J/A+A/513/L7 Post common envelope binaries from SDSS. VIII (Schreiber+, 2010)
Post common envelope binaries from SDSS. VIII: Evidence for disrupted magnetic braking. Schreiber M.R., Gaensicke B.T., Rebassa-Mansergas A., Nebot Gomez-Moran A., Southworth J., Schwope A.D., Mueller M., Papadaki C., Pyrzas S., Rabitz A., Rodriguez-Gil P., Schmidtobreick L., Schwarz R., Tappert C., Toloza O., Vogel J., Zorotovic M. <Astron. Astrophys. 513, L7 (2010)> =2010A&A...513L...7S
ADC_Keywords: Stars, double and multiple ; Stars, white dwarf ; Stars, dwarfs ; Radial velocities ; Stars, masses Keywords: binaries: close - magnetic fields - stars: low mass - white dwarfs Abstract: We present the results of a large survey of post common envelope binaries (PCEBs) among white dwarf/main sequence (WDMS) binaries from the SDSS that allows to determine the fraction of PCEBs as a function of secondary star mass and therewith to ultimately test the disrupted magnetic braking hypothesis. We obtained multiple spectroscopic observations spread over at least two nights of 589 WDMS binaries. Using mostly the NaI 8183.27,8194.81 absorption doublet we determined the corresponding radial velocities. Description: The file rv.dat contains the name of the WDMS binary, the time of the spectroscopic observation and the corresponding radial velocity. Using a spectral decomposition method we derived estimates of the stellar parameters and the distance to the system listed in sy.dat. This file also contains the statistical significance of the measured radial velocity variations derived from the velocities given in rv.dat. The stellar parameters have been taken from Rebassa-Mansergas et al. (2010, Cat. J/MNRAS/402/620) and Nebot-Gomez Moran (2010, A&A in prep.). The spectral decomposition method is described in Rebassa-Mansergas et al. (2007, Cat. J/MNRAS/382/1377). Some radial velocities have been published earlier in Schreiber et al. (2008A&A...484..441S) File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file sy.dat 111 670 Stellar parameters derived for the WDMS binaries by spectral decomposition of the SDSS spectrum and the statistical significance of radial velocity variations rv.dat 57 3306 Multiple radial velocities of the 670 WDMS binaries derived from 3308 spectra
See also: J/MNRAS/382/1377 : SDSS WD main-sequence binaries (Rebassa-Mansergas+, 2007) J/MNRAS/402/620 : SDSS WD main-sequence binaries (Rebassa-Mansergas+, 2010) Byte-by-byte Description of file: sy.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Nsp Number of spectra available for this system 4- 7 A4 --- --- [SDSS] 8- 16 A9 --- Name Name of the WDMS binary (HHMM+DDMM) 18- 22 A5 --- Type Type of WDMS binary (1) 24- 27 F4.2 solMass Mwd ?=- Mass of the white dwarf (1) 29- 32 F4.2 solMass e_Mwd ?=- Uncertainty (1 sigma) of Mwd estimate 34- 37 I4 pc d ?=- Distance to the WDMS binary as measured to the white dwarf 39- 42 I4 pc e_d ?=- Uncertainty of the distance estimate 44- 47 F4.2 --- SpT Spectral sub-type of the secondary star 49- 53 F5.3 solMass Msec Mass of the secondary (main sequence) star 55- 59 I5 K Twd ?=- White dwarf temperature 61- 66 F6.2 km/s RVvar Peak to peak radial velocity variation 68- 73 F6.2 km/s e_RVvar Error of peak to peak radial velocity variation 74- 85 E12.9 --- Signi [0/1] Statistical significance of radial velocity variation 87 I1 --- pc [0/4] PCEB (post common envelope binaries) candidate (3 or >4σ) or wide WDMS candidate (2) 89- 92 A4 --- --- [SDSS] 93-111 A19 --- SDSS SDSS designation (JHHMMSS.ss+DDMMSS.s)
Note (1): type of binary, generally a denegerate (DA, DB, DC, WD) and a low-mass (M) star. "LARP" stands for "Low Accretion Rate Polars", i.e. pre-cataclysmic variables containing a magnetic white dwarf. Note (2): In some cases the white dwarf type is DC, DB, or unknown and we could not estimate the white dwarf mass and the distance to the system.
Byte-by-byte Description of file: rv.dat
Bytes Format Units Label Explanations
1- 4 A4 --- --- [SDSS] 5- 13 A9 --- Name WDMS name (HHMM+DDMM) 15- 26 F12.4 d HJD ? Heliocentric Julian date (1) 28- 34 F7.2 km/s RV Radial velocity 36- 41 F6.2 km/s e_RV Radial velocity uncertainty (1 sigma) 43- 57 A15 --- Tel Telescope/Instrument (2)
Note (1): In some cases the date at which an SDSS spectrum (i.e. the combined SDSS spectrum from individual exposures) has been taken could not be reconstructed. This is indicated by a 0.00000 in the corresponding column. Note (2): The abbreviations for the telescopes we used are the following: CA3.5 = RV based on spectra taken with the Calar Alto 3.5m Telescope SDSS = RV derived from an SDSS spectrum or directly from the individual sub-exposures WHT = RV based on spectra taken with the William Herschel Telescope GS = RV based on spectra taken at Gemini South ESO = RV based on spectra taken with ESO VLT/FORS2 NTT = RV based on spectra taken with ESO NTT MAG = RV based on spectra taken with the Magellan Telescopes at LCO * "Na" after the abbreviation indicates in all cases that the Rvels were measured from the NaI doublet, Ha from the Halpha emission. * If nothing is indicated it implies that the RV were measured also from the NaI doublet.
Acknowledgements: Matthias Schreiber, References: Rebassa-Mansergas et al., Paper I 2007MNRAS.382.1377R (J/MNRAS/382/1377) Schreiber et al, Paper II 2008A&A...484..441S Rebassa-Mansergas et al., Paper III 2008MNRAS.390.1635R Nebot Gomez-Moran et al., Paper IV 2009A&A...495..561N Pyrzas et al., Paper V 2009MNRAS.394..978P Schwope et al., Paper VI 2009A&A...500..867S Rebassa-Mansergas et al., Paper VII 2010MNRAS.402..620R (J/MNRAS/402/620)
(End) Patricia Vannier [CDS] 19-Mar-2010
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