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J/A+A/536/A43    SDSS WD main-sequence binaries. XII. (Nebot Gomez-Moran+, 2011)

Post common envelope binaries from SDSS. XII: The orbital period distribution. Nebot Gomez-Moran A., Gaensicke B.T., Schreiber M.R., Rebassa-Mansergas A., Schwope A.D., Southworth J., Aungwerojwit A., Bothe M., Davis P.J., Kolb U., 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. 536, A43 (2011)> =2011A&A...536A..43N
ADC_Keywords: Stars, double and multiple ; Stars, white dwarf ; Stars, dwarfs ; Radial velocities ; Stars, masses Keywords: binaries: close - binaries: spectroscopic - white dwarfs - stars: low-mass Abstract: The complexity of the common-envelope phase and of magnetic stellar wind braking currently limits our understanding of close binary evolution. Because of their intrinsically simple structure, observational population studies of white dwarf plus main sequence (WDMS) binaries can potentially test theoretical models and constrain their parameters. The Sloan Digital Sky Survey (SDSS) has provided a large and homogeneously selected sample of WDMS binaries, which we characterise in terms of orbital and stellar parameters. We have obtained radial velocity information for 385 WDMS binaries from follow-up spectroscopy and for an additional 861 systems from the SDSS subspectra. Radial velocity variations identify 191 of these WDMS binaries as post common-envelope binaries (PCEBs). Orbital periods of 58 PCEBs were subsequently measured, predominantly from time-resolved spectroscopy, bringing the total number of SDSS PCEBs with orbital parameters to 79. Observational biases inherent to this PCEB sample were evaluated through extensive Monte Carlo simulations. We find that 21-24% of all SDSS WDMS binaries have undergone common-envelope evolution, which is in good agreement with published binary population models and high-resolution HST imaging of WDMS binaries unresolved from the ground. The bias-corrected orbital period distribution of PCEBs ranges from 1.9h to 4.3d and approximately follows a normal distribution in log(Porb), peaking at ∼10.3h. There is no observational evidence for a significant population of PCEBs with periods in the range of days to weeks. The large and homogeneous sample of SDSS WDMS binaries provides the means to test fundamental predictions of binary population models, hence to observationally constrain the evolution of all close compact binaries. Description: Table3.dat lists only radial velocities used for the identification of the binary as a close or wide binary candidate. Table4.dat contains the total number of spectra used for identification of the binary, the number of spectra from own spectroscopic follow-up observations and the statistical significance of the radial velocity variations. Table6.dat list radial velocities limited to the spectra used for the determination of the orbital period. Stellar parameters have been taken from Rebassa-Mansergas et al (2010, Cat., J/MNRAS/402/620, 2011, in prep.). Some radial velocities have already been published in Schreiber et al. (2008A&A...484..441S, 2010A&A...513L...7S) File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file stars.dat 54 1246 List of WDMS binaries (white dwarf + main sequence) table3.dat 64 6074 Multiple radial velocities of the 1246 WDMS table4.dat 46 1246 Statistical significance of the radial velocity variations table5.dat 186 58 Stellar and binary parameters derived for the 58 PCEBs (post common-envelope binaries) presented in this work table6.dat 64 1508 Multiple radial velocities of the 58 WDMS with measured orbital period
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: stars.dat
Bytes Format Units Label Explanations
1- 4 A4 --- --- [SDSS] 5- 23 A19 -- SDSS WDMS binary SDSS name (JHHMMSS.ss+DDMMSS.s) 26- 27 I2 h RAh Right ascension (J2000) (1) 29- 30 I2 min RAm Right ascension (J2000) (1) 32- 36 F5.2 s RAs Right ascension (J2000) (1) 38 A1 --- DE- Declination sign (J2000) (1) 39- 40 I2 deg DEd Declination (J2000) (1) 42- 43 I2 arcmin DEm Declination (J2000) (1) 45- 48 F4.1 arcsec DEs Declination (J2000) (1) 50- 51 I2 --- N3 Number of velocity observations in table3 53- 54 I2 --- N6 ? Number of velocity observations in table6
Note (1): Positions from SDSS name.
Byte-by-byte Description of file: table3.dat table6.dat
Bytes Format Units Label Explanations
1- 4 A4 --- --- [SDSS] 5- 23 A19 -- SDSS WDMS binary SDSS name (JHHMMSS.ss+DDMMSS.s) 25- 31 F7.2 km/s RV Radial velocity (1) 33- 37 F5.2 km/s e_RV Radial velocity uncertainty (1 sigma) 39- 52 F14.6 d HJD Heliocentric Julian date 54- 64 A11 -- Tel Telescope (2)
Note (1): note that * For table3, we limit to spectra used for the identification of the WDMS binary as a close or wide candidate. * For table6, we limit to spectra used for the measuring the orbital period of the WDMS binaries. Note (2): The abbreviations for the telescopes we used are the following: CA3.5 = radial velocities measured from NaI doublet, based on spectra taken with the Calar Alto 3.5m Telescope SDSS = radial velocities measured from NaI doublet, derived from an SDSS spectrum or directly from the individual sub-exposures WHT = radial velocities measured from NaI doublet, based on spectra taken with the William Herschel Telescope Gemini-S = radial velocities measured from NaI doublet, based on spectra taken at Gemini South Gemini-S_Ha = radial velocities measured from Halpha emission, based on spectra taken at Gemini South GN = radial velocities measured from NaI doublet, based on spectra taken at Gemini North VLT = radial velocities measured from NaI doublet, based on spectra taken with ESO VLT/FORS2 VLT_Ha = radial velocities measured from Halpha emission, based on spectra taken with ESO VLT/FORS2 NTT = radial velocities measured from NaI doublet, based on spectra taken with ESO NTT M-Clay = radial velocities measured from NaI doublet, based on spectra taken with the Magellan-Clay Telescopes at LCO M-Clay_Ha = radial velocities measured from Halpha emission, based on spectra taken with the Magellan-Clay Telescopes at LCO M-Baade = radial velocities measured from NaI doublet, based on spectra taken with the Magellan-Baade Telescopes at LCO M-Baade_Ha = radial velocities measured from Halpha emission, based on spectra taken with the Magellan-Baade Telescopes at LCO
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 4 A4 --- --- [SDSS] 5- 23 A19 -- SDSS WDMS binary SDSS name (JHHMMSS.ss+DDMMSS.s) 25- 26 I2 -- Nsp Total number of spectra (1) 28- 29 I2 -- Nobs Number of spectra from own observations (1) 31- 38 F8.3 d Deltat Time span between first and last observation (1) 40- 46 F7.5 -- Prob Statistical significance of radial velocity variation
Note (1): We limit to spectra used for the identification of the WDMS binary as a close or wide candidate.
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 4 A4 --- --- [SDSS] 5- 23 A19 --- SDSS WDMS binary SDSS name (JHHMMSS.ss+DDMMSS.s) 25- 33 A9 --- Name Short name (HHMM+DDMM) 34 A1 --- n_Name [*] Note on Name (1) 36- 46 F11.7 h Per Orbital period 49- 56 F8.7 h e_Per rms uncertainty on Per 58- 62 F5.1 km/s K2 ?=- Velocity amplitude K of the secondary 64- 67 F4.1 km/s e_K2 ?=- rms uncertainty on Ksec 69- 73 F5.1 km/s gam2 ?=- Systemic velocity gamma of the secondary 75- 77 F3.1 km/s e_gam2 ?=- rms uncertainty on gammasec 79- 83 A5 --- Type Spectral type of the binary 85- 89 I5 K Teff ?=- Effective temperature 91- 94 I4 K e_Teff ?=- rms uncertainty on Teff 96- 99 F4.2 [cm/s2] log(g) ?=- Gravity surface 101-103 F3.2 [cm/s2] e_log(g) ?=- rms uncertainty on log(g) 105-108 F4.2 Msun Mwd ?=- Mass of the white dwarf (primary) 110-112 F3.2 Msun e_Mwd ?=- rms uncertainty on Mwd 114-116 I3 pc dwd ?=- Distance of the white dwarf (primary) 118-120 I3 pc e_dwd ?=- rms uncertainty on dwd 122-125 F4.1 --- Sp2 ?=-1. dM spectral type of the secondary 126-127 A2 --- n_Sp2 [*] Spectrum could not be fitted (2) 129-132 I4 pc d2 ?=- Distance of the secondary 134-136 I3 pc e_d2 ?=- rms uncertainty on d2 138-141 F4.2 Msun M2 ?=- Mass of the secondary 143-145 F3.2 Msun e_M2 ?=- rms uncertainty on M2 147 A1 --- l_i1 [~] Limit flag on Incl1 148-149 I2 deg i1 ?=- First value of inclination interval 150 A1 --- --- [-] 151-152 I2 deg i2 ?=- Second value of inclination interval 154-156 I3 km/s Kwd ?=- Velocity amplitude K of the WD (3) 158-159 I2 km/s e_Kwd ?=- rms uncertainty on Kwd 161-164 F4.2 Rsun a ?=- Semi-major axis 166-168 F3.2 Rsun e_a ?=- rms uncertainty on a 170-173 F4.2 Rsun R2 ?=- Radius of the secondary 175-177 F3.2 Rsun e_R2 ?=- rms uncertainty on R2 179-182 F4.2 --- R2/Rlob ?=- Radius of the secondary in Lobe radius 184-186 F3.2 --- e_R2/Rlob ?=- rms uncertainty on Rsec/Rlob
Note (1): Radial velocities are measured from the NaI doublet, unless marked with * in which case it comes from the Hα emission line. Note (2): **: No spectral type could be derived from fitting the spectrum to template spectra. Note (3): Kwd are the calculated values in Sect. 4.2.3.
Acknowledgements: Ada Nebot Gomez-Moran, ada.nebot(at)astro.unistra.fr References: Rebassa-Mansergas et al., Paper I 2007MNRAS.382.1377R, Cat. 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, Cat. J/MNRAS/402/620 Schreiber et al., Paper VIII 2010A&A...513L...7S Zorotovoc et al., Paper IX 2010A&A...520A..86Z Rebassa-Mansergas et al., Paper X 2011MNRAS.413.1121R Zorotovic et al., Paper XI 2011arXiv1108.4600Z Rebassa-Mansergas et al., Paper XIV 2011arXiV1110.1000R Pyrzas et al., Paper XV 2011arXiv1109.1171P History: * 06-Dec-2011: Original catalog, from on-line version * 14-Feb-2013: table5 added
(End) Patricia Vannier [CDS] 14-Feb-2013
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