New white dwarf stars in the Sloan Digital Sky Survey Data Release 10

Kepler, S. O.; Pelisoli, Ingrid; Koester, D.; Ourique, Gustavo; Kleinman, S. J.; Romero, A. D.; Nitta, A.; Eisenstein, Daniel J.; Costa, J. E. S.; Külebi, Baybars; Jordan, S.; Dufour, P.; Giommi, P.; Rebassa‐Mansergas, A.

doi:10.1093/mnras/stu2388

Cited by 221 publications

(207 citation statements)

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“…Moreover, we note that we have identified 759 DR 9-10 WDMS binary spectra that are not included in the list of Kepler et al (2015). The fact that Kepler et al (2015) missed this large number of WDMS binary spectra is not too surprising, as their main focus was to identify single white dwarfs. Kepler et al (2016) presented an updated SDSS white dwarf catalogue from DR 12, which includes 160 new WDMS binary spectra.…”

Section: Comparison With Kepler Et Al (2015) and Kepler Et Al (2016)mentioning

confidence: 91%

“…We include the nine missed objects in our lists and increase to 1314 and 78 the number of WDMS binary and candidate spectra, respectively (Table 1). Moreover, we note that we have identified 759 DR 9-10 WDMS binary spectra that are not included in the list of Kepler et al (2015). The fact that Kepler et al (2015) missed this large number of WDMS binary spectra is not too surprising, as their main focus was to identify single white dwarfs.…”

Section: Comparison With Kepler Et Al (2015) and Kepler Et Al (2016)mentioning

confidence: 91%

“…An additional list of 177 DR 9-10 SDSS WDMS binary spectra has been provided by Kepler et al (2015). 153 (2) of these are included in our WDMS binary (candidate) list, we only missed 5 (4) WDMS binary (candidate) spectra (Table 1), the majority dominated by the flux contribution of the white dwarf.…”

Section: Comparison With Kepler Et Al (2015) and Kepler Et Al (2016)mentioning

confidence: 99%

“…Inspection of the numbers outlined above reveals that the χ 2 -SN ratio method has identified only ∼68 per cent of our total number Li et al (2014) 152 (4) 5(3) 1309(74) Kepler et al (2015) 158 (6) 5(4) 1314(78) Kepler et al (2016) 127 (2) 5 (1) 1319(79) Gentile Fusillo, Gänsicke & Greiss (2015) 93 ( of SDSS III WDMS binary spectra and that the WT method has successfully identified ∼84 per cent of the total number. That is, the WDMS binary samples identified by the χ 2 -SN and the WT methods are ∼68 and ∼84 per cent complete, respectively (the completeness of the overall sample is derived in the next section).…”

Section: The Sdss III Wdms Binary Samplementioning

confidence: 99%

“…We classify the remaining 13 spectra as single white dwarfs or main sequence plus main-sequence superpositions. Hence, we have successfully identified ∼94 per cent of the total sample provided by Kepler et al (2015). We include the nine missed objects in our lists and increase to 1314 and 78 the number of WDMS binary and candidate spectra, respectively (Table 1).…”

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confidence: 99%

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The SDSS spectroscopic catalogue of white dwarf-main-sequence binaries: new identifications from DR 9–12

Rebassa‐Mansergas

Ren

Parsons

et al. 2016

Mon. Not. R. Astron. Soc.

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We present an updated version of the spectroscopic catalogue of white dwarf-main-sequence (WDMS) binaries from the Sloan Digital Sky Survey (SDSS). We identify 938 WDMS binaries within the data releases (DR) 9-12 of SDSS plus 40 objects from DR 1-8 that we missed in our previous works, 646 of which are new. The total number of spectroscopic SDSS WDMS binaries increases to 3294. This is by far the largest and most homogeneous sample of compact binaries currently available. We use a decomposition/fitting routine to derive the stellar parameters of all systems identified here (white dwarf effective temperatures, surface gravities and masses, and secondary star spectral types). The analysis of the corresponding stellar parameter distributions shows that the SDSS WDMS binary population is seriously affected by selection effects. We also measure the Na I λλ 8183.27, 8194.81 absorption doublet and H α emission radial velocities (RV) from all SDSS WDMS binary spectra identified in this work. 98 objects are found to display RV variations, 62 of which are new. The RV data are sufficient enough to estimate the orbital periods of three close binaries.Key words: binaries: close -binaries: spectroscopic -stars: low-mass -white dwarfs. I N T RO D U C T I O NA large fraction of main-sequence stars are found in binary systems (Duquennoy & Mayor 1991;Raghavan et al. 2010;Yuan et al. 2015b). It is expected that ∼25 per cent of all main-sequence binaries are close enough to begin mass transfer interactions when the more massive star becomes a red giant or an asymptotic giant star (Willems & Kolb 2004). This has been observationally verified e.g. by Farihi, Hoard & Wachter (2010) and by Nebot . Because the mass transfer rate generally exceeds the Eddington limit, the secondary star is not able to accrete the transferred material and the system evolves through a common envelope phase. That is, the core of the giant and the main-sequence companion orbit within a common envelope formed by the outer layers of the giant star. Drag forces between the two stars and the envelope lead to the shrinkage of the orbit and therefore to the release E-mail: alberto.rebassa@upc.edu of orbital energy. The orbital energy is deposited into the envelope and is eventually used to eject it (Webbink 2008). The outcome of common envelope evolution is hence a close binary formed by the core of the giant star (which later becomes a white dwarf) and a main-sequence companion, i.e. a close white dwarf-main-sequence (WDMS) binary. These are commonly referred to as post-common envelope binaries (PCEBs). The remaining ∼75 per cent of mainsequence binaries are wide enough to avoid mass transfer interactions. In these cases the more massive stars evolve like single stars until they eventually become white dwarfs. The orbital separations of such WDMS binaries are similar to those of the main-sequence binaries from which they descend.During the last years we have mined the Sloan Digital Sky Survey (SDSS; York et al. 2000) spectroscopic data base to build up th...

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Section: Comparison With Kepler Et Al (2015) and Kepler Et Al (2016)mentioning

confidence: 91%

Section: Comparison With Kepler Et Al (2015) and Kepler Et Al (2016)mentioning

confidence: 91%

Section: Comparison With Kepler Et Al (2015) and Kepler Et Al (2016)mentioning

confidence: 99%