Single-Source Gravitational Wave Limits From the J1713+0747 24-hr Global Campaign

11th Edoardo Amaldi Conference on Gravitational Waves

Dolch, T.^1,2 ; Ellis, J.A.^3 ; Chatterjee, S.^1 ; Cordes, J.M.^2 ; Lam, M.T.^2 ; Bassa, C.^4,5 ; Bhattacharyya, B.^5 ; Champion, D.J.^6 ; Cognard, I.^7,23 ; Crowter, K.^8 ; Demorest, P.B.^9 ; Hessels, J.W.T.^4,10 ; Janssen, G.^4 ; Jenet, F.A.^11 ; Jones, G.^12 ; Jordan, C.^5 ; Karuppusamy, R.^6 ; Keith, M.^5 ; Kondratiev, V.I.^4,13 ; Kramer, M.^6,14 ; Lazarus, P.^6 ; Lazio, T.J.W.^3 ; Lorimer, D.R.^15 ; Madison, D.R.^2,16 ; McLaughlin, M.A.^15 ; Palliyaguru, N.^15 ; Perrodin, D.^17 ; Ransom, S.M.^16 ; Roy, J.^5,18 ; Shannon, R.M.^19 ; Smits, R.^4 ; Stairs, I.H.^8 ; Stappers, B.W.^5 ; Stinebring, D.R.^20 ; Stovall, K.^21 ; Verbiest, J.P.W.^6,22 ; Zhu, W.W.^6

Department of Physics, Hillsdale College, 33 E. College Street, Hillsdale

MI

49242, United States^1

Astronomy Department, Cornell University, Ithaca

NY

14853, United States^2

Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena

CA

91106, United States^3

ASTRON, The Netherlands Institute for Radio Astronomy, Postbus 2, Dwingeloo

7990 AA, Netherlands^4

Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Manchester

M13 9PL, United Kingdom^5

Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, Bonn

D-53121, Germany^6

Laboratoire de Physique et Chimie de l'Environnement et de l'Espace, LPC2E UMR 6115 CNRS, Orléans Cedex 02

F-45071, France^7

Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver

BC

1Z1, Canada^8

National Radio Astronomy Observatory, 1003 Lopezville Rd., Socorro

NM

87801, United States

(10) Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, Amsterdam

1098 XH, Netherlands

(11) Center for Advanced Radio Astronomy, University of Texas, Rio Grande Valley, Brownsville

TX

78520, United States

(12) Columbia Astrophysics Laboratory, Columbia University, NY

10027, United States

(13) Astro Space Center, Lebedev Physical Institute, Profsoyuznaya str. 84/32, Moscow

117997, Russia

(14) University of Manchester, Jodrell Bank Observatory, Macclesfield, Cheshire

SK11 9DL, United Kingdom

(15) Department of Physics and Astronomy, West Virginia Univ., Morgantown

WV

26506, United States

(16) National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville

VA

22901, United States

(17) INAF-Osservatorio Astronomico di Cagliari, Via della Scienza 5, Selargius (CA)

09047, Italy

(18) National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Pune

411007, India

(19) CSIRO Astronomy and Space Science, Australia Telescope National Facility, PO Box 76, Epping

NSW

1710, Australia

(20) Department of Physics and Astronomy, Oberlin College, Oberlin

OH

44074, United States

(21) Physics and Astronomy Department, University of New Mexico, 1919 Lomas Boulevard NE, Albuquerque

NM

87131-0001, United States

(22) Fakultat für Physik, Universitat Bielefeld, Postfach 100131, Bielefeld

D-33501, Germany

(23) Station de Radioastronomie de Nancay, Observatoire de Paris, CNRS, INSU, Nancay

F-18330, France^9

关键词: Dispersion measure;    Intermediate frequencies;    Millisecond pulsars;    North American;    Red noise;    Single source;    Upper limits;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/716/1/012014/pdf
DOI  :  10.1088/1742-6596/716/1/012014

来源: IOP

【 摘 要 】

Dense, continuous pulsar timing observations over a 24-hr period provide a method for probing intermediate gravitational wave (GW) frequencies from 10 microhertz to 20 millihertz. The European Pulsar Timing Array (EPTA), the North American Nanohertz Observatory for Gravitational Waves (NANOGrav), the Parkes Pulsar Timing Array (PPTA), and the combined International Pulsar Timing Array (IPTA) all use millisecond pulsar observations to detect or constrain GWs typically at nanohertz frequencies. In the case of the IPTA's nine-telescope 24-Hour Global Campaign on millisecond pulsar J1713+0747, GW limits in the intermediate frequency regime can be produced. The negligible change in dispersion measure during the observation minimizes red noise in the timing residuals, constraining any contributions from GWs due to individual sources. At 10-5Hz, the 95% upper limit on strain is 10-11for GW sources in the pulsar's direction.