2024ApJ...966..105A

Query : 2024ApJ...966..105A

2024ApJ...966..105A - Astrophys. J., 966, 105 (2024/May-1)

Comparing Recent Pulsar Timing Array Results on the Nanohertz Stochastic Gravitational-wave Background.

AGAZIE G., ANTONIADIS J., ANUMARLAPUDI A., ARCHIBALD A.M., ARUMUGAM P., ARUMUGAM S., ARZOUMANIAN Z., ASKEW J., BABAK S., BAGCHI M., BAILES M., BAK NIELSEN A.-S., BAKER P.T., BASSA C.G., BATHULA A., BECSY B., BERTHEREAU A., BHAT N.D.R., BLECHA L., BONETTI M., BORTOLAS E., BRAZIER A., BROOK P.R., BURGAY M., BURKE-SPOLAOR S., BURNETTE R., CABALLERO R.N., CAMERON A., CASE R., CHALUMEAU A., CHAMPION D.J., CHANLARIDIS S., CHARISI M., CHATTERJEE S., CHATZIIOANNOU K., CHEESEBORO B.D., CHEN S., CHEN Z.-C., COGNARD I., COHEN T., COLES W.A., CORDES J.M., CORNISH N.J., CRAWFORD F., CROMARTIE H.T., CROWTER K., CURYLO M., CUTLER C.J., DAI S., DANDAPAT S., DEB D., DECESAR M.E., DEGAN D., DEMOREST P.B., DENG H., DESAI S., DESVIGNES G., DEY L., DHANDA-BATRA N., DI MARCO V., DOLCH T., DRACHLER B., DWIVEDI C., ELLIS J.A., FALXA M., FENG Y., FERDMAN R.D., FERRARA E.C., FIORE W., FONSECA E., FRANCHINI A., FREEDMAN G.E., GAIR J.R., GARVER-DANIELS N., GENTILE P.A., GERSBACH K.A., GLASER J., GOOD D.C., GONCHAROV B., GOPAKUMAR A., GRAIKOU E., GRIESSMEIER J.-M., GUILLEMOT L., GULTEKIN K., GUO Y.J., GUPTA Y., GRUNTHAL K., HAZBOUN J.S., HISANO S., HOBBS G.B., HOURIHANE S., HU H., IRACI F., ISLO K., IZQUIERDO-VILLALBA D., JANG J., JAWOR J., JANSSEN G.H., JENNINGS R.J., JESSNER A., JOHNSON A.D., JONES M.L., JOSHI B.C., KAISER A.R., KAPLAN D.L., KAPUR A., KAREEM F., KARUPPUSAMY R., KEANE E.F., KEITH M.J., KELLEY L.Z., KERR M., KEY J.S., KHARBANDA D., KIKUNAGA T., KLEIN T.C., KOLHE N., KRAMER M., KRISHNAKUMAR M.A., KULKARNI A., LAAL N., LACKEOS K., LAM M.T., LAMB W.G., LARSEN B.B., LAZIO T.J.W., LEE K.J., LEVIN Y., LEWANDOWSKA N., LITTENBERG T.B., LIU K., LIU T., LIU Y., LOMMEN A., LORIMER D.R., LOWER M.E., LUO J., LUO R., LYNCH R.S., LYNE A.G., MA C.-P., MAAN Y., MADISON D.R., MAIN R.A., MANCHESTER R.N., MANDOW R., MATTSON M.A., McEWEN A., McKEE J.W., McLAUGHLIN M.A., McMANN N., MEYERS B.W., MEYERS P.M., MICKALIGER M.B., MILES M., MINGARELLI C.M.F., MITRIDATE A., NATARAJAN P., NATHAN R.S., NG C., NICE D.J., NITU I.C., NOBLESON K., OCKER S.K., OLUM K.D., OSLOWSKI S., PALADI A.K., PARTHASARATHY A., PENNUCCI T.T., PERERA B.B.P., PERRODIN D., PETITEAU A., PETROV P., POL N.S., PORAYKO N.K., POSSENTI A., PRABU T., QUELQUEJAY-LECLERE H., RADOVAN H.A., RANA P., RANSOM S.M., RAY P.S., REARDON D.J., ROGERS A.F., ROMANO J.D., RUSSELL C.J., SAMAJDAR A., SANIDAS S.A., SARDESAI S.C., SCHMIEDEKAMP A., SCHMIEDEKAMP C., SCHMITZ K., SCHULT L., SESANA A., SHAIFULLAH G., SHANNON R.M., SHAPIRO-ALBERT B.J., SIEMENS X., SIMON J., SINGHA J., SIWEK M.S., SPERI L., SPIEWAK R., SRIVASTAVA A., STAIRS I.H., STAPPERS B.W., STINEBRING D.R., STOVALL K., SUN J.P., SURNIS M., SUSARLA S.C., SUSOBHANAN A., SWIGGUM J.K., TAKAHASHI K., TARAFDAR P., TAYLOR J., TAYLOR S.R., THEUREAU G., THRANE E., THYAGARAJAN N., TIBURZI C., TOOMEY L., TURNER J.E., UNAL C., VALLISNERI M., VAN DER WATEREN E., VAN HAASTEREN R., VECCHIO A., VENKATRAMAN KRISHNAN V., VERBIEST J.P.W., VIGELAND S.J., WAHL H.M., WANG S., WANG Q., WITT C.A., WANG J., WANG L., WAYT K.E., WU Z., YOUNG O., ZHANG L., ZHANG S., ZHU X.-J., ZIC A. (The International Pulsar Timing Array Collaboration)

Abstract (from CDS):

The Australian, Chinese, European, Indian, and North American pulsar timing array (PTA) collaborations recently reported, at varying levels, evidence for the presence of a nanohertz gravitational-wave background (GWB). Given that each PTA made different choices in modeling their data, we perform a comparison of the GWB and individual pulsar noise parameters across the results reported from the PTAs that constitute the International Pulsar Timing Array (IPTA). We show that despite making different modeling choices, there is no significant difference in the GWB parameters that are measured by the different PTAs, agreeing within 1σ. The pulsar noise parameters are also consistent between different PTAs for the majority of the pulsars included in these analyses. We bridge the differences in modeling choices by adopting a standardized noise model for all pulsars and PTAs, finding that under this model there is a reduction in the tension in the pulsar noise parameters. As part of this reanalysis, we “extended” each PTA's data set by adding extra pulsars that were not timed by that PTA. Under these extensions, we find better constraints on the GWB amplitude and a higher signal-to-noise ratio for the Hellings-Downs correlations. These extensions serve as a prelude to the benefits offered by a full combination of data across all pulsars in the IPTA, i.e., the IPTA's Data Release 3, which will involve not just adding in additional pulsars but also including data from all three PTAs where any given pulsar is timed by more than a single PTA.

Abstract Copyright: © 2024. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Gravitational waves - Pulsars

Simbad objects: 30

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Number of rows : 30
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 J0437-47 Psr 04 37 15.7994581776 -47 15 08.544351636           DC 1032 0
3 PSR B0613-02.0 Psr 06 13 43.977070 -02 00 47.34294           ~ 319 1
4 PSR J0614-3329 Psr 06 14 10.3479 -33 29 54.116           ~ 134 1
5 PSR J0900-3144 Psr 09 00 43.95220 -31 44 30.8722           ~ 68 0
6 PSR J1012+5307 Psr 10 12 33.4345449600 +53 07 02.548542576     19.5     DA 419 1
7 PSR J1022+10 Psr 10 22 57.990 +10 01 52.92           ~ 279 2
8 PSR J1025-07 Psr 10 24 38.6991893112 -07 19 19.045523388     19.81 18.78 18.00 ~ 286 1
9 PSR J1455-3300 Psr 14 55 47.976991 -33 30 46.40280           ~ 165 1
10 PSR J1600-3053 Psr 16 00 51.902514 -30 53 49.45343           ~ 218 0
11 PSR J1640+2224 Psr 16 40 16.744850 +22 24 08.84119           ~ 210 0
12 PSR J1643-1224 Psr 16 43 38.16612 -12 24 58.6334           ~ 260 2
13 PSR J1713+0747 Psr 17 13 49.5367813 +07 47 37.450240           ~ 530 1
14 PSR J1730-2304 Psr 17 30 21.68471 -23 04 31.2590           ~ 194 1
15 PSR J1738+0333 Psr 17 38 53.966386 +03 33 10.87200           ~ 191 1
16 PSR J1741+1351 Psr 17 41 31.1499024 +13 51 44.279709           ~ 122 0
17 PSR J1744-1134 Psr 17 44 29.4220844 -11 34 54.801320           ~ 323 1
18 PSR J1751-2857 Psr 17 51 32.686848 -28 57 46.57130           ~ 65 1
19 PSR J1832-0836 Psr 18 32 27.589497 -08 36 55.14540           ~ 86 0
20 PSR J1843-1113 Psr 18 43 41.260405 -11 13 31.10310           ~ 86 0
21 PSR B1855+09 Psr 18 57 36.390620 +09 43 17.20712           DA 569 1
22 PSR J1902-5105 Psr 19 02 02.8476 -51 05 56.969           ~ 64 0
23 PSR J1909-3744 Psr 19 09 47.42820 -37 44 14.7740           ~ 343 2
24 PSR J1910+1256 Psr 19 10 09.701454 +12 56 25.48680           ~ 108 1
25 PSR J1911+1347 Psr 19 11 55.204694 +13 47 34.38383           ~ 72 0
26 PSR J1918-0642 Psr 19 18 48.027685 -06 42 34.95735           ~ 146 0
27 PSR B1937+21.4 Psr 19 39 38.560096 +21 34 59.13552           ~ 1142 0
28 PSR J2124-3358 Psr 21 24 43.834930 -33 58 45.49195           ~ 337 1
29 PSR B2145-07.8 Psr 21 45 50.45590 -07 50 18.5900           ~ 336 0
30 PSR J2322+2057 Psr 23 22 22.320041 +20 57 02.50080           ~ 129 1

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