[논문 리뷰] The NANOGrav 15-year Data Set: Search for Anisotropy in the Gravitational-Wave Background

Gabriella Agazie, Akash Anumarlapudi외 91명|arXiv (Cornell University)|2023. 06. 28.

Pulsars and Gravitational Waves Research인용 수 16

한 줄 요약

이 논문은 NANOGrav 15-year 데이터 세트를 사용하여 나노헤르츠 GWB에서 각방향성 anisotropy를 탐색한 결과를 보고합니다; 유의한 각방향성은 발견되지 않았으며, 95% Bayesian 상한은 (C_l>0 / C_l=0) < 20%이고, 시뮬레이션은 데이터가 예측된 각방향성의 큰 비율에 민감하다는 것을 시사합니다.

ABSTRACT

The North American Nanohertz Observatory for Gravitational Waves (NANOGrav) has reported evidence for the presence of an isotropic nanohertz gravitational wave background (GWB) in its 15 yr dataset. However, if the GWB is produced by a population of inspiraling supermassive black hole binary (SMBHB) systems, then the background is predicted to be anisotropic, depending on the distribution of these systems in the local Universe and the statistical properties of the SMBHB population. In this work, we search for anisotropy in the GWB using multiple methods and bases to describe the distribution of the GWB power on the sky. We do not find significant evidence of anisotropy, and place a Bayesian $95\%$ upper limit on the level of broadband anisotropy such that $(C_{l&gt;0} / C_{l=0}) &lt; 20\%$. We also derive conservative estimates on the anisotropy expected from a random distribution of SMBHB systems using astrophysical simulations conditioned on the isotropic GWB inferred in the 15-yr dataset, and show that this dataset has sufficient sensitivity to probe a large fraction of the predicted level of anisotropy. We end by highlighting the opportunities and challenges in searching for anisotropy in pulsar timing array data.

연구 동기 및 목표

• Motivate and quantify the expectation that a SMBHB-dominated GWB may be anisotropic due to host-galaxy distribution and source properties.
• Describe a comprehensive search for GWB anisotropy using multiple sky-basis representations and Bayesian/frequentist pipelines.
• Provide upper limits on broadband anisotropy and assess the data’s sensitivity to realistic anisotropy levels.
• Contextualize results with astrophysical simulations conditioned on isotropic GWB to interpret implications for SMBHB populations.

제안 방법

• Model GWB anisotropy using radiometer pixel and spherical-harmonic bases to describe the sky power distribution.
• Use a square-root spherical-harmonic basis to enforce positive-definite GWB power and compute angular power spectra C_l.
• Implement Bayesian and frequentist analysis pipelines to assess anisotropy, including comparisons via Hellinger distance between priors and posteriors.
• Represent the overlap reduction function (ORF) with Earth-term and pulsar-term contributions and compute the sky-integrated ORF accordingly.
• Quantify anisotropy with C_l and evaluate broadband anisotropy under a power-law GWB spectrum and a free spectrum approach.

Figure 1: The total and anisotropic signal-to-noise (S/N) ratio derived using the frequentist square-root spherical harmonic basis described in Sec. 2.3 . Both the total and anisotropic S/N start to saturate at an $l_{\rm max}=6$ , which we choose for all the analyses presented in this work.

실험 결과

연구 질문

• RQ1 Is there statistically significant anisotropy in the nanohertz GWB detected by NANOGrav 15-year data?
• RQ2 What are the constraints on the angular power spectrum (C_l) beyond the monopole, given the current PTA sensitivity?
• RQ3 How does the data constrain broadband anisotropy under a GWB power-law model and under a model-agnostic spectrum?
• RQ4 Are the NANOGrav 15-year observations sensitive enough to probe theoretically predicted levels of anisotropy from SMBHB populations?
• RQ5 How do different basis choices (radiometer pixels vs spherical harmonics) compare in capturing potential anisotropy?

주요 결과

• No significant evidence for GWB anisotropy is detected in the NANOGrav 15-year data.
• A Bayesian 95% upper limit on broadband anisotropy is established with (C_l>0 / C_l=0) < 20%.
• Astrophysical simulations conditioned on the isotropic GWB indicate the dataset has sufficient sensitivity to probe a large fraction of the predicted anisotropy.
• The analysis utilizes multiple bases (radiometer pixel and spherical-harmonic, including square-root formulations) and both Bayesian and frequentist pipelines.
• The work highlights opportunities and challenges in continuing to search for anisotropy with pulsar timing arrays.

Figure 2: The normalized square-root of the diagonal elements of the Fisher matrix over 5000 draws from the NMOS cross correlation uncertainties, representing the relative sensitivity of the PTA to anisotropy in different directions on the sky. As expected, the PTA has highest sensitivity in the par