2019ApJ...880..116A


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.17CEST00:53:38

2019ApJ...880..116A - Astrophys. J., 880, 116-116 (2019/August-1)

The NANOGrav 11 yr data set: limits on Gravitational Waves from individual supermassive black hole binaries.

AGGARWAL K., ARZOUMANIAN Z., BAKER P.T., BRAZIER A., BRINSON M.R., 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., HAZBOUN J.S., HOLGADO A.M., HUERTA E.A., ISLO K., JENNINGS R., JONES G., JONES M.L., KAISER A.R., KAPLAN D.L., KELLEY L.Z., KEY J.S., LAM M.T., LAZIO T.J.W., LEVIN L., 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., SIMON J., SPIEWAK R., STAIRS I.H., STINEBRING D.R., STOVALL K., SWIGGUM J., TAYLOR S.R., TURNER J.E., VALLISNERI M., VAN HAASTEREN R., VIGELAND S.J., WITT C.A., ZHU W.W. (The NANOGrav Collaboration)

Abstract (from CDS):

Observations indicate that nearly all galaxies contain supermassive black holes at their centers. When galaxies merge, their component black holes form SMBH binaries (SMBHBs), which emit low-frequency gravitational waves (GWs) that can be detected by pulsar timing arrays. We have searched the North American Nanohertz Observatory for Gravitational Waves 11 yr data set for GWs from individual SMBHBs in circular orbits. As we did not find strong evidence for GWs in our data, we placed 95% upper limits on the strength of GWs from such sources. At fgw = 8 nHz, we placed a sky-averaged upper limit of h0 < 7.3(3) x 10–15. We also developed a technique to determine the significance of a particular signal in each pulsar using "dropout" parameters as a way of identifying spurious signals. From these upper limits, we ruled out SMBHBs emitting GWs with fgw = 8 nHz within 120 Mpc for M =109M, and within 5.5 Gpc for M =1010M at our most sensitive sky location. We also determined that there are no SMBHBs with M > 1.6×109M emitting GWs with fgw = 2.8-317.8 nHz in the Virgo Cluster. Finally, we compared our strain upper limits to simulated populations of SMBHBs, based on galaxies in the Two Micron All-Sky Survey and merger rates from the Illustris cosmological simulation project, and found that only 34 out of 75,000 realizations of the local universe contained a detectable source.

Abstract Copyright: © 2019. The American Astronomical Society. All rights reserved.

Journal keyword(s): gravitational waves - pulsars: general - quasars: supermassive black holes

Simbad objects: 45

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Number of rows : 45

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 PSR J0023+09 Psr 00 23 16.890 +09 23 24.18           ~ 63 0
2 PSR J0030+0451 Psr 00 30 27.4277 +04 51 39.710           ~ 193 1
3 UGC 1841 Sy1 02 23 11.41124 +42 59 31.3840   15.71 14.81     ~ 524 2
4 ACO S 373 ClG 03 38 30 -35 27.3           ~ 1489 0
5 PSR J0340+41 Psr 03 40 23.2887 +41 30 45.300           ~ 47 0
6 PSR B0613-02.0 Psr 06 13 43.9759 -02 00 47.228           ~ 192 1
7 PSR J0645+5158 Psr 06 45 59.08191 +51 58 14.9210           ~ 24 0
8 QSO J0854+2006 BLL 08 54 48.8749311881 +20 06 30.642936668   15.91 15.43 15.56   ~ 1943 1
9 2MASSI J1000218+223318 Sy2 10 00 21.8027253239 +22 33 18.642206446   18.30 18 17   ~ 76 2
10 NGC 3115 GiG 10 05 13.978 -07 43 06.89   11   9.37   ~ 902 2
11 PSR J1012+5307 Psr 10 12 33.4341531837 +53 07 02.564526788     19.5     DA 308 1
12 PSR J1024-0719 Psr 10 24 38.697 -07 19 19.07           ~ 176 0
13 NGC 4151 Sy1 12 10 32.5771747733 +39 24 21.057727323   12.18 11.48     ~ 3305 2
14 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5642 0
15 M 49 Sy2 12 29 46.798 +08 00 01.48   13.21 12.17     ~ 1923 2
16 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6023 3
17 M 60 GiP 12 43 40.008 +11 33 09.40   10.3       ~ 1222 0
18 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4096 2
19 PSR J1455-3300 Psr 14 55 47.9624 -33 30 46.360           ~ 106 1
20 PSR J1600-3053 Psr 16 00 51.90403 -30 53 49.3190           ~ 112 0
21 PSR J1614-2230 Psr 16 14 36.5070 -22 30 31.207           ~ 250 1
22 PSR J1640+2224 Psr 16 40 16.74231 +22 24 08.9413           ~ 124 0
23 PSR J1643-1224 Psr 16 43 38.15583 -12 24 58.7200           ~ 153 1
24 PSR J1713+0447 Psr 17 13 49.53053 +07 47 37.5264           ~ 347 1
25 PSR J1738+0333 Psr 17 38 53.96317 +03 33 10.8390           ~ 108 1
26 PSR J1741+1351 Psr 17 41 32 +13 51.3           ~ 59 0
27 PSR J1744-1134 Psr 17 44 29.4103 -11 34 54.727           ~ 196 1
28 1FGL J1747.4-4035 gam 17 47 29.000 -40 36 00.00           ~ 41 0
29 PSR J1853+1303 Psr 18 53 57.3183 +13 03 44.088           ~ 62 1
30 PSR B1855+09 Psr 18 57 36.39161 +09 43 17.2322           DA 470 1
31 PSR J1903+0327 Psr 19 03 05.7937 +03 27 19.222           ~ 119 1
32 PSR J1909-3744 Psr 19 09 47.43788 -37 44 14.3240           ~ 187 2
33 PSR J1910+1256 Psr 19 10 09.7004 +12 56 25.528           ~ 54 1
34 PSR J1918-0642 Psr 19 18 48.0363 -06 42 34.800           ~ 65 0
35 PSR J1923+2515 Psr 19 23 22.494560 +25 15 40.64360           ~ 24 0
36 PSR B1937+21 Psr 19 39 39.6 +21 37 22           ~ 934 2
37 PSR J1944+0907 Psr 19 44 09.32 +09 07 23.2           ~ 31 1
38 PSR B1953+29 Psr 19 55 27.8757 +29 08 43.530           ~ 259 1
39 PSR J2010-1323 Psr 20 10 45.9196 -13 23 56.027           ~ 42 0
40 PSR J2017+0603 Psr 20 17 22.7048 +06 03 05.585           ~ 72 1
41 PSR J2043+1711 Psr 20 43 20.8828 +17 11 28.941           ~ 67 1
42 PSR B2145-07.8 Psr 21 45 50.47 -07 50 18.3           ~ 211 0
43 PSR J2214+3000 Psr 22 14 38.8480 +30 00 38.209           ~ 71 0
44 PSR J2302+4442 Psr 23 02 46.9789 +44 42 22.102           ~ 70 0
45 PSR J2317+1439 Psr 23 17 09.230 +14 39 31.18           ~ 138 1

    Equat.    Gal    SGal    Ecl

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2019.10.17-00:53:38

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