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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
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:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 93 307 Member stars table4.dat 93 129 Non-member stars
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
Bytes Format Units Label Explanations
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 Halpha 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)
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).
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 17-Jul-2008
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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