基于Enterprise的广义非线性贝塞尔脉冲星计时
Generalized Non-linear Bayesian Pulsar Timing with Enterprise
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中文总结 AI 辅助
本研究用Enterprise的贝叶斯方法，对4颗脉冲星开展广义非线性贝叶斯计时分析，得到新的脉冲星质量约束，首次发现PSR J2043+1711存在内在红噪声，可更好建模内在噪声与计时参数的相互作用。
中文摘要 AI 辅助
本研究中，我们使用Enterprise软件包中的贝叶斯方法，结合噪声对脉冲星计时模型的完全通用参数化进行研究。我们选取了4颗脉冲星：PSR J1600−3053、PSR J2043+1711、PSR J0740+6620和PSR J1640+2224，通过贝叶斯计时方法展开分析，这些脉冲星虽已被广泛研究，但在贝叶斯计时视角下呈现出有趣特性。利用NANOGrav 12.5年数据发布，我们基于完全通用的非线性贝叶斯计时模型得到新的脉冲星质量约束（中位数及68%置信区间）：PSR J2043+1711的质量为$m_{\rm p}=1.6(1)~\rm M_{\rm \bigodot}$，PSR J1600−3053的质量为$m_{\rm p}=2.3^{+0.9}_{-0.7}~\rm M_{\rm \bigodot}$；利用Fonseca等人2021年的数据，PSR J0740+6620的质量为$m_{\rm p}=2.06(6)~\rm M_{\rm \bigodot}$。我们研究了对计时模型参数施加物理先验的影响，包括对PSR J1640+2224的脉冲星质量设置上限，该脉冲星质量常被估计大于$3~\rm M_{\rm \bigodot}$。我们发现，利用NANOGrav 12.5年数据发布，将PSR J1640+2224的脉冲星质量允许采样空间限制为$m_{\rm p}<3~\rm M_{\rm \bigodot}$时，其质量为$m_{\rm p}=2.2(5)~\rm M_{\rm \bigodot}$。我们首次发现PSR J2043+1711存在内在红噪声的证据，表明完全通用的贝叶斯计时可更好地建模内在噪声与计时参数的相互作用。
英文摘要
In this study, we use the Bayesian methods in the Enterprise package to examine the fully general parameterization of pulsar timing models in tandem with noise. We investigate four pulsars, PSR J1600$-$3053, PSR J2043+1711, PSR J0740+6620, and PSR J1640+2224, through the lens of Bayesian timing. These four are selected as they are well-studied, but exhibit interesting characteristics under the lens of Bayesian timing. Our new pulsar mass constraints (medians and 68\% confidence intervals) for our fully general non-linear Bayesian timing models are $m_{\mathrm{p}}=1.6(1)~\mathrm{M}_{\odot}$ for PSR J2043+1711 and $m_{\mathrm{p}}=2.3^{+0.9}_{-0.7}~\mathrm{M}_{\odot}$ for PSR J1600$-$3053 both using the NANOGrav 12.5-yr data release, and $m_{\mathrm{p}}=2.06(6)~\mathrm{M}_{\odot}$ for PSR J0740+6620 using the data from Fonseca, et al., 2021. We investigate the effects on placing physical priors on timing model parameters, including restricting the upper limit on the pulsar mass for PSR J1640+2224, which has a mass often estimated to be greater than $3~\mathrm{M}_{\odot}$. We find \ark{that restricting the allowed sampling space of the pulsar mass for PSR J1640+2224 to} $m_{\mathrm{p}}<3~\mathrm{M}_{\odot}$ results in a pulsar mass of $m_{\mathrm{p}}=2.2(5)~\mathrm{M}_{\odot}$ for PSR J1640+2224 using the NANOGrav 12.5-yr data release. For the first time, we find evidence for intrinsic red noise in PSR J2043+1711. We show how fully general Bayesian timing can better model the interplay of the intrinsic noise and the timing parameters.
