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 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 2008A&A...484..441S,
2010A&A...513L...7S 2010A&A...513L...7S)
File Summary:
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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 63 1508 Multiple radial velocities of the 58 WDMS with
measured orbital period
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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
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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
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Note (1): Positions from SDSS name.
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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)
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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
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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
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Note (1): We limit to spectra used for the identification of the WDMS
binary as a close or wide candidate.
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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
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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.
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Acknowledgements:
Ada Nebot Gomez-Moran, ada.nebot(at)astro.unistra.fr
References:
Rebassa-Mansergas et al., Paper I 2007MNRAS.382.1377R 2007MNRAS.382.1377R, Cat. J/MNRAS/382/1377
Schreiber et al, Paper II 2008A&A...484..441S 2008A&A...484..441S
Rebassa-Mansergas et al., Paper III 2008MNRAS.390.1635R 2008MNRAS.390.1635R
Nebot Gomez-Moran et al., Paper IV 2009A&A...495..561N 2009A&A...495..561N
Pyrzas et al., Paper V 2009MNRAS.394..978P 2009MNRAS.394..978P
Schwope et al., Paper VI 2009A&A...500..867S 2009A&A...500..867S
Rebassa-Mansergas et al., Paper VII 2010MNRAS.402..620R 2010MNRAS.402..620R, Cat. J/MNRAS/402/620
Schreiber et al., Paper VIII 2010A&A...513L...7S 2010A&A...513L...7S
Zorotovoc et al., Paper IX 2010A&A...520A..86Z 2010A&A...520A..86Z
Rebassa-Mansergas et al., Paper X 2011MNRAS.413.1121R 2011MNRAS.413.1121R
Zorotovic et al., Paper XI 2011arXiv1108.4600Z 2011arXiv1108.4600Z
Rebassa-Mansergas et al., Paper XIV 2011arXiV1110.1000R 2011arXiV1110.1000R
Pyrzas et al., Paper XV 2011arXiv1109.1171P 2011arXiv1109.1171P
History:
* 06-Dec-2011: Original catalog, from on-line version
* 14-Feb-2013: table5 added
(End) Patricia Vannier [CDS] 14-Feb-2013