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Post common envelope binaries from SDSS: White dwarf/main sequence binaries from SEGUE

Post common envelope binaries from SDSS: White dwarf/main sequence binaries from SEGUE. Ada Nebot G ómez-Morán. The collaboration: Matthias Schreiber (UV)

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Post common envelope binaries from SDSS: White dwarf/main sequence binaries from SEGUE

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  1. Post common envelope binaries from SDSS:White dwarf/main sequence binaries from SEGUE Ada Nebot Gómez-Morán The collaboration:Matthias Schreiber (UV) Monica Zorotovic Fiebig (PUC Santiago) Robert Schwarz (AIP)Axel Schwope (AIP)Boris Gänsicke (Warwick)Alberto Rebassa-Mansergas (UV)John Southworth (Warwick)Pablo Rodriguez-Gil (IAC) Tucson, 16th March 2009

  2. Evolution into close binaries Post Common Envelope Binaries (PCEB) Angular Momentum Loss by Magnetic Braking (MB) Common Envelope (CE) CV Willems & Kolb 2004

  3. WDMS sample • Before SDSS: 30 PCEBs (Schreiber & Gänsicke, 2003) • Hot WD + Late type secondary • The old population of WDMS is missing • In the SDSS: ~1300 new WDMS (Silvestri et al. 2006, Rebassa et al. 2007) Lack of cold WD and early SpT SpT peak @ M4 Teff Peak @ 2x104K N N Silvestri et al 2006

  4. WDMS with SEGUE TWD • Calculated colors cover • 104K  TWD  6104K • K0  SpT  M6 4104 K 3104 K 2104 K 1.5104 K 1104 K SEGUE: ~10 Sloan fibers/plate pair 278 new WDMS (Schreiber et al. 2006, 2009 in prep.) Success rate ~ 60%

  5. Stellar parameters SpT-R SpT dsec Teff,log(g) dwd GALEX Rebassa-Mansergas et al 2007, Scheiber et al 2009

  6. Stellar parameters Peak @104K Activity ? Peak @ M3 Schreiber et al 2009 (in prep.)

  7. Completeness, space density and scale height Space density Completeness space density (10-4 pc-3) d (pc) |b|  ~310-5-610-6 pc-3 cooling age (years)  exp(-z/h) h = 100-150 pc

  8. SDSSJ030138.24+050218.9 RVs from the SDSS subexposures RV > 3 Identification of 44 PCEB candidates Flux (10-17 ergs-1cm2Å-1 Fraction PCEB/WDMS ≥16% Wavelength (Å) Nebot Gómez-Morán et al in prep.

  9. Orbital Periods Nebot Gómez-Morán et al in prep.

  10. Outlook • With SEGUE the old population has been identified • 44 new PCEB from the sub-exposures of the SDSS spectra PCEB fraction > 16% • The ~2000 WDMS systems form the database to constrain close binary evolution.

  11. Thanks!

  12. White dwarf effective temperature

  13. White dwarf mass

  14. Number of M stars Silvestri et al. 2006

  15. Spectra Flux (10-17erg cm2 s-1 Å-1) Wavelength (Å)

  16. Space density Ncand : Number of objects inside the criteria Nspec : Total number of spectra NWDMS: Number of WDMS Nout : Number of WDMS outside the criteria V : Volume

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