2023ApJ...951L..11A

Query : 2023ApJ...951L..11A

2023ApJ...951L..11A - Astrophys. J., 951, L11 (2023/July-1)

The NANOGrav 15 yr Data Set: Search for Signals from New Physics.

AFZAL A., AGAZIE G., ANUMARLAPUDI A., ARCHIBALD A.M., ARZOUMANIAN Z., BAKER P.T., BECSY B., BLANCO-PILLADO J.J., BLECHA L., BODDY K.K., 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., VON ECKARDSTEIN R., FERRARA E.C., FIORE W., FONSECA E., FREEDMAN G.E., GARVER-DANIELS N., GENTILE P.A., GERSBACH K.A., GLASER J., GOOD D.C., GUERTIN L., 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., LAAL N., LAM M.T., LAMB W.G., LAZIO T.J.W., LEE V.S.H., LEWANDOWSKA N., LINO DOS SANTOS R.R., LITTENBERG T.B., LIU T., LORIMER D.R., LUO J., LYNCH R.S., MA C.-P., MADISON D.R., McEWEN A., McKEE J.W., McLAUGHLIN M.A., McMANN N., MEYERS B.W., MEYERS P.M., MINGARELLI C.M.F., MITRIDATE A., NAY J., 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., SCHRODER T., SCHULT L., SHAPIRO-ALBERT B.J., SIEMENS X., SIMON J., SIWEK M.S., STAIRS I.H., STINEBRING D.R., STOVALL K., STRATMANN P., SUN J.P., SUSOBHANAN A., SWIGGUM J.K., TAYLOR J., TAYLOR S.R., TRICKLE T., TURNER J.E., UNAL C., VALLISNERI M., VERMA S., VIGELAND S.J., WAHL H.M., WANG Q., WITT C.A., WRIGHT D., YOUNG O., ZUREK K.M. (The NANOGrav Collaboration)

Abstract (from CDS):

The 15 yr pulsar timing data set collected by the North American Nanohertz Observatory for Gravitational Waves (NANOGrav) shows positive evidence for the presence of a low-frequency gravitational-wave (GW) background. In this paper, we investigate potential cosmological interpretations of this signal, specifically cosmic inflation, scalar-induced GWs, first-order phase transitions, cosmic strings, and domain walls. We find that, with the exception of stable cosmic strings of field theory origin, all these models can reproduce the observed signal. When compared to the standard interpretation in terms of inspiraling supermassive black hole binaries (SMBHBs), many cosmological models seem to provide a better fit resulting in Bayes factors in the range from 10 to 100. However, these results strongly depend on modeling assumptions about the cosmic SMBHB population and, at this stage, should not be regarded as evidence for new physics. Furthermore, we identify excluded parameter regions where the predicted GW signal from cosmological sources significantly exceeds the NANOGrav signal. These parameter constraints are independent of the origin of the NANOGrav signal and illustrate how pulsar timing data provide a new way to constrain the parameter space of these models. Finally, we search for deterministic signals produced by models of ultralight dark matter (ULDM) and dark matter substructures in the Milky Way. We find no evidence for either of these signals and thus report updated constraints on these models. In the case of ULDM, these constraints outperform torsion balance and atomic clock constraints for ULDM coupled to electrons, muons, or gluons.

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

Journal keyword(s): Gravitational waves - Cosmology - Particle astrophysics - Gravitational wave sources

Errata: erratum vol. 971, art. L27 (2024)

Simbad objects: 4

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Number of rows : 4
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 J0614-3329 Psr 06 14 10.3479 -33 29 54.116           ~ 134 1
2 ClG 0657-56 ClG 06 58 26.9 -55 58 21           ~ 1077 1
3 PSR J1909-3744 Psr 19 09 47.42820 -37 44 14.7740           ~ 343 2
4 PSR J2144-3939 Psr 21 44 12.01000 -39 33 58.4000           ~ 145 0

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