Early Advanced LIGO binary neutron-star sky localization and parameter estimation

11th Edoardo Amaldi Conference on Gravitational Waves

Berry, C.P.L.^1 ; Farr, B.^2 ; Farr, W.M.^1 ; Haster, C.-J.^1 ; Mandel, I.^1 ; Middleton, H.^1 ; Singer, L.P.^3 ; Urban, A.L.^4 ; Vecchio, A.^1 ; Vitale, S.^1 ; Cannon, K.^6,7,8,9 ; Graff, P.B.^7,8 ; Hanna, C.^9,10 ; Mohapatra, S.^5,11 ; Pankow, C.^4 ; Price, L.R.^12 ; Sidery, T.^1 ; Veitch, J.^1

School of Physics and Astronomy, University of Birmingham, Birmingham

B15 2TT, United Kingdom^1

Enrico Fermi Institute, University of Chicago, Chicago

IL

60637, United States^2

Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt

MD

20771, United States^3

Leonard E. Parker Center for Gravitation, Cosmology and Astrophysics, University of Wisconsin-Milwaukee, Milwaukee

WI

53201, United States^4

Massachusetts Institute of Technology, 185 Albany St, Cambridge

MA

02139, United States^5

Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto

ON

M5S 3H8, Canada^6

Department of Physics, University of Maryland-College Park, College Park

MD

20742, United States^7

Gravitational Astrophysics Lab, NASA Goddard Space Flight Center, Greenbelt

MD

20771, United States^8

Perimeter Institute for Theoretical Physics, Ontario

N2L 2Y5, Canada

(10) Pennsylvania State University, University Park

PA

16802, United States

(11) Syracuse University, Syracuse

NY

13244, United States

(12) LIGO Laboratory, California Institute of Technology, Pasadena

CA

91125, United States^9

关键词: Accuracy of parameters;    Advanced detector;    Binary neutron stars;    Follow up;    Ground based;    GW detectors;    Measurements of;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/716/1/012031/pdf
DOI  :  10.1088/1742-6596/716/1/012031

来源: IOP

【 摘 要 】

2015 will see the first observations of Advanced LIGO and the start of the gravitational-wave (GW) advanced-detector era. One of the most promising sources for ground- based GW detectors are binary neutron-star (BNS) coalescences. In order to use any detections for astrophysics, we must understand the capabilities of our parameter-estimation analysis. By simulating the GWs from an astrophysically motivated population of BNSs, we examine the accuracy of parameter inferences in the early advanced-detector era. We find that sky location, which is important for electromagnetic follow-up, can be determined rapidly (∼ 5 s), but that sky areas may be hundreds of square degrees. The degeneracy between component mass and spin means there is significant uncertainty for measurements of the individual masses and spins; however, the chirp mass is well measured (typically better than 0.1%).