NGC 2264 Kinematics

Kinematic and Spatial Substructure in NGC 2264111Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona; This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile

John J. Tobin1 2 , Lee Hartmann3 , Gabor Fűrész4 , Wen-Hsin Hsu3 , Mario Mateo3
2affiliation: Hubble Fellow, National Radio Astronomy Observatory, Charlottesville, VA 22903
5affiliation: Current Address: Leiden Observatory, Leiden University, P.O. Box 9513, 2300-RA Leiden, The Netherlands; tobin@strw.leidenuniv.nl
3affiliation: Department of Astronomy, University of Michigan, Ann Arbor, MI 48109
4affiliation: Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138
Abstract

We present an expanded kinematic study of the young cluster NGC 2264 based upon optical radial velocities measured using multi-fiber echelle spectroscopy at the 6.5 meter MMT and Magellan telescopes. We report radial velocities for 695 stars, of which approximately 407 stars are confirmed or very likely members. Our results more than double the number of members with radial velocities from Fűrész et al. , resulting in a much better defined kinematic relationship between the stellar population and the associated molecular gas. In particular, we find that there is a significant subset of stars that are systematically blueshifted with respect to the molecular (CO) gas. The detection of Lithium absorption and/or infrared excesses in this blue-shifted population suggests that at least some of these stars are cluster members; we suggest some speculative scenarios to explain their kinematics. Our results also more clearly define the redshifted population of stars in the northern end of the cluster; we suggest that the stellar and gas kinematics of this region are the result of a bubble driven by the wind from O7 star S Mon. Our results emphasize the complexity of the spatial and kinematic structure of NGC 2264, important for eventually building up a comprehensive picture of cluster formation.

stars: formation

1 Introduction

Most stars form in clusters (Carpenter, 2000; Lada & Lada, 2003; Allen et al., 2007; Krumholz et al., 2014), and it is important to understand the processes that lead to the formation of these clusters, in addition to physics of the formation of the individual stars themselves. Star cluster formation theories are generally comprised of two classes: highly dynamic, non-equilibrium models that form within a crossing time (e.g. Bonnell et al., 2003; Bate, 2012) and quasi-equilibrium and/or slow contraction scenarios that require several crossing times to form (e.g., Tan et al., 2006). Studies of both the spatial distribution of stars (e.g., Feigelson et al., 2013) and their kinematics (e.g., Fűrész et al., 2006, 2008; Tobin et al., 2009; Cottaar et al., 2014; Foster et al., 2014) in young clusters that may not be dynamically relaxed and still have substantial mass in molecular gas can help distinguish between these two main possibilities.

The closest region of significant clustered star formation after the Orion Nebula Cluster is NGC 2264 (see Dahm 2008) at a distance of 760 - 900 pc (Sung et al., 1997; Baxter et al., 2009). This cluster is spatially elongated along a distance  pc with significant sub-clusterings. Combining mid-infrared data from the Spitzer Space Telescope with previous optical photometric and H emission surveys, Sung et al. (2009) identified several distinct regions: a large, extended region of low extinction  pc in diameter centered on the O7V B1.5V binary S Mon (Skiff, 2013). The two other sub-clusters are the “Cone” and “Spokes” (Texeira et al. 2006), and they are denser and more highly extincted, each centered around very luminous protostars. Sung et al. (2008) and Feigelson et al. (2013) also highlighted a “halo” population of young stars that were distributed throughout the cluster.

Fűrész et al. (2006) (Paper I) found a strong correlation between the velocities of the molecular gas and the associated stellar population as a function of position, with the optically-visible members of the subclusters showing distinct velocity components. The correlation of spatial substructure with kinematics clearly demonstrates that NGC 2264 is not dynamically relaxed, consistent with the youth of the stellar population (Sung et al., 2008, 2009). In this paper we present new radial velocity observations which, when added to the previous measurements over the past six years, enable a refined study of the spatio-kinematic structure of the cluster. We defer a characterization of the spectroscopic binary population to a subsequent paper. While the overall correlation between stellar and gas motions remains much the same as in Fűrész et al. (2006), we find additional velocity substructure that was not apparent in our initial study. The results contribute to the development of a quantitative picture of the kinematics of NGC 2264 which can ultimately be used as a testing ground for theories of cluster formation.

2 Observations and Data Reduction

2.1 Target Selection

Because of the proximity of NGC 2264 to the Galactic Plane, careful selection of candidate members was necessary to reduce contamination as much as possible. This continuing study uses the same target selection from Fűrész et al. (2006) which drew sources from X-ray (Ramírez et al., 2004), H surveys, and some additional sources showing UV or IR excess from Park et al. (2000). We have added additional targets from Rebull et al. (2002) whose V-band magnitudes fall within the range of magnitudes expected for cluster members. Selection from these catalogs attempts to identify pre-main sequence cluster members in different stages of evolution; stars from the H and Park et al. (2000) optical study will preferentially find Classical T Tauri Stars (CTTSs) or Class II accreting objects while the X-ray sources will find Class III or weak T Tauri Stars (WTTSs) without substantial accretion activity. The additional targets from Rebull et al. (2002) are meant to fill unused fibers, enabling us to identify additional members not selected based on other criteria.

A subset of stars whose membership was questionable because their radial velocities differ significantly from the molecular gas in the region (the “blueshifted population”; section 3 and 4.2) were selected as the main targets for multi-slit observations with the Inamori-Magellan Areal Camera & Spectrograph (IMACS; Bigelow & Dressler 2003) (Section 2.4) to verify membership via detection of Li I absorption.

2.2 Hectochelle

We have observed NGC 2264 with the multi-fiber echelle spectrograph Hectochelle (Szentgyorgyi et al., 1998) on the MMT during several epochs over the past six years. Hectochelle uses robots to position 240 fibers on a 1 field of view (FOV). The fibers subtend 14 on the sky yielding a spectral resolution of 35000. There are limitations of fiber spacing in a given configuration; no targets may be closer than 30. We used an order-separating filter (RV31) to cover the wavelength range of 5150 - 5300Å.

The spectra were reduced with an automated pipeline developed by G. Fűrész that utilizes standard spectral reduction procedures within the Image Reduction and Analysis Facility (IRAF)222IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation.. A more detailed description of Hectochelle data reduction can be found in Sicilia-Aguilar et al. (2006). An additional manual step not taken care of by the pipeline was sky subtraction. A number of fibers (20) must be allocated for sky observations because Hectochelle observations are generally conducted in bright time and the scattered moonlight must be subtracted to measure velocities for faint sources. To subtract the sky observations, we normalized the fiber throughputs using the flat-field exposure, and then subtracted the average spectrum taken from all the sky fibers.

Fűrész et al. (2006) observed NGC 2264 in March 2004 and December 2005; our new observations were conducted in the fall of 2007, 2008, spring 2009, fall 2009, and spring 2010, see Table 1 for details of the observations. When possible two epochs were taken of each field in a particular observing season to identify short period radial velocity variability. Because Hectochelle observations are conducted in queue mode, the second epochs could be days or even a month apart from the first epoch.

2.3 MIKE Fibers

We also used MIKE Fibers (Bernstein et al., 2003; Walker et al., 2007) on the Magellan Clay telescope to observe NGC 2264 in the spectral range 5150 - 5210Å. This instrument uses 256 manually-plugged fibers that fit within a pre-drilled plate on a 25 FOV. Each fiber subtends 125 on the sky, resulting in a resolution 18000 and fibers must be spaced at least 14 apart. MIKE Fibers has two independent spectrograph channels; at 5200Å we are able to use both channels with 128 fibers going to each channel. The two channels are essentially separate spectrographs with different gratings, optics, and CCDs in the same enclosure.

Because MIKE Fibers has a smaller field of view than Hectochelle, we selected two fields with the highest stellar density for these observations: one in the northern part of the cluster near the O7V star S Mon, and another in the southern part centered between the Spokes and Cone “clusters”. As in the case of the Hectochelle observations, data were taken on two epochs several days apart.

The data were reduced using IRAF. We used the task ccdproc, to carry out initial reductions on the raw CCD imaging data: subtracting the overscan, trimming, and subtracting the bias. We combined our individual exposures with ‘imcombine’ set for cosmic ray rejection. The spectra were extracted using ‘twodspec’, by first tracing the apertures in a flat field frame taken of a continuum source to create a map of aperture traces to extract the science spectra. The wavelength solution was calibrated by fitting a 4th order Legendre polynomial to the Thorium-Argon (Th-Ar) lamp spectrum taken before and after the sets of science observations.

2.4 IMACS spectra

Low-resolution spectra for the purpose of determining membership from Li I 6707 Å absorption were obtained with IMACS on the Magellan Baade telescope, during December 20-22 2010 (UT). The setup was the same as used in our study of the L1641 region of the Orion A cloud (Hsu et al., 2012). We used the IMACS f/2 camera in multi-slit spectroscopy mode with the 300 line grism at a blaze angle of 17.5. With a 06 slit, this configuration yields a resolution of 4 Å and spectral coverage from approximately 4000 Å to 9000 Å. The standard observation time for each field is 5 x 10 minutes, but we increased the time to 6 x 10 minutes for a few observations at higher airmasses. A total of 160 stars were observed, selected primarily from the stars that appear slightly blueshifted from the gas (see Section 3 and 4.2).

2.5 Radial velocity measurements

We used rvsao package in IRAF (Mink & Kurtz, 1998), to measure the radial velocities of our observed targets. The radial velocity of an object is determined by cross-correlating the observed spectrum with a template spectrum of known velocity. The cross-correlation signal-to-noise (S/N) or quality is given by , defined as

(1)

where is the peak height of the correlation function and is the rms noise estimated from the antisymmetric portion of the correlation function. The velocity measurement error also depends on the spectral resolution; it is of the form

(2)

where is 20 km s for MIKE Fibers and 14 km s for Hectochelle. These values were determined empirically by adding random noise to a high S/N spectrum as in Hartmann et al. (1986).

We used libraries of synthetic stellar spectra as velocity templates rather than observed velocity standards, enabling us to explore a wider range of stellar parameters than a few observed templates. We used the library by Coelho et al. (2005) for velocity measurement of spectra from both Hectochelle and MIKE Fibers. The Coelho et al. (2005) templates are computed with a resolution of R 100,000, much higher resolution than the observed spectra. However, a cosine-bell filter function is applied to the Fourier transform of the template and observed spectrum within the xcsao task. This effectively reduces the template resolution to that of the Hectochelle or MIKE Fibers instrument. The filter applied to the data from both instruments (and templates) has an inner cutoff at a wave number of 10 and the filter function increases to 1 at a wave number of 40. The purpose of the inner cutoff is to limit the effect of large-scale features in the cross-correlation. The outer cutoff values depend on the instrument and limit on the smallest features considered in the cross-correlation. Tonry & Davis (1979) suggests an outer cutoff of N/(2 FWHM/2.355), yielding 400 for Hectochelle and 80 for MIKE Fibers. However, we found that outer wavenumber cutoff beginning at 120 and reaching zero at 450 worked the best for MIKE Fibers and a cutoff beginning at 600, reaching zero at 1000 worked best for Hectochelle.

We used a subset of the spectral templates with surface gravity log(g) = 3.5, effective temperatures (T) ranging from 3500 - 7000K in steps of 250K, and solar metallicity. There was no need to explore a wider parameter space with the templates because the most important factor determining the quality of a correlation was the T of the template.

The results from the correlation with the highest value are selected, matched to the appropriate target coordinates, and stored in a Starbase database (Roll, 1996). The right ascension and declination are used to correlate the new observations with the existing catalog and the coordinates are used to generate a truncated 2MASS ID number (2MASSID), throwing out fractional seconds in right ascension and declination. Once the targets have been matched in right ascension and declination, the 2MASSID is used to identify sources in further analysis.

To combine radial velocities taken in different epochs, it is necessary to determine zeropoint velocity shifts for an entire observation. This compensates for possibly different calibration schemes, different wavelengths, different instruments, as well as temperature variations within the spectrograph (Sicilia-Aguilar et al., 2006; Fűrész et al., 2006, 2008). We also accounted for the well-characterized fiber-to-fiber velocity offset caused by the calibration lamps not illuminating the fibers in the same way as astronomical objects.

We adopted the results of Fűrész et al. (2006) as baseline velocities to shift our observations to match. This is because the Fűrész et al. (2006) velocities are referenced to the radial velocity standard star W23870 (Latham et al., 1991), having an absolute velocity accuracy of 0.2 km s (Stefanik et al., 1999). We applied a constant shift for each field given by the mean of a Gaussian fit to the distribution of radial velocity differences for each target in a field. The zeropoint shifts for the Hectochelle and MIKE Fibers fields are generally quite small, less than 0.5 km s and are given in Tables 1 and 2. In contrast, observations of the ONC in Tobin et al. (2009) had zeropoint shifts 1 km s. Given than many NGC 2264 fields were conducted in the same semester and even same nights as the Orion fields, the zeropoint shifts may be overestimated in Tobin et al. (2009). We believe that the NGC 2264 fields track the zeropoint shift better than the Orion fields due to the inclusion of many bright non-members in the Galactic Plane that give velocity precisions of 0.5-0.2 km s (note that this is the formal error and does not include systematic effects.)

We have converted the heliocentric radial velocities of each target to the kinematic local standard of rest (LSR) velocities (Kerr & Lynden-Bell, 1986). In order to compare the velocity structure of the stars and gas, the LSR velocities are used exclusively in the plots, but the heliocentric radial velocities are given in Table 3.

The multi-epoch observations have enabled us to also identify a number of candidate spectroscopic binaries from radial velocity variability and/or double-peaked correlation functions. We have removed these from the cluster kinematic analysis because they will broaden the cluster velocity distribution. These candidate spectroscopic binaries will be presented in a subsequent paper along with observations from later epochs.

2.6 Li and spectral types

Spectral types and Li I 6707 Å absorption equivalent widths were determined for a subset of target stars observed with IMACS. We used SPTCLASS, a semi-automatic spectral-typing program (Hernández et al., 2004), which uses empirical relations of spectral type and absorption line equivalent widths for classification (see Hsu et al. (2012) for details). SPTCLASS also automatically measures Li I equivalent widths, but we made manual determinations because of the uncertainty in automatically setting continuum levels at this resolution when strong TiO bands are present.

3 Results

The combined radial velocity measurements from our observations are presented in Table 3. Of the 695 stars with measured non-variable radial velocities, approximately 407 are probable members based on their radial velocities, with more certain identification for those objects with IR excess and/or Li I absorption. This approximately doubles the number of stars with radial velocities (excluding spectroscopic binaries) available in the previous study of (Paper I).

Figure 1 shows an overview of the spatial and kinematic properties of our sample and its correlation with the molecular gas in the region. The left panel shows the positions of all the radial velocity targets overplotted on the corresponding CO intensity map from Ridge et al. (2006) for comparison. In the right panel, we show the position-velocity (PV) distribution of the stars summed over right ascension and plotted as function of declination to correspond roughly to the long axis of the cluster, with the corresponding CO PV plot. Targets that show infrared (IR) excess emission, as defined by - [3.6] 0.4 and [3.6] - [4.5] 0.2, where is from 2MASS and the other colors are IRAC bands 1 and 2, are marked as filled stars; targets with detectable Li absorption but no IR excess are shown as open stars.

The spatial and kinematic correlations between stellar members and molecular gas are evident. The targets with projected spatial positions well off the main molecular gas emission are mostly taken with Hectochelle, chosen to use “left-over” fibers; these are largely non-members, as expected, based on their radial velocities that differ substantially from the cluster mean.

Figure 2 focuses on the same comparisons between stars and gas in more detail by removing stars with LSR velocities - 2 km s and 15 km s. The overall kinematic properties of the stars are similar to that found by Fűrész et al. (2006) (compare the right panel of their Figure 6), but by approximately doubling the number of members with radial velocity measurements several aspects become much clearer. First, the addition of many new members in the region of the Spokes Cluster (Teixeira et al., 2006) at , RA shows a substantial velocity dispersion with an extension to blueshifted velocities, corresponding to a similar feature in the CO emission between 2 km s and 5 km s. Second, the population of redshifted stars in the north corresponding to the molecular gas component at 10 km s is better defined; there appears to be a gap at 9.85, V(lsr) 7 km s in both distributions. Finally, there is a “blueshifted population with velocities -2 km s  V(lsr) 2 km s which does not have corresponding CO emission and was not apparent in Fűrész et al. (2006).

To further examine the velocity distributions relative to the gas, we have plotted histograms of the stellar and gas velocities in Figure 3 in the noted declination bins. We only include a range of RA between 100.05 and 100.4 to focus on the main cluster and limit the contribution of the dispersed population. The histograms show that while there is a strong overlap in velocity space between stars and molecular gas, there is a modest but significant population of blueshifted stars which do not have associated CO emission at their velocity. A substantial fraction of these blueshifted stars show either infrared excess or strong Li I absorption (Figure 2), indicating that they are not substantially older foreground objects. Moreover, contamination by field stars (for which we do not have either Li measurements or observed infrared excess) is unlikely to have a major effect on this distribution; we estimate a contamination of 13 non-members in Figure 3. We determine this number by counting the number of stars with velocities between km s  V(lsr) -5 km s and 20 km s  V(lsr) 50 km s in the same range of right ascension and assuming a uniform distribution in radial velocity.

The other obvious feature of note is the redshifted population of stars at (Figure 2). This group corresponds in velocity space to a corresponding clump of CO emission at 7 km s  V(lsr) 12 km s. There is a gap or minimum in the CO emission at V(lsr) 7 km s, and there is an indication of a similar minimum in the stellar velocity distribution, though it is statistically insignificant (Figure 3). We suggest that this structure is the result of the strong wind of S Mon driving a bubble into the molecular gas, triggering star formation as the gas is compressed.

The histogram of the full sample with in a RA range of 100.05 and 100.4 and a Dec. range of 9.35° to 10.0° is shown in the bottom panel of Figure 3. We fit a Gaussian to this histogram and derive a velocity dispersion of 2.8 km s. We account for the average velocity error of 1.2 km s for the stars used in the calculation by subtracting this error in quadrature from the velocity dispersion and the corrected velocity dispersion is then 2.5 km s.

Figure 4 provides another view of the cluster structure in terms of position-velocity maps, but by stepping across the cluster in 0.1° swaths of RA. The symbols have the same meaning as in Figure 2, but they are now color-coded to emphasize blue- and red-shifted populations. Here we call attention to the small group of stars shown in the bottom left panel (RA = 100.4 to 100.5) centered around V(lsr) 2 km s, and not associated with CO emission. Only one of these stars exhibits infrared excess, suggesting that this might be a slightly older group; on the other hand, many show Li absorption. The population blueshifted stars is apparent in nearly all RA bins across the cluster.

4 Discussion

4.1 Kinematics and gravitational binding

The overall kinematic structure of NGC 2264 bears a striking similarity to that found in the Orion Nebula Cluster (ONC). As shown in Figure 3 of Tobin et al. (2009), the position-velocity plot of both stars and gas shows a northern region redshifted with respect to the central region. The right panel of Figure 2 shows qualitatively similar behavior, although more clearly in the gas than in the stars. One also observes the same asymmetry between the stellar and gas velocities, with a population of stars blueshifted with respect to the molecular gas. The 1-dimensional velocity dispersions of the two clusters are also similar, = 3.1 km s for Orion (Fűrész et al., 2008) and = 2.5 km s for NGC 2264. NGC 2264 does differ from the ONC with its two components in the molecular gas in the north near S Mon (three if the clump west of S Mon is considered), and the gas in the ONC has only one component. The stars in the northern part of the ONC also have a smaller velocity dispersion with respect to the center of the ONC, while in NGC 2264 the stars in the north have a larger spread in velocity than the northern ONC stars.

Proszkow et al. (2009) suggested that the transition from redshifted stars and gas in the northern regions of the ONC to more blueshifted velocities near the cluster center could be the signature of gravitationally-driven infall. The interpretation is qualitatively similar to using “caustics” in position-velocity space to infer gravitational motion in galaxy clusters (e.g., Geller et al., 2013). To see whether a similar interpretation could hold for NGC 2264, we compute a “binding velocity” . Crutcher et al. (1978) estimated a total gas mass of 8000 spanning a total length of 10 pc. Using this mass and setting  pc yields v 3.6 km s.

However, while this scenario was plausible for Orion, it seems less likely to explain the red-shifted population in the north of NGC 2264. This group has V(lsr) 10 km s which is redshifted by about 5 km s with respect to the gas and stellar velocities at the position of the Spokes Cluster. Unless the gas mass (which is the dominant contributor) is underestimated by roughly a factor of four, it seems very likely that this redshifted population is not bound to the rest of the cloud. Rather, we suggest this group is more likely to be the result of blowout by the wind from S Mon; this would also explain the “hole” in the gas at , km s.

With respect to the rest of the cluster, the binding velocity calculated from the molecular gas is larger than the 1-dimensional velocity dispersion ( = 2.5 km s) within a restricted range of RA (bottom right panel of Figure 3). However, if the velocity dispersion is isotropic, the 3-dimensional velocity dispersion would be 4.3 km s and thus suggests that the region is unbound. In addition, if our suggestion that a redshifted population is missing from our optical sample is correct, the 1-d velocity dispersion of the total stellar population is larger than we measure here. Resolution of these question will wait until we have proper motions from Gaia. For now, we conjecture that the true situation is a mix of possibilities, with some fraction of the stars that will eventually be left behind in a bound cluster and some dispersing.

4.2 Blueshifted population

As discussed in the previous section, it appears that a substantial fraction of the blueshifted stars are causally-related to NGC 2264 if not members, based on the indicators of youth - infrared excesses and Li absorption. One possibility for explaining why this population is not at the same velocity as the molecular gas is that it might be older, resulting from a previous episode of star formation. To test this idea, we constructed color-magnitude diagrams for the various kinematic groups. As seen in Figure 5, the color magnitude diagram (CMD) of the “field” stars with velocities -5 km s and 18 km s from the cluster mean shows a much larger dispersion around the median color-magnitude line of the cluster. We observed an excess of faint stars, as would be expected for foreground main sequence stars, and brighter, redder background giants. Moreover, the blue-shifted stars tend to be brighter and bluer in color, while the red-shifted stars are fainter, redder, and have more dispersion in magnitude.

The CMDs of the various probable cluster member velocity groups are essentially indistinguishable except for the redshifted group with 8 km s  km s, which exhibits a broader dispersion. This could be due to contamination because the northern region, where much of the 8 km s  km s population is found, has less extinction to cut out background stars (and is also sparser). The blue-shifted group (-2 km s  km s) appears to have a larger fraction of redder stars than the main cluster as well. However, because these photometric data have not been de-reddened, it is impossible to decouple evolutionary effects or population differences from extinction. Notice that the reddening vector shown in Figure 5 is nearly parallel to the median CMD of the cluster. On the whole, there is a significant spread in at a given color, but much of this is undoubtedly due to an unresolved binary population; other sources of error are probably present but poorly-understood (Jeffries, 2012). In any case, there is little evidence for any systematic age differences larger than about  Myr, comparable to the median estimated age of the cluster (Sung & Bessell, 2010).

Systematic ejection of stars toward Earth seems unlikely if not implausible, especially because the ONC shows the same excess of blueshifted stellar velocities relative to the molecular gas velocities. We next consider other possibilities for the asymmetry between the stellar and gas velocities. The first possibility recognizes that we have an optically-biased sample of radial velocities; stars moving away from us would move more deeply into the molecular cloud and thus have much higher line-of-sight extinctions. It seems very likely that some bias exists; as shown in Figure 3, we observe relatively few stars at the reddest velocities of the molecular gas, which would be surprising if not attributable to sample bias. Whether there exists a substantial population of redshifted stars with velocity shifts of comparable magnitude to the blueshifted population is not clear. If such a population did exist, the overall velocity dispersion would increase to km s, making it even less likely that any part of the region is gravitationally-bound.

An alternative possibility to explain the asymmetry between stars and gas is preferential dispersal of blueshifted (nearside) gas by stellar energy input. We argued above that S Mon is blowing away gas, producing the “hole” in the CO emission at km s, . It seems conceivable that this O7 star could have dispersed additional molecular gas. Schwartz et al. (1985) argued that S Mon is responsible for photoionizing the rim of the Cone Nebula at a projected distance of about 6 pc. Furthermore, they argued that S Mon and the Cone Nebula might actually lie a substantial distance in the foreground from other dense molecular gas in the region (basically, the Spokes Cluster region). Whether or not this picture is correct, it is possible that S Mon photoevaporated and photoionized the gas originally on the near side of the original molecular cloud.

The simulations of photodissociation and ionization of initially molecular gas with magnetic fields and turbulence by Arthur et al. (2011) show substantial evacuation of a region of size 4 pc and initial density in only  yr for an assumed O9 star, which emits a factor of fewer ionizing photons than an O7 star is expected to provide (Osterbrock & Ferland, 2006, Table 2.3). Thus, it is possible that there had been and episode of star formation in the near side of the molecular cloud, prior to the formation of S Mon. Once S Mon formed and began photoionizing the molecular gas associated with the previous generation of star formation, the molecular gas removal caused the previously formed stars to become unbound and expand (e.g., Lada & Lada, 2003). This scenario would produce a population of stars systematically blue-shifted with respect to the cloud velocity, because we are able to observe the blue-shifted stars due to their low extinction, but the red-shifted stars move into the molecular cloud and become too extincted to determine radial velocities in the optical. We therefore suggest that the observed kinematic differences between the stellar population and the molecular gas result from a combination of optical bias against stars moving into the molecular gas and blowout of molecular gas on the near side by S Mon. The low extinction observed toward some members (Walker, 1956; Park et al., 2000) is clear evidence for some gas dispersal to have taken place.

While we cannot determine a systematic age difference between the blue-shifted population and the rest of the cluster, Sung & Bessell (2010) argued that the ‘field’ and ‘halo’ populations of NGC 2264 are older than the rest of the cluster. These regions are designated as such because they they are spread across the NGC 2264 region on the sky and the blue-shifted population of stars is found at all positions in NGC 2264 (see Figure 4). It is noteworthy that Orion also has several know foreground populations as well, projected on the same region of the sky as the ONC (e.g., Bally, 2008; Alves & Bouy, 2012), possibly contributing to the blue-shifted population observed there.

5 Summary

The comparison of the spatial-kinematic properties of stars and molecular gas suggests that NGC 2264 may be better understood as a loose collection of star-forming clumps rather than as a single, distinct, strongly-bound cluster. Future astrometric surveys to determine distances and proper motions are needed to fully develop the true picture of this object.

We wish to thank the anonymous referee for comments which improved the clarity of the manuscript. The authors wish to thank the staff of the MMT and Magellan telescopes and the Hectochelle queue observers of 2007, 2008, 2009, and 2010 for their efforts in obtaining the data used in this paper. We also thank M. Walker and E. Olszewski for assistance with MIKE Fibers data acquisition/reduction and Jesus Hernandez for useful discussions. J. T. and L. H. acknowledge funding from NSF grant AST 08070305. J.J.T. acknowledges support provided by NASA through Hubble Fellowship grant #HST-HF-51300.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. This research has made use of NASA’s Astrophysics Data System. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.

Facilities: Spitzer (IRAC), Magellan:Clay (MIKE), MMT (Hectochelle)

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Figure 1: NGC 2264 radial velocity targets superimposed on the CO integrated intensity map (grayscale) from Ridge et al. (2006) (left panel) and the radial velocity targets are overlaid on a position-velocity plot (right panel) summing over the RA range in the left panel. The lower resolution portion at the edges of the left panel is from J. Bally (unpublished). Star symbols represent members as determined from IRAC infrared excesses (filled stars) or the detection of Li I absorption (open stars); blue circles denote non-excess stars that were not observed for Li absorption, but whose velocities -2 km s  km s suggest possible membership. Gray squares represent stars with LSR velocities and 15 km s that are unlikely to be cluster members. The non-members (gray squares) are roughly distributed uniformly in velocity and declination. From north to south, the cyan stars in the left panel correspond to the position of S Mon, the Spokes Cluster center, and the Cone cluster center.
Figure 2: Radial velocities of known and likely members again superimposed upon the CO integrated intensity map, as in Figure 1 projected spatially (left) and in the declination position-velocity map (right). Symbol shapes are the same as in Figure 1 - filled stars for infrared-excess stars, open stars for Li absorption detections, and filled circles for possible members that do not have infrared-excess (or lack photometry) and/or Li absorption measurements. The red circles are sources without an infrared-excess excess and do not have IMACS observations to detection Li absorption. The green circles are sources without infrared-excess, have IMACS observations. The large open circles highlight two regions that show a clustering of blue-shifted stars. From north to south, the cyan stars in the left panel correspond to the position of S Mon, the Spokes Cluster center, and the Cone cluster center.
Figure 3: RV histograms for stars and gas (thick line) for selected bins in declination. Note the systematic blue shift of the stellar distribution compared to the gas in the southern part of the cluster. The smooth curve in the bottom panel is a Gaussian fit to the stellar RV histogram, yielding a one-dimensional velocity dispersion of = 2.8 km s; after accounting for the average error of 1.2 km s, the velocity dispersion is reduced to 2.5 km s. Note that we only plot stars with RA between 100.4 and 100.05 to focus on the main cluster area and limit contamination.
Figure 4: PV plots for different bins in RA across the cluster. Important to note are the 100.2 to 100.4 bins which show that moving north in the cluster there are three distinct velocity components. The blue points are used for stars with V (lsr) 2 km s, the green points are used for stars with 2 km s V(lsr) 8 km s, and the red points are used for stars with V(lsr) 8 km s.

Figure 5: Optical color magnitude diagrams of our NGC 2264 targets with optical photometry from Rebull et al. (2001); the photometry are not corrected for extinction. The top left panel is the CMD of stars with radial velocity that is consistent with cluster membership, -5.0 km s  V(lsr) 18.0 km s. The top right panel shows stars within the group that is blue-shifted of the gas velocity -2.0 km s  V(lsr) 2.0 km s. The middle left panel shows stars with the main cluster velocity, 2.0 km s  V(lsr) 8.0 km s. The middle right panel shows stars that a redshifted of the main cluster 8.0 km s  V(lsr) 15.0 km s. The bottom panel shows stars that are anti-correlated with the cluster velocity; the blue or red boxes denote whether the stars is significantly blue or red-shifted away from the cluster velocity. The solid line in both panels is the median V-I color for stars with velocities consistent with NGC 2264. The CMDs of the three groups within the cluster velocity are all consistent with each other, showing that they are at similar distances and ages. The stars outside the main cluster velocities show a significantly different CMD that is comprised of both foreground and background sources.
Field ID Date Julian Date RA Dec. Airmass Exposure Time Binning Filter Zeropoint ShiftaaShift applied is relative to the velocities in Fűrész et al. (2006). Number of Targets Seeing
UT Date (2400000) (J2000) (J2000) # seconds km s arcsec
F1-E1-2007 10-12-2007 54385.42 06:40:57.74 09:40:26.20 1.33 3x1200 2x2 RV31 -0.18 0.02 147 1.07
F1-E2-2007 10-26-2007 54399.42 06:40:57.74 09:40:26.20 1.19 3x1200 2x2 RV31 +0.23 0.02 147 0.64
F2-E1-2007 10-12-2007 54385.48 06:40:39.15 09:45:23.48 1.12 3x1200 2x2 RV31 -0.08 0.04 147 0.61
F2-E2-2007 10-28-2007 54401.40 06:40:39.15 09:45:23.48 1.25 3x1200 2x2 RV31 +0.23 0.03 147 1.4
F3-E1-2007 10-29-2007 54402.44 06:41:06.09 09:42:34.69 1.12 3x1200 2x2 RV31 -0.02 0.02 144 1.97
F3-E2-2007 11-25-2007 54429.40 06:41:06.09 09:42:34.69 1.08 3x1200 2x2 RV31 -0.18 0.08 144 2.32
F4-E1-2007 10-29-2007 54402.49 06:40:51.25 09:33:13.59 1.08 1x1200 2x2 RV31 +0.14 0.04 143 1.97
F1-E1-2008 10-22-2008 54761.49 06:40:46.44 09:37:36.39 1.08 3x1200 2x2 RV31 -0.30 0.02 138 1.38
F1-E2-2008 10-26-2008 54765.42 06:40:46.44 09:37:36.39 1.19 3x1200 2x2 RV31 -0.30 0.03 138 0.82
F2-E1-2008 10-24-2008 54763.46 06:40:53.44 09:47:21.13 1.10 3x1200 2x2 RV31 -0.10 0.04 147 0.64
F2-E2-2008 10-25-2008 54764.44 06:40:53.44 09:47:21.13 1.14 3x1200 2x2 RV31 -0.13 0.04 147 1.02
F3-E1-2008 10-25-2008 54764.48 06:41:02.64 09:42:42.26 1.08 3x1200 2x2 RV31 -0.42 0.03 152 1.02
F4-E1-2008 10-23-2008 54762.45 06:40:46.12 09:32:39.73 1.12 3x1200 2x2 RV31 -0.51 0.05 148 0.95
F1-E1-S2009 03-13-2009 54903.19 06:40:56.18 09:41:16.03 1.20 2x1200 2x2 RV31 -0.37 0.02 191 1.91
F2-E1-S2009 03-14-2009 54904.19 06:40:46.08 09:32:41.51 1.21 4x1200 2x2 RV31 -0.44 0.04 187 1.69
F3-E1-S2009 04-10-2009 54931.14 06:40:39.83 09:45:12.39 1.36 2x1200 2x2 RV31 +0.07 0.03 193 0.67
F3-E2-S2009 04-13-2009 54934.15 06:40:39.83 09:45:12.39 1.49 3x1200 2x2 RV31 +0.24 0.02 193 1.90
F1-E1-F2009 10-25-2009 55129.43 06:40:39.86 09:43:59.35 1.17 3x1200 2x2 RV31 -0.18 0.02 216 1.08
F1-E2-F2009 10-26-2009 55130.46 06:40:39.86 09:43:59.35 1.09 3x1200 2x2 RV31 +0.23 0.02 216 1.93
F2-E1-F2009 10-25-2009 55129.48 06:40:48.66 09:35:52.50 1.08 3x1200 2x2 RV31 -0.08 0.04 220 1.08
F2-E2-F2009 10-31-2009 55135.37 06:40:48.66 09:35:52.50 1.33 3x1200 2x2 RV31 +0.23 0.03 220 0.88
F3-E1-F2009 10-31-2009 55135.42 06:40:54.85 09:41:10.59 1.13 3x1200 2x2 RV31 -0.02 0.02 218 0.88
F3-E2-F2009 11-02-2009 55137.34 06:40:54.85 09:41:10.59 1.50 3x1200 2x2 RV31 -0.18 0.08 218 0.97
F4-E1-F2009 10-31-2009 55135.48 06:40:41.37 09:46:36.31 1.08 3x1200 2x2 RV31 +0.14 0.04 192 0.88
F4-E2-F2009 11-27-2009 55162.33 06:40:41.37 09:46:36.31 1.19 3x1200 2x2 RV31 +0.14 0.04 208 0.79
F5-E1-F2009 11-02-2009 55137.40 06:40:50.32 09:35:29.87 1.20 3x1200 2x2 RV31 -0.02 0.02 218 0.97
F5-E2-F2009 11-27-2009 55162.38 06:40:50.32 09:35:29.87 1.09 3x1200 2x2 RV31 -0.18 0.08 218 0.79
F1-E1-S2010 01-31-2010 55227.28 06:40:42.70 09:44:11.34 1.14 3x1200 2x2 RV31 -0.07 0.08 193 1.09
F1-E2-S2010 02-02-2010 55229.10 06:40:42.70 09:44:11.34 1.44 3x1200 2x2 RV31 0.03 0.1 193 1.53
F2-E1-S2010 02-06-2010 55233.31 06:40:45.82 09:34:58.50 1.32 3x1200 2x2 RV31 0.01 0.1 213 1.48
F2-E2-S2010 03-03-2010 55258.25 06:40:45.82 09:34:58.50 1.34 3x1200 2x2 RV31 0.19 0.07 213 0.60
F3-E1-S2010 03-05-2010 55260.19 06:41:06.61 09:37:16.59 1.15 3x1200 2x2 RV31 0.20 0.03 215 1.93
F3-E2-S2010 03-06-2010 55262.28 06:41:06.61 09:37:16.59 1.82 3x1200 2x2 RV31 0.12 0.04 212 1.33
F4-E1-S2010 03-31-2010 55262.28 06:40:41.37 09:46:48.31 1.13 3x1200 2x2 RV31 0.05 0.04 209 1.52
F4-E2-S2010 04-03-2010 55262.28 06:40:41.37 09:46:48.31 1.15 4x1200 2x2 RV31 -0.1 0.04 209 1.63
Table 1: Hectochelle Observations
Field ID Start Date Julian Date RA Dec. Airmass Exposure Time Binning Filter Zeropoint Shift Number of Targets
UT Date (2400000) (J2000) (J2000) # seconds km s
A-1 12-10-2009 55175.81 06:41:00.98 09:32:44.4 1.4 3x1200 2x2 Mg 0.05 0.1 220
B-1 12-11-2009 55179.81 06:40:48.90 09:51:44.4 1.4 3x1200 2x2 Mg -0.13 0.05 215
A-2 12-14-2009 55176.80 06:41:00.98 09:32:44.4 1.4 3x1200 2x2 Mg 0.31 0.05 220
B-2 12-15-2009 55180.83 06:40:48.90 09:51:44.4 1.5 3x900 2x2 Mg 0.08 0.0.04 215

Note. –

Table 2: MIKE Fibers Observations
2massID RA Dec. aaShift applied is relative to the velocities in Fűrész et al. (2006). N EpochsbbNumber of observations with R 6.0. Lithium EW Spectral Type K - [3.6] [3.6] - [4.5]
(J2000) (J2000) (km s) (Å)
0639037+094023 06:39: 3.75 09:40:23.4 5.32 0.13 4 -99.00 -99.0 -99.00 -99.00
0639152+093937 06:39:15.25 09:39:37.8 29.88 0.24 7 -99.00 -99.0 -99.00 -99.00
0639153+095303 06:39:15.37 09:53:03.6 102.33 0.95 3 -99.00 -99.0 -99.00 -99.00
0639155+092444 06:39:15.55 09:24:44.8 10.94 0.07 2 -99.00 -99.0 -99.00 -99.00
0639156+093912 06:39:15.63 09:39:13.0 1.43 0.42 9 -99.00 -99.0 -99.00 -99.00
0639157+092929 06:39:15.70 09:29:29.4 18.65 0.02 3 -99.00 -99.0 -99.00 -99.00
0639163+091953 06:39:16.37 09:19:53.3 50.59 0.05 3 -99.00 -99.0 -99.00 -99.00
0639164+093116 06:39:16.45 09:31:16.1 1.63 0.11 2 -99.00 -99.0 -99.00 -99.00
0639166+100055 06:39:16.62 10:00:55.3 -15.80 0.06 2 -99.00 -99.0 -99.00 -99.00
0639168+091741 06:39:16.85 09:17:41.0 41.96 0.12 2 -99.00 -99.0 -99.00 -99.00
0639172+093052 06:39:17.25 09:30:52.9 2.87 0.17 2 -99.00 -99.0 -99.00 -99.00
0639174+092137 06:39:17.43 09:21:37.8 23.83 0.27 5 -99.00 -99.0 -99.00 -99.00
0639174+092537 06:39:17.43 09:25:37.9 15.92 0.16 2 -99.00 -99.0 -99.00 -99.00
0639175+095314 06:39:17.50 09:53:14.8 1.47 0.42 2 -99.00 -99.0 -99.00 -99.00
0639176+093326 06:39:17.68 09:33:26.4 67.09 0.20 2 -99.00 -99.0 -99.00 -99.00
0639179+091822 06:39:17.97 09:18:22.6 39.78 0.01 2 -99.00 -99.0 -99.00 -99.00
0639180+092957 06:39:18.06 09:29:57.5 80.57 0.28 2 -99.00 -99.0 -99.00 -99.00
0639180+094115 06:39:18.02 09:41:15.4 46.02 0.31 2 -99.00 -99.0 -99.00 -99.00
0639185+094250 06:39:18.54 09:42:50.4 48.01 0.30 2 -99.00 -99.0 -99.00 -99.00
0639186+094752 06:39:18.67 09:47:52.3 128.27 4.50 2 -99.00 -99.0 -99.00 -99.00
0639189+093105 06:39:18.98 09:31:05.5 21.90 0.09 2 -99.00 -99.0 -99.00 -99.00
0639189+094222 06:39:18.97 09:42:22.9 26.30 0.20 2 -99.00 -99.0 -99.00 -99.00
0639190+092100 06:39:19.09 09:21:00.0 31.14 0.17 2 -99.00 -99.0 -99.00 -99.00
0639191+092743 06:39:19.19 09:27:43.6 50.19 0.37 2 -99.00 -99.0 -99.00 -99.00
0639192+095135 06:39:19.21 09:51:35.6 20.82 0.01 2 -99.00 -99.0 -99.00 -99.00
0639196+092856 06:39:19.60 09:28:56.0 53.08 0.05 2 -99.00 -99.0 -99.00 -99.00
0639196+093111 06:39:19.60 09:31:11.8 1.17 0.39 2 -99.00 -99.0 -99.00 -99.00
0639197+092650 06:39:19.70 09:26:50.2 34.87 0.01 2 -99.00 -99.0 -99.00 -99.00
0639201+095014 06:39:20.15 09:50:14.5 79.71 0.01 2 -99.00 -99.0 -99.00 -99.00
0639201+095034 06:39:20.13 09:50:34.9 65.94 0.72 2 -99.00 -99.0 -99.00 -99.00
0639206+095856 06:39:20.66 09:58:56.4 -1.20 0.39 2 -99.00 -99.0 -99.00 -99.00
0639211+093627 06:39:21.11 09:36:27.9 0.09 0.34 2 -99.00 -99.0 -99.00 -99.00
0639214+095949 06:39:21.42 09:59:49.4 -14.85 0.06 2 -99.00 -99.0 -99.00 -99.00
0639216+094507 06:39:21.62 09:45:07.6 22.26 2.10 2 -99.00 -99.0 -99.00 -99.00
0639217+095423 06:39:21.71 09:54:23.2 51.59 0.14 2 -99.00 -99.0 -99.00 -99.00
0639218+095559 06:39:21.88 09:55:59.3 20.01 0.05 2 -99.00 -99.0 -99.00 -99.00
0639220+093523 06:39:22.02 09:35:23.7 77.90 0.14 2 -99.00 -99.0 -99.00 -99.00
0639223+094321 06:39:22.33 09:43:21.6 53.24 0.48 2 -99.00 -99.0 -99.00 -99.00
0639224+094510 06:39:22.44 09:45:10.6 23.42 0.95 2 -99.00 -99.0 -99.00 -99.00
0639226+093038 06:39:22.60 09:30:38.0 43.78 0.46 3 -99.00 -99.0 -99.00 -99.00
0639226+095430 06:39:22.69 09:54:30.7 4.30 0.88 7 -99.00 -99.0 -99.00 -99.00
0639229+093523 06:39:22.93 09:35:23.4 -27.28 0.19 6 -99.00 -99.0 -99.00 -99.00
0639229+093616 06:39:22.94 09:36:16.9 -0.68 0.09 7 -99.00 -99.0 -99.00 -99.00
0639232+094008 06:39:23.26 09:40:08.7 5.61 0.04 2 -99.00 -99.0 -99.00 -99.00
0639232+094703 06:39:23.20 09:47:03.6 29.55 0.08 2 -99.00 -99.0 -99.00 -99.00
0639235+092055 06:39:23.56 09:20:55.0 60.13 0.75 2 -99.00 -99.0 -99.00 -99.00
0639239+094201 06:39:23.97 09:42:01.7 66.55 0.18 5 -99.00 -99.0 -99.00 -99.00
0639240+092550 06:39:24.01 09:25:50.8 28.97 0.20 4 -99.00 -99.0 -99.00 -99.00
0639240+095231 06:39:24.05 09:52:31.4 98.19 0.65 2 -99.00 -99.0 -99.00 -99.00
0639241+091805 06:39:24.15 09:18:05.8 -34.26 0.16 4 -99.00 -99.0 -99.00 -99.00
0639243+095619 06:39:24.32 09:56:19.3 -29.75 0.32 6 -99.00 -99.0 -99.00 -99.00
0639244+094903 06:39:24.42 09:49:03.7 31.90 1.06 2 -99.00 -99.0 -99.00 -99.00
0639245+095040 06:39:24.55 09:50:40.2 70.09 0.11 5 -99.00 -99.0 -99.00 -99.00
0639246+091721 06:39:24.68 09:17:21.6 54.04 0.31 3 -99.00 -99.0 -99.00 -99.00
0639246+092233 06:39:24.65 09:22:33.2 3.18 0.10 7 -99.00 -99.0 -99.00 -99.00
0639249+092207 06:39:24.97 09:22:07.5 1.73 1.10 2 -99.00 -99.0 -99.00 -99.00
0639253+092535 06:39:25.35 09:25:35.7 20.35 0.03 2 -99.00 -99.0 -99.00 -99.00
0639253+094314 06:39:25.36 09:43:14.7 -22.56 0.01 2 -99.00 -99.0 -99.00 -99.00
0639256+094253 06:39:25.64 09:42:53.6 2.50 0.19 2 -99.00 -99.0 -99.00 -99.00
0639258+093812 06:39:25.81 09:38:12.4 1.76 0.35 2 -99.00 -99.0 -99.00 -99.00
0639262+094110 06:39:26.26 09:41:10.8 0.72 0.23 10 -99.00 -99.0 -99.00 -99.00
0639264+094329 06:39:26.49 09:43:29.8 -1.19 0.77 2 -99.00 -99.0 -99.00 -99.00
0639266+093037 06:39:26.65 09:30:37.9 12.79 0.03 2 -99.00 -99.0 -99.00 -99.00
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0641490+094106 06:41:49.02 09:41:06.1 1.56 0.31 8 -99.00 -99.0 0.12 0.01
0641504+093927 06:41:50.41 09:39:27.1 20.20 0.28 2 -99.00 -99.0 0.19 -0.07
0641504+094601 06:41:50.46 09:46:01.7 35.68 0.24 5 -99.00 -99.0 0.23 -0.10
0641508+094725 06:41:50.87 09:47:25.8 -10.26 0.21 4 -99.00 -99.0 0.23 -0.12
0641510+094200 06:41:51.04 09:42:00.4 1.64 3.44 2 0.00 72.1 -99.00 0.16
0641514+094409 06:41:51.48 09:44:09.7 0.99 0.89 7 -99.00 -99.0 0.25 0.03
0641514+095342 06:41:51.46 09:53:42.6 4.57 0.43 9 -99.00 -99.0 0.04 0.01
0641518+093256 06:41:51.84 09:32:56.6 76.39 0.10 2 -99.00 -99.0 -99.00 -0.01
0641521+094622 06:41:52.19 09:46:22.1 -7.16 0.10 2 -99.00 -99.0 0.18 0.04
0641530+094915 06:41:53.06 09:49:15.9 25.69 0.25 2 -99.00 -99.0 0.18 0.10
0641530+100002 06:41:53.06 10:00:02.3 -15.72 0.53 3 -99.00 -99.0 0.27 0.11
0641531+095047 06:41:53.16 09:50:47.4 5.54 0.17 5 -99.00 -99.0 0.36 0.25
0641536+094203 06:41:53.69 09:42:03.3 -10.51 0.09 5 -99.00 -99.0 0.03 -0.09
0641536+094615 06:41:53.61 09:46:15.0 2.48 0.56 2 -99.00 -99.0 0.24 -0.04
0641544+092915 06:41:54.48 09:29:16.0 1.10 0.10 5 -99.00 -99.0 0.15 -0.01
0641546+094127 06:41:54.69 09:41:27.2 -0.71 0.03 2 -99.00 -99.0 0.16 -0.05
0641548+092528 06:41:54.84 09:25:28.9 30.17 0.22 4 -99.00 -99.0 0.26 -0.09
0641549+094252 06:41:54.93 09:42:52.7 -0.94 2.16 4 0.40 70.0 0.11 0.10
0641557+093958 06:41:55.79 09:39:58.0 0.33 0.55 2 0.24 69.7 0.10 0.03
0641563+095005 06:41:56.36 09:50:05.9 0.89 0.07 6 -99.00 -99.0 0.01 -0.04
0641567+093407 06:41:56.72 09:34:07.8 13.43 0.46 2 -99.00 -99.0 0.14 -0.05
0641571+095741 06:41:57.15 09:57:41.5 27.92 0.07 4 -99.00 -99.0 0.24 -0.11
0641580+094306 06:41:58.04 09:43:06.2 6.56 0.66 8 0.57 66.6 0.12 0.01
0641580+095054 06:41:58.03 09:50:54.2 40.04 0.16 2 -99.00 -99.0 -99.00 -0.09
0641585+093936 06:41:58.56 09:39:36.8 -4.22 0.66 2 0.00 65.4 -99.00 0.03
0641590+092621 06:41:59.01 09:26:21.4 32.16 0.08 5 -99.00 -99.0 0.11 0.03
0642011+100026 06:42: 1.11 10:00:26.2 87.48 0.03 3 -99.00 -99.0 0.11 20.15
0642025+093652 06:42: 2.56 09:36:52.5 2.39 0.51 9 0.93 66.3 -0.13 0.06
0642026+095827 06:42: 2.68 09:58:27.9 9.56 0.22 5 -99.00 -99.0 0.10 21.55
0642029+092729 06:42: 2.98 09:27:29.2 22.14 0.47 5 -99.00 -99.0 0.20 -0.04
0642030+093413 06:42: 3.03 09:34:13.9 21.58 0.14 2 -99.00 -99.0 0.16 19.84
0642033+093713 06:42: 3.37 09:37:13.0 -9.39 1.00 2 -99.00 -99.0 -99.00 -99.00
0642037+094122 06:42: 3.71 09:41:22.1 38.29 0.20 2 -99.00 -99.0 0.26 -0.06
0642037+094959 06:42: 3.79 09:49:59.2 23.82 1.03 2 -99.00 -99.0 0.15 0.05
0642042+093728 06:42: 4.20 09:37:28.6 45.05 2.24 2 -99.00 -99.0 -99.00 -99.00
0642044+094238 06:42: 4.49 09:42:38.2 40.80 0.11 2 -99.00 -99.0 0.09 -0.15
0642056+094436 06:42: 5.60 09:44:36.5 -88.87 0.35 4 -99.00 -99.0 21.87 -21.53
0642071+095344 06:42: 7.16 09:53:44.5 9.72 0.33 4 -99.00 -99.0 0.13 -0.03
0642071+100013 06:42: 7.12 10:00:13.9 59.79 0.14 4 -99.00 -99.0 0.23 20.46
0642073+094947 06:42: 7.36 09:49:47.1 15.93 0.27 4 -99.00 -99.0 0.27 -0.12
0642078+094652 06:42: 7.86 09:46:52.4 -21.21 0.13 5 -99.00 -99.0 -99.00 -99.00
0642084+093321 06:42: 8.43 09:33:21.8 22.28 0.23 2 -99.00 -99.0 -99.00 -99.00
0642087+094121 06:42: 8.70 09:41:21.2 2.34 0.66 9 -99.00 -99.0 -99.00 -99.00
0642089+094208 06:42: 8.93 09:42:08.6 3.92 0.55 2 -99.00 -99.0 -99.00 -99.00
0642091+094804 06:42: 9.15 09:48:04.9 11.55 0.19 10 -99.00 -99.0 -99.00 -99.00
0642091+095902 06:42: 9.11 09:59:02.8 14.53 0.21 9 -99.00 -99.0 0.19 19.48
0642091+095945 06:42: 9.12 09:59:45.5 45.84 0.20 3 -99.00 -99.0 0.14 21.22
0642092+094403 06:42: 9.24 09:44:03.4 2.45 0.44 9 -99.00 -99.0 -99.00 -99.00
0642094+093205 06:42: 9.48 09:32:05.5 -95.64 0.14 5 -99.00 -99.0 -99.00 -99.00
0642098+094522 06:42: 9.89 09:45:22.1 44.22 0.22 5 -99.00 -99.0 -99.00 -99.00
0642101+094024 06:42:10.10 09:40:25.0 -18.38 0.22 4 -99.00 -99.0 -99.00 -99.00
0642102+093604 06:42:10.22 09:36:04.5 30.65 0.10 5 -99.00 -99.0 -99.00 -99.00
0642103+095914 06:42:10.33 09:59:14.6 55.69 0.14 2 -99.00 -99.0 0.22 21.14
0642107+095559 06:42:10.77 09:55:59.6 68.44 1.89 2 -99.00 -99.0 -99.00 -99.00
0642113+092903 06:42:11.37 09:29:03.3 -15.71 0.21 5 -99.00 -99.0 -99.00 -99.00
0642113+092904 06:42:11.35 09:29:04.4 -16.94 1.34 2 -99.00 -99.0 -99.00 -99.00
0642113+094345 06:42:11.38 09:43:45.6 -0.21 1.84 2 -99.00 -99.0 -99.00 -99.00
0642114+093423 06:42:11.43 09:34:23.9 23.54 0.05 2 -99.00 -99.0 -99.00 -99.00
0642125+095907 06:42:12.57 09:59:07.1 8.96 1.02 6 -99.00 -99.0 -99.00 -99.00
0642126+093131 06:42:12.67 09:31:31.6 59.96 0.32 5 -99.00 -99.0 -99.00 -99.00
0642127+093009 06:42:12.74 09:30:09.1 66.97 0.20 7 -99.00 -99.0 -99.00 -99.00
0642131+094603 06:42:13.13 09:46:03.5 14.35 0.27 9 -99.00 -99.0 -99.00 -99.00
0642139+095012 06:42:13.95 09:50:12.6 -15.45 0.08 2 -99.00 -99.0 -99.00 -99.00
0642141+094308 06:42:14.15 09:43:08.9 -34.91 0.10 5 -99.00 -99.0 -99.00 -99.00
0642154+092637 06:42:15.46 09:26:37.2 6.52 0.36 2 -99.00 -99.0 -99.00 -99.00
0642157+094033 06:42:15.77 09:40:33.1 -64.86 0.15 5 -99.00 -99.0 -99.00 -99.00
0642166+093400 06:42:16.67 09:34:00.4 -7.14 0.05 2 -99.00 -99.0 -99.00 -99.00
0642167+093652 06:42:16.75 09:36:52.9 16.26 1.74 2 -99.00 -99.0 -99.00 -99.00
0642169+093351 06:42:16.99 09:33:51.3 76.17 0.28 4 -99.00 -99.0 -99.00 -99.00
0642169+094725 06:42:16.91 09:47:25.2 13.54 0.12 3 -99.00 -99.0 -99.00 -99.00
0642177+094052 06:42:17.79 09:40:52.0 78.21 0.21 2 -99.00 -99.0 -99.00 -99.00
0642198+093102 06:42:19.88 09:31:02.0 -7.19 0.12 2 -99.00 -99.0 -99.00 -99.00
0642200+093850 06:42:20.07 09:38:50.2 82.75 0.08 5 -99.00 -99.0 -99.00 -99.00
0642202+093704 06:42:20.27 09:37:04.5 7.76 1.43 6 -99.00 -99.0 -99.00 -99.00
0642227+094612 06:42:22.77 09:46:12.4 21.89 0.48 2 -99.00 -99.0 -99.00 -99.00
0642245+093126 06:42:24.52 09:31:26.2 8.97 0.47 2 -99.00 -99.0 -99.00 -99.00
0642256+094115 06:42:25.69 09:41:15.6 19.51 0.20 2 -99.00 -99.0 -99.00 -99.00
0642257+094151 06:42:25.77 09:41:51.5 36.88 0.07 2 -99.00 -99.0 -99.00 -99.00
0642265+094030 06:42:26.57 09:40:30.4 43.92 0.11 2 -99.00 -99.0 -99.00 -99.00
0642266+093750 06:42:26.69 09:37:50.4 46.67 0.09 2 -99.00 -99.0 -99.00 -99.00
0642272+093940 06:42:27.20 09:39:40.6 -25.20 0.24 2 -99.00 -99.0 -99.00 -99.00

Note. – Abridged table of target IDs, positions, average radial velocities, Lithium 6707 Å Equivalent Widths, Spectral Types, and near infrared colors. Entries with -99 signify that these data are unavailable for a given target. aafootnotetext: Velocities from Fűrész et al. (2006) are included in average. For a measurement to be included in the average R must be 6.0; R is defined in Equation 1.

Table 3: Velocity Summary
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