A NICER VIEW OF PSR J0030+0451: MILLISECOND PULSAR PARAMETER ESTIMATION

A NICER VIEW OF PSR J0030+0451: MILLISECOND PULSAR PARAMETER ESTIMATION

2019 December 12 | T. E. Riley, A. L. Watts, S. Bogdanov, P. S. Ray, R. M. Ludlam, S. Guillot, Z. Arzoumanian, C. L. Baker, A. V. Bilous, D. Chakrabarty, K. C. Gendreau, A. K. Harding, W. C. G. Ho, J. M. Lattimer, S. M. Morsink, and T. E. Strohmayer
This paper presents a Bayesian parameter estimation of the millisecond pulsar PSR J0030+0451, focusing on its mass and equatorial radius. The analysis is based on pulse-profile modeling of Neutron Star Interior Composition Explorer (NICER) X-ray spectral-timing event data, which involves relativistic ray-tracing of thermal emission from hot regions on the pulsar's surface. The study explores various configurations of these hot regions, including their shapes and temperatures, and uses the X-PSI software package for Bayesian modeling. The results indicate that both hot regions are located in the same rotational hemisphere, with one being a small circular spot and the other a narrow arc. The inferred mass and equatorial radius are $1.34^{+0.15}_{-0.16} \, \text{M}_\odot$ and $12.71^{+1.14}_{-1.14} \, \text{km}$, respectively, with a compactness of $0.156^{+0.008}_{-0.010}$. The paper also discusses the implications of these findings for understanding dense matter, pulsar emission mechanisms, and stellar evolution.This paper presents a Bayesian parameter estimation of the millisecond pulsar PSR J0030+0451, focusing on its mass and equatorial radius. The analysis is based on pulse-profile modeling of Neutron Star Interior Composition Explorer (NICER) X-ray spectral-timing event data, which involves relativistic ray-tracing of thermal emission from hot regions on the pulsar's surface. The study explores various configurations of these hot regions, including their shapes and temperatures, and uses the X-PSI software package for Bayesian modeling. The results indicate that both hot regions are located in the same rotational hemisphere, with one being a small circular spot and the other a narrow arc. The inferred mass and equatorial radius are $1.34^{+0.15}_{-0.16} \, \text{M}_\odot$ and $12.71^{+1.14}_{-1.14} \, \text{km}$, respectively, with a compactness of $0.156^{+0.008}_{-0.010}$. The paper also discusses the implications of these findings for understanding dense matter, pulsar emission mechanisms, and stellar evolution.
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[slides and audio] A NICER View of PSR J0030%2B0451%3A Millisecond Pulsar Parameter Estimation