Hallakoun, N.Maoz, D.Kilic, M.Mazeh, T.Gianninas, A.Agol, E.Bell, K. J.Bloemen, S.Brown, W. R.Debes, J.Faigler, S.Kull, I.Kupfer, T.Loeb, AbrahamMorris, B. M.Mullally, F.2017-04-062016Hallakoun, N., D. Maoz, M. Kilic, T. Mazeh, A. Gianninas, E. Agol, K. J. Bell, et al. 2016. “SDSS J1152+0248: An Eclipsing Double White Dwarf from theKeplerK2campaign.” Monthly Notices of the Royal Astronomical Society 458 (1) (February 17): 845–854. doi:10.1093/mnras/stw364.0035-8711http://nrs.harvard.edu/urn-3:HUL.InstRepos:32072397We report the discovery of the sixth known eclipsing double white dwarf (WD) system, SDSS J1152+0248, with a 2.3968 +/- 0.0003 h orbital period, in data from the Kepler Mission's K2 continuation. Analysing and modelling the K2 data together with ground-based fast photometry, spectroscopy, and radial-velocity measurements, we determine that the primary is a DA-type WD with mass M1 = 0.47 +/- 0.11 Msun, radius R1 = 0.0197 +/- 0.0035 Rsun, and cooling age t1 = 52 +/- 36 Myr. No lines are detected, to within our sensitivity, from the secondary WD, but it is likely also of type DA. Its central surface brightness, as measured from the secondary eclipse, is 0.31 of the primary's surface brightness. Its mass, radius, and cooling age, respectively, are M2 = 0.44 +/- 0.09 Msun, R2 = 0.0223 +0.0064 -0.0050 Rsun, and t2 = 230 +/- 100 Myr. SDSS J1152+0248 is a near twin of the double-lined eclipsing WD system CSS 41177.en-USmethods: statisticaltechniques: radial velocitiesbinaries: eclipsingwhite dwarfsstarsSDSS J115219.99 + 024814.4Journal Article2017-02-1420152017-04-0610.1093/mnras/stw364