Access to Astronomical Catalogues

← Click to display the menu
J/A+A/496/191     Spectral analysis of 636 SDSS WD-M binaries    (Heller+, 2009)

Spectral analysis of 636 white dwarf - M star binaries from the Sloan Digital Sky Survey. Heller R., Homeier D., Dreizler S., Oestensen R. <Astron. Astrophys. 496, 191 (2009)> =2009A&A...496..191H
ADC_Keywords: Binaries, spectroscopic ; Stars, white dwarf ; Stars, M-type Keywords: binaries: spectroscopic - white dwarfs - stars: late-type - stars: fundamental parameters - methods: data analysis - binaries: visual Abstract: We present a catalog of 857 WD-M star binaries from the Sloan Digital Sky Survey (SDSS), most of which were previously identified by other authors, and the results of our spectral analysis for a subsample of 636 WD-M composite spectra. Our automatic fitting procedure bases on a chi2 minimization technique, yielding a decomposition of each combined spectrum and a derivation of independent parameter estimates for both components. On the respective photometric data from the SDSS, we also find 41 optically resolved binaries. We also investigated the spectra for hydrogen and helium emission. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 68 41 Orbital and physical parameters of optically resolved binaries table2.dat 127 636 Physical parameters for spectral fits on 636 WD-M binaries table3.dat 186 857 Coordinates and references to the whole catalog of 857 objects
See also: J/ApJ/607/426 : Catalog of white dwarfs in SDSS-DR1 (Kleinman+, 2004) J/AJ/131/1674 : Close binary systems from SDSS DR4 (Silvestri+, 2006) J/ApJS/167/40 : SDSS4 confirmed white dwarfs catalog (Eisenstein+, 2006) J/MNRAS/382/1377 : SDSS WD main-sequence binaries (Rebassa-Mansergas+, 2007) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 10 A10 --- SDSSs Short SDSS name (JHHMM+DDMM) 11 A1 --- n_SDSSs [+] very-low-mass-object candidate (G1) 13- 15 F3.1 arcsec dproj Projected separation of WD and M 17- 20 I4 pc dmean Mean distance of WD and M 22- 25 I4 AU d Projected orbital separation 27- 30 I4 AU dcorr Statistically corrected separation d 32- 35 F4.2 solMass MM Mass of the M component from spectral fit 37- 41 I5 yr P Lower limit for orbital period 43- 48 I6 yr Pcorr Statistically corrected P 50- 68 A19 --- SDSS SDSS long name (JHHMMSS.ss+DDMMSS.s)
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 2 A2 --- n_SDSSs [p +*] Note on the binary (G1) 3- 12 A10 --- SDSSs Short SDSS name (JHHMM+DDMM) 13 A1 --- m_SDSSs [AC] Multiplicity index on SDSSs 15 A1 --- u_dWD [?] fit to a fixed Teff=40kK (2) 16 A1 --- l_dWD Limit flag on dWD 17- 22 F6.1 pc dWD Distance of the WD to Earth 25 A1 --- l_dM Limit flag on dM 26- 31 F6.1 pc dM ?=- Distance of the M dwarf to Earth 33 A1 --- u_C [?] fit to a fixed Teff=40kK (2) 34 A1 --- l_C Limit flag on C 35- 40 F6.3 --- C ?=- Distance evaluation coefficient (3) 42 A1 --- u_TeffWD [?] fit to a fixed Teff=40kK (2) 43 A1 --- l_TeffWD Limit flag on TeffWD 44- 50 F7.1 K TeffWD Effective temperature of the WD 52- 57 F6.1 K TeffM Effective temperature of the M dwarf 59- 63 F5.3 solRad radWD Radius of the WD 65 A1 --- l_radM Limit flag on radM 66- 70 F5.3 solRad radM Radius of the M dwarf 72- 74 F3.1 [cm/s2] loggWD Surface gravity of the WD 76- 78 F3.1 [cm/s2] loggM Surface gravity of the M dwarf 80- 82 F3.1 solMass MWD Mass of the WD 84 A1 --- l_MWD Limit flag on MWD 85- 88 F4.2 solMass MM Mass of the M dwarf 90- 93 F4.1 [-] [Fe/H] Metallicity of the M dwarf 95-106 A12 --- Emiss Emission features (4) 108-109 A2 --- WD WD type, DA or DO (5) 111 A1 --- Res [oO*?] Optically resolved (6) 113-116 I4 --- m Nb of data points used from spectrum 118-121 I4 --- DOF Nb of degrees of freedom from the fit 123-127 F5.2 --- Chi2 Chi2 of the fit
Note (3): As defined in Eq. (16) in the paper: C = sqrt(2)[(dWD-dM)/(dWD+dM)] Note (2): For most of the helium-rich white dwarfs (DO) that we fitted to have an effective temperature of 40000K. Since this temperature is the lowest of our grid of DO template spectra, it could also be that the real Teff of that object is smaller than 40kK. Since the WD distances are derived from the stars' temperatures, we can also only give an upper limit for dWD for those (?<40000K) objects because lower temperature would mean that they would have to closer to Earth. Note (4): Emission features code as follows: H = Halpha and possibly other Balmer emission HeI = Helium I emission HeII = Helium II emission rm* = WD parameters taken from Rebassa-Mansergas et al. (2007, Cat. J/MNRAS/382/1377) Note (5): WD types are: DA = DA white dwarf (hydrogen-rich), DO = DO white dwarf (helium-rich) Note (6): Optically resolved code as follows: o = Clearly resolved binary with projected angular distance <1.5" O = Binary components with slight angular separation and without further treatment * = Objects separated by >1.5", likely to be not those represented in the spectrum ? = Photometric data corresponding to the object id not available in the SDSS database
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 10 A10 --- SDSSs Short name (JHHMM+DDMM) 12- 30 A19 --- SDSS SDSS long name (JHHMMSS.ss+DDMMSS.s) 32- 38 A7 --- --- [spSpec-] 39- 52 A14 --- SDSS-sp Spectral plate (SDSS) (1) 53- 56 A4 --- --- [.fit] 58- 71 A14 --- Ref References (2) 73- 81 A9 --- Name ?=- Alternative name (dash when none found) 83-106 A24 --- SName1 Simbad Name (4) 108-111 F4.1 arcsec Off1 ? Offset from target for SName1 113-137 A25 --- SName2 Simbad Name (4) 139-142 F4.1 arcsec Off2 ? Offset from target for SName2 144-168 A25 --- SName3 Simbad Name (4) 170-173 F4.1 arcsec Off3 ? Offset from target for SName3 175-181 A7 --- SName4 Simbad Name (4) 183-186 F4.1 arcsec Off4 ? Offset from target for SName4
Note (1): Spectral plate on which the object was taken, coded as mmmmm-pppp-fff, where mmmmm is the Modified Julian Date, pppp is the plate ID number and fff is the fiber ID number Note (2): References as follows: g = Greenstein et al. (1986AJ.....92..867G) l99b = Luyten (1999, Cat. III/70) r = Raymond et al. (2003AJ....125.2621R) kl = Kleinmann et al. (2004, Cat. J/ApJ/607/426) e = Eisenstein et al. (2006, Cat. J/ApJS/167/40) h = Huegelmeyer et al. (2006A&A...454..617H) s6 = Silvestri et al. (2006, Cat. J/AJ/131/1674) s7 = Silvestri et al. (2007AJ....134..741S) rm = Rebassa-Mansergas et al. (2007, Cat. J/MNRAS/382/1377) (non-PCEB) rm* = Rebassa-Mansergas et al. (2007, Cat. J/MNRAS/382/1377) (PCEB) Note (4): We have searched SIMBAD for objects closer than 30 arcmin to the target. Most of the found objects have a distance of order 1arcmin. Those with much larger distances, which were found in more recent catalogs, might not be the same objects as the SDSS targets.
Global Notes: Note (G1): Notes as follows: p = Objects mentioned as post-common envelope binary (PCEB) or PCEB candidates in Rebassa-Mansergas et al. (2007, Cat. J/MNRAS/382/1377) + = M component very-low-mass-object candidate * = M component probably giant due to the low surface gravity of 3dex
Acknowledgements: Rene Heller, rheller(at)hs.uni-hamburg.de History: * 13-Mar-2009: Original files * 13-Jul-2010: In table3, 39 long SDSS names corrected * 14-Jul-2010: In table3, 2 positions and SDSS-sp numbers corrected
(End) Rene Heller [Hamburger Sternwart], Patricia Vannier [CDS] 13-Mar-2009
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

catalogue service

© UDS/CNRS

Contact