	0.00	9.99	0.00	9.99	21.55	0.09	22.30	0.06	22.02	0.07	21.94	0.09	001111
142	1142	352.096	105.152	0.00	9.99	99.99	-9.99	22.38	0.14	22.11	0.15	21.63	0.14	21.67	0.20	091111
143	1143	377.968	104.546	0.00	9.99	20.58	0.09	21.65	0.11	21.66	0.14	21.43	0.16	21.48	0.19	011111
144	1144	453.135	104.413	0.00	9.99	99.99	-9.99	23.41	0.43	23.42	0.47	23.32	0.50	22.31	0.27	091111
145	1145	475.340	105.122	0.00	9.99	20.18	0.06	21.07	0.04	20.93	0.05	20.70	0.04	20.29	0.04	011111
146	1146	397.474	106.157	0.00	9.99	19.81	0.10	21.15	0.10	21.10	0.11	21.58	0.18	22.05	0.34	011111
147	1147	410.945	105.834	0.00	9.99	18.07	0.02	19.25	0.02	19.22	0.03	19.16	0.02	18.98	0.02	011111
148	1148	415.709	109.093	0.00	9.99	16.50	0.02	17.49	0.02	17.57	0.03	17.33	0.02	17.10	0.01	011111
149	1149	429.999	108.378	0.00	9.99	99.99	-9.99	21.36	0.07	21.46	0.07	21.58	0.09	21.40	0.11	091111
150	1150	245.238	109.357	0.00	9.99	99.99	-9.99	20.89	0.03	20.25	0.04	19.66	0.03	19.22	0.02	091111
151	1151	426.941	108.102	0.00	9.99	99.99	-9.99	21.36	0.08	21.50	0.10	21.58	0.09	21.40	0.11	091111
152	1152	473.021	109.365	0.00	9.99	19.86	0.04	20.79	0.03	20.85	0.04	20.83	0.04	20.62	0.04	011111
153	1153	430.416	108.867	0.00	9.99	99.99	-9.99	21.38	0.07	21.46	0.07	21.58	0.09	21.40	0.11	091111
154	1154	487.870	109.881	0.00	9.99	19.77	0.04	21.06	0.04	22.10	0.11	21.16	0.07	20.76	0.05	011111
155	1155	672.961	109.929	0.00	9.99	0.00	9.99	22.40	0.07	22.22	0.06	21.73	0.06	21.86	0.10	001111
156	1156	234.086	110.853	0.00	9.99	99.99	-9.99	22.20	0.13	21.92	0.17	22.02	0.26	21.53	0.23	091111
157	1157	525.969	111.427	0.00	9.99	19.75	0.03	20.73	0.03	20.68	0.04	20.57	0.04	20.51	0.04	011111
158	1158	613.295	111.807	0.00	9.99	0.00	9.99	22.65	0.09	22.54	0.08	22.44	0.09	22.08	0.10	001111
159	1159	135.102	113.381	0.00	9.99	99.99	-9.99	21.75	0.06	21.46	0.05	21.50	0.06	21.22	0.07	091111
160	1160	414.054	114.495	0.00	9.99	16.50	0.02	17.49	0.02	17.57	0.03	17.33	0.02	17.10	0.01	011111
161	1161	475.255	114.628	0.00	9.99	99.99	-9.99	21.26	0.06	21.45	0.08	21.13	0.08	21.53	0.13	091111
162	1162	496.061	114.045	0.00	9.99	99.99	-9.99	21.77	0.08	21.50	0.07	21.76	0.12	20.85	0.06	091111
163	1163	348.226	115.666	0.00	9.99	99.99	-9.99	21.84	0.06	21.35	0.05	20.98	0.05	20.69	0.06	091111
164	1164	522.145	115.464	0.00	9.99	18.57	0.02	19.63	0.02	19.54	0.03	19.33	0.02	19.09	0.01	011111
165	1165	446.677	116.857	0.00	9.99	99.99	-9.99	21.89	0.08	21.80	0.08	21.57	0.08	21.35	0.10	091111
166	1166	451.367	116.589	0.00	9.99	20.67	0.09	22.14	0.12	22.15	0.14	22.15	0.15	21.70	0.13	011111
167	1167	541.180	116.845	0.00	9.99	99.99	-9.99	22.40	0.07	22.51	0.09	22.50	0.14	22.53	0.15	091111
168	1168	469.400	118.084	0.00	9.99	21.37	0.17	22.78	0.19	22.19	0.11	21.27	0.08	22.32	0.26	011111
169	1169	716.418	118.179	0.00	9.99	0.00	9.99	24.18	0.31	22.61	0.08	21.83	0.06	21.41	0.06	001111
170	1170	459.401	119.990	0.00	9.99	18.72	0.02	20.07	0.02	20.14	0.04	20.04	0.03	19.69	0.02	011111
171	1171	471.780	119.950	0.00	9.99	21.37	0.17	22.78	0.19	22.13	0.11	22.30	0.20	22.32	0.26	011111
172	1172	416.513	120.609	0.00	9.99	99.99	-9.99	20.41	0.03	20.33	0.04	17.33	0.02	19.87	0.04	091111
173	1173	486.892	120.683	0.00	9.99	99.99	-9.99	21.18	0.07	21.28	0.08	20.64	0.05	20.61	0.06	091111
174	1174	476.982	122.271	0.00	9.99	99.99	-9.99	21.62	0.08	21.38	0.08	20.48	0.05	21.11	0.10	091111
175	1175	647.727	123.019	0.00	9.99	0.00	9.99	22.46	0.08	22.03	0.08	21.40	0.06	20.69	0.04	001111
176	1176	153.655	124.498	0.00	9.99	99.99	-9.99	21.89	0.07	21.70	0.07	21.33	0.06	21.16	0.08	091111
177	1177	440.604	124.492	0.00	9.99	99.99	-9.99	22.19	0.17	22.38	0.22	21.89	0.17	21.91	0.25	091111
178	1178	486.491	123.202	0.00	9.99	99.99	-9.99	21.18	0.07	21.28	0.08	20.64	0.05	20.61	0.06	091111
179	1179	135.862	124.935	0.00	9.99	99.99	-9.99	24.84	0.88	23.09	0.20	22.19	0.11	22.06	0.14	091111
180	1180	406.409	126.653	0.00	9.99	99.99	-9.99	21.91	0.13	21.73	0.12	21.41	0.12	21.12	0.12	091111
181	1181	440.482	126.922	0.00	9.99	99.99	-9.99	22.16	0.17	22.57	0.29	21.84	0.16	21.91	0.25	091111
182	1182	517.099	127.917	0.00	9.99	99.99	-9.99	22.86	0.11	22.65	0.11	22.31	0.11	21.82	0.11	091111
183	1183	297.191	128.703	0.00	9.99	99.99	-9.99	20.86	0.03	20.90	0.04	20.84	0.04	20.83	0.06	091111
184	1184	481.097	130.185	0.00	9.99	21.31	0.16	22.41	0.14	22.59	0.16	22.41	0.25	23.15	0.45	011111
185	1185	151.339	132.077	0.00	9.99	99.99	-9.99	20.64	0.03	20.50	0.04	20.23	0.03	19.89	0.03	091111
186	1186	154.151	132.335	0.00	9.99	99.99	-9.99	20.64	0.03	20.50	0.04	20.23	0.03	19.89	0.03	091111
187	1187	193.494	133.460	0.00	9.99	99.99	-9.99	23.27	0.14	22.44	0.08	21.93	0.08	21.66	0.09	091111
188	1188	498.866	133.593	0.00	9.99	99.99	-9.99	23.15	0.15	22.99	0.13	23.35	0.29	23.30	0.36	091111
189	1189	402.413	134.892	0.00	9.99	99.99	-9.99	22.72	0.17	22.03	0.10	21.64	0.09	21.22	0.09	091111
190	1190	550.386	135.865	0.00	9.99	99.99	-9.99	22.09	0.06	21.97	0.07	21.73	0.08	21.40	0.08	091111
191	1191	562.401	135.982	0.00	9.99	99.99	-9.99	22.98	0.17	23.07	0.19	22.89	0.24	23.56	0.55	091111
192	1192	431.855	136.863	0.00	9.99	19.62	0.04	20.92	0.05	21.06	0.07	20.92	0.06	21.08	0.09	011111
193	1193	317.895	137.896	0.00	9.99	19.94	0.03	21.20	0.03	21.14	0.05	20.85	0.05	21.24	0.09	011111
194	1194	428.466	137.245	0.00	9.99	19.61	0.04	21.08	0.06	21.22	0.09	21.22	0.09	21.45	0.13	011111
195	1195	437.186	137.972	0.00	9.99	99.99	-9.99	20.80	0.04	20.67	0.05	20.52	0.04	20.34	0.04	091111
196	1196	444.269	137.927	0.00	9.99	19.39	0.03	20.69	0.03	21.11	0.05	20.39	0.04	20.50	0.05	011111
197	1197	140.904	138.663	0.00	9.99	99.99	-9.99	23.99	0.42	22.65	0.13	21.65	0.07	21.16	0.06	091111
198	1198	379.244	139.400	0.00	9.99	99.99	-9.99	22.28	0.06	22.20	0.06	21.60	0.05	20.92	0.04	091111
199	1199	783.240	140.479	0.00	9.99	0.00	9.99	21.14	0.03	20.66	0.04	20.55	0.03	20.47	0.03	001111
200	1200	471.725	140.765	0.00	9.99	99.99	-9.99	22.43	0.12	22.33	0.12	21.73	0.09	21.52	0.10	091111
201	1201	143.796	142.576	0.00	9.99	99.99	-9.99	22.04	0.06	21.91	0.07	21.65	0.06	21.10	0.05	091111
202	1202	427.794	141.887	0.00	9.99	99.99	-9.99	21.80	0.08	21.86	0.13	21.75	0.13	21.99	0.21	091111
203	1203	442.189	141.829	0.00	9.99	99.99	-9.99	21.91	0.08	21.11	0.05	20.44	0.04	20.50	0.05	091111
204	1204	168.161	143.513	0.00	9.99	99.99	-9.99	21.92	0.08	21.81	0.09	21.53	0.09	21.31	0.10	091111
205	1205	317.332	142.152	0.00	9.99	99.99	-9.99	21.63	0.04	21.42	0.05	20.96	0.05	21.11	0.06	091111
206	1206	432.512	144.294	0.00	9.99	99.99	-9.99	21.50	0.05	21.11	0.05	20.77	0.05	20.60	0.05	091111
207	1207	458.792	145.245	0.00	9.99	99.99	-9.99	21.78	0.06	21.60	0.06	21.23	0.06	20.59	0.04	091111
208	1208	552.811	146.929	0.00	9.99	99.99	-9.99	21.95	0.07	21.83	0.08	21.33	0.07	20.70	0.05	091111
209	1209	652.383	146.002	0.00	9.99	0.00	9.99	23.06	0.11	22.52	0.07	22.30	0.08	22.03	0.09	001111
210	1210	165.547	147.420	0.00	9.99	99.99	-9.99	22.14	0.09	21.61	0.07	21.20	0.06	20.89	0.06	091111
211	1211	171.888	147.449	0.00	9.99	99.99	-9.99	21.63	0.05	21.52	0.05	21.16	0.05	20.97	0.06	091111
212	1213	482.922	150.388	0.00	9.99	0.00	9.99	0.00	9.99	0.00	9.99	0.00	9.99	0.00	9.99	000000
213	1212	563.034	148.772	0.00	9.99	99.99	-9.99	22.20	0.09	21.99	0.08	22.04	0.12	21.56	0.11	091111
214	1214	543.059	150.162	0.00	9.99	99.99	-9.99	21.96	0.06	21.81	0.07	21.47	0.07	20.79	0.05	091111
215	1215	551.958	151.297	0.00	9.99	18.59	0.02	19.68	0.02	19.68	0.03	19.55	0.02	19.20	0.02	011111
216	1216	625.650	150.977	0.00	9.99	0.00	9.99	23.17	0.13	21.56	0.04	20.44	0.03	19.48	0.01	001111
217	1217	554.317	152.134	0.00	9.99	18.59	0.02	19.68	0.02	19.68	0.03	19.56	0.02	19.20	0.02	011111
218	1218	173.014	152.422	0.00	9.99	99.99	-9.99	22.36	0.09	22.13	0.09	21.69	0.09	21.51	0.10	091111
219	1219	76.712	153.974	0.00	9.99	99.99	-9.99	21.67	0.04	21.41	0.05	21.06	0.04	20.61	0.03	091111
220	1220	449.109	155.155	0.00	9.99	99.99	-9.99	20.71	0.03	20.59	0.04	20.42	0.03	20.20	0.03	091111
221	1221	464.020	154.630	0.00	9.99	99.99	-9.99	22.77	0.13	22.54	0.13	22.34	0.15	21.35	0.08	091111
222	1222	576.236	154.866	0.00	9.99	99.99	-9.99	21.22	0.04	20.80	0.04	20.33	0.03	19.84	0.03	091111
223	1223	267.129	155.509	0.00	9.99	99.99	-9.99	23.58	0.13	22.63	0.07	22.15	0.08	21.80	0.08	091111
224	1224	440.125	156.231	0.00	9.99	99.99	-9.99	21.81	0.05	21.67	0.06	21.37	0.05	21.24	0.05	091111
225	1225	468.083	155.978	0.00	9.99	99.99	-9.99	22.59	0.13	22.54	0.14	21.98	0.10	21.28	0.09	091111
226	1226	197.650	156.911	0.00	9.99	99.99	-9.99	22.44	0.13	22.20	0.11	21.88	0.13	21.44	0.13	091111
227	1227	218.221	157.162	0.00	9.99	99.99	-9.99	21.47	0.05	21.29	0.05	20.93	0.05	20.77	0.06	091111
228	1228	586.927	157.341	0.00	9.99	0.00	9.99	18.79	0.02	18.42	0.03	18.00	0.02	17.42	0.01	001111
229	1229	712.688	158.235	0.00	9.99	0.00	9.99	22.66	0.07	22.31	0.07	21.81	0.07	21.74	0.08	001111
230	1230	774.800	158.757	0.00	9.99	0.00	9.99	21.98	0.06	22.00	0.06	21.41	0.08	21.58	0.08	001111
231	1231	170.856	160.297	0.00	9.99	99.99	-9.99	21.44	0.05	21.34	0.05	21.11	0.05	20.92	0.06	091111
232	1232	229.008	160.129	0.00	9.99	99.99	-9.99	17.67	0.02	19.86	0.04	19.88	0.03	19.59	0.03	091111
233	1233	511.266	159.796	0.00	9.99	99.99	-9.99	23.01	0.13	22.65	0.10	22.41	0.10	21.68	0.08	091111
234	1234	771.407	160.291	0.00	9.99	0.00	9.99	21.39	0.05	21.41	0.05	21.08	0.06	21.21	0.06	001111
235	1235	193.329	161.619	0.00	9.99	99.99	-9.99	21.63	0.07	21.44	0.07	21.22	0.07	20.95	0.07	091111
236	1236	444.023	161.916	0.00	9.99	99.99	-9.99	22.23	0.07	22.03	0.07	21.60	0.05	21.33	0.06	091111
237	1237	198.992	164.200	0.00	9.99	99.99	-9.99	21.91	0.12	21.87	0.14	21.94	0.17	21.58	0.17	091111
238	1238	250.978	163.745	0.00	9.99	99.99	-9.99	22.73	0.08	22.30	0.07	21.93	0.09	22.08	0.16	091111
239	1239	442.796	164.152	0.00	9.99	99.99	-9.99	22.25	0.07	21.86	0.06	21.60	0.05	21.33	0.06	091111
240	1240	178.263	164.472	0.00	9.99	99.99	-9.99	22.11	0.10	21.55	0.07	20.98	0.06	20.36	0.04	091111
241	1241	393.315	164.962	0.00	9.99	99.99	-9.99	22.36	0.07	21.85	0.06	21.39	0.06	21.19	0.07	091111
242	1242	477.204	165.177	0.00	9.99	99.99	-9.99	21.86	0.05	21.58	0.05	21.33	0.05	20.54	0.03	091111
243	1243	593.177	165.057	0.00	9.99	0.00	9.99	21.58	0.04	21.13	0.04	20.68	0.04	20.08	0.03	001111
244	1244	227.235	166.089	0.00	9.99	99.99	-9.99	17.67	0.02	17.85	0.03	17.70	0.02	17.66	0.01	091111
245	1245	530.638	165.648	0.00	9.99	99.99	-9.99	22.05	0.06	22.00	0.07	21.91	0.08	21.56	0.09	091111
246	1246	116.845	167.640	0.00	9.99	99.99	-9.99	22.70	0.09	22.63	0.08	22.59	0.10	22.14	0.10	091111
247	1247	209.038	169.004	0.00	9.99	99.99	-9.99	21.42	0.07	21.02	0.06	21.23	0.08	20.95	0.08	091111
248	1248	198.282	170.913	0.00	9.99	99.99	-9.99	21.54	0.06	21.52	0.06	21.42	0.07	20.97	0.06	091111
249	1249	469.180	171.103	0.00	9.99	99.99	-9.99	22.09	0.07	22.00	0.06	22.01	0.08	21.91	0.11	091111
250	1250	193.004	171.876	0.00	9.99	20.87	0.09	21.56	0.07	21.54	0.08	21.32	0.08	21.07	0.09	011111
251	1251	478.618	171.301	0.00	9.99	18.87	0.02	19.86	0.02	19.64	0.03	19.30	0.02	19.08	0.01	011111
252	1252	761.977	171.959	0.00	9.99	0.00	9.99	19.46	0.02	19.06	0.03	18.57	0.02	18.55	0.01	001111
253	1253	406.479	172.852	0.00	9.99	99.99	-9.99	21.64	0.04	21.40	0.05	21.07	0.06	21.09	0.07	091111
254	1254	125.184	174.287	0.00	9.99	99.99	-9.99	23.04	0.11	22.09	0.05	21.60	0.05	21.43	0.06	091111
255	1255	220.929	175.567	0.00	9.99	99.99	-9.99	22.01	0.15	22.38	0.20	21.16	0.10	22.49	0.40	091111
256	1256	238.557	176.754	0.00	9.99	99.99	-9.99	20.24	0.04	20.24	0.05	20.15	0.05	20.12	0.06	091111
257	1257	315.003	176.212	0.00	9.99	20.23	0.04	21.16	0.03	20.88	0.03	20.26	0.02	20.50	0.03	011111
258	1258	762.869	175.889	0.00	9.99	0.00	9.99	19.06	0.02	18.85	0.03	18.48	0.02	18.56	0.01	001111
259	1259	538.674	177.052	0.00	9.99	99.99	-9.99	22.73	0.08	22.03	0.06	21.39	0.05	21.17	0.05	091111
260	1260	221.525	179.227	0.00	9.99	99.99	-9.99	21.78	0.14	21.91	0.17	21.22	0.11	21.79	0.26	091111
261	1261	241.271	178.794	0.00	9.99	99.99	-9.99	20.24	0.04	19.91	0.04	20.15	0.05	20.11	0.06	091111
262	1262	96.085	179.939	0.00	9.99	99.99	-9.99	22.18	0.07	22.10	0.07	21.92	0.07	21.86	0.09	091111
263	1263	225.326	179.898	0.00	9.99	99.99	-9.99	21.57	0.15	21.60	0.19	21.36	0.17	21.51	0.24	091111
264	1264	275.185	180.237	0.00	9.99	99.99	-9.99	22.70	0.08	21.74	0.04	21.07	0.04	20.99	0.05	091111
265	1265	237.719	182.073	0.00	9.99	99.99	-9.99	19.88	0.03	19.91	0.04	19.74	0.04	19.46	0.03	091111
266	1266	243.732	181.948	0.00	9.99	99.99	-9.99	21.16	0.09	21.12	0.10	21.01	0.11	20.86	0.11	091111
267	1267	192.082	183.092	0.00	9.99	99.99	-9.99	22.34	0.10	21.76	0.07	21.46	0.07	21.18	0.07	091111
268	1268	231.755	183.316	0.00	9.99	99.99	-9.99	20.83	0.06	20.88	0.06	20.90	0.09	21.02	0.12	091111
269	1269	757.788	184.618	0.00	9.99	0.00	9.99	22.42	0.07	21.79	0.05	21.09	0.04	20.98	0.04	001111
270	1270	326.378	186.117	0.00	9.99	99.99	-9.99	21.88	0.05	21.33	0.04	20.88	0.04	20.69	0.04	091111
271	1271	693.326	185.736	0.00	9.99	0.00	9.99	23.49	0.12	22.74	0.07	22.67	0.09	22.17	0.09	001111
272	1272	93.590	187.158	0.00	9.99	99.99	-9.99	20.53	0.02	20.49	0.03	20.27	0.03	19.95	0.02	091111
273	1273	198.157	186.395	0.00	9.99	99.99	-9.99	23.08	0.21	22.76	0.17	22.14	0.11	21.66	0.10	091111
274	1274	251.995	186.998	0.00	9.99	21.25	0.20	22.25	0.21	22.20	0.21	21.98	0.22	22.04	0.28	011111
275	1275	234.903	190.884	0.00	9.99	99.99	-9.99	21.71	0.11	21.76	0.11	21.61	0.13	21.32	0.14	091111
276	1276	312.176	193.338	0.00	9.99	99.99	-9.99	23.10	0.14	22.32	0.08	21.74	0.07	21.36	0.07	091111
277	1277	177.685	194.908	0.00	9.99	99.99	-9.99	22.42	0.08	20.64	0.04	21.92	0.07	21.67	0.08	091111
278	1278	55.000	195.885	0.00	9.99	99.99	-9.99	21.76	0.05	22.05	0.05	21.81	0.05	21.75	0.06	091111
279	1279	98.305	195.650	0.00	9.99	99.99	-9.99	21.41	0.04	21.34	0.04	21.17	0.04	20.91	0.04	091111
280	1280	184.310	195.910	0.00	9.99	99.99	-9.99	21.73	0.04	22.17	0.07	21.67	0.06	21.25	0.05	091111
281	1281	239.130	196.182	0.00	9.99	19.78	0.06	20.77	0.06	20.73	0.06	20.49	0.06	20.05	0.05	011111
282	1282	257.804	196.094	0.00	9.99	99.99	-9.99	21.29	0.06	21.28	0.07	20.98	0.07	20.77	0.06	091111
283	1283	535.906	197.098	0.00	9.99	99.99	-9.99	21.78	0.04	21.39	0.04	20.97	0.03	20.59	0.03	091111
284	1284	113.560	200.205	0.00	9.99	99.99	-9.99	22.54	0.08	22.42	0.07	22.19	0.07	22.02	0.09	091111
285	1285	98.201	200.485	0.00	9.99	99.99	-9.99	21.85	0.06	21.84	0.06	21.66	0.06	21.29	0.06	091111
286	1286	156.011	200.994	0.00	9.99	99.99	-9.99	22.16	0.06	22.20	0.06	22.00	0.07	21.94	0.08	091111
287	1287	745.025	203.105	0.00	9.99	0.00	9.99	22.36	0.07	22.00	0.06	21.64	0.06	21.35	0.05	001111
288	1288	219.665	203.973	0.00	9.99	99.99	-9.99	22.15	0.09	22.44	0.12	21.69	0.07	21.22	0.07	091111
289	1289	210.106	204.396	0.00	9.99	99.99	-9.99	21.27	0.04	21.29	0.05	21.17	0.05	20.91	0.05	091111
290	1290	246.936	206.467	0.00	9.99	99.99	-9.99	19.65	0.02	19.71	0.03	19.53	0.02	19.03	0.02	091111
291	1291	244.752	208.282	0.00	9.99	99.99	-9.99	19.65	0.02	19.71	0.03	19.53	0.02	19.03	0.01	091111
292	1292	249.136	210.442	0.00	9.99	99.99	-9.99	19.65	0.02	21.23	0.06	20.75	0.04	19.03	0.02	091111
293	1293	330.085	210.968	0.00	9.99	99.99	-9.99	22.93	0.08	22.92	0.08	22.81	0.11	23.13	0.21	091111
294	1294	581.383	210.739	0.00	9.99	99.99	-9.99	21.91	0.04	21.96	0.05	21.81	0.05	21.92	0.08	091111
295	1295	183.402	212.829	0.00	9.99	99.99	-9.99	22.51	0.10	22.24	0.08	22.17	0.09	21.81	0.08	091111
296	1296	237.546	213.026	0.00	9.99	99.99	-9.99	21.99	0.09	22.04	0.09	21.37	0.06	21.54	0.10	091111
297	1297	659.825	214.287	0.00	9.99	0.00	9.99	21.43	0.03	21.22	0.04	20.82	0.03	20.68	0.03	001111
298	1298	230.042	215.639	0.00	9.99	99.99	-9.99	21.58	0.06	21.40	0.05	21.34	0.06	21.20	0.07	091111
299	1299	383.854	216.066	0.00	9.99	99.99	-9.99	22.90	0.09	22.38	0.08	22.10	0.09	21.89	0.10	091111
300	1300	491.575	215.700	0.00	9.99	99.99	-9.99	21.56	0.04	21.36	0.04	21.10	0.04	20.89	0.04	091111
301	1301	243.092	216.722	0.00	9.99	21.36	0.15	22.26	0.14	21.98	0.12	21.68	0.10	21.47	0.11	011111
302	1302	678.140	217.986	0.00	9.99	0.00	9.99	23.76	0.20	23.25	0.12	23.20	0.20	24.42	0.79	001111
303	1303	695.466	218.089	0.00	9.99	0.00	9.99	23.00	0.09	22.36	0.06	21.90	0.05	21.71	0.07	001111
304	1304	234.841	218.825	0.00	9.99	99.99	-9.99	22.63	0.15	22.52	0.13	22.42	0.15	22.09	0.17	091111
305	1305	724.244	219.581	0.00	9.99	0.00	9.99	22.60	0.08	22.31	0.06	21.96	0.07	21.74	0.07	001111
306	1306	553.184	220.894	0.00	9.99	99.99	-9.99	22.82	0.08	22.41	0.06	21.87	0.05	21.59	0.07	091111
307	1307	114.751	222.439	0.00	9.99	99.99	-9.99	22.52	0.10	22.29	0.09	21.87	0.08	21.51	0.06	091111
308	1308	177.013	227.138	0.00	9.99	99.99	-9.99	21.96	0.06	22.17	0.08	22.34	0.11	22.85	0.24	091111
309	1309	498.134	226.436	0.00	9.99	19.26	0.03	20.36	0.02	20.29	0.03	19.84	0.02	20.20	0.03	011111
310	1310	114.117	229.568	0.00	9.99	99.99	-9.99	22.46	0.09	22.18	0.08	21.98	0.08	21.52	0.07	091111
311	1311	644.052	230.965	0.00	9.99	0.00	9.99	22.26	0.05	22.13	0.06	21.74	0.05	21.40	0.06	001111
312	1312	366.510	231.988	0.00	9.99	99.99	-9.99	22.69	0.08	22.29	0.06	21.94	0.07	21.70	0.08	091111
313	1313	188.896	232.238	0.00	9.99	99.99	-9.99	22.80	0.10	22.54	0.09	22.04	0.08	21.46	0.06	091111
314	1314	285.409	238.197	0.00	9.99	99.99	-9.99	22.50	0.09	22.15	0.07	21.83	0.07	21.32	0.05	091111
315	1315	369.496	237.240	0.00	9.99	99.99	-9.99	22.61	0.07	22.21	0.06	21.89	0.06	21.61	0.07	091111
316	1316	481.521	238.142	0.00	9.99	99.99	-9.99	23.27	0.11	21.52	0.04	21.53	0.04	21.19	0.04	091111
317	1317	781.069	239.560	0.00	9.99	0.00	9.99	22.86	0.11	22.82	0.09	22.86	0.12	22.68	0.16	001111
318	1318	790.452	241.712	0.00	9.99	0.00	9.99	22.62	0.09	22.56	0.07	22.36	0.09	22.02	0.11	001111
319	1319	509.446	243.256	0.00	9.99	99.99	-9.99	23.37	0.18	23.02	0.14	22.54	0.13	21.93	0.11	091111
320	1320	522.954	246.119	0.00	9.99	99.99	-9.99	23.28	0.18	22.46	0.10	22.01	0.11	21.83	0.12	091111
321	1321	384.379	248.110	0.00	9.99	99.99	-9.99	22.65	0.09	22.63	0.11	22.30	0.11	21.94	0.10	091111
322	1322	207.093	249.622	0.00	9.99	99.99	-9.99	22.61	0.09	22.37	0.08	22.11	0.08	21.96	0.10	091111
323	1323	257.423	251.784	0.00	9.99	99.99	-9.99	21.00	0.03	20.93	0.04	20.68	0.03	20.25	0.02	091111
324	1324	421.774	251.744	0.00	9.99	99.99	-9.99	22.61	0.07	22.44	0.08	22.09	0.09	21.70	0.08	091111
325	1325	612.788	251.916	0.00	9.99	99.99	-9.99	22.79	0.12	22.50	0.10	22.14	0.09	22.18	0.13	091111
326	1326	638.086	252.501	0.00	9.99	99.99	-9.99	22.55	0.08	22.52	0.09	22.24	0.11	21.98	0.12	091111
327	1327	468.869	255.764	0.00	9.99	99.99	-9.99	22.40	0.06	22.16	0.05	22.24	0.09	22.24	0.12	091111
328	1328	702.861	257.060	0.00	9.99	0.00	9.99	21.51	0.04	20.83	0.04	20.17	0.03	19.69	0.02	001111
329	1329	705.664	257.350	0.00	9.99	0.00	9.99	21.60	0.04	20.83	0.04	20.17	0.03	19.69	0.02	001111
330	1330	657.341	257.564	0.00	9.99	99.99	-9.99	19.89	0.02	19.62	0.03	19.33	0.02	18.93	0.01	091111
331	1331	573.572	259.194	0.00	9.99	20.37	0.04	21.50	0.03	21.35	0.04	20.94	0.03	20.83	0.04	011111
332	1332	577.679	260.279	0.00	9.99	99.99	-9.99	21.74	0.04	21.43	0.04	21.13	0.04	21.05	0.05	091111
333	1333	700.652	261.325	0.00	9.99	0.00	9.99	21.58	0.04	21.36	0.04	21.03	0.04	20.65	0.03	001111
334	1334	120.392	262.588	0.00	9.99	99.99	-9.99	20.76	0.02	20.82	0.03	20.98	0.03	21.45	0.04	091111
335	1335	596.583	262.190	0.00	9.99	99.99	-9.99	22.39	0.11	22.30	0.13	22.35	0.17	22.27	0.19	091111
336	1336	458.408	262.669	0.00	9.99	99.99	-9.99	22.54	0.08	22.37	0.08	22.22	0.09	21.90	0.09	091111
337	1337	572.660	262.122	0.00	9.99	20.37	0.04	21.50	0.03	21.40	0.04	20.94	0.03	20.92	0.04	011111
338	1338	634.544	262.777	0.00	9.99	0.00	9.99	0.00	9.99	0.00	9.99	0.00	9.99	0.00	9.99	000000
339	1339	121.851	264.705	0.00	9.99	99.99	-9.99	20.76	0.02	20.82	0.03	20.63	0.02	20.92	0.03	091111
340	1340	274.418	263.762	0.00	9.99	99.99	-9.99	21.68	0.04	21.58	0.05	21.35	0.04	20.93	0.04	091111
341	1341	700.818	263.679	0.00	9.99	0.00	9.99	21.71	0.04	21.71	0.05	21.03	0.04	20.68	0.03	001111
342	1342	257.498	265.258	0.00	9.99	99.99	-9.99	22.91	0.11	22.58	0.08	22.37	0.09	22.03	0.09	091111
343	1343	644.108	264.730	0.00	9.99	99.99	-9.99	21.61	0.04	21.34	0.05	20.97	0.05	20.82	0.05	091111
344	1344	85.219	266.023	0.00	9.99	99.99	-9.99	22.80	0.07	22.45	0.05	22.31	0.06	22.25	0.08	091111
345	1345	396.001	266.344	0.00	9.99	99.99	-9.99	23.90	0.26	22.70	0.09	21.98	0.06	21.91	0.08	091111
346	1346	430.427	266.360	0.00	9.99	99.99	-9.99	22.59	0.07	22.51	0.07	22.41	0.09	22.24	0.09	091111
347	1347	121.032	267.844	0.00	9.99	99.99	-9.99	20.76	0.02	20.82	0.03	20.63	0.02	20.92	0.03	091111
348	1348	668.688	268.287	0.00	9.99	0.00	9.99	22.22	0.07	22.09	0.09	21.99	0.11	21.81	0.12	001111
349	1349	678.477	272.223	0.00	9.99	0.00	9.99	22.42	0.07	21.39	0.05	21.22	0.05	20.99	0.05	001111
350	1350	718.201	277.104	0.00	9.99	0.00	9.99	23.19	0.15	22.75	0.11	22.21	0.09	21.60	0.06	001111
351	1351	625.958	279.178	0.00	9.99	99.99	-9.99	22.47	0.07	21.90	0.06	21.42	0.06	20.85	0.04	091111
352	1352	576.906	280.631	0.00	9.99	19.67	0.03	20.68	0.02	20.50	0.03	20.12	0.02	20.23	0.02	011111
353	1353	761.831	282.349	0.00	9.99	0.00	9.99	22.58	0.10	22.67	0.11	22.48	0.12	22.38	0.14	001111
354	1354	655.040	284.117	0.00	9.99	99.99	-9.99	23.15	0.13	22.29	0.09	21.13	0.05	21.21	0.07	091111
355	1355	640.273	287.156	0.00	9.99	99.99	-9.99	21.83	0.05	21.32	0.05	20.79	0.05	20.56	0.06	091111
356	1356	647.456	286.853	0.00	9.99	99.99	-9.99	22.34	0.08	21.75	0.06	21.24	0.07	21.05	0.08	091111
357	1357	653.180	294.814	0.00	9.99	99.99	-9.99	21.91	0.06	21.78	0.08	20.65	0.04	21.20	0.08	091111
358	1358	695.672	294.934	0.00	9.99	0.00	9.99	22.44	0.06	21.72	0.05	21.33	0.04	21.14	0.05	001111
359	1359	786.421	295.248	0.00	9.99	0.00	9.99	20.43	0.02	20.50	0.03	20.56	0.03	20.61	0.03	001111
360	1360	240.319	296.961	0.00	9.99	99.99	-9.99	21.56	0.03	21.31	0.04	21.10	0.03	20.99	0.04	091111
361	1361	392.329	297.108	0.00	9.99	99.99	-9.99	22.79	0.07	22.45	0.06	21.72	0.05	22.37	0.13	091111
362	1362	778.883	296.946	0.00	9.99	0.00	9.99	21.33	0.03	20.42	0.03	19.55	0.02	18.90	0.01	001111
363	1363	634.303	298.757	0.00	9.99	99.99	-9.99	21.84	0.05	21.63	0.05	21.18	0.05	21.32	0.07	091111
364	1364	66.352	300.331	0.00	9.99	99.99	-9.99	22.65	0.08	22.57	0.07	22.44	0.08	22.35	0.10	091111
365	1365	637.469	299.677	0.00	9.99	21.52	0.14	21.82	0.06	21.59	0.05	21.18	0.05	21.32	0.07	011111
366	1366	234.913	301.540	0.00	9.99	99.99	-9.99	22.11	0.05	21.97	0.04	21.67	0.04	21.55	0.05	091111
367	1367	345.180	301.664	0.00	9.99	99.99	-9.99	21.35	0.03	21.04	0.04	20.74	0.03	20.61	0.03	091111
368	1368	705.675	303.015	0.00	9.99	0.00	9.99	21.96	0.05	21.78	0.05	21.47	0.04	21.10	0.04	001111
369	1369	745.420	302.893	0.00	9.99	0.00	9.99	22.52	0.09	22.32	0.09	22.23	0.10	21.80	0.09	001111
370	1370	292.676	305.130	0.00	9.99	99.99	-9.99	21.91	0.04	21.47	0.04	21.02	0.03	20.72	0.03	091111
371	1371	372.611	308.925	0.00	9.99	99.99	-9.99	22.10	0.08	21.91	0.07	21.63	0.07	21.58	0.09	091111
372	1372	607.323	311.292	0.00	9.99	99.99	-9.99	22.33	0.09	21.91	0.08	21.35	0.07	20.83	0.05	091111
373	1373	520.041	312.956	0.00	9.99	99.99	-9.99	22.12	0.08	21.92	0.06	21.31	0.05	21.25	0.07	091111
374	1374	573.292	311.746	0.00	9.99	99.99	-9.99	22.84	0.12	21.92	0.06	21.71	0.08	21.41	0.07	091111
375	1375	633.303	312.877	0.00	9.99	99.99	-9.99	22.29	0.10	22.09	0.08	21.73	0.07	21.54	0.07	091111
376	1376	67.116	316.429	0.00	9.99	99.99	-9.99	20.55	0.02	20.49	0.03	20.24	0.02	19.90	0.02	091111
377	1377	616.342	313.086	0.00	9.99	99.99	-9.99	21.74	0.05	21.50	0.05	21.64	0.07	21.05	0.06	091111
378	1378	366.238	315.475	0.00	9.99	99.99	-9.99	21.28	0.04	20.89	0.04	20.41	0.03	20.35	0.03	091111
379	1379	358.816	315.812	0.00	9.99	99.99	-9.99	22.23	0.07	22.16	0.07	22.24	0.11	22.04	0.12	091111
380	1380	771.792	315.887	0.00	9.99	0.00	9.99	23.87	0.25	22.73	0.09	22.57	0.12	22.35	0.13	001111
381	1381	65.627	317.298	0.00	9.99	99.99	-9.99	20.55	0.02	20.49	0.03	20.24	0.02	19.90	0.02	091111
382	1382	367.376	318.562	0.00	9.99	99.99	-9.99	21.39	0.04	20.73	0.04	20.41	0.03	20.35	0.03	091111
383	1383	530.284	320.621	0.00	9.99	20.09	0.05	20.87	0.03	21.69	0.07	21.45	0.06	21.12	0.06	011111
384	1384	640.468	318.574	0.00	9.99	99.99	-9.99	22.13	0.08	21.91	0.06	21.64	0.06	21.13	0.05	091111
385	1385	659.958	318.780	0.00	9.99	18.97	0.02	19.90	0.02	19.75	0.03	19.58	0.02	19.27	0.02	011111
386	1386	675.544	320.022	0.00	9.99	99.99	-9.99	21.83	0.04	21.86	0.05	21.40	0.05	21.67	0.07	091111
387	1387	382.617	320.888	0.00	9.99	99.99	-9.99	22.15	0.05	21.10	0.04	20.54	0.03	20.26	0.02	091111
388	1388	518.795	321.500	0.00	9.99	99.99	-9.99	21.68	0.09	21.44	0.08	21.21	0.09	20.98	0.09	091111
389	1389	639.460	323.041	0.00	9.99	99.99	-9.99	22.42	0.09	21.68	0.05	21.24	0.05	20.97	0.04	091111
390	1390	70.089	324.102	0.00	9.99	99.99	-9.99	22.84	0.09	22.83	0.09	22.46	0.09	21.97	0.08	091111
391	1391	742.346	325.130	0.00	9.99	0.00	9.99	22.75	0.09	22.39	0.07	21.82	0.05	21.24	0.05	001111
392	1392	523.821	327.533	0.00	9.99	99.99	-9.99	20.37	0.03	20.27	0.04	20.07	0.03	20.43	0.04	091111
393	1393	507.441	329.724	0.00	9.99	18.85	0.02	19.67	0.02	19.41	0.03	19.17	0.02	19.00	0.02	011111
394	1394	515.574	329.224	0.00	9.99	18.85	0.03	19.98	0.03	19.91	0.04	19.86	0.03	19.81	0.03	011111
395	1395	522.365	329.554	0.00	9.99	99.99	-9.99	20.38	0.03	20.27	0.04	20.03	0.03	20.17	0.04	091111
396	1396	502.218	330.325	0.00	9.99	99.99	-9.99	20.78	0.03	20.35	0.04	19.88	0.03	19.66	0.02	091111
397	1397	500.895	330.278	0.00	9.99	99.99	-9.99	20.78	0.03	20.35	0.04	19.88	0.03	19.66	0.02	091111
398	1398	513.952	331.584	0.00	9.99	18.85	0.03	19.98	0.03	19.87	0.04	20.27	0.05	20.57	0.06	011111
399	1399	535.934	332.194	0.00	9.99	99.99	-9.99	23.83	0.35	22.67	0.15	21.95	0.10	21.55	0.09	091111
400	1400	503.724	332.195	0.00	9.99	99.99	-9.99	20.78	0.03	20.35	0.04	19.88	0.03	19.66	0.02	091111
401	1401	506.082	336.965	0.00	9.99	99.99	-9.99	21.78	0.08	21.48	0.06	21.15	0.07	21.03	0.08	091111
402	1402	735.398	338.561	0.00	9.99	0.00	9.99	22.52	0.06	22.17	0.05	21.71	0.04	21.20	0.04	001111
403	1403	80.959	339.909	0.00	9.99	99.99	-9.99	21.86	0.05	21.82	0.04	21.26	0.04	20.82	0.03	091111
404	1404	356.485	340.251	0.00	9.99	99.99	-9.99	22.31	0.06	22.08	0.05	21.81	0.05	21.77	0.06	091111
405	1405	740.499	340.542	0.00	9.99	0.00	9.99	20.92	0.03	20.65	0.03	20.27	0.02	19.84	0.02	001111
406	1406	83.613	342.449	0.00	9.99	99.99	-9.99	21.86	0.05	21.65	0.04	21.26	0.04	20.82	0.03	091111
407	1407	499.951	342.674	0.00	9.99	0.00	9.99	0.00	9.99	0.00	9.99	0.00	9.99	0.00	9.99	000000
408	1408	509.943	344.754	0.00	9.99	17.52	0.02	18.24	0.02	18.03	0.03	17.69	0.02	17.42	0.01	011111
409	1409	530.316	346.233	0.00	9.99	99.99	-9.99	21.96	0.07	21.85	0.08	21.72	0.10	21.60	0.12	091111
410	1410	525.887	346.958	0.00	9.99	99.99	-9.99	21.75	0.08	21.41	0.07	21.12	0.06	20.97	0.07	091111
411	1411	520.191	348.847	0.00	9.99	99.99	-9.99	21.27	0.05	21.11	0.05	21.03	0.06	20.93	0.05	091111
412	1412	375.218	352.436	0.00	9.99	99.99	-9.99	21.56	0.04	21.20	0.04	20.42	0.02	20.18	0.02	091111
413	1413	353.668	354.261	0.00	9.99	99.99	-9.99	21.84	0.04	21.77	0.04	21.57	0.04	21.51	0.04	091111
414	1414	528.702	355.436	0.00	9.99	99.99	-9.99	22.90	0.19	22.43	0.16	21.90	0.13	21.55	0.12	091111
415	1415	409.568	358.809	0.00	9.99	99.99	-9.99	23.28	0.15	23.03	0.12	22.81	0.13	22.51	0.15	091111
416	1416	518.279	358.820	0.00	9.99	99.99	-9.99	21.82	0.07	21.30	0.05	20.92	0.06	20.53	0.05	091111
417	1417	86.342	360.671	0.00	9.99	99.99	-9.99	21.76	0.04	21.88	0.05	21.82	0.05	21.92	0.07	091111
418	1418	545.248	362.365	0.00	9.99	99.99	-9.99	23.28	0.13	22.60	0.08	22.14	0.09	21.90	0.09	091111
419	1419	397.012	365.292	0.00	9.99	19.96	0.03	21.17	0.03	21.16	0.04	21.16	0.04	20.94	0.04	011111
420	1420	458.168	364.807	0.00	9.99	99.99	-9.99	23.09	0.14	22.54	0.08	21.86	0.05	21.45	0.05	091111
421	1421	756.497	373.788	0.00	9.99	0.00	9.99	21.00	0.03	20.83	0.03	20.59	0.03	20.22	0.02	001111
422	1422	760.769	378.468	0.00	9.99	0.00	9.99	21.50	0.04	21.19	0.04	20.80	0.03	20.42	0.03	001111
423	1423	574.165	381.224	0.00	9.99	99.99	-9.99	22.02	0.07	22.02	0.07	21.87	0.07	21.14	0.05	091111
424	1424	77.553	382.010	0.00	9.99	99.99	-9.99	21.36	0.03	21.24	0.04	20.85	0.03	20.28	0.02	091111
425	1425	85.056	381.430	0.00	9.99	99.99	-9.99	22.61	0.08	22.11	0.05	21.72	0.05	21.56	0.05	091111
426	1426	743.209	382.714	0.00	9.99	99.99	-9.99	22.26	0.06	22.22	0.05	22.13	0.06	22.21	0.10	091111
427	1427	578.207	384.554	0.00	9.99	19.37	0.03	20.54	0.03	20.53	0.04	20.44	0.03	20.38	0.03	011111
428	1428	558.318	386.355	0.00	9.99	99.99	-9.99	22.05	0.07	22.10	0.08	21.99	0.10	21.48	0.08	091111
429	1429	787.239	387.785	0.00	9.99	0.00	9.99	21.88	0.05	21.74	0.05	21.47	0.05	21.34	0.05	001111
430	1430	572.304	389.421	0.00	9.99	19.10	0.03	20.11	0.03	20.01	0.04	19.78	0.02	19.79	0.02	011111
431	1431	600.856	388.513	0.00	9.99	99.99	-9.99	23.57	0.13	22.49	0.05	22.00	0.05	21.65	0.05	091111
432	1432	740.053	388.987	0.00	9.99	99.99	-9.99	23.17	0.13	22.89	0.09	22.69	0.10	22.21	0.09	091111
433	1433	574.714	389.043	0.00	9.99	19.10	0.03	20.12	0.03	20.01	0.04	19.78	0.02	19.79	0.02	011111
434	1434	77.688	391.805	0.00	9.99	99.99	-9.99	22.33	0.06	22.30	0.05	22.21	0.07	22.00	0.08	091111
435	1435	554.757	392.964	0.00	9.99	99.99	-9.99	22.88	0.13	22.80	0.13	22.10	0.08	21.18	0.05	091111
436	1436	726.172	392.632	0.00	9.99	99.99	-9.99	23.09	0.10	23.11	0.09	22.77	0.09	22.06	0.08	091111
437	1437	541.099	393.613	0.00	9.99	99.99	-9.99	23.70	0.17	22.81	0.08	22.22	0.07	21.86	0.07	091111
438	1438	207.021	395.349	0.00	9.99	99.99	-9.99	23.07	0.09	22.82	0.06	22.81	0.08	22.55	0.09	091111
439	1439	693.810	395.236	0.00	9.99	99.99	-9.99	22.82	0.07	21.98	0.04	21.46	0.04	21.14	0.04	091111
440	1440	577.768	396.660	0.00	9.99	99.99	-9.99	21.32	0.06	21.21	0.06	20.99	0.06	20.87	0.05	091111
441	1441	564.649	399.310	0.00	9.99	18.86	0.03	20.15	0.03	20.21	0.04	20.18	0.03	20.07	0.03	011111
442	1442	338.775	400.490	0.00	9.99	99.99	-9.99	23.08	0.09	23.09	0.09	22.74	0.09	22.33	0.09	091111
443	1443	569.160	400.406	0.00	9.99	99.99	-9.99	21.84	0.09	22.08	0.10	21.65	0.07	22.24	0.16	091111
444	1444	582.837	401.940	0.00	9.99	19.75	0.05	21.02	0.05	21.89	0.09	21.32	0.06	21.21	0.07	011111
445	1445	580.811	402.288	0.00	9.99	19.75	0.05	21.02	0.05	21.89	0.09	21.32	0.06	21.21	0.07	011111
446	1446	584.695	402.582	0.00	9.99	19.75	0.05	21.02	0.05	21.89	0.09	21.32	0.06	21.21	0.07	011111
447	1447	771.187	403.004	0.00	9.99	0.00	9.99	22.06	0.05	21.97	0.05	21.57	0.04	21.63	0.04	001111
448	1448	608.346	403.752	0.00	9.99	99.99	-9.99	22.52	0.06	22.55	0.06	22.68	0.08	22.54	0.10	091111
449	1449	575.207	405.051	0.00	9.99	19.93	0.05	21.18	0.04	21.33	0.05	21.39	0.06	21.43	0.07	011111
450	1450	68.627	406.425	0.00	9.99	99.99	-9.99	22.92	0.12	22.36	0.07	22.05	0.06	21.62	0.06	091111
451	1451	566.511	405.532	0.00	9.99	99.99	-9.99	20.74	0.03	20.81	0.04	20.59	0.04	20.70	0.05	091111
452	1452	429.004	407.007	0.00	9.99	99.99	-9.99	23.04	0.08	22.83	0.07	22.67	0.08	22.32	0.09	091111
453	1453	74.312	408.103	0.00	9.99	99.99	-9.99	21.70	0.04	21.75	0.04	21.75	0.05	21.49	0.05	091111
454	1454	750.368	407.886	0.00	9.99	18.89	0.02	20.10	0.02	20.20	0.03	20.14	0.02	19.90	0.02	011111
455	1455	575.155	410.131	0.00	9.99	20.09	0.08	21.35	0.08	21.23	0.07	21.32	0.09	21.19	0.09	011111
456	1456	529.407	412.153	0.00	9.99	99.99	-9.99	23.74	0.19	23.45	0.14	23.51	0.22	23.45	0.25	091111
457	1457	343.549	416.367	0.00	9.99	99.99	-9.99	23.05	0.10	22.71	0.08	22.40	0.08	22.04	0.07	091111
458	1458	583.810	417.413	0.00	9.99	21.26	0.12	22.32	0.09	22.20	0.07	22.08	0.10	22.27	0.15	011111
459	1459	573.905	420.682	0.00	9.99	99.99	-9.99	21.12	0.03	21.16	0.04	21.04	0.04	21.21	0.06	091111
460	1460	708.407	421.076	0.00	9.99	99.99	-9.99	23.09	0.08	23.23	0.08	23.23	0.12	23.20	0.18	091111
461	1461	574.669	421.910	0.00	9.99	19.94	0.04	21.15	0.04	21.15	0.04	21.04	0.04	21.21	0.06	011111
462	1462	93.641	424.773	0.00	9.99	99.99	-9.99	22.79	0.08	22.41	0.05	21.93	0.05	21.47	0.04	091111
463	1463	583.625	425.486	0.00	9.99	99.99	-9.99	22.08	0.06	21.84	0.05	21.06	0.04	21.07	0.05	091111
464	1464	583.665	426.524	0.00	9.99	99.99	-9.99	22.09	0.06	21.84	0.05	21.06	0.04	21.07	0.05	091111
465	1465	131.027	428.645	0.00	9.99	99.99	-9.99	22.60	0.06	22.40	0.05	21.92	0.05	21.83	0.05	091111
466	1466	575.922	430.165	0.00	9.99	99.99	-9.99	22.66	0.09	22.47	0.07	22.19	0.06	21.93	0.08	091111
467	1467	591.644	431.560	0.00	9.99	99.99	-9.99	22.11	0.06	22.04	0.05	21.80	0.05	21.88	0.07	091111
468	1468	602.371	435.672	0.00	9.99	99.99	-9.99	22.31	0.06	22.29	0.05	22.23	0.06	21.97	0.07	091111
469	1469	164.477	447.565	0.00	9.99	99.99	-9.99	22.40	0.06	22.28	0.05	21.82	0.04	21.74	0.05	091111
470	1470	600.978	447.663	0.00	9.99	99.99	-9.99	22.42	0.07	22.01	0.05	21.73	0.05	21.59	0.06	091111
471	1471	583.941	451.530	0.00	9.99	99.99	-9.99	22.91	0.08	22.79	0.07	22.56	0.07	22.16	0.08	091111
472	1472	607.492	453.791	0.00	9.99	19.88	0.03	20.83	0.03	20.77	0.03	20.58	0.03	20.15	0.02	011111
473	1473	613.518	453.901	0.00	9.99	18.57	0.02	19.63	0.02	19.60	0.03	19.42	0.02	18.97	0.01	011111
474	1474	568.311	457.146	0.00	9.99	99.99	-9.99	23.11	0.10	22.88	0.07	22.54	0.08	21.35	0.04	091111
475	1475	677.263	459.161	0.00	9.99	99.99	-9.99	21.80	0.04	21.87	0.04	21.47	0.03	21.73	0.05	091111
476	1476	80.880	462.483	0.00	9.99	99.99	-9.99	22.19	0.05	22.31	0.06	21.75	0.05	22.52	0.12	091111
477	1477	573.105	466.017	0.00	9.99	99.99	-9.99	22.61	0.06	22.69	0.06	22.68	0.08	22.43	0.10	091111
478	1478	561.298	470.198	0.00	9.99	99.99	-9.99	22.50	0.07	22.58	0.07	22.64	0.09	22.76	0.12	091111
479	1479	54.251	471.523	0.00	9.99	99.99	-9.99	22.19	0.09	21.48	0.10	20.59	0.06	20.64	0.09	091111
480	1480	762.296	472.885	0.00	9.99	99.99	-9.99	22.60	0.06	21.74	0.04	21.23	0.03	20.99	0.03	091111
481	1481	619.964	477.800	0.00	9.99	99.99	-9.99	23.13	0.09	22.95	0.08	22.69	0.09	22.33	0.09	091111
482	1482	110.818	479.012	0.00	9.99	99.99	-9.99	21.69	0.03	21.74	0.04	21.67	0.04	21.34	0.04	091111
483	1483	677.965	481.104	0.00	9.99	99.99	-9.99	22.47	0.06	22.52	0.06	22.71	0.08	22.88	0.14	091111
484	1484	614.170	481.829	0.00	9.99	99.99	-9.99	22.61	0.06	22.02	0.04	21.49	0.04	21.02	0.03	091111
485	1485	676.112	481.294	0.00	9.99	99.99	-9.99	22.47	0.06	22.52	0.06	22.71	0.08	22.88	0.14	091111
486	1486	656.304	487.128	0.00	9.99	99.99	-9.99	22.96	0.08	23.05	0.07	23.01	0.09	22.99	0.14	091111
487	1487	577.481	489.622	0.00	9.99	99.99	-9.99	22.03	0.04	21.71	0.04	21.36	0.03	21.13	0.03	091111
488	1488	640.808	489.188	0.00	9.99	99.99	-9.99	22.08	0.04	22.25	0.05	22.54	0.06	22.39	0.08	091111
489	1489	621.604	490.109	0.00	9.99	99.99	-9.99	22.58	0.07	22.13	0.05	21.45	0.04	21.05	0.03	091111
490	1490	569.109	490.439	0.00	9.99	99.99	-9.99	23.08	0.12	22.57	0.07	22.28	0.07	22.01	0.07	091111
491	1491	673.196	490.984	0.00	9.99	99.99	-9.99	22.10	0.05	22.67	0.06	22.22	0.06	22.37	0.08	091111
492	1492	584.576	501.115	0.00	9.99	99.99	-9.99	22.30	0.06	22.22	0.05	22.15	0.06	21.51	0.05	091111
493	1493	208.900	503.134	0.00	9.99	99.99	-9.99	21.81	0.04	21.77	0.04	20.81	0.03	21.77	0.05	091111
494	1494	265.427	506.604	0.00	9.99	99.99	-9.99	21.96	0.04	21.88	0.04	21.72	0.04	21.53	0.04	091111
495	1495	94.427	508.649	0.00	9.99	99.99	-9.99	23.12	0.10	22.98	0.08	22.65	0.08	22.21	0.09	091111
496	1496	279.016	513.754	0.00	9.99	99.99	-9.99	21.58	0.04	21.52	0.04	21.40	0.04	20.95	0.03	091111
497	1497	106.812	515.020	0.00	9.99	99.99	-9.99	21.76	0.04	21.60	0.04	21.42	0.03	21.09	0.04	091111
498	1498	284.425	517.005	0.00	9.99	99.99	-9.99	21.96	0.04	21.66	0.04	21.32	0.03	21.05	0.03	091111
499	1499	280.813	521.272	0.00	9.99	99.99	-9.99	21.98	0.05	21.94	0.04	21.95	0.05	21.37	0.04	091111
500	1500	778.926	523.741	0.00	9.99	99.99	-9.99	22.47	0.05	22.37	0.05	22.16	0.04	21.87	0.05	091111
501	1501	355.119	533.099	0.00	9.99	99.99	-9.99	24.07	0.20	22.92	0.06	22.26	0.05	21.89	0.05	091111
502	1502	270.240	534.588	0.00	9.99	99.99	-9.99	23.11	0.09	22.98	0.07	22.83	0.08	22.70	0.10	091111
503	1503	333.068	545.974	0.00	9.99	99.99	-9.99	22.30	0.05	22.30	0.05	22.22	0.05	22.20	0.07	091111
504	1504	756.161	548.588	0.00	9.99	99.99	-9.99	22.65	0.06	22.66	0.06	22.61	0.07	22.50	0.10	091111
505	1505	619.495	549.322	0.00	9.99	99.99	-9.99	23.42	0.10	23.28	0.07	22.78	0.07	22.87	0.11	091111
506	1506	190.048	555.667	0.00	9.99	99.99	-9.99	22.71	0.07	22.55	0.06	22.42	0.06	22.29	0.08	091111
507	1507	356.846	557.002	0.00	9.99	99.99	-9.99	23.07	0.09	23.03	0.07	22.77	0.07	22.68	0.10	091111
508	1508	281.730	560.533	0.00	9.99	99.99	-9.99	22.96	0.09	23.02	0.08	23.05	0.11	22.69	0.11	091111
509	1509	794.213	567.502	0.00	9.99	0.00	9.99	22.24	0.05	21.96	0.04	21.60	0.04	21.15	0.04	001111
510	1510	241.093	568.960	0.00	9.99	99.99	-9.99	21.68	0.03	21.51	0.04	21.23	0.03	20.75	0.02	091111
511	1511	483.708	568.902	0.00	9.99	99.99	-9.99	23.07	0.08	22.90	0.06	22.55	0.06	22.25	0.06	091111
512	1512	693.710	574.871	0.00	9.99	99.99	-9.99	22.87	0.08	22.57	0.05	22.40	0.05	22.22	0.08	091111
513	1513	794.071	578.376	0.00	9.99	0.00	9.99	23.29	0.14	23.29	0.11	23.47	0.20	23.94	0.51	001111
514	1514	784.719	591.197	0.00	9.99	0.00	9.99	21.91	0.04	21.85	0.04	21.65	0.04	21.40	0.03	001111
515	1515	286.385	594.533	0.00	9.99	20.52	0.05	21.45	0.03	21.31	0.04	21.06	0.03	21.00	0.03	011111
516	1516	378.652	596.342	0.00	9.99	99.99	-9.99	22.73	0.07	22.71	0.06	22.41	0.06	22.06	0.06	091111
517	1517	692.201	596.785	0.00	9.99	99.99	-9.99	22.67	0.07	22.00	0.04	21.65	0.03	21.41	0.04	091111
518	1518	742.849	598.391	0.00	9.99	0.00	9.99	22.72	0.06	22.53	0.05	22.25	0.05	21.87	0.05	001111
519	1519	349.408	599.087	0.00	9.99	99.99	-9.99	22.17	0.05	22.07	0.04	21.73	0.04	21.24	0.03	091111
520	1520	677.031	602.605	0.00	9.99	99.99	-9.99	22.53	0.06	22.55	0.05	22.42	0.06	22.47	0.08	091111
521	1521	356.900	602.607	0.00	9.99	99.99	-9.99	23.81	0.16	23.69	0.12	23.31	0.12	23.07	0.13	091111
522	1522	371.832	628.318	0.00	9.99	99.99	-9.99	22.14	0.05	22.00	0.04	21.87	0.04	21.70	0.05	091111
523	1523	116.305	629.372	0.00	9.99	99.99	-9.99	23.48	0.15	23.36	0.13	22.67	0.09	22.41	0.11	091111
524	1524	413.275	630.313	0.00	9.99	99.99	-9.99	22.59	0.06	21.74	0.04	21.00	0.03	21.01	0.03	091111
525	1525	429.057	629.706	0.00	9.99	99.99	-9.99	22.32	0.05	22.38	0.05	22.24	0.05	21.91	0.05	091111
526	1526	381.028	641.851	0.00	9.99	99.99	-9.99	22.30	0.05	22.26	0.05	22.06	0.05	21.89	0.06	091111
527	1527	254.082	646.700	0.00	9.99	99.99	-9.99	22.89	0.08	22.69	0.06	22.77	0.07	22.53	0.09	091111
528	1528	299.524	647.450	0.00	9.99	99.99	-9.99	22.20	0.05	22.02	0.05	21.83	0.04	21.66	0.05	091111
529	1529	330.648	656.099	0.00	9.99	99.99	-9.99	22.56	0.06	22.49	0.05	22.36	0.06	22.38	0.08	091111
530	1530	84.115	657.317	0.00	9.99	99.99	-9.99	21.19	0.03	21.09	0.04	20.80	0.03	20.62	0.03	091111
531	1531	113.040	656.399	0.00	9.99	99.99	-9.99	22.58	0.07	22.35	0.05	22.05	0.06	21.76	0.07	091111
532	1532	294.015	657.809	0.00	9.99	99.99	-9.99	22.33	0.05	22.24	0.05	22.15	0.05	22.12	0.08	091111
533	1533	400.417	658.118	0.00	9.99	99.99	-9.99	22.66	0.07	22.58	0.06	22.43	0.06	22.00	0.07	091111
534	1534	328.081	665.089	0.00	9.99	99.99	-9.99	23.34	0.11	23.46	0.11	23.56	0.18	23.09	0.16	091111
535	1535	399.068	679.284	0.00	9.99	99.99	-9.99	21.98	0.04	21.85	0.04	21.61	0.04	21.30	0.04	091111
536	1536	117.021	696.737	0.00	9.99	99.99	-9.99	21.63	0.04	21.44	0.04	21.13	0.03	20.74	0.03	091111
537	1537	111.042	708.182	0.00	9.99	99.99	-9.99	22.93	0.11	22.57	0.10	22.32	0.09	21.80	0.08	091111
538	1538	134.911	717.622	0.00	9.99	99.99	-9.99	22.78	0.09	22.73	0.08	22.66	0.10	22.31	0.11	091111
539	1539	224.082	717.442	0.00	9.99	99.99	-9.99	22.36	0.05	22.05	0.05	21.89	0.04	21.61	0.05	091111
540	1540	308.373	721.547	0.00	9.99	99.99	-9.99	21.41	0.03	21.17	0.04	20.87	0.03	20.64	0.03	091111
541	1541	652.167	720.258	0.00	9.99	0.00	9.99	23.61	0.13	22.79	0.05	22.26	0.05	22.03	0.05	001111
542	1542	103.527	735.360	0.00	9.99	99.99	-9.99	23.55	0.14	23.16	0.12	22.31	0.08	23.23	0.25	091111
543	1543	432.117	735.118	0.00	9.99	99.99	-9.99	22.90	0.08	22.93	0.08	22.77	0.09	22.64	0.12	091111
544	1544	607.231	738.921	0.00	9.99	0.00	9.99	21.26	0.03	21.22	0.04	21.07	0.03	20.70	0.03	001111
545	1545	601.138	741.525	0.00	9.99	0.00	9.99	19.80	0.02	19.74	0.03	19.53	0.02	19.20	0.01	001111
546	1546	486.824	744.689	0.00	9.99	99.99	-9.99	22.62	0.06	22.51	0.05	22.30	0.06	21.85	0.06	091111
547	1547	79.173	758.036	0.00	9.99	0.00	9.99	23.41	0.18	22.99	0.13	22.60	0.14	22.43	0.15	001111
548	1548	183.112	768.732	0.00	9.99	99.99	-9.99	23.31	0.17	22.86	0.12	22.57	0.13	22.37	0.14	091111
549	1549	188.603	769.760	0.00	9.99	99.99	-9.99	22.86	0.10	22.66	0.10	22.45	0.11	22.48	0.13	091111
550	1550	92.636	771.057	0.00	9.99	0.00	9.99	23.15	0.14	22.88	0.11	22.04	0.07	22.17	0.10	001111
551	1551	450.931	775.354	0.00	9.99	99.99	-9.99	22.27	0.06	22.14	0.06	21.86	0.05	21.51	0.05	091111
552	1552	193.780	777.790	0.00	9.99	99.99	-9.99	21.82	0.04	21.10	0.04	20.60	0.03	20.36	0.02	091111
553	1553	190.247	779.389	0.00	9.99	99.99	-9.99	21.78	0.04	21.45	0.04	21.20	0.04	21.04	0.04	091111
554	1554	205.240	780.272	0.00	9.99	99.99	-9.99	23.46	0.16	22.17	0.05	21.63	0.05	21.27	0.04	091111
555	1555	540.705	796.984	0.00	9.99	0.00	9.99	23.28	0.18	22.90	0.21	23.40	0.23	22.78	0.17	001111
556	2001	191.725	39.718	0.00	9.99	0.00	9.99	20.91	0.12	19.61	0.05	20.29	0.18	99.99	-9.99	001119
557	2003	207.260	44.400	0.00	9.99	99.99	-9.99	18.71	0.02	18.78	0.04	18.59	0.04	99.99	-9.99	091119
558	2005	195.225	49.074	0.00	9.99	18.79	0.03	20.87	0.04	20.30	0.04	20.01	0.03	99.99	-9.99	011119
559	2007	213.963	50.610	0.00	9.99	99.99	-9.99	22.25	0.09	22.33	0.11	21.82	0.13	99.99	-9.99	091119
560	2008	198.511	52.734	0.00	9.99	99.99	-9.99	20.36	0.03	20.30	0.04	20.01	0.03	99.99	-9.99	091119
561	2013	787.242	59.741	0.00	9.99	0.00	9.99	22.97	0.10	22.85	0.08	22.61	0.10	99.99	-9.99	001119
562	2015	236.292	61.166	0.00	9.99	20.58	0.07	21.53	0.08	21.01	0.05	20.80	0.06	99.99	-9.99	011119
563	2016	293.684	62.570	0.00	9.99	99.99	-9.99	22.30	0.10	22.11	0.10	22.13	0.14	99.99	-9.99	091119
564	2017	188.961	64.985	0.00	9.99	99.99	-9.99	21.58	0.10	21.83	0.13	21.57	0.11	99.99	-9.99	091119
565	2019	540.953	68.418	0.00	9.99	0.00	9.99	22.45	0.10	21.75	0.06	21.94	0.11	99.99	-9.99	001119
566	2023	347.951	79.284	0.00	9.99	20.76	0.07	21.85	0.08	21.79	0.12	21.46	0.16	99.99	-9.99	011119
567	2024	385.095	79.916	0.00	9.99	99.99	-9.99	21.99	0.09	22.06	0.10	21.65	0.08	99.99	-9.99	091119
568	2026	778.882	81.427	0.00	9.99	0.00	9.99	20.80	0.03	20.98	0.04	20.98	0.03	99.99	-9.99	001119
569	2027	394.191	84.468	0.00	9.99	19.13	0.03	20.36	0.03	20.61	0.04	20.56	0.03	99.99	-9.99	011119
570	2029	483.056	86.934	0.00	9.99	21.31	0.15	22.42	0.12	22.26	0.09	21.93	0.11	99.99	-9.99	011119
571	2030	193.553	88.581	0.00	9.99	15.88	0.02	17.03	0.02	17.52	0.03	17.21	0.02	99.99	-9.99	011119
572	2035	189.493	94.219	0.00	9.99	15.88	0.02	17.03	0.02	17.52	0.03	17.21	0.02	99.99	-9.99	011119
573	2036	104.463	94.127	0.00	9.99	0.00	9.99	22.48	0.12	22.53	0.12	22.27	0.11	99.99	-9.99	001119
574	2037	139.203	95.932	0.00	9.99	99.99	-9.99	22.39	0.11	22.46	0.12	21.70	0.08	99.99	-9.99	091119
575	2038	391.481	94.591	0.00	9.99	20.34	0.10	21.42	0.08	21.37	0.09	21.48	0.11	99.99	-9.99	011119
576	2040	292.400	96.467	0.00	9.99	99.99	-9.99	23.12	0.11	22.77	0.11	22.48	0.14	99.99	-9.99	091119
577	2042	494.850	97.992	0.00	9.99	17.48	0.02	18.92	0.02	19.08	0.03	18.69	0.02	99.99	-9.99	011119
578	2043	130.798	98.891	0.00	9.99	99.99	-9.99	21.88	0.08	22.16	0.10	22.02	0.11	99.99	-9.99	091119
579	2046	453.130	100.285	0.00	9.99	21.33	0.16	22.66	0.15	22.87	0.17	22.65	0.20	99.99	-9.99	011119
580	2047	414.876	102.298	0.00	9.99	18.07	0.02	19.33	0.03	20.23	0.07	20.26	0.05	99.99	-9.99	011119
581	2048	448.130	103.276	0.00	9.99	20.01	0.05	21.22	0.05	21.31	0.05	21.37	0.06	99.99	-9.99	011119
582	2049	406.016	103.548	0.00	9.99	18.07	0.02	19.33	0.03	19.35	0.04	19.21	0.03	99.99	-9.99	011119
583	2052	286.040	108.788	0.00	9.99	99.99	-9.99	23.08	0.14	23.22	0.15	22.93	0.17	99.99	-9.99	091119
584	2053	143.525	110.868	0.00	9.99	99.99	-9.99	22.55	0.12	22.53	0.10	22.49	0.17	99.99	-9.99	091119
585	2054	426.402	110.319	0.00	9.99	19.98	0.07	21.46	0.08	21.61	0.08	21.69	0.13	99.99	-9.99	011119
586	2055	349.419	113.489	0.00	9.99	99.99	-9.99	21.97	0.06	21.51	0.05	21.09	0.05	99.99	-9.99	091119
587	2058	404.706	115.327	0.00	9.99	20.13	0.08	21.57	0.10	21.66	0.11	21.52	0.14	99.99	-9.99	011119
588	2059	424.022	114.720	0.00	9.99	16.50	0.02	17.51	0.02	17.63	0.03	17.33	0.02	99.99	-9.99	011119
589	2062	388.805	123.669	0.00	9.99	99.99	-9.99	22.36	0.13	22.18	0.11	21.99	0.16	99.99	-9.99	091119
590	2063	158.887	126.317	0.00	9.99	99.99	-9.99	22.24	0.11	22.21	0.11	22.08	0.15	99.99	-9.99	091119
591	2064	305.644	126.717	0.00	9.99	99.99	-9.99	23.17	0.15	23.31	0.17	22.58	0.15	99.99	-9.99	091119
592	2066	474.234	125.668	0.00	9.99	20.05	0.06	21.28	0.05	21.23	0.06	20.81	0.06	99.99	-9.99	011119
593	2068	468.594	125.989	0.00	9.99	99.99	-9.99	21.85	0.11	21.25	0.06	21.47	0.10	99.99	-9.99	091119
594	2069	151.309	127.938	0.00	9.99	20.52	0.06	21.52	0.05	21.34	0.05	20.93	0.05	99.99	-9.99	011119
595	2073	161.170	131.454	0.00	9.99	99.99	-9.99	21.83	0.08	22.04	0.13	21.60	0.10	99.99	-9.99	091119
596	2075	376.920	134.378	0.00	9.99	99.99	-9.99	22.41	0.09	22.37	0.10	22.24	0.13	99.99	-9.99	091119
597	2077	165.460	133.908	0.00	9.99	99.99	-9.99	22.10	0.08	22.11	0.09	21.97	0.14	99.99	-9.99	091119
598	2078	310.281	134.889	0.00	9.99	99.99	-9.99	22.21	0.06	22.04	0.05	21.58	0.07	99.99	-9.99	091119
599	2079	379.342	139.608	0.00	9.99	99.99	-9.99	22.35	0.06	22.26	0.07	21.71	0.06	99.99	-9.99	091119
600	2080	581.277	146.574	0.00	9.99	0.00	9.99	22.58	0.11	22.62	0.13	21.41	0.06	99.99	-9.99	001119
601	2081	563.052	148.677	0.00	9.99	99.99	-9.99	22.22	0.09	22.25	0.11	22.24	0.17	99.99	-9.99	091119
602	2082	148.023	149.684	0.00	9.99	99.99	-9.99	23.15	0.15	23.35	0.17	23.19	0.19	99.99	-9.99	091119
603	2083	169.135	149.575	0.00	9.99	99.99	-9.99	21.85	0.06	21.94	0.08	21.19	0.09	99.99	-9.99	091119
604	2084	764.724	154.427	0.00	9.99	0.00	9.99	21.32	0.05	21.17	0.05	20.44	0.05	99.99	-9.99	001119
605	2087	241.037	178.739	0.00	9.99	19.17	0.04	20.50	0.06	20.03	0.04	20.40	0.07	99.99	-9.99	011119
606	2088	638.398	182.929	0.00	9.99	0.00	9.99	23.48	0.15	23.28	0.11	23.38	0.17	99.99	-9.99	001119
607	2091	558.473	203.885	0.00	9.99	99.99	-9.99	22.61	0.07	22.77	0.09	22.80	0.17	99.99	-9.99	091119
608	2092	125.056	213.875	0.00	9.99	99.99	-9.99	23.39	0.19	23.28	0.15	23.21	0.19	99.99	-9.99	091119
609	2093	664.617	213.141	0.00	9.99	0.00	9.99	22.57	0.08	21.29	0.04	20.84	0.03	99.99	-9.99	001119
610	2094	139.945	217.994	0.00	9.99	99.99	-9.99	22.63	0.09	22.72	0.08	22.48	0.09	99.99	-9.99	091119
611	2095	293.363	218.359	0.00	9.99	99.99	-9.99	23.15	0.14	22.83	0.11	22.52	0.11	99.99	-9.99	091119
612	2096	696.593	218.428	0.00	9.99	0.00	9.99	23.01	0.09	22.34	0.05	21.82	0.04	99.99	-9.99	001119
613	2097	168.077	222.960	0.00	9.99	99.99	-9.99	22.32	0.08	22.39	0.09	22.25	0.09	99.99	-9.99	091119
614	2099	275.565	229.883	0.00	9.99	99.99	-9.99	22.24	0.05	22.05	0.05	21.88	0.07	99.99	-9.99	091119
615	2100	219.325	232.792	0.00	9.99	99.99	-9.99	22.81	0.09	22.83	0.09	22.81	0.12	99.99	-9.99	091119
616	2101	690.322	235.533	0.00	9.99	0.00	9.99	23.39	0.13	23.27	0.12	23.20	0.16	99.99	-9.99	001119
617	2102	412.326	243.561	0.00	9.99	99.99	-9.99	22.54	0.08	22.22	0.07	21.68	0.07	99.99	-9.99	091119
618	2104	141.199	254.152	0.00	9.99	99.99	-9.99	23.42	0.19	23.15	0.12	23.02	0.17	99.99	-9.99	091119
619	2105	295.125	253.615	0.00	9.99	99.99	-9.99	23.15	0.14	23.16	0.13	22.84	0.15	99.99	-9.99	091119
620	2106	585.300	254.149	0.00	9.99	99.99	-9.99	23.09	0.16	23.19	0.18	22.80	0.18	99.99	-9.99	091119
621	2109	701.345	261.524	0.00	9.99	0.00	9.99	21.64	0.04	21.49	0.05	21.02	0.05	99.99	-9.99	001119
622	2113	642.761	295.684	0.00	9.99	99.99	-9.99	21.70	0.06	21.89	0.07	21.39	0.09	99.99	-9.99	091119
623	2114	781.920	298.601	0.00	9.99	0.00	9.99	21.23	0.03	20.90	0.03	19.53	0.02	99.99	-9.99	001119
624	2115	374.024	302.674	0.00	9.99	99.99	-9.99	22.56	0.11	22.62	0.13	22.39	0.16	99.99	-9.99	091119
625	2117	344.436	306.309	0.00	9.99	99.99	-9.99	22.69	0.09	22.78	0.11	21.61	0.06	99.99	-9.99	091119
626	2119	372.441	308.898	0.00	9.99	99.99	-9.99	22.22	0.07	22.14	0.08	21.85	0.09	99.99	-9.99	091119
627	2120	531.124	315.122	0.00	9.99	99.99	-9.99	22.77	0.12	22.89	0.16	22.80	0.19	99.99	-9.99	091119
628	2121	110.674	316.445	0.00	9.99	99.99	-9.99	23.07	0.10	23.23	0.09	23.23	0.14	99.99	-9.99	091119
629	2123	653.436	316.168	0.00	9.99	99.99	-9.99	21.89	0.06	21.58	0.05	21.23	0.05	99.99	-9.99	091119
630	2124	671.436	319.543	0.00	9.99	99.99	-9.99	22.36	0.06	22.36	0.07	21.96	0.06	99.99	-9.99	091119
631	2125	69.990	324.321	0.00	9.99	99.99	-9.99	22.98	0.11	23.07	0.12	22.61	0.09	99.99	-9.99	091119
632	2126	103.311	326.203	0.00	9.99	99.99	-9.99	23.48	0.12	23.67	0.11	23.44	0.14	99.99	-9.99	091119
633	2128	522.515	329.313	0.00	9.99	99.99	-9.99	20.39	0.03	20.31	0.04	20.01	0.03	99.99	-9.99	091119
634	2129	627.281	331.272	0.00	9.99	99.99	-9.99	22.10	0.06	21.51	0.04	22.05	0.07	99.99	-9.99	091119
635	2134	429.915	368.082	0.00	9.99	99.99	-9.99	22.47	0.08	22.57	0.10	22.23	0.12	99.99	-9.99	091119
636	2136	422.994	370.288	0.00	9.99	99.99	-9.99	22.34	0.07	22.31	0.08	22.03	0.09	99.99	-9.99	091119
637	2137	428.915	373.280	0.00	9.99	99.99	-9.99	23.04	0.14	22.92	0.13	22.70	0.17	99.99	-9.99	091119
638	2138	763.401	380.570	0.00	9.99	0.00	9.99	21.64	0.04	21.56	0.04	20.82	0.03	99.99	-9.99	001119
639	2139	558.459	386.504	0.00	9.99	99.99	-9.99	22.19	0.07	22.45	0.08	22.14	0.08	99.99	-9.99	091119
640	2140	77.927	387.649	0.00	9.99	99.99	-9.99	22.65	0.09	22.67	0.09	22.89	0.14	99.99	-9.99	091119
641	2141	735.327	389.035	0.00	9.99	99.99	-9.99	23.25	0.14	23.35	0.10	23.08	0.11	99.99	-9.99	091119
642	2142	405.318	391.936	0.00	9.99	99.99	-9.99	23.35	0.11	23.37	0.10	23.11	0.13	99.99	-9.99	091119
643	2143	64.533	397.287	0.00	9.99	99.99	-9.99	22.73	0.09	22.75	0.08	22.68	0.12	99.99	-9.99	091119
644	2144	76.297	395.499	0.00	9.99	99.99	-9.99	22.39	0.07	22.50	0.08	22.85	0.12	99.99	-9.99	091119
645	2146	64.388	396.236	0.00	9.99	99.99	-9.99	22.71	0.09	22.76	0.08	22.66	0.12	99.99	-9.99	091119
646	2147	699.038	397.055	0.00	9.99	99.99	-9.99	22.48	0.06	22.57	0.06	22.54	0.09	99.99	-9.99	091119
647	2149	574.550	421.590	0.00	9.99	19.94	0.04	21.20	0.04	21.31	0.05	21.19	0.05	99.99	-9.99	011119
648	2150	659.331	431.846	0.00	9.99	99.99	-9.99	23.08	0.08	22.93	0.06	22.79	0.08	99.99	-9.99	091119
649	2151	165.742	447.270	0.00	9.99	99.99	-9.99	22.36	0.05	22.31	0.05	21.76	0.04	99.99	-9.99	091119
650	2152	165.108	447.619	0.00	9.99	99.99	-9.99	22.38	0.05	22.31	0.05	21.76	0.04	99.99	-9.99	091119
651	2153	543.975	463.884	0.00	9.99	99.99	-9.99	23.36	0.11	23.19	0.08	22.83	0.09	99.99	-9.99	091119
652	2154	615.180	490.618	0.00	9.99	99.99	-9.99	22.84	0.08	22.85	0.09	22.28	0.08	99.99	-9.99	091119
653	2155	627.507	498.859	0.00	9.99	99.99	-9.99	23.22	0.12	23.08	0.09	23.29	0.16	99.99	-9.99	091119
654	2156	634.673	500.907	0.00	9.99	99.99	-9.99	23.24	0.11	23.26	0.08	22.98	0.11	99.99	-9.99	091119
655	2157	365.699	508.740	0.00	9.99	99.99	-9.99	22.86	0.08	23.15	0.08	22.73	0.07	99.99	-9.99	091119
656	2158	215.571	518.575	0.00	9.99	99.99	-9.99	21.94	0.04	22.04	0.04	21.94	0.05	99.99	-9.99	091119
657	2159	750.015	549.377	0.00	9.99	99.99	-9.99	23.72	0.17	23.41	0.12	22.91	0.10	99.99	-9.99	091119
658	2160	693.675	574.964	0.00	9.99	99.99	-9.99	22.95	0.09	22.66	0.06	22.44	0.06	99.99	-9.99	091119
659	2161	397.200	589.510	0.00	9.99	99.99	-9.99	23.00	0.08	22.94	0.06	23.45	0.13	99.99	-9.99	091119
660	2163	265.637	599.170	0.00	9.99	99.99	-9.99	23.10	0.09	23.08	0.07	22.91	0.09	99.99	-9.99	091119
661	2164	383.590	638.152	0.00	9.99	99.99	-9.99	22.98	0.10	23.52	0.14	23.61	0.16	99.99	-9.99	091119
662	2165	399.244	680.139	0.00	9.99	21.11	0.07	21.97	0.04	21.94	0.04	21.60	0.04	99.99	-9.99	011119
663	2166	476.093	709.264	0.00	9.99	99.99	-9.99	23.54	0.13	23.49	0.09	23.47	0.13	99.99	-9.99	091119
664	2168	177.466	739.666	0.00	9.99	99.99	-9.99	23.14	0.14	23.07	0.11	22.95	0.15	99.99	-9.99	091119
665	2169	141.720	746.099	0.00	9.99	99.99	-9.99	22.84	0.09	23.08	0.08	22.84	0.09	99.99	-9.99	091119
666	2170	182.887	746.890	0.00	9.99	99.99	-9.99	22.48	0.06	22.21	0.05	22.51	0.08	99.99	-9.99	091119
667	2171	422.010	755.157	0.00	9.99	99.99	-9.99	23.44	0.17	23.46	0.14	23.20	0.14	99.99	-9.99	091119
668	2172	465.286	755.062	0.00	9.99	99.99	-9.99	22.27	0.05	22.33	0.05	22.17	0.06	99.99	-9.99	091119
669	3057	786.075	69.995	0.00	9.99	0.00	9.99	99.99	-9.99	22.31	0.05	21.92	0.05	21.50	0.05	009111
670	3063	186.756	75.080	0.00	9.99	99.99	-9.99	99.99	-9.99	21.10	0.06	20.79	0.05	20.72	0.07	099111
671	3064	342.793	76.268	0.00	9.99	99.99	-9.99	99.99	-9.99	21.12	0.07	21.10	0.11	20.84	0.11	099111
672	3071	147.880	80.387	0.00	9.99	99.99	-9.99	99.99	-9.99	21.97	0.08	21.38	0.07	21.49	0.10	099111
673	3073	773.783	80.484	0.00	9.99	0.00	9.99	99.99	-9.99	20.98	0.04	20.98	0.03	21.13	0.04	009111
674	3074	423.992	83.424	0.00	9.99	18.07	0.02	99.99	-9.99	19.20	0.03	19.01	0.02	19.01	0.02	019111
675	3075	394.610	84.231	0.00	9.99	99.99	-9.99	99.99	-9.99	20.61	0.04	20.56	0.03	20.53	0.05	099111
676	3076	159.617	86.250	0.00	9.99	99.99	-9.99	99.99	-9.99	19.11	0.03	18.25	0.02	18.07	0.01	099111
677	3077	450.666	85.986	0.00	9.99	18.93	0.03	99.99	-9.99	20.47	0.04	20.28	0.04	20.06	0.03	019111
678	3078	588.801	86.906	0.00	9.99	0.00	9.99	99.99	-9.99	21.93	0.06	21.53	0.06	21.83	0.12	009111
679	3079	458.568	88.719	0.00	9.99	17.94	0.02	99.99	-9.99	19.26	0.03	19.04	0.02	18.97	0.01	019111
680	3082	583.138	93.717	0.00	9.99	0.00	9.99	99.99	-9.99	19.99	0.03	19.66	0.02	19.22	0.01	009111
681	3083	118.589	95.417	0.00	9.99	0.00	9.99	99.99	-9.99	21.90	0.09	21.46	0.08	21.05	0.08	009111
682	3085	239.431	97.636	0.00	9.99	99.99	-9.99	99.99	-9.99	22.05	0.13	21.57	0.10	20.98	0.08	099111
683	3086	351.064	97.557	0.00	9.99	18.76	0.02	99.99	-9.99	18.90	0.03	18.38	0.02	18.19	0.01	019111
684	3088	411.197	100.692	0.00	9.99	19.05	0.05	99.99	-9.99	20.39	0.07	20.25	0.05	19.95	0.04	019111
685	3092	405.891	104.326	0.00	9.99	18.07	0.02	99.99	-9.99	19.35	0.04	19.21	0.03	19.07	0.03	019111
686	3098	411.168	105.771	0.00	9.99	18.07	0.02	99.99	-9.99	19.35	0.04	19.21	0.03	19.07	0.03	019111
687	3099	198.325	106.783	0.00	9.99	99.99	-9.99	99.99	-9.99	21.73	0.15	20.95	0.11	20.96	0.12	099111
688	3102	426.865	108.712	0.00	9.99	19.98	0.07	99.99	-9.99	21.65	0.08	21.72	0.13	21.96	0.17	019111
689	3103	473.227	109.490	0.00	9.99	19.86	0.04	99.99	-9.99	20.92	0.05	20.80	0.04	20.64	0.05	019111
690	3105	426.056	109.546	0.00	9.99	19.98	0.07	99.99	-9.99	21.61	0.08	21.69	0.13	21.95	0.17	019111
691	3111	437.354	119.007	0.00	9.99	20.61	0.10	99.99	-9.99	21.75	0.08	21.84	0.09	21.97	0.16	019111
692	3114	437.032	119.426	0.00	9.99	20.61	0.10	99.99	-9.99	21.75	0.08	21.84	0.09	21.97	0.16	019111
693	3116	662.671	119.739	0.00	9.99	0.00	9.99	99.99	-9.99	22.70	0.09	22.21	0.08	21.97	0.09	009111
694	3117	416.674	120.525	0.00	9.99	16.50	0.02	99.99	-9.99	20.47	0.05	17.33	0.02	19.90	0.04	019111
695	3118	466.371	121.412	0.00	9.99	99.99	-9.99	99.99	-9.99	21.19	0.06	21.29	0.07	21.04	0.07	099111
696	3120	517.112	123.075	0.00	9.99	99.99	-9.99	99.99	-9.99	22.93	0.14	22.50	0.13	21.89	0.12	099111
697	3121	440.818	124.797	0.00	9.99	20.79	0.14	99.99	-9.99	22.09	0.10	21.73	0.10	21.67	0.14	019111
698	3122	465.491	124.071	0.00	9.99	99.99	-9.99	99.99	-9.99	21.25	0.06	21.29	0.07	21.04	0.07	099111
699	3124	407.128	125.122	0.00	9.99	99.99	-9.99	99.99	-9.99	21.69	0.09	21.41	0.08	21.10	0.09	099111
700	3131	193.724	133.594	0.00	9.99	99.99	-9.99	99.99	-9.99	22.36	0.05	21.88	0.08	21.57	0.07	099111
701	3133	662.772	132.407	0.00	9.99	0.00	9.99	99.99	-9.99	22.68	0.09	22.48	0.11	22.39	0.14	009111
702	3134	162.160	132.573	0.00	9.99	99.99	-9.99	99.99	-9.99	21.97	0.11	21.60	0.10	21.00	0.06	099111
703	3136	499.093	133.520	0.00	9.99	99.99	-9.99	99.99	-9.99	22.81	0.08	22.74	0.11	22.64	0.16	099111
704	3137	430.548	135.423	0.00	9.99	19.62	0.04	99.99	-9.99	21.26	0.07	20.99	0.06	21.38	0.11	019111
705	3138	306.500	135.586	0.00	9.99	99.99	-9.99	99.99	-9.99	22.59	0.12	22.24	0.16	21.94	0.13	099111
706	3141	318.137	137.793	0.00	9.99	19.94	0.03	99.99	-9.99	21.23	0.04	20.88	0.04	21.18	0.06	019111
707	3144	443.346	140.092	0.00	9.99	99.99	-9.99	99.99	-9.99	21.20	0.07	20.47	0.04	20.36	0.04	099111
708	3146	144.016	142.781	0.00	9.99	99.99	-9.99	99.99	-9.99	22.02	0.07	21.76	0.07	21.19	0.05	099111
709	3147	442.854	141.020	0.00	9.99	99.99	-9.99	99.99	-9.99	21.20	0.07	20.47	0.04	20.50	0.04	099111
710	3149	764.284	141.686	0.00	9.99	0.00	9.99	99.99	-9.99	22.61	0.09	21.72	0.07	21.56	0.07	009111
711	3151	472.053	143.729	0.00	9.99	99.99	-9.99	99.99	-9.99	22.11	0.08	21.68	0.09	21.55	0.09	099111
712	3152	182.359	145.464	0.00	9.99	99.99	-9.99	99.99	-9.99	21.17	0.05	21.08	0.05	20.85	0.05	099111
713	3153	463.769	144.695	0.00	9.99	99.99	-9.99	99.99	-9.99	22.93	0.17	22.50	0.17	22.02	0.15	099111
714	3159	563.719	148.727	0.00	9.99	99.99	-9.99	99.99	-9.99	22.25	0.11	22.24	0.17	21.84	0.16	099111
715	3160	253.495	150.355	0.00	9.99	99.99	-9.99	99.99	-9.99	22.58	0.07	21.60	0.06	21.21	0.06	099111
716	3162	625.847	151.020	0.00	9.99	0.00	9.99	99.99	-9.99	21.57	0.04	20.43	0.03	19.50	0.02	009111
717	3164	564.867	150.841	0.00	9.99	99.99	-9.99	99.99	-9.99	22.24	0.11	22.24	0.17	21.80	0.14	099111
718	3167	76.884	153.926	0.00	9.99	99.99	-9.99	99.99	-9.99	21.55	0.04	21.14	0.04	20.71	0.03	099111
719	3168	600.230	155.234	0.00	9.99	0.00	9.99	99.99	-9.99	22.86	0.15	22.35	0.14	21.77	0.13	009111
720	3170	267.730	155.296	0.00	9.99	99.99	-9.99	99.99	-9.99	22.68	0.07	22.09	0.08	21.79	0.09	099111
721	3171	361.304	157.029	0.00	9.99	99.99	-9.99	99.99	-9.99	22.73	0.07	21.96	0.06	21.61	0.06	099111
722	3172	587.162	156.919	0.00	9.99	0.00	9.99	99.99	-9.99	18.48	0.03	17.98	0.02	17.42	0.01	009111
723	3173	712.477	158.412	0.00	9.99	0.00	9.99	99.99	-9.99	22.38	0.06	21.83	0.05	21.80	0.07	009111
724	3174	763.076	157.516	0.00	9.99	0.00	9.99	99.99	-9.99	21.17	0.05	20.46	0.05	20.60	0.05	009111
725	3176	478.373	161.316	0.00	9.99	99.99	-9.99	99.99	-9.99	21.55	0.05	21.73	0.08	21.09	0.07	099111
726	3177	185.996	160.586	0.00	9.99	99.99	-9.99	99.99	-9.99	21.88	0.08	21.30	0.06	21.08	0.08	099111
727	3178	444.636	161.591	0.00	9.99	99.99	-9.99	99.99	-9.99	22.25	0.07	21.81	0.07	21.48	0.06	099111
728	3182	598.917	162.759	0.00	9.99	0.00	9.99	99.99	-9.99	22.55	0.11	21.83	0.11	21.25	0.10	009111
729	3185	600.409	167.101	0.00	9.99	0.00	9.99	99.99	-9.99	22.61	0.06	21.77	0.07	21.42	0.06	009111
730	3188	761.007	167.444	0.00	9.99	0.00	9.99	99.99	-9.99	19.16	0.03	18.64	0.02	18.59	0.01	009111
731	3191	223.006	169.180	0.00	9.99	16.46	0.02	99.99	-9.99	17.92	0.03	17.70	0.02	17.68	0.01	019111
732	3192	469.369	171.041	0.00	9.99	99.99	-9.99	99.99	-9.99	22.14	0.09	22.13	0.12	22.03	0.19	099111
733	3193	478.644	171.151	0.00	9.99	18.87	0.02	99.99	-9.99	19.70	0.03	19.29	0.02	19.09	0.01	019111
734	3194	125.701	174.253	0.00	9.99	99.99	-9.99	99.99	-9.99	22.14	0.05	21.59	0.05	21.39	0.05	099111
735	3196	733.236	175.105	0.00	9.99	0.00	9.99	99.99	-9.99	22.90	0.09	22.30	0.09	21.90	0.09	009111
736	3198	471.303	179.697	0.00	9.99	99.99	-9.99	99.99	-9.99	22.86	0.11	22.57	0.14	22.21	0.15	099111
737	3201	237.947	182.077	0.00	9.99	18.81	0.03	99.99	-9.99	20.03	0.04	19.75	0.03	19.51	0.02	019111
738	3202	757.904	184.616	0.00	9.99	0.00	9.99	99.99	-9.99	21.97	0.05	21.24	0.05	21.05	0.04	009111
739	3203	326.695	186.159	0.00	9.99	99.99	-9.99	99.99	-9.99	21.43	0.05	20.90	0.04	20.72	0.04	099111
740	3204	693.765	185.835	0.00	9.99	0.00	9.99	99.99	-9.99	22.70	0.06	22.62	0.08	22.03	0.09	009111
741	3206	93.841	187.162	0.00	9.99	99.99	-9.99	99.99	-9.99	20.56	0.04	20.28	0.02	19.96	0.02	099111
742	3211	536.134	196.881	0.00	9.99	99.99	-9.99	99.99	-9.99	21.47	0.04	20.96	0.03	20.62	0.03	099111
743	3212	616.556	196.556	0.00	9.99	0.00	9.99	99.99	-9.99	22.97	0.08	22.19	0.06	21.82	0.07	009111
744	3213	242.471	199.162	0.00	9.99	19.80	0.04	99.99	-9.99	20.90	0.05	20.80	0.05	20.49	0.06	019111
745	3215	265.802	199.730	0.00	9.99	99.99	-9.99	99.99	-9.99	22.30	0.13	22.39	0.17	22.20	0.17	099111
746	3216	183.926	201.785	0.00	9.99	20.60	0.05	99.99	-9.99	22.08	0.07	22.61	0.17	21.81	0.13	019111
747	3218	404.075	202.950	0.00	9.99	99.99	-9.99	99.99	-9.99	22.31	0.05	21.61	0.04	21.63	0.05	099111
748	3219	744.730	203.583	0.00	9.99	0.00	9.99	99.99	-9.99	22.09	0.05	21.65	0.06	21.41	0.05	009111
749	3222	756.556	203.072	0.00	9.99	0.00	9.99	99.99	-9.99	22.57	0.07	22.55	0.13	22.31	0.13	009111
750	3223	401.872	204.899	0.00	9.99	99.99	-9.99	99.99	-9.99	22.50	0.05	21.61	0.04	21.63	0.05	099111
751	3226	700.812	207.074	0.00	9.99	0.00	9.99	99.99	-9.99	22.89	0.08	21.98	0.06	21.45	0.05	009111
752	3227	245.891	208.370	0.00	9.99	18.61	0.02	99.99	-9.99	19.78	0.03	19.53	0.02	19.08	0.02	019111
753	3228	177.438	208.920	0.00	9.99	99.99	-9.99	99.99	-9.99	22.53	0.10	22.11	0.08	21.83	0.09	099111
754	3230	724.677	209.583	0.00	9.99	0.00	9.99	99.99	-9.99	22.30	0.07	21.94	0.07	21.62	0.06	009111
755	3232	249.493	210.361	0.00	9.99	18.61	0.02	99.99	-9.99	19.78	0.03	19.53	0.02	19.08	0.02	019111
756	3233	546.863	213.163	0.00	9.99	99.99	-9.99	99.99	-9.99	22.70	0.08	21.42	0.04	22.11	0.11	099111
757	3234	183.718	212.644	0.00	9.99	99.99	-9.99	99.99	-9.99	22.24	0.07	22.10	0.09	21.93	0.11	099111
758	3237	242.951	214.657	0.00	9.99	99.99	-9.99	99.99	-9.99	22.06	0.11	21.70	0.09	21.68	0.13	099111
759	3239	659.935	214.262	0.00	9.99	0.00	9.99	99.99	-9.99	21.29	0.04	20.84	0.03	20.70	0.03	009111
760	3241	384.122	216.068	0.00	9.99	99.99	-9.99	99.99	-9.99	22.56	0.08	22.10	0.10	21.96	0.11	099111
761	3242	491.924	215.358	0.00	9.99	99.99	-9.99	99.99	-9.99	21.52	0.05	21.20	0.05	20.99	0.05	099111
762	3244	293.593	217.401	0.00	9.99	99.99	-9.99	99.99	-9.99	22.87	0.11	22.52	0.11	22.33	0.13	099111
763	3245	695.860	218.065	0.00	9.99	0.00	9.99	99.99	-9.99	22.34	0.05	21.82	0.04	21.61	0.05	009111
764	3246	770.931	218.883	0.00	9.99	0.00	9.99	99.99	-9.99	22.85	0.10	22.63	0.14	22.36	0.14	009111
765	3251	550.552	225.627	0.00	9.99	99.99	-9.99	99.99	-9.99	22.80	0.10	21.80	0.07	22.40	0.15	099111
766	3254	487.843	226.080	0.00	9.99	99.99	-9.99	99.99	-9.99	22.37	0.07	21.72	0.05	21.47	0.06	099111
767	3256	562.795	229.845	0.00	9.99	99.99	-9.99	99.99	-9.99	22.11	0.06	21.31	0.04	21.04	0.05	099111
768	3260	189.251	232.807	0.00	9.99	99.99	-9.99	99.99	-9.99	22.59	0.07	22.04	0.08	21.45	0.06	099111
769	3264	369.385	237.791	0.00	9.99	99.99	-9.99	99.99	-9.99	22.19	0.06	21.80	0.06	21.77	0.09	099111
770	3265	148.631	238.327	0.00	9.99	99.99	-9.99	99.99	-9.99	22.77	0.14	22.10	0.10	21.33	0.06	099111
771	3273	411.627	243.288	0.00	9.99	99.99	-9.99	99.99	-9.99	22.21	0.07	21.68	0.07	21.62	0.08	099111
772	3275	523.201	245.754	0.00	9.99	99.99	-9.99	99.99	-9.99	22.37	0.06	21.90	0.08	21.62	0.08	099111
773	3278	384.815	248.267	0.00	9.99	99.99	-9.99	99.99	-9.99	22.68	0.11	22.23	0.10	22.01	0.11	099111
774	3283	702.988	256.921	0.00	9.99	0.00	9.99	99.99	-9.99	20.91	0.04	20.17	0.02	19.72	0.02	009111
775	3289	572.429	262.411	0.00	9.99	99.99	-9.99	99.99	-9.99	21.51	0.04	20.93	0.04	20.93	0.04	099111
776	3291	121.744	265.527	0.00	9.99	99.99	-9.99	99.99	-9.99	20.88	0.03	20.64	0.03	20.91	0.03	099111
777	3292	274.665	263.570	0.00	9.99	99.99	-9.99	99.99	-9.99	21.60	0.05	21.29	0.05	20.90	0.04	099111
778	3295	257.840	265.301	0.00	9.99	99.99	-9.99	99.99	-9.99	22.48	0.06	22.24	0.08	21.98	0.09	099111
779	3296	85.481	266.093	0.00	9.99	99.99	-9.99	99.99	-9.99	22.47	0.05	22.31	0.06	22.15	0.07	099111
780	3297	396.279	266.193	0.00	9.99	99.99	-9.99	99.99	-9.99	22.73	0.08	22.03	0.06	21.98	0.09	099111
781	3298	416.842	266.281	0.00	9.99	99.99	-9.99	99.99	-9.99	22.98	0.08	22.63	0.09	22.55	0.15	099111
782	3302	668.334	268.700	0.00	9.99	0.00	9.99	99.99	-9.99	22.36	0.08	22.13	0.10	22.05	0.13	009111
783	3303	698.190	268.797	0.00	9.99	0.00	9.99	99.99	-9.99	22.73	0.07	22.19	0.07	22.86	0.19	009111
784	3305	349.508	274.424	0.00	9.99	99.99	-9.99	99.99	-9.99	22.29	0.09	22.08	0.09	21.71	0.08	099111
785	3306	483.675	275.599	0.00	9.99	99.99	-9.99	99.99	-9.99	22.23	0.07	21.61	0.05	21.49	0.06	099111
786	3307	623.115	278.435	0.00	9.99	99.99	-9.99	99.99	-9.99	22.02	0.07	21.49	0.07	20.94	0.05	099111
787	3308	625.659	279.119	0.00	9.99	99.99	-9.99	99.99	-9.99	22.03	0.07	21.48	0.06	20.93	0.05	099111
788	3310	615.923	283.795	0.00	9.99	99.99	-9.99	99.99	-9.99	22.57	0.09	21.87	0.08	21.46	0.07	099111
789	3311	654.863	284.668	0.00	9.99	99.99	-9.99	99.99	-9.99	22.18	0.06	21.02	0.06	21.15	0.09	099111
790	3314	647.496	286.718	0.00	9.99	99.99	-9.99	99.99	-9.99	22.04	0.11	21.57	0.14	21.46	0.19	099111
791	3316	251.600	289.114	0.00	9.99	99.99	-9.99	99.99	-9.99	22.89	0.09	21.87	0.06	21.61	0.07	099111
792	3318	654.968	288.543	0.00	9.99	99.99	-9.99	99.99	-9.99	22.27	0.06	20.96	0.04	21.13	0.08	099111
793	3319	788.855	290.080	0.00	9.99	0.00	9.99	99.99	-9.99	22.44	0.07	20.63	0.03	22.35	0.15	009111
794	3324	669.764	294.361	0.00	9.99	99.99	-9.99	99.99	-9.99	22.71	0.08	21.91	0.08	21.58	0.07	099111
795	3325	240.653	296.905	0.00	9.99	99.99	-9.99	99.99	-9.99	21.37	0.04	21.08	0.03	21.03	0.04	099111
796	3327	66.729	300.317	0.00	9.99	99.99	-9.99	99.99	-9.99	22.52	0.07	22.43	0.07	22.26	0.09	099111
797	3332	520.967	312.596	0.00	9.99	99.99	-9.99	99.99	-9.99	22.10	0.06	21.46	0.07	21.47	0.09	099111
798	3333	67.570	314.602	0.00	9.99	99.99	-9.99	99.99	-9.99	20.53	0.03	20.22	0.02	19.91	0.02	099111
799	3338	517.465	315.865	0.00	9.99	99.99	-9.99	99.99	-9.99	22.11	0.11	21.52	0.11	21.96	0.19	099111
800	3339	673.144	316.398	0.00	9.99	99.99	-9.99	99.99	-9.99	21.89	0.05	22.20	0.10	21.88	0.10	099111
801	3342	660.244	318.597	0.00	9.99	18.97	0.02	99.99	-9.99	19.80	0.03	19.54	0.02	19.29	0.02	019111
802	3346	526.747	322.633	0.00	9.99	20.09	0.05	99.99	-9.99	20.82	0.04	20.40	0.04	20.12	0.03	019111
803	3349	522.864	329.922	0.00	9.99	99.99	-9.99	99.99	-9.99	20.37	0.04	20.01	0.03	20.10	0.03	099111
804	3350	516.043	329.142	0.00	9.99	18.85	0.03	99.99	-9.99	19.98	0.04	19.86	0.03	19.85	0.03	019111
805	3352	521.050	331.682	0.00	9.99	99.99	-9.99	99.99	-9.99	20.32	0.04	20.01	0.03	20.13	0.03	099111
806	3356	83.825	342.383	0.00	9.99	99.99	-9.99	99.99	-9.99	21.68	0.04	21.27	0.04	20.81	0.03	099111
807	3358	526.122	346.925	0.00	9.99	99.99	-9.99	99.99	-9.99	21.55	0.08	21.27	0.08	21.10	0.08	099111
808	3361	511.814	350.526	0.00	9.99	17.52	0.02	99.99	-9.99	18.09	0.03	17.67	0.02	20.68	0.07	019111
809	3367	528.884	355.226	0.00	9.99	99.99	-9.99	99.99	-9.99	22.53	0.14	21.94	0.13	21.79	0.14	099111
810	3369	514.940	356.607	0.00	9.99	99.99	-9.99	99.99	-9.99	21.89	0.05	21.20	0.05	20.86	0.05	099111
811	3371	535.451	363.758	0.00	9.99	99.99	-9.99	99.99	-9.99	21.43	0.05	21.74	0.07	21.54	0.07	099111
812	3373	421.161	369.810	0.00	9.99	99.99	-9.99	99.99	-9.99	22.40	0.09	22.01	0.09	22.24	0.15	099111
813	3380	760.960	378.426	0.00	9.99	0.00	9.99	99.99	-9.99	21.27	0.04	20.82	0.03	20.41	0.02	009111
814	3382	77.735	381.935	0.00	9.99	99.99	-9.99	99.99	-9.99	21.30	0.04	20.81	0.03	20.28	0.02	099111
815	3384	557.089	383.877	0.00	9.99	99.99	-9.99	99.99	-9.99	22.35	0.08	22.20	0.09	21.58	0.07	099111
816	3386	558.841	386.148	0.00	9.99	99.99	-9.99	99.99	-9.99	22.43	0.08	22.14	0.08	21.58	0.07	099111
817	3391	555.272	392.308	0.00	9.99	21.54	0.13	99.99	-9.99	22.87	0.19	22.12	0.13	21.28	0.09	019111
818	3392	562.751	393.559	0.00	9.99	99.99	-9.99	99.99	-9.99	21.23	0.05	21.13	0.06	20.61	0.04	099111
819	3393	562.667	393.148	0.00	9.99	99.99	-9.99	99.99	-9.99	21.20	0.05	21.13	0.06	20.61	0.04	099111
820	3395	693.694	395.132	0.00	9.99	99.99	-9.99	99.99	-9.99	22.05	0.04	21.50	0.04	21.14	0.03	099111
821	3397	64.819	396.520	0.00	9.99	99.99	-9.99	99.99	-9.99	22.75	0.08	22.68	0.12	22.44	0.13	099111
822	3402	65.737	399.040	0.00	9.99	99.99	-9.99	99.99	-9.99	22.75	0.08	22.68	0.12	22.49	0.14	099111
823	3404	583.411	400.841	0.00	9.99	99.99	-9.99	99.99	-9.99	21.94	0.07	21.34	0.07	21.31	0.08	099111
824	3406	580.906	402.229	0.00	9.99	99.99	-9.99	99.99	-9.99	21.79	0.08	21.38	0.07	21.31	0.08	099111
825	3407	776.334	404.832	0.00	9.99	0.00	9.99	99.99	-9.99	22.52	0.06	22.35	0.07	22.00	0.07	009111
826	3411	107.215	408.869	0.00	9.99	99.99	-9.99	99.99	-9.99	22.94	0.08	22.74	0.09	22.92	0.16	099111
827	3415	343.478	416.871	0.00	9.99	99.99	-9.99	99.99	-9.99	22.81	0.07	22.31	0.07	22.01	0.06	099111
828	3417	177.953	417.540	0.00	9.99	99.99	-9.99	99.99	-9.99	22.91	0.07	22.72	0.08	22.52	0.10	099111
829	3419	578.659	422.064	0.00	9.99	19.94	0.04	99.99	-9.99	21.45	0.05	21.09	0.05	21.25	0.07	019111
830	3420	92.317	426.676	0.00	9.99	99.99	-9.99	99.99	-9.99	22.47	0.05	21.92	0.04	21.43	0.04	099111
831	3424	766.451	433.663	0.00	9.99	99.99	-9.99	99.99	-9.99	22.51	0.05	22.20	0.05	21.78	0.05	099111
832	3430	583.974	451.190	0.00	9.99	99.99	-9.99	99.99	-9.99	22.91	0.06	22.57	0.07	22.19	0.09	099111
833	3431	74.747	454.029	0.00	9.99	99.99	-9.99	99.99	-9.99	22.67	0.06	22.12	0.05	21.47	0.04	099111
834	3434	679.091	461.621	0.00	9.99	20.30	0.04	99.99	-9.99	21.89	0.04	21.43	0.03	22.08	0.06	019111
835	3438	54.720	471.494	0.00	9.99	99.99	-9.99	99.99	-9.99	21.55	0.10	20.88	0.03	20.69	0.10	099111
836	3440	762.278	473.001	0.00	9.99	99.99	-9.99	99.99	-9.99	21.80	0.04	21.24	0.03	20.99	0.03	099111
837	3446	577.110	489.525	0.00	9.99	99.99	-9.99	99.99	-9.99	21.77	0.04	21.33	0.03	21.10	0.03	099111
838	3447	621.659	490.239	0.00	9.99	99.99	-9.99	99.99	-9.99	22.24	0.05	21.47	0.04	21.08	0.04	099111
839	3451	527.801	499.113	0.00	9.99	99.99	-9.99	99.99	-9.99	22.90	0.05	22.45	0.05	22.29	0.07	099111
840	3453	584.541	501.005	0.00	9.99	99.99	-9.99	99.99	-9.99	22.38	0.06	22.23	0.07	21.65	0.06	099111
841	3456	660.710	504.099	0.00	9.99	99.99	-9.99	99.99	-9.99	22.81	0.05	22.32	0.06	22.94	0.12	099111
842	3457	265.742	506.331	0.00	9.99	99.99	-9.99	99.99	-9.99	21.98	0.04	21.74	0.04	21.58	0.04	099111
843	3459	684.418	506.969	0.00	9.99	99.99	-9.99	99.99	-9.99	22.80	0.05	22.08	0.05	22.05	0.06	099111
844	3460	94.534	508.788	0.00	9.99	99.99	-9.99	99.99	-9.99	22.96	0.06	22.58	0.07	22.24	0.09	099111
845	3464	284.742	516.575	0.00	9.99	99.99	-9.99	99.99	-9.99	21.74	0.04	21.38	0.04	21.09	0.04	099111
846	3465	697.507	517.887	0.00	9.99	99.99	-9.99	99.99	-9.99	22.94	0.07	22.59	0.07	22.71	0.10	099111
847	3467	280.469	521.160	0.00	9.99	99.99	-9.99	99.99	-9.99	21.98	0.05	21.91	0.06	21.41	0.05	099111
848	3468	283.989	524.166	0.00	9.99	99.99	-9.99	99.99	-9.99	22.14	0.05	22.21	0.08	21.70	0.07	099111
849	3471	107.178	528.285	0.00	9.99	99.99	-9.99	99.99	-9.99	22.98	0.09	22.66	0.09	22.39	0.12	099111
850	3474	160.962	530.828	0.00	9.99	99.99	-9.99	99.99	-9.99	22.92	0.06	22.54	0.06	22.24	0.07	099111
851	3478	355.771	532.929	0.00	9.99	99.99	-9.99	99.99	-9.99	22.97	0.06	22.17	0.05	21.83	0.05	099111
852	3479	270.686	534.886	0.00	9.99	99.99	-9.99	99.99	-9.99	23.00	0.06	22.83	0.07	22.60	0.09	099111
853	3483	756.344	548.441	0.00	9.99	99.99	-9.99	99.99	-9.99	22.74	0.06	22.65	0.07	22.50	0.09	099111
854	3488	189.590	565.543	0.00	9.99	99.99	-9.99	99.99	-9.99	22.85	0.07	22.16	0.05	21.65	0.05	099111
855	3489	483.678	568.473	0.00	9.99	99.99	-9.99	99.99	-9.99	22.98	0.06	22.51	0.06	22.29	0.06	099111
856	3492	693.770	574.488	0.00	9.99	99.99	-9.99	99.99	-9.99	22.67	0.06	22.44	0.06	22.21	0.06	099111
857	3498	554.105	584.408	0.00	9.99	99.99	-9.99	99.99	-9.99	22.37	0.05	21.55	0.03	21.01	0.03	099111
858	3499	78.325	588.904	0.00	9.99	99.99	-9.99	99.99	-9.99	22.58	0.06	22.09	0.05	21.95	0.07	099111
859	3501	378.933	596.287	0.00	9.99	99.99	-9.99	99.99	-9.99	22.76	0.06	22.37	0.06	22.01	0.06	099111
860	3504	677.184	602.218	0.00	9.99	99.99	-9.99	99.99	-9.99	22.62	0.05	22.45	0.06	22.60	0.10	099111
861	3506	167.631	609.193	0.00	9.99	99.99	-9.99	99.99	-9.99	22.95	0.07	22.79	0.08	22.48	0.10	099111
862	3510	413.802	630.151	0.00	9.99	99.99	-9.99	99.99	-9.99	21.77	0.04	20.97	0.03	21.03	0.03	099111
863	3512	254.244	647.120	0.00	9.99	99.99	-9.99	99.99	-9.99	22.73	0.06	22.73	0.08	22.64	0.11	099111
864	3513	776.356	647.286	0.00	9.99	0.00	9.99	99.99	-9.99	22.71	0.05	21.74	0.03	22.00	0.05	009111
865	3514	645.371	649.398	0.00	9.99	0.00	9.99	99.99	-9.99	22.75	0.05	22.43	0.06	22.15	0.07	009111
866	3518	113.300	656.633	0.00	9.99	99.99	-9.99	99.99	-9.99	22.40	0.06	22.06	0.06	21.66	0.05	099111
867	3519	330.494	655.928	0.00	9.99	99.99	-9.99	99.99	-9.99	22.57	0.05	22.37	0.06	22.49	0.09	099111
868	3521	115.587	657.942	0.00	9.99	99.99	-9.99	99.99	-9.99	22.40	0.06	22.05	0.06	21.64	0.05	099111
869	3527	117.695	696.573	0.00	9.99	99.99	-9.99	99.99	-9.99	21.48	0.04	21.10	0.03	20.72	0.03	099111
870	3528	571.378	698.581	0.00	9.99	99.99	-9.99	99.99	-9.99	22.84	0.06	22.77	0.08	22.49	0.09	099111
871	3531	66.218	702.070	0.00	9.99	99.99	-9.99	99.99	-9.99	22.67	0.08	21.75	0.05	21.57	0.06	099111
872	3532	72.336	705.016	0.00	9.99	99.99	-9.99	99.99	-9.99	22.85	0.08	21.67	0.04	22.73	0.16	099111
873	3536	490.174	710.649	0.00	9.99	99.99	-9.99	99.99	-9.99	22.36	0.05	21.71	0.04	21.26	0.03	099111
874	3537	135.139	717.314	0.00	9.99	99.99	-9.99	99.99	-9.99	22.87	0.09	22.78	0.11	22.43	0.11	099111
875	3538	652.532	720.315	0.00	9.99	0.00	9.99	99.99	-9.99	22.87	0.06	22.24	0.05	22.06	0.06	009111
876	3539	308.584	721.434	0.00	9.99	99.99	-9.99	99.99	-9.99	21.21	0.04	20.84	0.03	20.63	0.03	099111
877	3553	465.446	754.750	0.00	9.99	99.99	-9.99	99.99	-9.99	22.33	0.05	22.17	0.06	22.12	0.07	099111
878	3554	79.770	757.472	0.00	9.99	0.00	9.99	99.99	-9.99	22.80	0.09	22.56	0.12	22.33	0.14	009111
879	3563	92.888	770.598	0.00	9.99	0.00	9.99	99.99	-9.99	22.98	0.12	22.07	0.07	22.08	0.09	009111
880	3565	497.280	773.707	0.00	9.99	0.00	9.99	99.99	-9.99	22.94	0.08	21.90	0.05	21.49	0.05	009111
881	3570	197.398	793.743	0.00	9.99	99.99	-9.99	99.99	-9.99	22.97	0.09	22.31	0.10	21.99	0.10	099111

Photometry and coordinates by Nate Bastian, Oct 2001

  Table 5: Coordinates and HST-WFPC2 narrow-band $H\alpha$ and [OIII] photometry
of 114 sources in the inner regions of the M51.

Explanations of the columns:
(1) : id-nr of $H\alpha$ sources
(2) : corresponding number in the table of broadband photometry
(3) : x-coordinate of $H\alpha$ source on HST-WF2-chip
(4) : y-coordinate of $H\alpha$ source on HST-WF2-chip
pixel (x=1,y=1) is RA(2000) 13h 29 m 55.90 s,    DEC(2000) = +47 degr 11 min 27.2 sec
pixel (x=800, y=800) is RA(2000) 13h 29 m 57.94 s,    DEC(2000) = +47 degr 13 min 16.6 sec
(5) and (6) : magnitude and uncertainty of F656N filter ($H\alpha$)
(7) and (8) : magnitude and uncertainty of F502N filter ([OIII])
(9) and (10): magnitude and uncertainty of F814W broadband filter
(11) : ch = indication of position-overlap of $H\alpha$ source and F814W-source
ch=1 or 2: position overlap is okay ( $\Delta x<1.5$ and $\Delta y<1.5$ pixels)
ch=0: positioin overlap is suspect = ( $1.5<\Delta x<2.0$ or $1.5<\Delta y<2.0$ pixels)
(12) : co = indication of position-overlap of [OIII]-source and F814W source
co=2: position overlap is okay ( $\Delta x<1.5$ and $\Delta y<1.5$ pixels)
co=0: position overlap is suspect = ( $1.5<\Delta x<2.0$ or $1.5<\Delta y<2.0$ pixels)

 

i	i	x	y	mag	$\Delta$mag	mag	$\Delta$mag	mag	$\Delta$mag	ch	co
				F656N	F656N	F502N	F502N	F814W	F814W
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)
1	3	205.734	39.004	17.42	0.06	0.00	-9.99	18.52	0.04	2	2
2	23	198.238	48.140	18.81	0.10	20.32	0.08	19.97	0.03	2	2
3	29	323.266	50.958	18.63	0.07	0.00	-9.99	21.21	0.11	0	0
4	36	332.184	58.848	17.46	0.04	0.00	-9.99	19.88	0.04	2	2
5	46	236.283	61.998	18.49	0.03	0.00	-9.99	20.75	0.06	2	2
6	64	346.368	70.546	18.37	0.06	0.00	-9.99	20.64	0.05	2	2
7	69	365.066	72.801	18.02	0.04	0.00	-9.99	21.45	0.09	2	2
8	73	191.900	74.562	20.90	0.34	0.00	-9.99	20.93	0.06	0	0
9	78	739.484	78.126	19.94	0.09	0.00	-9.99	22.14	0.09	2	2
10	82	366.854	80.942	19.94	0.26	0.00	-9.99	21.02	0.08	2	2
11	86	211.518	81.431	20.74	0.23	0.00	-9.99	21.14	0.07	2	2
12	89	391.984	84.434	20.47	0.28	20.98	0.14	20.58	0.05	2	2
13	90	409.678	83.898	17.48	0.03	0.00	-9.99	19.35	0.03	2	2
14	92	424.573	84.913	18.09	0.05	0.00	-9.99	19.00	0.02	2	2
15	95	405.611	85.742	19.37	0.32	19.63	0.05	19.70	0.03	2	2
16	97	211.500	85.842	20.64	0.22	0.00	-9.99	20.33	0.04	1	1
17	101	588.464	87.906	19.38	0.06	0.00	-9.99	21.58	0.05	2	2
18	104	458.625	89.786	18.25	0.04	0.00	-9.99	19.03	0.02	2	2
19	114	597.938	92.990	19.11	0.05	0.00	-9.99	21.20	0.05	2	2
20	115	193.332	92.727	16.76	0.01	17.36	0.01	17.21	0.02	2	2
21	123	347.589	96.067	17.96	0.04	0.00	-9.99	18.38	0.02	2	2
22	124	494.469	95.977	16.02	0.01	0.00	-9.99	18.69	0.02	2	2
23	125	265.415	96.590	20.12	0.09	21.33	0.17	20.32	0.03	2	2
24	126	216.358	97.176	18.23	0.03	18.65	0.02	18.23	0.02	2	2
25	128	406.709	98.486	18.96	0.07	0.00	-9.99	20.07	0.04	1	1
26	138	411.013	102.215	20.05	0.21	20.60	0.14	20.17	0.04	2	2
27	146	397.815	107.243	20.90	0.37	0.00	-9.99	21.57	0.18	2	2
28	147	411.708	106.580	19.17	0.09	19.74	0.06	19.15	0.02	2	2
29	150	244.717	109.584	19.94	0.08	20.83	0.10	19.65	0.03	2	2
30	152	473.422	110.659	19.74	0.14	0.00	-9.99	20.82	0.04	2	2
31	157	526.143	112.444	19.35	0.08	0.00	-9.99	20.56	0.04	2	2
32	160	414.819	115.533	17.02	0.01	0.00	-9.99	17.32	0.02	2	2
33	163	348.436	116.523	20.68	0.40	0.00	-9.99	20.97	0.05	2	2
34	164	522.710	117.270	18.76	0.05	0.00	-9.99	19.32	0.02	0	0
35	170	460.479	121.079	18.61	0.06	0.00	-9.99	20.03	0.03	2	2
36	174	477.496	123.460	17.32	0.03	0.00	-9.99	20.47	0.05	2	2
37	183	297.456	129.003	19.84	0.14	0.00	-9.99	20.83	0.04	2	2
38	193	318.314	138.756	18.42	0.03	0.00	-9.99	20.84	0.05	0	0
39	194	428.711	138.168	18.68	0.05	0.00	-9.99	21.21	0.09	2	2
40	195	437.139	138.800	19.79	0.20	0.00	-9.99	20.51	0.04	2	2
41	200	470.953	140.956	20.43	0.38	0.00	-9.99	21.72	0.09	2	2
42	206	433.796	145.512	20.59	0.37	0.00	-9.99	20.76	0.05	2	2
43	207	459.587	146.881	20.46	0.17	0.00	-9.99	21.22	0.06	0	0
44	217	555.034	153.558	19.50	0.05	0.00	-9.99	19.54	0.02	1	1
45	220	449.924	156.498	20.83	0.30	20.81	0.11	20.41	0.03	2	2
46	223	267.576	156.680	20.65	0.20	0.00	-9.99	22.14	0.08	2	2
47	227	218.344	157.311	18.26	0.04	0.00	-9.99	20.92	0.05	2	2
48	238	251.239	164.356	20.06	0.22	0.00	-9.99	21.92	0.09	2	2
49	244	226.605	165.671	17.55	0.06	17.99	0.01	17.69	0.02	2	2
50	251	479.256	172.567	19.50	0.05	20.16	0.06	19.29	0.02	2	2
51	253	407.696	173.420	19.66	0.09	0.00	-9.99	21.06	0.06	2	2
52	255	221.566	175.051	17.55	0.04	0.00	-9.99	21.15	0.10	2	2
53	256	239.506	175.965	18.76	0.10	0.00	-9.99	20.14	0.05	1	1
54	257	316.032	176.069	17.58	0.01	0.00	-9.99	20.25	0.02	2	2
55	259	538.957	178.281	20.02	0.07	0.00	-9.99	21.38	0.05	2	2
56	264	275.305	179.902	18.87	0.04	0.00	-9.99	21.06	0.04	2	2
57	265	237.222	181.948	18.32	0.06	20.10	0.07	19.73	0.04	2	2
58	267	191.514	183.677	19.66	0.14	0.00	-9.99	21.45	0.07	2	2
59	268	231.634	182.526	19.60	0.28	21.40	0.25	20.89	0.09	2	2
60	270	327.000	186.435	20.06	0.12	0.00	-9.99	20.87	0.04	2	2
61	274	251.996	186.189	20.62	0.35	0.00	-9.99	21.97	0.22	2	2
62	275	236.816	191.118	18.97	0.09	0.00	-9.99	21.60	0.13	0	0
63	281	238.834	195.885	20.01	0.15	20.93	0.13	20.48	0.06	2	2
64	282	257.190	196.812	19.60	0.09	0.00	-9.99	20.97	0.07	2	2
65	290	247.325	206.211	18.87	0.04	19.97	0.06	19.52	0.02	1	1
66	298	230.047	215.142	21.76	0.43	0.00	-9.99	21.33	0.06	2	2
67	300	493.298	216.898	20.32	0.13	0.00	-9.99	21.09	0.04	0	0
68	309	498.931	227.331	17.20	0.01	20.77	0.09	19.83	0.02	2	2
69	316	482.880	239.218	20.97	0.17	0.00	-9.99	21.52	0.04	2	2
70	320	522.998	245.496	21.21	0.26	0.00	-9.99	22.00	0.11	2	2
71	323	257.476	251.589	20.38	0.09	21.57	0.22	20.67	0.03	2	2
72	330	657.732	259.238	19.33	0.06	0.00	-9.99	19.32	0.02	0	0
73	332	578.737	261.714	19.50	0.07	0.00	-9.99	21.11	0.04	2	2
74	337	573.339	263.968	19.13	0.05	0.00	-9.99	20.93	0.03	0	0
75	352	578.367	281.535	19.64	0.08	0.00	-9.99	20.11	0.02	2	2
76	354	655.349	286.803	18.10	0.03	0.00	-9.99	21.12	0.05	0	0
77	358	696.580	296.227	21.08	0.19	0.00	-9.99	21.33	0.04	2	2
78	360	240.901	296.493	20.84	0.18	0.00	-9.99	21.09	0.03	2	2
79	361	393.765	297.706	18.63	0.02	0.00	-9.99	21.71	0.05	2	2
80	362	778.417	298.349	19.40	0.06	0.00	-9.99	19.53	0.02	2	2
81	363	635.102	299.969	19.44	0.09	0.00	-9.99	21.17	0.05	2	2
82	367	346.413	301.989	19.66	0.09	21.38	0.14	20.73	0.03	2	2
83	368	706.253	302.946	21.16	0.19	0.00	-9.99	21.46	0.04	2	2
84	372	607.908	312.120	20.86	0.19	0.00	-9.99	21.34	0.07	2	2
85	373	521.081	313.978	18.65	0.05	0.00	-9.99	21.30	0.05	2	2
86	378	367.258	314.923	20.64	0.16	0.00	-9.99	20.40	0.03	2	2
87	385	660.420	319.656	19.72	0.10	0.00	-9.99	19.57	0.02	2	2
88	388	519.272	321.917	19.73	0.21	0.00	-9.99	21.20	0.09	2	2
89	389	640.391	323.850	21.79	0.39	0.00	-9.99	21.23	0.05	2	2
90	393	508.769	330.281	18.90	0.10	19.81	0.05	19.16	0.02	2	2
91	394	517.462	328.769	18.86	0.12	0.00	-9.99	19.85	0.03	0	0
92	395	523.567	329.997	18.46	0.04	20.45	0.09	20.02	0.03	2	2
93	398	515.020	331.707	18.86	0.12	20.19	0.08	20.26	0.05	2	2
94	400	503.500	330.923	18.93	0.09	0.00	-9.99	19.87	0.03	2	2
95	405	740.318	341.535	20.22	0.08	0.00	-9.99	20.26	0.02	2	2
96	408	511.225	345.512	17.12	0.01	18.38	0.02	17.68	0.02	2	2
97	412	375.872	353.236	20.62	0.13	0.00	-9.99	20.42	0.02	2	2
98	416	519.026	359.529	20.65	0.19	0.00	-9.99	20.91	0.06	2	2
99	418	546.091	363.307	19.79	0.13	0.00	-9.99	22.13	0.09	2	2
100	419	398.875	365.987	21.34	0.26	0.00	-9.99	21.15	0.04	0	0
101	421	757.357	375.226	20.91	0.17	0.00	-9.99	20.58	0.03	2	2
102	422	762.276	378.157	20.66	0.13	0.00	-9.99	20.79	0.03	0	0
103	427	579.265	385.113	20.01	0.12	0.00	-9.99	20.43	0.03	2	2
104	429	787.790	389.245	20.46	0.11	0.00	-9.99	21.46	0.05	2	2
105	433	573.541	389.542	18.84	0.05	0.00	-9.99	19.77	0.02	0	0
106	441	566.322	400.157	18.89	0.04	0.00	-9.99	20.17	0.03	0	0
107	451	567.262	406.989	18.89	0.04	0.00	-9.99	20.58	0.04	2	2
108	454	750.864	407.931	20.21	0.09	0.00	-9.99	20.13	0.02	2	2
109	455	576.244	409.934	21.45	0.46	0.00	-9.99	21.31	0.09	2	2
110	464	584.322	426.102	18.27	0.04	0.00	-9.99	21.05	0.04	0	0
111	466	576.255	431.149	20.70	0.27	0.00	-9.99	22.18	0.06	2	2
112	467	592.140	432.517	20.08	0.11	0.00	-9.99	21.79	0.05	2	2
113	473	615.455	454.496	19.38	0.04	0.00	-9.99	19.42	0.02	0	0
114	515	287.260	594.394	19.17	0.04	0.00	-9.99	21.05	0.03	2	2

Photometry and coordinates by Nate Bastian and Henny Lamers, Oct 2001