2023ApJ...951L...8A

Query : 2023ApJ...951L...8A

2023ApJ...951L...8A - Astrophys. J., 951, L8 (2023/July-1)

The NANOGrav 15 yr Data Set: Evidence for a Gravitational-wave Background.

AGAZIE G., ANUMARLAPUDI A., ARCHIBALD A.M., ARZOUMANIAN Z., BAKER P.T., BECSY B., BLECHA L., BRAZIER A., BROOK P.R., BURKE-SPOLAOR S., BURNETTE R., CASE R., CHARISI M., CHATTERJEE S., CHATZIIOANNOU K., CHEESEBORO B.D., CHEN S., COHEN T., CORDES J.M., CORNISH N.J., CRAWFORD F., CROMARTIE H.T., CROWTER K., CUTLER C.J., DECESAR M.E., DEGAN D., DEMOREST P.B., DENG H., DOLCH T., DRACHLER B., ELLIS J.A., FERRARA E.C., FIORE W., FONSECA E., FREEDMAN G.E., GARVER-DANIELS N., GENTILE P.A., GERSBACH K.A., GLASER J., GOOD D.C., GULTEKIN K., HAZBOUN J.S., HOURIHANE S., ISLO K., JENNINGS R.J., JOHNSON A.D., JONES M.L., KAISER A.R., KAPLAN D.L., KELLEY L.Z., KERR M., KEY J.S., KLEIN T.C., LAAL N., LAM M.T., LAMB W.G., LAZIO T.J.W., LEWANDOWSKA N., LITTENBERG T.B., LIU T., LOMMEN A., LORIMER D.R., LUO J., LYNCH R.S., MA C.-P., MADISON D.R., MATTSON M.A., McEWEN A., McKEE J.W., McLAUGHLIN M.A., McMANN N., MEYERS B.W., MEYERS P.M., MINGARELLI C.M.F., MITRIDATE A., NATARAJAN P., NG C., NICE D.J., OCKER S.K., OLUM K.D., PENNUCCI T.T., PERERA B.B.P., PETROV P., POL N.S., RADOVAN H.A., RANSOM S.M., RAY P.S., ROMANO J.D., SARDESAI S.C., SCHMIEDEKAMP A., SCHMIEDEKAMP C., SCHMITZ K., SCHULT L., SHAPIRO-ALBERT B.J., SIEMENS X., SIMON J., SIWEK M.S., STAIRS I.H., STINEBRING D.R., STOVALL K., SUN J.P., SUSOBHANAN A., SWIGGUM J.K., TAYLOR J., TAYLOR S.R., TURNER J.E., UNAL C., VALLISNERI M., VAN HAASTEREN R., VIGELAND S.J., WAHL H.M., WANG Q., WITT C.A., YOUNG O. (The NANOGrav Collaboration)

Abstract (from CDS):

We report multiple lines of evidence for a stochastic signal that is correlated among 67 pulsars from the 15 yr pulsar timing data set collected by the North American Nanohertz Observatory for Gravitational Waves. The correlations follow the Hellings-Downs pattern expected for a stochastic gravitational-wave background. The presence of such a gravitational-wave background with a power-law spectrum is favored over a model with only independent pulsar noises with a Bayes factor in excess of 1014, and this same model is favored over an uncorrelated common power-law spectrum model with Bayes factors of 200-1000, depending on spectral modeling choices. We have built a statistical background distribution for the latter Bayes factors using a method that removes interpulsar correlations from our data set, finding p = 10–3 (≈3σ) for the observed Bayes factors in the null no-correlation scenario. A frequentist test statistic built directly as a weighted sum of interpulsar correlations yields p = 5 × 10–5 to 1.9 × 10–4 (≈3.5σ-4σ). Assuming a fiducial f–2/3 characteristic strain spectrum, as appropriate for an ensemble of binary supermassive black hole inspirals, the strain amplitude is ${2.4}_{-0.6}^{+0.7}\times {10}^{-15}$ (median + 90% credible interval) at a reference frequency of 1 yr–1. The inferred gravitational-wave background amplitude and spectrum are consistent with astrophysical expectations for a signal from a population of supermassive black hole binaries, although more exotic cosmological and astrophysical sources cannot be excluded. The observation of Hellings-Downs correlations points to the gravitational-wave origin of this signal.

Abstract Copyright: © 2023. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Gravitational waves - Gravitational wave astronomy - Millisecond pulsars - Radio pulsars - Supermassive black holes

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 J0437-47 Psr 04 37 15.7994581776 -47 15 08.544351636           DC 1032 0
2 PSR J0614-3329 Psr 06 14 10.3479 -33 29 54.116           ~ 134 1
3 PSR J1600-3053 Psr 16 00 51.902514 -30 53 49.45343           ~ 218 0
4 PSR J1643-1224 Psr 16 43 38.16612 -12 24 58.6334           ~ 260 2
5 PSR J1713+0747 Psr 17 13 49.5367813 +07 47 37.450240           ~ 530 1
6 PSR J1903+0327 Psr 19 03 05.7937 +03 27 19.222           ~ 187 1
7 PSR J1909-3744 Psr 19 09 47.42820 -37 44 14.7740           ~ 343 2
8 PSR B1937+21.4 Psr 19 39 38.560096 +21 34 59.13552           ~ 1142 0
9 PSR J2317+1439 Psr 23 17 09.235606 +14 39 31.29559           ~ 211 1

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