European Pulsar Timing Array Limits on Continuous Gravitational Waves from Individual Supermassive Black Hole Binaries
European Pulsar Timing Array Limits on Continuous Gravitational Waves from Individual Supermassive Black Hole Binaries
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DOI：
10.1093/mnras/stv2092
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发表时间：
2015-09
影响因子：
4.8
通讯作者：
S. Babak;A. Petiteau;A. Sesana;P. Brem;P. Rosado;S. Taylor;A. Lassus;J. Hessels;C. Bassa;M. Burgay;R. N. Caballero;D. Champion;I. Cognard;G. Desvignes;J. Gair;L. Guillemot;G. Janssen;R. Karuppusamy;M. Kramer;P. Lazarus;K. Lee;L. Lentati;Kuo Liu;C. Mingarelli;S. Osłowski;D. Perrodin;A. Possenti;M. Purver;S. Sanidas;R. Smits;B. Stappers;G. Theureau;C. Tiburzi;R. V. Haasteren;A. Vecchio;J. Verbiest
中科院分区：
文献类型：
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作者：
S. Babak;A. Petiteau;A. Sesana;P. Brem;P. Rosado;S. Taylor;A. Lassus;J. Hessels;C. Bassa;M. Burgay;R. N. Caballero;D. Champion;I. Cognard;G. Desvignes;J. Gair;L. Guillemot;G. Janssen;R. Karuppusamy;M. Kramer;P. Lazarus;K. Lee;L. Lentati;Kuo Liu;C. Mingarelli;S. Osłowski;D. Perrodin;A. Possenti;M. Purver;S. Sanidas;R. Smits;B. Stappers;G. Theureau;C. Tiburzi;R. V. Haasteren;A. Vecchio;J. Verbiest
我们已经在最新的欧洲脉冲星定时阵列（EPTA）数据集中搜索了由单独可分辨的圆形超大质量黑洞双星（SMBHB）产生的连续引力波（CGW）信号，该数据集由41 ms脉冲星的超精确定时数据组成。我们开发频率论和贝叶斯检测算法来搜索单色和频率演化系统。所采用的算法没有证据表明存在这样一个CGW信号，表明数据是最好的描述脉冲星和辐射计噪声。根据所采用的探测算法，天空平均应变振幅的95%上限位于6 × 10−15 10^9M外至约25 Mpc距离的范围内，当Mc > 10^10M外至约1Gpc（z = 0.2）距离时。我们发现，最先进的SMBHB群体模型预测，使用当前EPTA数据集检测CGW的概率<1%，与报告的未检测一致。然而，我们强调，PTA对个人CGW的限制在过去五年中几乎提高了一个数量级。脉冲星定时数据获取和分析技术的不断进步将使附近的SMBHB的人口在康宁年强大的天体物理约束。
We have searched for continuous gravitational wave (CGW) signals produced by individually resolvable, circular supermassive black hole binaries (SMBHBs) in the latest European Pulsar Timing Array (EPTA) data set, which consists of ultraprecise timing data on 41-ms pulsars. We develop frequentist and Bayesian detection algorithms to search both for monochromatic and frequency-evolving systems. None of the adopted algorithms show evidence for the presence of such a CGW signal, indicating that the data are best described by pulsar and radiometer noise only. Depending on the adopted detection algorithm, the 95 per cent upper limit on the sky-averaged strain amplitude lies in the range 6 × 10−15 10^9M⊙ out to a distance of about 25 Mpc, and with Mc > 10^10M⊙ out to a distance of about 1Gpc (z ≈ 0.2). We show that state-of-the-art SMBHB population models predict <1 per cent probability of detecting a CGW with the current EPTA data set, consistent with the reported non-detection. We stress, however, that PTA limits on individual CGW have improved by almost an order of magnitude in the last five years. The continuing advances in pulsar timing data acquisition and analysis techniques will allow for strong astrophysical constraints on the population of nearby SMBHBs in the corning years.