A Gravitational Redshift Determination Of The Mean Mass Of White Dwarfs: DBA And DB Stars

We measure apparent velocities (nu(app)) of absorption lines for 36 white dwarfs (WDs) with helium-dominated atmospheres-16 dbAs and 20 dbs-using optical spectra taken for the European Southern Observatory SN Ia progenitor survey. We find a difference of 6.9 +/- 6.9 kms(-1) in the average apparent velocity of the H alpha lines versus that of the He I 5876 angstrom lines for our dbAs. This is a measure of the blueshift of this He line due to pressure effects. By using this as a correction, we extend the gravitational redshift method employed by Falcon et al. to use the apparent velocity of the He I 5876 angstrom line and conduct the first gravitational redshift investigation of a group of WDs without visible hydrogen lines. We use biweight estimators to find an average apparent velocity, (BI), (and hence average gravitational redshift, (BI)) for our WDs; from that we derive an average mass, (BI). For the dbAs, we find (BI) = 40.8 +/- 4.7 kms(-1) and derive (BI) = 0.71(-0.05)(+0.04) M-circle dot. Though different from of DAs (32.57 km s(-1)) at the 91% confidence level and suggestive of a larger dbA mean mass than that for normal DAs derived using the same method (0.647(-0.014)(+0.013) M-circle dot; Falcon et al.), we do not claim this as a stringent detection. Rather, we emphasize that the difference between (BI) of the dbAs and of normal DAs is no larger than 9.2 kms(-1), at the 95% confidence level; this corresponds to roughly 0.10 M-circle dot. For the dbs, we find (BI) = 42.9 +/- 8.49 km s(-1) after applying the blueshift correction and determine (BI) = 0.74(-0.09)(+0.08) M-circle dot. The difference between (BI) of the dbs and of DAs is <= 11.5 kms(-1) (similar to 0.12 M-circle dot), at the 95% confidence level. The gravitational redshift method indicates much larger mean masses than the spectroscopic determinations of the same sample by Voss et al. Given the small sample sizes, it is possible that systematic uncertainties are skewing our results due to the potential of kinematic substructures that may not average out. We estimate this to be unlikely, but a larger sample size is necessary to rule out these systematics.National Science Foundation AST-0909107, AST-0602288Norman Hackerman Advanced Research Program 003658-255-2007, 003658-0252-2009Institute for High Energy Density ScienceUniversity of Texas SystemSandia National LaboratoriesNational Physical Science ConsortiumDelaware Asteroseismic Research CenterNASA NNX11AG82G, HST-GO-11141McDonald Observator