White dwarf cooling sequences for massive white dwarfs with oxygen-neon cores and stellar masses from 1.06 to 1.28 Msun, and described in Althaus, García-Berro , Isern at al. 2007, A&A, 465, 249, are provided. Element diffusion and detailed non-gray model atmospheres to derive the outer boundary conditions of the evolving models are considered. Calculations are extended down to stellar luminosities of log L/Lsun=-5.2. Our cooling sequences are based on evolutionary calculations that take into account the chemical composition expected from massive white dwarf progenitors that burned carbon in partially degenerate conditions. Thus, an oxygen-neon composition is expected in the core of our massive white dwarfs. Broadband color indices have been calculated using the optical BVRI and infrared JHK passbands of Bessell (1990) and Bessell & Brett (1988), respectively, with calibration constants from Bergeron et al. (1997), see Althaus et al 2007 for details.

White dwarf cooling tracks are provided for stellar masses of 1.06, 1.10, 1.16, 1.20, 1.24 and 1.28 Msun. Each cooling sequence file lists from left to right:

Log L/Lo: The logarithm of the surface luminosity in solar unit

Log Teff: The logarithm of the effective temperature (K)

B_V: B-V color index

V_R: V-R color index

V_K: V-K color index

R_I: R-I color index

J_H: J-H color index

H_K: H-K color index

V_I: V-I color index

U_V: U-V color index

BC(V): bolometric correction

dmag_v: Absolute visual magnitude

Log age (yr): The logarthm of cooling age in year

All the evolutionary sequences have the same core composition and shell profile. In particular, the chemical abundance distribution is displayed in the figure below