多信使光谱学
Multimessenger Spectroscopy
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中文总结 AI 辅助
本文提出一种多信使方法，利用LISA引力波数据预测双白矮星双星的轨道相位，以调度光学光谱观测，从而无偏地测量质量并预测相位精度。
中文摘要 AI 辅助
我们开发了一种多信使方法，用于根据激光干涉空间天线（LISA）的数据调度超紧凑双白矮星双星的光学光谱观测。从引力波（GW）信号推断出的轨道参数被用来预测纬度辐角 $u(t)$，它决定了径向速度的相位依赖性。由于 $u(t)$ 可以提前得知，光谱可以在选定的轨道相位处获取。引力波和光谱描述通过 $u(t)=\Phi_{\rm GW}(t)/2+\delta_{e,\omega}(t)+\mathcal{O}(e^2)$ 联系起来，其中 $\Phi_{\rm GW}$ 是引力波相位，$e$ 是偏心率，$\delta_{e,\omega}$ 是中心方程到 $\mathcal{O}(e)$ 阶，对于圆轨道该项为零。径向速度对 $\cos u$ 进行回归；对于双线双星，两个斜率决定了半振幅 $K_1$ 和 $K_2$。利用LISA测量的倾角和轨道周期，通过开普勒第三定律，两个分量质量都可由半振幅得出，由此得到的啁啾质量与引力波振幅一起给出源的距离。我们推导了拉普拉斯-拉格朗日参数一阶的波形；当 $e\to0$ 时，恢复圆形四极波形。使用一个圆形和一个偏心系统的模拟LISA数据，我们预测了 $u(t)$ 在足够精度下可用于相位分辨光谱的时间长度。由速度振幅推导出的质量避免了仅使用 $\dot f_{\rm GW}$ 时潮汐、质量转移或视线方向加速度引入的偏差。对于四年的LISA观测，在观测结束后大约十年内，在方照点进行调度仍然是可行的。观测中点四年后，星历表预测的轨道相位对于偏心系统为 $0.3$ 秒，对于圆形系统为 $0.9$ 秒，而光学星历表在同一基线传播的预测误差为 $1$ 至 $30$ 秒。
英文摘要
A multimessenger method is developed for scheduling optical spectroscopy of ultracompact double white dwarf binaries from Laser Interferometer Space Antenna (LISA) data. The orbital parameters inferred from the gravitational wave (GW) signal are used to predict the argument of latitude $u(t)$, which sets the phase dependence of the radial velocity. With $u(t)$ known in advance, spectra can be taken at selected orbital phases. The GW and spectroscopic descriptions are linked by $u(t)=Φ_{\rm GW}(t)/2+δ_{e,ω}(t)+\mathcal{O}(e^2)$, where $Φ_{\rm GW}$ is the GW phase, $e$ the eccentricity, and $δ_{e,ω}$ the equation of the centre to $\mathcal{O}(e)$, which vanishes for a circular orbit. Radial velocities are regressed on $\cos u$; for double-lined binaries, the two slopes determine the semi-amplitudes $K_1$ and $K_2$. With the inclination and orbital period measured by LISA, both component masses follow from the semi-amplitudes through Kepler's third law, and the resulting chirp mass with the GW amplitude gives the source distance. We derive waveforms to first order in the Laplace--Lagrange parameters; the circular quadrupole waveform is recovered as $e\to0$. Using simulated LISA data for one circular and one eccentric system, we forecast how long $u(t)$ remains accurate enough for phase-resolved spectroscopy. Masses derived from the velocity amplitudes are free of the biases that tides, mass transfer, or acceleration along the line of sight introduce when $\dot f_{\rm GW}$ alone is used. For a four-year LISA observation, scheduling at quadrature remains viable for roughly a decade after the observation ends. Four years after the observation midpoint, the ephemeris predicts the orbital phase to $0.3$~s for the eccentric system and $0.9$~s for the circular one, compared with $1$--$30$~s for optical ephemerides propagated over the same baseline.
发表机构
- Deutsches Zentrum für Astrophysik (DZA)（德国天体物理中心）
- Max-Planck-Institut für Radioastronomie (MPIfR)（马克斯·普朗克射电天文研究所）
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