Accretion dynamics and disk evolution in NGC 2264: a study based on the CorotThe CoRoT space mission was developed and is operated by the French space agency CNES, with participation of ESA’s RSSD and Science Programmes, Austria, Belgium, Brazil, Germany, and Spain photometric observations

Accretion dynamics and disk evolution in NGC 2264: a study based on the Corotthanks: The CoRoT space mission was developed and is operated by the French space agency CNES, with participation of ESA’s RSSD and Science Programmes, Austria, Belgium, Brazil, Germany, and Spain photometric observations

S.H.P. Alencar Departamento de Física – ICEx – UFMG, Av. Antônio Carlos, 6627, 30270-901, Belo Horizonte, MG, Brazil    P.S. Teixeira ESO, Karl-Schwarzschild-Strasse 2, D-85748 Garching bei München, Germany    M.M. Guimarães Departamento de Física – ICEx – UFMG, Av. Antônio Carlos, 6627, 30270-901, Belo Horizonte, MG, Brazil UFSJ – Campus Alto Paraopeba – Rodovia MG 443, KM 7, 36420-000, Ouro Branco, MG, Brazil    P.T. McGinnis Departamento de Física – ICEx – UFMG, Av. Antônio Carlos, 6627, 30270-901, Belo Horizonte, MG, Brazil    J.F. Gameiro Centro de Astrofisica da Universidade do Porto, Rua das Estrelas, 4150 Porto, Portugal    J. Bouvier Laboratoire d’Astrophysique, Observatoire de Grenoble, BP 53, F-38041 Grenoble Cédex 9, France    S. Aigrain School of Physics, University of Exeter, Exeter, EX4 4QL, UK Astrophysics, University of Oxford, Denys Wilkinson Building, Oxford, OX4 1DQ, UK    E. Flaccomio INAF - Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy    F. Favata European Space Agency, 8-10 rue Mario Nikis, 75015 Paris, France
Received ; accepted
Key Words.:
Stars: pre-main sequence – Techniques: photometry – Accretion, accretion disks

Context:The young cluster NGC 2264 was observed with the Corot satellite for 23 days uninterruptedly in March 2008 with unprecedent photometric accuracy. We present here the first results of the analysis of the accreting population that belongs to the cluster and was observed by Corot.

Aims:We intended to look for possible light curve variability of the same nature as that observed in the classical T Tauri star AA Tau, which was attributed to a magnetically controlled inner disk warp. The inner warp dynamics is directly associated with the interaction between the stellar magnetic field and the inner disk region.

Methods:We analysed the Corot light curves of 83 previously known classical T Tauri stars that belong to NGC 2264 and classified them according to their morphology. We also studied the Corot light curve morphology as a function of a Spitzer-based classification of the star-disk systems.

Results:The classification derived on the basis of the Corot light curve morphology agrees very well with the Spitzer IRAC-based classification of the systems. The percentage of AA Tau-like light curves decreases as the inner disk dissipates, from 40% 10% in systems with thick inner disks to 36% 16% in systems with anemic disks and none in naked photosphere systems. Indeed, 91% 29% of the CTTS with naked photospheres exhibit pure spot-like variability, while only 18% 7% of the thick disk systems do so, presumably those seen at low inclination and thus free of variable obscuration.

Conclusions: AA Tau-like light curves are found to be fairly common, with a frequency of at least 30 to 40% in young stars with inner dusty disks. The temporal evolution of the light curves indicates that the structure of the inner disk warp, located close to the corotation radius and responsible for the obscuration episodes, varies over a timescale of a few (1-3) rotational periods. This probably reflects the highly dynamical nature of the star-disk magnetospheric interaction.

1 Introduction

T Tauri stars are young, optically visible, low-mass stars still contracting toward the main sequence. They have strong magnetic fields (2 kG) and are X-ray emitters. The so-called weak line T Tauri stars (WTTSs) do not exhibit evidence of disk accretion, while the classical T Tauri stars (CTTSs) do. CTTSs present broad emission lines and sometimes also forbidden emission lines. They are spectroscopically and photometrically variable, and show ultraviolet (UV), optical and infrared (IR) excess with respect to the photospheric flux.

Magnetospheric accretion models are the current consensus to explain the main observed characteristics of CTTSs (Shu et al., 1994; Hartmann et al., 1994; Muzerolle et al., 2001; Kurosawa et al., 2006). In these models, the stellar magnetosphere is strong enough to disrupt the circumstellar disk at a few stellar radii. Material in the inner disk, ionized by stellar radiation, falls towards the star following magnetic field lines and hits the stellar photosphere at near free-fall velocities, creating hot spots on the stellar surface. Part of the ionized material in the inner disk region is ejected in a magnetically controlled wind. In this scenario, the broad permitted emission lines are formed partly in the accretion funnel and the hot spot emits a continuum flux that is responsible for the UV and optical excess that veils the photospheric lines. The IR excess comes from reprocessing by the dust in the disk of the stellar and accretion radiation and, at least for high accretion rate systems, viscous heating may also contribute to it. When observed, forbidden emission lines are thought to be formed in the low density wind.

In the last decade, numerical simulations of accreting young stars have predicted a very dynamical star-disk interaction, mediated by the stellar magnetic field (Goodson et al., 1999; Matt et al., 2002; Romanova et al., 2009; Zanni, 2009). Many magneto-hydrodynamical (MHD) model predictions derive from the idea that the stellar magnetic field interacts with the inner disk region near the co-rotation radius but not only at the co-rotation point. Consequently, due to differential rotation between the star and the inner disk region, the magnetic field lines become distorted after a few rotational periods and eventually reconnect, restoring the initial field configuration. This process goes on as the star rotates. The time scale for the reconnection events depends on the diffusivity of the stellar magnetic field lines in the inner disk region, which is a very poorly constrained parameter.

AA Tau is one of a few CTTSs studied with enough detail to test the MHD model dynamical predictions. The star was observed photometrically for a month during three different campaigns, two of which included high-resolution simultaneous spectroscopy (Bouvier et al., 1995, 2003, 2007). AA Tau shows a light curve (LC) with a flat maximum interrupted by deep quasi-periodical minima that vary in depth and width from one rotational cycle to the other. The minima occur with little color change and are thought to be due to obscuration of the stellar photosphere by circumstellar disk material present in an inner disk warp. The warp is due to the interaction of the stellar magnetic field, inclined with respect to the rotation axis, and the inner disk region. The spectroscopic results showed that the magnetic field lines inflate in the course of a few rotational cycles, as measured by the radial velocity of the red and blue absorption components of the H line. Moreover, when the field lines are the most inflated, accretion to the star is suppressed, with no apparent veiling, and low emission-line equivalent widths, which again corroborates the MHD model predictions. After reconnection, accretion starts all over again. The last two AA Tau observational campaigns were separated by 5 years and the field line inflation discovered in the second campaign was still present with the same characteristics in the third one.

Although the AA Tau observations gave strong support to the MHD results, it was still unclear whether this behaviour was common among CTTSs. In order to test this, one needs good photometric measurements of a large number of CTTSs, covering several rotational cycles. In Taurus the typical rotational period of a CTTS is around 8 days, so that stars need to be monitored for at least a month continuoulsy. This is not an easy task from the ground, due to telescope time allocation and weather conditions. The Corot satellite additional program to observe the young stellar cluster NGC 2264 has allowed us to perform such study on a large sample of CTTSs.

NGC 2264 is a well studied young stellar cluster with an age of Myr located at a distance of about 760 pc (see Dahm, 2008, for a recent review on the cluster). We matched the various available datasets on the cluster from the literature based on spatial coincidence using a 2” tolerance. In a small number of cases, double identifications (i.e. more than one object within 2”) were transformed into single ones, specifically in cases in which one of the two objects had a small offset and the other a large one. Due to the many studies on the cluster, going from UV to X-rays, it was possible to establish reasonable criteria for cluster membership. We considered as likely members of NGC 2264 stars selected according to one or more of the following criteria: i) photometric H and variability with the data of Lamm et al. (2004) and following their criteria, ii) X-ray detection (Ramírez et al., 2004; Flaccomio et al., 2006) and location on the cluster sequence in the (, ) diagram if and magnitudes are available, iii) spectroscopic H equivalent width greater than 10 Å and iv) H emission line width at 10% intensity greater than 270  km s, as proposed by White & Basri (2003) to identify accreting T Tauri stars, and measured by Fűrész et al. (2006) for many cluster members.

The mean rotational period of CTTSs in NGC 2264 is around 3 to 4 days (see Sect. 4). Corot observed the cluster for 23 days uninterruptedly, covering several rotational cycles for most of the stars, thus allowing the identification of AA Tau-like candidates and the determination of precise rotational periods for cluster members. The complete rotation analysis will be discussed separately in another paper (Affer et al. in preparation).

2 Observations

Corot observed NGC 2264 from the 7th to the 30th of March 2008. The whole cluster fitted in one of the two CCDs normally used for the exo-planet observations, and stars were observed down to . We used the light curves delivered by the Corot pipeline after nominal corrections (Samadi et al., 2007). We further corrected the pipeline light curves removing outliers, mainly due to the South Atlantic Anomaly crossings, by applying a sigma clipping filter, taking care not to remove flaring events. The data was also corrected for the effects due to the entrance and exit into Earth eclipses. We did not make use of the color information provided by Corot for the brightest stars, and based our analysis on the broadband, “white light” light curves. All the light curves presented here were rebinned to 512 s and correspond to the integrated flux in the Corot mask. The flux RMS over 512 s achieved is of the order of 0.0005 for a star and 0.004 for a star, yielding the most detailed light curves of young accreting systems up to now, as shown in Figure 1. A complete catalog of the observations will be published in a subsequent paper (Favata et al. in preparation).

3 Results

3.1 Classical T Tauri sample selection

Figure 1: A sample of 6 CTTS light curves from the COROT observation of NGC 2264. corresponds to the maximum flux value of each LC. Light curves and have been classified as spot-like, and as AA Tau-like and and as irregular.

After selecting the cluster members as described in Sect. 1, we classified as CTTSs stars that presented either H equivalent width greater than 10 Å, excess less than a threshold calculated below, or H width at 10% intensity greater than 270  km s. Some stars presented more than one of the above characteristics. White & Basri (2003) showed that the accretion criterium based on H equivalent width is spectral-type dependent, the threshold being smaller than 10 Å for spectral types earlier than K7 and greater than 10 Å for spectral types later than M2.5. Whenever spectral type information was available, we followed the accretion criteria proposed by White & Basri (2003), instead of using the standard 10 Å value. Rebull et al. (2002) proposed that stars in NGC 2264 with excess less than could be classified as disk candidates. This threshold value was based on a study of the Orion star forming region (Rebull et al., 2000). However, the excess is also expected to be spectral-type dependent, stars with later spectral types presenting higher excess compared to earlier ones, for the same mass accretion rate, due to the higher contrast between the hot spot and the stellar photosphere in later spectral types. Therefore we looked for all the stars of our sample that were selected as CTTS based on excess and another criterion (H equivalent width or H width at 10% intensity). We separated them in two spectral type ranges (K0-K6 with 14 stars and K7-M3 with 10 stars) and computed the mean excesses in each dataset. The K0-K6 CTTSs present excess of mag and the K7-M3 CTTSs present excess of mag. Using the one sigma upper boundary in each spectral type range as a threshold to separate CTTS from WTTS ( for K0-K6 and for K7-M3), we select 7 stars as CTTSs based only on excess. While the value of mag proposed by Rebull et al. (2002) seems to be adequate for stars in the K0-K6 spectral range, it is apparently too high to select K7-M3 CTTSs in NGC 2264.

We found 83 CTTSs among the 301 observed cluster members and present in Table 1 the data used to make the CTTS classification. The H equivalent width was taken from Rebull et al. (2002) and Dahm & Simon (2005) except for six stars (CID 223957455, 223959618, 223964667, 223968688, 223991832, 223994721) for which we measured the H equivalent width ourselves, using the high resolution hectoechelle spectra kindly provided by Gabor Fűrész. The excess data was obtained from Rebull et al. (2002) and Fallscheer & Herbst (2006) (the data table was kindly provided by Cassandra Fallscheer) and the H width at 10% intensity comes from Fűrész et al. (2006).

Some CTTSs that were selected based on their excess have H values that are below 10 Å and would therefore not be selected as CTTS based only on H equivalent width. However, their excess is lower than our established threshold values and in the same range as many other systems that present either H equivalent width greater than 10 Å or H width at 10% larger than 270  km s. We have to be aware that both H equivalent width and excess are strongly variable in these stars and were not measured simultaneously. So it seems reasonable to use both criteria to select possible CTTSs.

3.2 Morphological light curve classification

We looked for periodical variations in the LCs of the observed CTTSs, using the Scargle periodogram as modified by Horne & Baliunas (1986), and found that 51 out of 83 CTTSs presented periodical variability. Periodic LCs were divided in two groups: group PI, containing sinusoidal-like LCs with stable shape from cycle to cycle, and group PII, flat-topped LCs with a clear maximum interrupted by minima that can vary in width and depth from cycle to cycle. The variations in group PI are associated with long-lived spots with lifetime of at least of weeks, while group PII is associated with AA Tau-like systems, where most of the variability is due to obscuration by circumstellar disk material. The non-periodical LCs (group NP) can be due to obscuration by non-uniformly distributed circumstellar material or to non-steady accretion or both.

A total of 83 CTTSs that belong to NGC 2264 were observed by Corot, 28 of which were classified as spot-like (group PI), 23 as AA Tau-like (group PII) and 32 as irregular (group NP). A sample of light curves of each type is shown in Fig. 1. In Figure 2 we present the periodical LCs of Fig. 1 folded in phase with the periods determined with the Scargle periodogram as modified by Horne & Baliunas (1986). We can notice the stability of the spot-like LCs (Fig. 1 and Fig. 2 and ) in the timescale of the observations, which makes them, in general, easily distinguishable from the AA Tau-like ones (Fig. 1 and Fig. 2 and ). Among the irregular LCs, some look more like due to variable accretion events (variable hot spots, Fig. 1 ) and others to obscuration by non-uniform circumstellar material (Fig. 1 ), but it is hard to decide which process is the dominant one based only on the Corot light curves without any color information. Therefore we did not make any attempt to further classify the irregular systems.

Figure 2: The four periodic LCs from Fig. 1 folded in phase. Different colors correspond to different cycles.

We measured the variability amplitude of a LC as . In our sample, the observed CTTS variability amplitudes range from 3% to 137%, excluding flaring events. The variability amplitude of spot-like LCs is generally around 10% to 15% and most of the stars that present more than 20% of variability amplitude have LCs that are classified as due to obscuration by circumstellar material (AA Tau-like). The AA Tau system variability amplitude, measured from data in the literature, is 76% and 8 out of 83 stars observed by Corot have a higher variability amplitude than AA Tau. This shows that, although AA Tau presents a high variability amplitude, probably due to its high inclination with respect to our line of sight ( 75° Bouvier et al., 2003), it is not exceptional among CTTS systems.

From the results in this Section, it becomes clear that the AA Tau photometric behavior is not an exception, but a rather common occurence among young stellar systems, representing 28% 6% of the CTTS systems in NGC 2264 observed with Corot. The percentage of AA Tau-like systems among the observed CTTSs seems reasonable, given that only some geometric configurations (i.e. high inclination) would produce occultation of the stellar photosphere, and the chances for occultation events will also depend on the disk warp’s location and scale-height. This result is however higher than the value of 10% to 15% calculated by Bertout (2000) using flared disk models for the propability of observing partial occultation events in CTTS systems. However, the disk models by Bertout (2000) did not include an inner disk warp, and consequently underestimate the probability of obscuration. Assuming a random distribution of axial inclinations, the fraction of AA Tau-like LCs in our sample () suggests for inner disk warps, where and are the inner warp height and distance to the central star. This is larger than the standard value used in -disk models, where (Bertout et al., 1988; Duchêne et al., 2010).

3.3 Merging Corot and Spitzer data

Spitzer IRAC data were also available for the cluster (Teixeira, 2008), with a total of 68 CTTSs present in both Spitzer and Corot observations. IRAC is useful to identify near-infrared excess emission that arises from warm dusty circumstellar material. We used the index, which represents the slope of the spectral energy distribution between 3.6 m and 8 m, to classify the inner disk structure of the observed systems, following the criteria proposed by Lada et al. (2006). Stars with are classified as naked photospheres (i.e., these systems are devoid of dust within a few AU), stars with have anemic disks (optically thin inner disks), stars with have optically thick inner disks (referred to as thick disks henceforth), those with are flat spectra sources and the ones with are Class I objects.

We combined both datasets in order to see if the light curve morphology was related to the evolution of the inner disk structure. The result, presented in Figure 3, shows that the agreement between the two classification approaches of CTTS (based on the Corot light curves and on the Spitzer photometry) is excellent. None of the systems with naked photospheres exhibit AA Tau-like LCs and 10/11 (91% 29%) of them show pure spot-like variability. The percentage of AA Tau-like LCs, which are due to obscuration by circumstellar disk material, thus increases from 0% for the evolved inner disk systems (naked photospheres) to 36% 16% for the anemic disk systems and 40% 10% for the thick disk systems. Because some of the non-periodic LCs may also be partly caused by circumstellar obscuration (see a possible example in Fig. 1), the fractional estimates of obscuration LCs are lower limits for systems with anemic and thick disks.

Spot-like systems represent 91% 29% of the naked photospheres, 28% 14% of the anemic disks and 18% 7% of thick disk systems. They are observed in systems where there is no obscuring material in our line of sight towards the star. This could be due to inner disk clearing, corresponding to spot-like LCs which represent naked photosphere systems and some anemic disks, shown in Fig. 3. Spot-like LCs could also come from low inclination systems. In this case, there could be inner disk material, but it would not obscure the star. This probably corresponds to some anemic disk systems and to all thick disk systems that show spot-like LCs.

Figure 3: NGC 2264 classical T Tauri stars observed with Corot and Spitzer. Diamonds correspond to spot-like LCs, triangles to AA Tau-like LCs and squares to non-periodical LCs. The four stars with large overplotted diamonds are fast rotators ( days). One fast rotator was not included in this figure (CID 500007354, days), because of the huge uncertainty (2.89) on its index. It is nevertheless included in Table 1 and in our LC analysis.

The non-periodical LCs represent 9% 9% of the naked photospheres, 36% 16% of the anemic disks and 42% 10% of the thick disk systems. The irregular LCs among naked photosphere systems can be due to non-steady accretion, which will produce short-lived and variable hot spots. Some irregular systems among anemic disks and thick disks are also likely due to a combination of non-steady accretion and low inclination, as apparently observed in TW Hya (Rucinski et al., 2008). It may however not be straightforward to assign non-periodical LCs to non-steady accretion, as recently shown by Kulkarni & Romanova (2009). They computed MHD models of the interaction between a magnetized star and its circumstellar disk with non-steady accretion and showed that, at large misalignment angles (°) between the stellar rotation and magnetic axis, hotspots are approximately fixed on the star’s surface, even during strongly unstable accretion, and consequently the LCs always show the stellar rotation period. Assuming that the circumstellar environment of a CTTS may be complex, random accretion events due to circumstellar blobs, which fall towards the star, could also temporarily occult the star and explain some of the observed non-periodical systems, as proposed by DeWarf et al. (2003) to explain the irregular photometric variability of the CTTS SU Aur. Another situation that could produce irregular LCs is a flared disk seen at high inclination. We could then expect to see partial obscuration by circumstellar disk material from the disk outer layers. Bertout (2000) calculated the partial obscuration probability by a flared disk and showed that, for a typical CTTS, it would be of the order of 10% to 15%. In this case, assuming Keplerian disk rotation and a typical CTTS disk with an outer radius of 100 AU, we would unfortunately not be able to measure short scale variability, as observed with Corot, due to material located in most disk radii because of the limited duration of our observations.

4 Discussion

We calculated periods for all CTTSs that presented periodic variations (51 out of 83 CTTSs), using the Scargle periodogram as modified by Horne & Baliunas (1986). We present in Fig. 4 the period distribution of the spot-like (black histogram) and AA Tau-like (red histogram) systems. A complete discussion on period distribution in NGC 2264 is presented in another paper (Affer et al. in preparation).

The major difference between the period distributions of spot-like and AA Tau-like systems is that fast rotators ( days) are only found with spot-like LCs. Among the seven fast rotating CTTSs, five also have Spitzer IRAC measurements. Four of them are classified as naked photosphere systems and another is a thick disk system. The thick disk system (CID 223980447, , days) is a K6 star (Dahm & Simon, 2005) and has high-resolution hectoechelle spectra (Fűrész et al., 2006) that Gabor Fűrész kindly made available to us. We measured  km s, using the SYNTH3 code provided by Dr. Oleg Kochukhov (Kochukhov, 2007), together with MARCS atmospheres (Gustafsson et al., 2008) and atomic lines from VALD (Kupka et al., 2000, 1999). Assuming R, we obtain °. This low inclination can explain the presence of circumstellar material with no obscuration in the LC. Except for this system, most fast rotators are found among systems that have cleared out their inner disk regions, which could be an indication that as the star-disk coupling decreases, stars tend to spin-up, as also found by Rebull et al. (2006) and Cieza & Baliber (2007) in Orion and NGC 2264. This is not a straghtforward conclusion, however, from our data, since the number of fast rotators is small and on the other hand some naked photosphere and anemic disk systems are actually found to rotate slowly, with periods up to 10 to 15 days.

The periods measured in the AA Tau-like LCs fall in the range of periods obtained from spot-like LCs. The periods measured from the spot-like LCs correspond to stellar rotational periods, since spots are located at the stellar photosphere. This indicates that AA Tau-like periods are within the range of stellar rotational periods of CTTSs in NGC 2264 and therefore the material that obscures the star must be located close to the corotation radius. Since the inner warp is by definition located close or at the dust disk truncation radius, this implies that the dust truncation radius is near the corotation radius in the systems we classified as AA Tau-like. Carr (2007) showed that the inner gas radius is on average slightly smaller than the corotation radius, while the inner dust radius falls at or outside the corotation radius. This is quite consistent with the Corot results.

Since the inner disk warp is located near the corotation radius, the variations observed from cycle to cycle in width and depth of the photometric minima should be related to the dynamical star-disk interaction in the inner disk region, that is thought to be responsible for the accumulation of material near the disk truncation region, forming inner disk warps. Like AA Tau, the star-disk interaction is seen to be very dynamic on a rotational timescale, as predicted by MHD models of young magnetized star-disk systems (Goodson et al., 1999; Matt et al., 2002; Romanova et al., 2009; Zanni, 2009). In our observations some systems are more regular and stable than others, but it is quite common to see systems that present photometric minima that vary substantially from cycle to cycle, still keeping their overall periodic nature (see Figs.1,2 and ).

Figure 4: Period distribution of CTTSs. The black histogram corresponds to spot-like LCs and the red histogram to the AA Tau-like LCs.

5 Conclusions

We showed that the AA Tau photometric behavior is common among CTTSs, being present in 28% 6% of the CTTSs in our sample. This represents a lower limit, since the AA Tau-like LCs are more likely produced at high inclinations, and we are probably missing about 20% to 30% of the very high inclination systems, according to the calculations by Bertout (2000), which will be totally obscured by a flared disk and thus too faint to be observed by Corot.

If our interpretation of such systems is correct, the photometric minima are due to obscuring material located in the inner disk region, near the corotation radius. This material is built up through the interaction between an inclined stellar magnetosphere and the inner disk region. The observed periodical changes in width and depth of the observed minima, over a timescale of a few ( 1-3) rotational periods, would then reflect the dynamics of such an interaction, as predicted by MHD models of young low mass star-disk systems.

We compared the Corot light curves with Spitzer IRAC data of the same systems and showed that the agreement between classifications based on the two datasets is excellent. The percentage of AA Tau-like light curves, which are due to obscuration by circumstellar material in the inner disk region, varies as the inner disk dissipates, decreasing from 40% 10% in systems with thick inner disks to 36% 16% in systems with anemic disks and none in naked photosphere systems. Indeed, 91% 29% of the systems with naked photospheres exhibit pure spot-like variability, while only 18% 7% of the thick disk systems do so, presumably those seen at low inclination and thus free of variable obscuration.

We thank Gabor Fűrész for making his Hectoechelle spectra and the updated electronic version of his tables available to us. We thank Cassandra Fallscheer for making available to us her table of U-V excess measurements. This research is based on data collected on the Corot satellite. SHPA and MMG acknowledge support from CNPq, CAPES and Fapemig. JFG acknowleges support from the FCT project PTDC/CTE-AST/66181/2006.


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RA Dec V Corot ID HEW UV1 UV2 H10% SpT LC group Period
(deg) (deg) (mag) (Å) (mag) (mag) (days)
99.89338 9.91424 16.64 223957455 22.1 x NP
99.92281 9.77214 14.64 223959618 28.4 x PII 3.87
99.99684 9.45681 16.34 223964667 42.2 x PII 6.45 -1.87
100.04666 9.63501 16.67 223968039 52.9 -1.15 x K6 NP -1.35
100.05673 9.41375 13.02 223968688 0.60 x K0 PI 1.11 -2.81
100.05710 9.94183 17.02 400007614 130.2 x M2 NP 0.0149
100.09620 9.46176 16.04 223971231 49.5 -1.62 x K5 NP -1.73
100.09889 9.92330 17.55 223971383 80.6 x PI 4.66 -1.22
100.12006 9.51718 15.20 223972652 39.1 -0.89 K4 NP -0.56
100.12186 9.73542 17.69 400007809 31.3 -1.36 x M2 NP
100.12859 9.57794 16.03 223973200 22.2 x K1 NP -1.29
100.13013 9.51864 15.43 223973292 1.7 -0.91 K6 PI 1.96
100.15217 9.84601 16.67 400007538 21.1 -2.11 -1.687 M2 NP -1.29
100.15262 9.80638 15.62 500007298 4.9 -1.43 -0.606 K5 PI 15.70 -4.19
100.15781 9.58167 16.64 400007528 23.4 x M3 NP -1.87
100.16297 9.84961 15.43 500007252 46.5 -1.89 x K4 PII 7.06 -1.55
100.16840 9.84735 15.50 500007272 58.3 K7 PI 3.76 -2.42
100.17086 9.46509 16.53 500007505 13.2 NP -1.97
100.17095 9.79936 16.01 500007379 7.5 -1.22 -0.984 K7 PI 14.15 -1.97
100.17216 9.85066 15.70 500007315 24.5 -2.13 K7 PII 7.80 -1.19
100.17233 9.90385 13.57 223975844 12.2 0.02 x G3 PI 3.31
100.17435 9.86237 15.49 500007269 23.4 K5 PI 3.75 -1.53
100.17576 9.56040 12.09 223976028 7.3 x G0 NP -1.12
100.18006 9.78535 16.33 500007460 27.1 x K6 NP
100.18580 9.54061 18.13 500007930 60.0 M3 NP -2.61
100.18819 9.47901 14.55 223976747 7.2 -0.16 x K2 PII 3.16
100.19793 9.82471 14.14 500007120 12.8 -0.806 x K1 PII 4.23 -1.41
100.19968 9.55087 18.24 500007963 -0.917 PI 2.56
100.20505 9.96077 17.46 500007730 50.8 M1 PI 11.85 -2.67
100.20789 9.61375 15.37 223977953 66.3 -1.79 -1.906 K4 PII 4.96 -1.43
100.21081 9.91593 15.13 500007209 11.2 x K2 PII 2.51 -2.14
100.21326 9.74615 12.05 223978308 3.5 x G0 PII 5.40 -1.69
100.22346 9.55686 14.70 223978921 18.2 -0.643 x K1 NP -2.29
100.22607 9.82232 16.39 500007473 161.1 -2.11 x M0 NP -0.38
100.22990 9.84718 15.89 500007354 2.8 -0.64 -0.774 K5.5 PI 1.17 -9.15
100.23215 9.85385 15.54 500007283 8.00 K5.5 PI 3.23 -0.29
100.23663 9.63029 15.09 223979728 113.2 -1.353 x M1 NP -1.17
100.24208 9.61483 18.05 223980048 34.0 PII 4.06 -1.41
100.24447 9.60368 17.40 223980233 22.2 M4 NP
100.24510 9.65522 17.02 223980258 27.9 x M0 PI 7.05 -1.39
100.24516 9.51592 14.04 223980264 14.3 x K2.5 PII 3.46 -1.51
100.24770 9.99596 15.34 223980412 7.41 -0.53 K5 PI 3.23
100.24792 9.49770 17.00 500007610 26.2 M3 PII 4.66 -1.16
100.24811 9.58636 15.58 223980447 6.4 -1.01 -0.427 x K6 PI 1.67 -1.14
100.25209 9.75088 15.39 223980688 15.0 -0.59 -0.723 x K3 PII 4.16 -2.10
100.25214 9.48776 14.56 223980693 16.6 x K4 PII 5.35 -1.72
100.25323 9.85620 14.63 500007157 1.6 -0.658 K1 PI 4.36
100.25408 9.54568 13.51 223980807 6.4 x K1 NP -1.56
100.25767 9.64475 14.70 223981023 1.5 x K4 PII 7.05 -2.41
100.26266 9.62660 19.17 500008211 34.1 M1 NP -1.22
100.26503 9.50806 17.67 400007803 20.4 PII 9.75 -1.12
100.26789 9.41449 15.79 500007335 101.8 -2.34 x M0 PII 7.36 -0.97
100.26905 9.64190 17.88 500007857 108. M3 NP -0.78
100.27071 9.84613 14.36 223981811 36.5 -0.29 -0.816 x K1 PII 3.73 -1.91
100.27124 9.86239 15.39 500007248 1.7 -0.75 -0.570 K5 PI 1.88 -3.06
100.27583 9.60638 13.52 223982136 10.0 x G3 PI 3.01 -2.03
100.27595 9.41769 18.01 500007896 34.7 M5 PI 9.30 -1.58
100.27679 9.47745 17.30 400007686 56.1 x M1.5 NP -1.57
100.27808 9.57943 15.97 500007369 49.4 x G6 NP
100.28734 9.56278 17.53 500007752 51.0 x M3 PI 4.01 -0.88
100.29582 9.59881 17.44 500007727 61.5 -2.037 x K7 NP -0.93
100.30241 9.87533 14.07 500007115 35.3 x G PII 2.01 -1.72
100.30362 9.43746 13.76 500007089 85.6 x K4 NP -1.33
100.31035 9.62065 17.23 500007667 4.1 -0.697 PI 5.41 -2.96
100.32188 9.90899 15.64 223985009 58.3 -2.40 K7 NP
100.32467 9.48364 18.55 500008049 231.4 M2.5 NP -0.68
100.32534 9.64038 18.58 500008061 32.5 M3 PI 0.98 -2.89
100.32613 9.56488 15.02 223985261 28.9 -0.97 x K4 NP -2.39
100.33752 9.56005 15.20 223985987 10.6 x K6 PII 3.31 -1.44
100.34851 9.78788 17.93 500007872 5.2 -0.767 PI 8.20 -2.01
100.35227 9.62653 17.38 400007709 8.9 -0.99 M3 PI 0.76
100.35677 9.57861 16.15 223987178 15.9 -0.61 -1.233 M0 PII 4.96 -1.11
100.36250 9.50365 17.47 400007734 25.8 M1 NP -1.88
100.37968 9.44951 14.19 500007122 25.9 x PII 12.53 -1.44
100.38169 9.80912 14.63 223988742 5.16 -0.08 -0.409 K2 PI 5.03 -2.84
100.38331 10.0068 15.59 223988827 13.1 K5 PI 4.78 -2.69
100.38543 9.63540 14.66 223988965 1.3 -0.67 K6 PI 3.23 -2.83
100.39397 9.60904 17.16 223989567 4.5 -0.83 x M1 NP
100.40536 9.75186 15.44 223990299 35.0 -0.826 x K4 PI 4.51 -0.93
100.41155 9.53661 15.40 500007249 58.6 x K4 NP -1.55
100.41564 9.67443 13.86 223990964 52.5 -1.061 K4 NP -1.46
100.42867 9.41900 16.65 223991832 75.8 x PII 8.40 -1.38
100.47104 9.96747 14.99 223994721 9.5 x K7 NP -1.47
Table 1: continued.
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