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J/A+A/447/173 3D-kinematics of white dwarfs from SPY project. II. (Pauli+, 2006)

3D kinematics of white dwarfs from the SPY project. II. Pauli E.-M., Napiwotzki R., Heber U.,M.altmann, Odenkirchen M. <Astron. Astrophys. 447, 173 (2006)> =2006A&A...447..173P
ADC_Keywords: Stars, white dwarf ; Radial velocities ; Space velocities ; Proper motions ; Stars, distances Keywords: stars : white dwarfs - stars: kinematic - Galaxy: halo - Galaxy: kinematics and dynamics - Galaxy: disk Abstract: We present the kinematics of a sample of 398 DA white dwarfs from the SPY project (ESO SN Ia Progenitor surveY) and discuss kinematic criteria for distinguishing of thin-disk, thick-disk, and halo populations. This is the largest homogeneous sample of white dwarfs for which 3D space motions have been determined. Since the percentage of old stars among white dwarfs is higher than among main-sequence stars, they are presumably valuable tools in studies of old populations, such as the halo and the thick disk. Studies of white-dwarf kinematics can help to determine the fraction of the total mass of our Galaxy contained in the form of thick-disk and halo white dwarfs, an issue which is still under discussion. Radial velocities and spectroscopic distances obtained by the SPY project were combined with our measurements of proper motions to derive 3D space motions. Galactic orbits and further kinematic parameters were computed. We calculated individual errors of kinematic parameters by means of a Monte Carlo error propagation code. Our kinematic criteria for assigning population membership were deduced from a sample of F and G stars taken from the literature, for which chemical criteria can be used to distinguish between a thin-disk, a thick-disk and a halo star. Our kinematic population classification scheme is based on the position in the U-V-velocity diagram, the position in the Jz-eccentricity diagram, and the Galactic orbit. We combined this with age information and found seven halo and 23 thick-disk white dwarfs in this brightness limited sample. Another four rather cool white dwarfs probably also belong to the thick disk. Correspondingly 2% of the white dwarfs belong to the halo and 7% to the thick disk. The mass contribution of the thick-disk white dwarfs is found to be substantial, but is insufficient to account for the missing dark matter. Description: Kinematic parameters for 398 white dwarfs from the ESO Supernova-Progenitor Survey (SPY) are presented. Proper motions, spectroscopic distances and high-precision radial velocities (corrected for gravitational redshift) are measured or compiled. From these data galactic velocity components U, V, W as well as the eccentricity and z-component of the angular momentum of the Galactic orbit are computed and tabulated File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table8.dat 61 398 Radial velocities (corrected for gravitational redshift), proper motions, and spectroscopic distances of the 398 SPY white dwarfs table8.tex 177 501 LaTeX version of table8 table9.dat 67 398 Kinematic parameters of the 398 SPY white dwarfs table9.tex 194 498 LaTeX version of table9
See also: J/A+A/400/877 : 3D kinematics of white dwarfs from SPY project (Pauli+, 2003) Byte-by-byte Description of file: table8.dat
Bytes Format Units Label Explanations
1- 12 A12 --- Name Star name 14- 19 F6.1 km/s RV Radial velocity, corrected for gravitational redshift 21- 24 F4.1 km/s e_RV rms uncertainty on RV 25 A1 --- n_RV [*] *: stars with only one spectrum 27- 31 I5 mas/yr pmRA Proper motion, mualpha*cos(delta) 33- 35 I3 mas/yr e_pmRA rms uncertainty on pmRA 37- 40 I4 mas/yr pmDE Proper motion, mudelta 42- 43 I2 mas/yr e_pmDE rms uncertainty on pmDE 45- 49 F5.1 pc Dist Spectroscopic distance 51- 55 F5.2 [pc] logDist Log of the distance 58- 61 F4.2 [pc] e_logDist rms uncertainty on logDist
Byte-by-byte Description of file: table9.dat
Bytes Format Units Label Explanations
1- 12 A12 --- Name Star name 14- 17 F4.2 -- ecc Excentricity of Galactic orbit 19- 22 F4.2 --- e_ecc rms uncertainty on ecc 24- 28 I5 kpc.km/s Jz z component of angular momentum of the Galactic orbit 30- 32 I3 kpc.km/s e_Jz rms uncertainty on Jz 34- 39 F6.1 km/s Uvel U component of Galactic space velocity 41- 44 F4.1 km/s e_Uvel rms uncertainty on Uvel 46- 51 F6.1 km/s Vvel V component of Galactic space velocity 53- 56 F4.1 km/s e_Vvel rms uncertainty on Vvel 58- 62 F5.1 km/s Wvel W component of Galactic space velocity 64- 67 F4.1 km/s e_Wvel rms uncertainty on Wvel
Acknowledgements: Ulrich Heber, heber(at)sternwarte.uni-erlangen.de
(End) U. Heber [Dr. Remeis-Sternwarte, Germany], P. Vannier [CDS] 20-Oct-2005
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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