An 8.8 minute orbital period eclipsing detached double white dwarf binary

Abstract

We report the discovery of ZTF J2243+5242, an eclipsing double white dwarf binary with an orbital period of just $8.8$ minutes, the second known eclipsing binary with an orbital period less than ten minutes. The system likely consists of two low-mass white dwarfs, and will merge in approximately 400,000 years to form either an isolated hot subdwarf or an R Coronae Borealis star. Like its $6.91\min$ counterpart, ZTF J1539+5027, ZTF J2243+5242 will be among the strongest gravitational wave sources detectable by the space-based gravitational-wave detector The Laser Space Interferometer Antenna (LISA) because its gravitational-wave frequency falls near the peak of LISA's sensitivity. Based on its estimated distance of $d=2120_{-115}^{+131}\mathrm{pc}$, LISA should detect the source within its first few months of operation, and should achieve a signal-to-noise ratio of $87\pm 5$ after four years. We find component masses of $M_A=0.349_{-0.074}^{+0.093}{M}_{\odot }$ and $M_B=0.384_{-0.074}^{+0.114}{M}_{\odot }$, radii of $R_A=0.0308_{-0.0025}^{+0.0026}{R}_{\odot }$ and $R_B=0.0291_{-0.0024}^{+0.0032}{R}_{\odot }$, and effective temperatures of $T_A=22200_{-1600}^{+1800}\mathrm{K}$ and $T_B=16200_{-1000}^{+1200}\mathrm{K}$. We determined all of these properties, and the distance to this system, using only photometric measurements, demonstrating a feasible way to estimate parameters for the large population of optically faint ($r>21m_{\mathrm{AB}}$) gravitational-wave sources which the Vera Rubin Observatory (VRO) and LISA should identify.

arXiv comment12 pages, 7 figures, 3 tables, submitted

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