J/other/RAA/15.1197 LAMOST DR2 star clusters candidate members (Zhang+, 2015)
Candidate members of star clusters from LAMOST DR2.
Zhang B., Chen X.-Y., Liu C., Chen L., Deng L.-C., Hou J.-L., Shao Z.-Y.,
Yang F., Wu Y., Yang M., Zhang Y., Hou Y.-H., Wang Y.-F.
<Res. Astron. Astrophys., 15, 1197-1208 (2015)>
=2015RAA....15.1197Z 2015RAA....15.1197Z (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Clusters, open ;
Keywords: open clusters and associations: general - stars: statistics -
catalogs - surveys - methods: data analysis
Abstract:
In this work, we provide 2189 photometrically- and
kinematically-selected candidate members of 24 star clusters from the
LAMOST DR2 catalog. We perform two-step membership identification:
selection along the stellar track in the color-magnitude diagram,
i.e., photometric identification, and selection from the distribution
of radial velocities, i.e. the kinematic identification. We find that
the radial velocities from the LAMOST data are very helpful in the
membership identification. The mean probability of membership is 40%
for the sample selected with radial velocity. With these 24 star
clusters, we investigate the performance of the radial velocity and
metallicity estimated with the LAMOST pipeline. We find that the
systematic offsets in radial velocity and metallicity are
0.85±1.26km/s and -0.08±0.04dex, with dispersions of
5.47+1.16-0.71km/s and 0.13+0.04-0.02dex, respectively.
Finally, we propose that the photometrically-selected candidate
members of the clusters covered by the LAMOST footprint should be
assigned higher priority so that more candidate stars can be observed.
Description:
We adopt the Milky Way Star Cluster (MWSC) catalog (Kharchenko et al.
2012, Cat. J/A+A/543/A156; 2013, Cat. J/A+A/558/A53) as the list of
target star clusters since it provides homogeneous parameters of Milky
Way star clusters and is complete in the volume observed by LAMOST.
Thus we use the MWSC radius parameters for star clusters, i.e., r0
in the MWSC is the angular radius of the core of the cluster, and r2
(hereafter rewritten as rc) stands for the angular radius of the
cluster. A star cluster is covered by the LAMOST footprint if the
number of stars located within 2rc of the cluster is larger than
zero. In total, 457 star clusters, including open clusters, globular
clusters, stellar associations and moving groups, are included in
LAMOST DR2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
clusters.dat 42 24 List of studied clusters
tablea2.dat 84 2189 Member stars of 24 clusters and their parameters
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See also:
V/146 : LAMOST DR1 catalogs (Luo+, 2015)
J/A+A/543/A156 : Milky Way star clusters global survey. I. (Kharchenko+, 2012)
J/A+A/558/A53 : Milky Way star clusters global survey. II. (Kharchenko+, 2013)
Byte-by-byte Description of file: clusters.dat
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Bytes Format Units Label Explanations
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1- 2 I2 h RAh Simbad right ascension (J2000)
4- 5 I2 min RAm Simbad right ascension (J2000)
7- 11 F5.2 s RAs Simbad right ascension (J2000)
13 A1 --- DE- Declination sign (J2000)
14- 15 I2 deg DEd Declination (J2000)
17- 18 I2 arcmin DEm Declination (J2000)
20- 23 F4.1 arcsec DEs ? Declination (J2000)
27- 38 A12 --- Cluster Cluster name
40- 42 I3 --- N Number of stars in tablea2.dat
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Cluster Cluster name
14- 23 F10.6 deg RAdeg Right ascension (J2000)
25- 34 F10.6 deg DEdeg Declination (J2000)
36- 42 F7.2 K Teff Effective temperature
44- 49 F6.2 K e_Teff rms uncertainty on Teff
51- 54 F4.2 [cm/s2] logg Surface gravity
56- 59 F4.2 [cm/s2] e_logg rms uncertainty on logg
61- 65 F5.2 [-] [Fe/H] Metallicity
67- 70 F4.2 [-] e_[Fe/H] rms uncertainty on [Fe/H]
72- 78 F7.2 km/s RV Radial velocity
80- 84 F5.2 % Pmemb Membership probability for membership in
terms of RV, pRVc
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 25-Nov-2015