2020ApJ...890..108H

Query : 2020ApJ...890..108H

2020ApJ...890..108H - Astrophys. J., 890, 108-108 (2020/February-3)

The NANOGrav 11 yr data set: evolution of gravitational-wave background statistics.

HAZBOUN J.S., SIMON J., TAYLOR S.R., LAM M.T., VIGELAND S.J., ISLO K., KEY J.S., ARZOUMANIAN Z., BAKER P.T., BRAZIER A., BROOK P.R., BURKE-SPOLAOR S., CHATTERJEE S., CORDES J.M., CORNISH N.J., CRAWFORD F., CROWTER K., CROMARTIE H.T., DECESAR M., DEMOREST P.B., DOLCH T., ELLIS J.A., FERDMAN R.D., FERRARA E., FONSECA E., GARVER-DANIELS N., GENTILE P., GOOD D., HOLGADO A.M., HUERTA E.A., JENNINGS R., JONES G., JONES M.L., KAISER A.R., KAPLAN D.L., KELLEY L.Z., LAZIO T.J.W., LEVIN L., LOMMEN A.N., LORIMER D.R., LUO J., LYNCH R.S., MADISON D.R., McLAUGHLIN M.A., McWILLIAMS S.T., MINGARELLI C.M.F., NG C., NICE D.J., PENNUCCI T.T., POL N.S., RANSOM S.M., RAY P.S., SIEMENS X., SPIEWAK R., STAIRS I.H., STINEBRING D.R., STOVALL K., SWIGGUM J., TURNER J.E., VALLISNERI M., VAN HAASTEREN R., WITT C.A., ZHU W.W. (The NANOGrav Collaboration)

Abstract (from CDS):

An ensemble of inspiraling supermassive black hole binaries should produce a stochastic background of very low frequency gravitational waves. This stochastic background is predicted to be a power law, with a gravitational-wave strain spectral index of -2/3, and it should be detectable by a network of precisely timed millisecond pulsars, widely distributed on the sky. This paper reports a new "time slicing" analysis of the 11 yr data release from the North American Nanohertz Observatory for Gravitational Waves (NANOGrav) using 34 millisecond pulsars. Methods to flag potential "false-positive" signatures are developed, including techniques to identify responsible pulsars. Mitigation strategies are then presented. We demonstrate how an incorrect noise model can lead to spurious signals, and we show how independently modeling noise across 30 Fourier components, spanning NANOGrav's frequency range, effectively diagnoses and absorbs the excess power in gravitational-wave searches. This results in a nominal, and expected, progression of our gravitational-wave statistics. Additionally, we show that the first interstellar medium event in PSR J1713+0747 pollutes the common red-noise process with low spectral index noise, and we use a tailored noise model to remove these effects.

Abstract Copyright: © 2020. The American Astronomical Society. All rights reserved.

Journal keyword(s): Millisecond pulsars - Pulsar timing method - Radio pulsars - Red noise - Gravitational waves - Gravitational wave detectors

Simbad objects: 9

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Number of rows : 9
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 PSR J0030+0451 Psr 00 30 27.42348 +04 51 39.7144           ~ 596 1
2 PSR B0613-02.0 Psr 06 13 43.977070 -02 00 47.34294           ~ 319 1
3 PSR J1640+2224 Psr 16 40 16.744850 +22 24 08.84119           ~ 210 0
4 PSR J1713+0747 Psr 17 13 49.5367813 +07 47 37.450240           ~ 530 1
5 PSR B1855+09 Psr 18 57 36.390620 +09 43 17.20712           DA 569 1
6 PSR J1909-3744 Psr 19 09 47.42820 -37 44 14.7740           ~ 343 2
7 PSR B1937+21.4 Psr 19 39 38.560096 +21 34 59.13552           ~ 1142 0
8 PSR J2043+1711 Psr 20 43 20.8828 +17 11 28.941           ~ 129 1
9 PSR J2317+1439 Psr 23 17 09.235606 +14 39 31.29559           ~ 211 1

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