J/ApJ/648/1090 Radial velocities of NGC 2264 stars (Furesz+, 2006)
Kinematics of NGC 2264: signs of cluster formation.
Furesz G., Hartmann L.W., Szentgyorgyi A.H., Ridge N.A., Rebull L.,
Stauffer J., Latham D.W., Conroy M.A., Fabricant D.G., Roll J.
<Astrophys. J., 648, 1090-1098 (2006)>
=2006ApJ...648.1090F 2006ApJ...648.1090F
ADC_Keywords: Clusters, open ; Radial velocities
Keywords: ISM: kinematics and dynamics - stars: formation - stars: kinematics -
stars: premain-sequence
Abstract:
We present results from 1078 high-resolution spectra of 990 stars in
the young open cluster NGC 2264, obtained with the Hectochelle
multiobject echelle spectrograph on the 6.5m MMT. We confirm 471
stars as members on the basis of their radial velocity and/or Hα
emission.
Description:
The stellar spectra were obtained with Hectochelle, a fiber-fed,
bench-mounted echelle spectrograph that operates at the
post-conversion MMT. Our first observations in NGC 2264
were taken in 2004 March.
Observations of the CO transition of CO (110.201GHz) were obtained at
the Five College Radio Astronomy Observatory (FCRAO) 14m telescope
located in New Salem, Massachusetts, during 2002 September,
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 93 307 Member stars
table4.dat 85 129 Non-member stars
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See also:
J/AJ/123/1528 : UBV(RI)C and JHK photometry in NGC 2264 (Rebull+, 2002)
J/A+A/417/557 : Rotation + variability of PMS Stars in NGC 2264 (Lamm, 2004)
J/AJ/127/1117 : Halpha emission-line stars in NGC2264 (Reipurth+, 2004)
Byte-by-byte Description of file: table3.dat table4.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- 2MASS Truncated 2MASS identification (1)
16- 20 A5 --- RMS Rebull et al. (2002, J/AJ/123/1528)
identification, Cl* NGC 2264 RMS NNNN
22- 24 I3 --- ESO-HA ? Reipurth et al. (2004, J/AJ/127/1117)
identification, ESO-HA NNN
26- 31 A6 --- LBM Lamm et al. (2004, Cat. J/A+A/417/557)
identification, Cl* NGC 2264 LBM NNNNN
33- 37 F5.2 mag Jmag 2MASS J band magnitude
39- 42 F4.2 mag J-H 2MASS (J-H) color index
44- 48 F5.2 mag H-K 2MASS (H-K) color index
50 A1 --- Ha Hα emission detected flag (2)
52- 59 F8.2 km/s HRV1 ? Heliocentric radial velocity in Dec 2004
61- 66 F6.2 km/s HRV2 ? Heliocentric radial velocity in Mar 2004
68- 74 F7.1 --- R1 ? The R value of cross correlation in Dec 2004
76- 79 F4.1 --- R2 ? The R value of cross correlation in Mar 2004
81- 93 A13 --- Notes Additional notes (3)
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Note (1): Truncated RA and Dec coordinates as HHMMSSs+DDMMSS.
Hectochelle targets in NGC 2264 found to be members based on measured
RV value or detected Hα emission. The criteria of being RV
member is to have at least one velocity measurement within 4σ of
the cluster mean velocity: 8km/s<RV<36km/s. (Stars listed only with R
value of cross correlation larger than 2.)
Note (2): Hα emission detected flag as follows:
c = CTTS (Classical T Tau star)
w = WTTS (Weak T Tau star)
x = V642 Mon
r = reduction error in 2004 Dec data set, categorized as WTTS in
2004Mar data.
Note (3): The flags include membership, accuracy, binarity as follows:
vm = at least one RV measurement suggest membership, but R value is low
hm = just Hα emission suggest membership, none of the RV values
(if there are two).
H = most of the templates gave the same velocity, R value of
cross-correlation is high, accurate RV value
(typical error <1.5km/s for one RV measurement)
RDB = resolved, double lined binary, with RV at 2 epochs (separated
double peak in correlation function)
UDB = unresolved double lined binary, with RV at 2 epochs
(blended/side lobed peak, but clear asymmetry in correlation function)
rdb = same as for RDB, but only 1 RV measurement
udb = same as for UDB, but only 1 RV measurement
sb = likely single lined binary, RV at two epochs and at least one
suggest membership, some also have Hα emission
hsb = member based on Hα emission detected, but
for members (table3) correlation either had just acceptable R
value (barely larger than 2) or radial velocity is close to
the edge of RV distribution;
for non-members (table4) have unusable RV measurement due to
low SNR; only three of these have trustable velocities
with R>2.5 (see text).
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 17-Jul-2008