2024A&A...690A.118E

Query : 2024A&A...690A.118E

2024A&A...690A.118E - Astronomy and Astrophysics, volume 690A118 (2024/10-1)

The second data release from the European Pulsar Timing Array V. Search for continuous gravitational wave signals.

EPTA COLLABORATION AND INPTA COLLABORATION, ANTONIADIS J., ARUMUGAM P., ARUMUGAM S., BABAK S., BAGCHI M., BAK NIELSEN A.-S., BASSA C.G., BATHULA A., BERTHEREAU A., BONETTI M., BORTOLAS E., BROOK P.R., BURGAY M., CABALLERO R.N., CHALUMEAU A., CHAMPION D.J., CHANLARIDIS S., CHEN S., COGNARD I., DANDAPAT S., DEB D., DESAI S., DESVIGNES G., DHANDA-BATRA N., DWIVEDI C., FALXA M., FERRANTI I., FERDMAN R.D., FRANCHINI A., GAIR J.R., GONCHAROV B., GOPAKUMAR A., GRAIKOU E., GRIESSMEIER J.-M., GUILLEMOT L., GUO Y.J., GUPTA Y., HISANO S., HU H., IRACI F., IZQUIERDO-VILLALBA D., JANG J., JAWOR J., JANSSEN G.H., JESSNER A., JOSHI B.C., KAREEM F., KARUPPUSAMY R., KEANE E.F., KEITH M.J., KHARBANDA D., KIKUNAGA T., KOLHE N., KRAMER M., KRISHNAKUMAR M.A., LACKEOS K., LEE K.J., LIU K., LIU Y., LYNE A.G., McKEE J.W., MAAN Y., MAIN R.A., MANZINI S., MICKALIGER M.B., NITU I.C., NOBLESON K., PALADI A.K., PARTHASARATHY A., PERERA B.B.P., PERRODIN D., PETITEAU A., PORAYKO N.K., POSSENTI A., PRABU T., QUELQUEJAY LECLERE H., RANA P., SAMAJDAR A., SANIDAS S.A., SESANA A., SHAIFULLAH G., SINGHA J., SPERI L., SPIEWAK R., SRIVASTAVA A., STAPPERS B.W., SURNIS M., SUSARLA S.C., SUSOBHANAN A., TAKAHASHI K., TARAFDAR P., THEUREAU G., TIBURZI C., VAN DER WATEREN E., VECCHIO A., VENKATRAMAN KRISHNAN V., VERBIEST J.P.W., WANG J., WANG L. and WU Z.

Abstract (from CDS):

We present the results of a search for continuous gravitational wave signals (CGWs) in the second data release (DR2) of the European Pulsar Timing Array (EPTA) Collaboration. The most significant candidate event from this search has a gravitational wave frequency of 4-5 nHz. Such a signal could be generated by a supermassive black hole binary (SMBHB) in the local Universe. We present the results of a follow-up analysis of this candidate using both Bayesian and frequentist methods. The Bayesian analysis gives a Bayes factor of 4 in favour of the presence of the CGW over a common uncorrelated noise process. In contrast, the frequentist analysis estimates the p-value of the candidate to be < 1%, also assuming the presence of common uncorrelated red noise. However, comparing a model that includes both a CGW and a gravitational wave background (GWB) to a GWB only, the Bayes factor in favour of the CGW model is only 0.7. Therefore, we cannot conclusively determine the origin of the observed feature, nor can we rule it out as a CGW source. We present results of simulations that demonstrate that data containing a weak gravitational wave background can be misinterpreted as data including a CGW and vice versa, providing two plausible explanations for the EPTA DR2 data. Further investigations combining data from all PTA collaborations will be needed to reveal the true origin of this feature.

Abstract Copyright: © The Authors 2024

Journal keyword(s): gravitational waves - methods: data analysis - pulsars: general

Simbad objects: 4

Full paper

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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	Sp type	#ref 1850 - 2026	#notes
1	NGC 1316	rG	03 22 41.789	-37 12 29.52	9.81	9.15	8.53	7.66	~	1491	1
2	ACO S 373	ClG	03 38 29.4	-35 27 08					~	2029	0
3	NAME Virgo Cluster	ClG	12 30 47.8	+12 23 07					~	7107	0
4	PSR J1713+0747	Psr	17 13 49.5367813	+07 47 37.450240					~	530	1

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