| Name | Period | Pdot | d | M2 | q | M1 | i | Mv | V | RA | DEC | l | b |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| [s] | [s/s] | [pc] | Msun | Msun | [deg] | [h:m:s] | [d:m:s] | [deg] | [deg] | ||||
| SDSS J0651+2844 | 765.4+/-7.9 | ? | ~1000 | 0.50 | 0.5 | 0.25 | 86.9+1.6-1 | ? | g=19.1 | 06 51 33.338 | +28 44 23.37 | 186.93 | 12.69 |
| SDSS J0935+4411 | 1188+/-44 | ? | ~660 | >0.14 | ? | 0.32 | ? | ? | g=17.7 | 09 35 XX | +44 11 YY | ||
| SDSS J0106-1000 | 2346+/-2 | ? | ~2400 | 0.43 | 0.4 | 0.17 | 67+/-13 | ? | g=19.8 | 01 06 57.39 | -10 00 03.3 | 135.72 | -72.47 |
| SDSS J1630+4233 | 2390+/-4 | ? | ~830 | >0.52 | ? | 0.31 | ? | ? | g= | 16 30 XX | +42 33 YY | ||
| SDSS J1053+5200 | 3680+/-10 | ? | ~1100 | >0.26 | ? | 0.20 | ? | ? | g=18.87 | 10 53 53.89 | +52 00 31.0 | 156.40 | +56.79 |
| SDSS J0923+3028 | 3884 | ? | 270 | >0.34 | ? | 0.23 | ? | ? | g= | 09 23 45.59 | +30 28 05.0 | 195.82 | 44.78 |
| SDSS J1436+5010 | 3957 +/-10 | ? | ~800 | >0.46 | ? | 0.24 | ? | ? | g=18.16 | 14 36 33.29 | +50 10 26.8 | 089.01 | +59.46 |
| WD 0957-666 | 5269.81080+/-0.00007 | ? | 135 +/- 20 | 0.32 +/- 0.03 | 1.15 +/- 0.10 | 0.37 +/- 0.02 | 50 – 86 | 8.94 | 14.60 | 09 58 54.96 | –66 53 10.2 | 287.14 | -9.46 |
| SDSS J0755+4906 | 5445 | ? | 2620 | >0.81 | ? | 0.17 | ? | ? | 07 55 52.40 | +49 06 27.9 | 169.76 | 30.42 | |
| SDSS J0849+0445 | 6800 | ? | 930 | >0.64 | ? | 0.17 | ? | ? | 08 49 10.13 | +04 45 28.7 | 222.70 | 28.27 | |
| SDSS J0022-1014 | 6902 | ? | 790 | >0.19 | ? | 0.33 | ? | ? | 00 22 07.65 | -10 14 23.5 | 99.30 | -71.75 | |
| SDSS J2119-0018 | 7497 | ? | 2500 | >0.75 | ? | 0.17 | ? | ? | 21 19 21.96 | -00 18 25.8 | 51.58 | -32.54 | |
| SDSS J1234-0228 | 7900 | ? | 780 | >0.09 | ? | 0.23 | ? | ? | 12 34 10.36 | -02 28 02.8 | 294.25 | 60.11 | |
| WD 1101+364 | 12503 +/- 5 | ? | 97 +/- 15 | 0.36 | 0.87 +/- 0.03 | 0.31 | 25 | 9.55 | 14.49 | 11 04 32.61 | +36 10 49.5 | 184.48 | +65.62 |
| WD 1704+4807BC | 12511 +/- 2 | ? | 0.56 +/- 0.07 | 0.70 +/- 0.03 | 0.39 +/- 0.05 | 61 | 14.5 | 17 05 30.1 | +48 03 17 | 74.25 | +37.19 |
For low mass SDSS systems see Kilic et al. 2011a still need to add more information (GN)
12 minute system found by Kilic & co Brown et al. 2011
20 min system, Kilic & co Kilic et al. 2014
Kilic et al. 2011b
Paper now out Kilic et al. 2010
Reported by Badenes in KITP conference, 2009, http://online.kitp.ucsb.edu/online/sdeath_c09/ as a short period double white dwarf. It has a radial velocity amplitude of 310 +/- 14 km/s. They observed the star as it was one of the targets discussed by Kilic et al (2007) for being a very low mass white dwarf (0.19 Msun). Such stars are very likely to be binary as this one indeed is (TRM). The mass of the unseen (secondary) star is a lower limit calculated from the radial velocity amplitude and the 0.19 Msun mass for the primary. Kilic et al (2007) lists a temperature of 15,900K, which combined with the mass of the brighter object should give a distance.
See Giannidas et al. 2014
Paper now out Kilic et al. 2010
Second system reported by Badenes at KITP conference, 2009, http://online.kitp.ucsb.edu/online/sdeath_c09/ (see SDSS J1053+5200). This is also another star from Kilic et al (2007). The radial velocity semi-amplitude K = 388 +/- 21 km/s, which leads to the lower limit on the mass of the secondary star assuming the quoted mass for the primary star. Kilic et al (2007) list a temperature of 18,400 K cf 17,000 K from Eisenstein et al (2006) where this star was first identified as a low mass white dwarf.
Period from Moran et al (1997); distance from Bragaglia et al (1995). Uncertainty in the distance is a bit of a guess; formal uncertainties are lower, but things are never quite as good as formal uncertainties suggest. Nevertheless, this distance (which is based upon the apparent magnitude versus model atmosphere fits (with a 20% correction for the light of the companion which I have used to raise the absolute magnitude of the system by 0.2 mags), and should be pretty good. (TRM)
Mass ratio q = M1/M2 (brighter over fainter). This is a double-lined system and so the mass ratio is well determined. (TRM)
The masses are from Moran et al (1997). The inclination comes from taking a 2-sigma lower limit on sin i from Moran et al (1997) together with an absence of observed eclipses from Hoard & Wachter (2002) (TRM).
Marsh (1995) discovered this star to be a binary. It is a double-lined system (TRM). The absolute magnitude has been corrected up by 0.75 mags from a straight model atmosphere fit because the system is a very equal double (TRM). Masses and inclination are not well constrained; mass ratio is OK (TRM). As usual for the double white dwarfs, the mass ratio = M(bright)/M(faint) (TRM).
Maxted et al (2000) discovered that this star was a close binary. It is part of a triple system with another white dwarf and hence the 'BC' designation (TRM). Mass ratio is ratio of masses of the bright over the faint component (TRM).