The role of FAST in pulsar timing arrays
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摘要
The Five-hundred-meter Aperture Spherical radio Telescope(FAST) will become one of the world-leading telescopes for pulsar timing array(PTA) research. The primary goals for PTAs are to detect(and subsequently study) ultra-low-frequency gravitational waves, to develop a pulsar-based time standard and to improve solar system planetary ephemerides. FAST will have the sensitivity to observe known pulsars with significantly improved signal-to-noise ratios and will discover a large number of currently unknown pulsars. We describe how FAST will contribute to PTA research and show that jitter-and timing-noise will be the limiting noise processes for FAST data sets. Jitter noise will limit the timing precision achievable over data spans of a few years while timing noise will limit the precision achievable over many years.
The Five-hundred-meter Aperture Spherical radio Telescope(FAST) will become one of the world-leading telescopes for pulsar timing array(PTA) research. The primary goals for PTAs are to detect(and subsequently study) ultra-low-frequency gravitational waves, to develop a pulsar-based time standard and to improve solar system planetary ephemerides. FAST will have the sensitivity to observe known pulsars with significantly improved signal-to-noise ratios and will discover a large number of currently unknown pulsars. We describe how FAST will contribute to PTA research and show that jitter-and timing-noise will be the limiting noise processes for FAST data sets. Jitter noise will limit the timing precision achievable over data spans of a few years while timing noise will limit the precision achievable over many years.
The Five-hundred-meter Aperture Spherical radio Telescope(FAST) will become one of the world-leading telescopes for pulsar timing array(PTA) research. The primary goals for PTAs are to detect(and subsequently study) ultra-low-frequency gravitational waves, to develop a pulsar-based time standard and to improve solar system planetary ephemerides. FAST will have the sensitivity to observe known pulsars with significantly improved signal-to-noise ratios and will discover a large number of currently unknown pulsars. We describe how FAST will contribute to PTA research and show that jitter-and timing-noise will be the limiting noise processes for FAST data sets. Jitter noise will limit the timing precision achievable over data spans of a few years while timing noise will limit the precision achievable over many years.
引文
Babak,S.,&Sesana,A. 2012, Phys. Rev. D,85, 044034
Backer, D. C., Kulkarni, S. R., Heiles, C., Davis, M. M.,&Goss,W. M. 1982, Nature, 300, 615
Boyles,J.,Lynch, R. S.,Ransom,S. M.,et al. 2013, ApJ,763,80
Chamberlin, S. J.,&Siemens, X. 2012, Phys. Rev. D, 85, 082001
Champion, D. J., Ransom, S. M., Lazarus, P., et al. 2008, Science,320,1309
Champion,D. J.,Hobbs,G. B.,Manchester,R. N.,et al. 2010,ApJ,720, L201
Cognard,I.,&Backer,D. C. 2004, ApJ,612, L125
Cognard,I.,Bourgois,G.,Lestrade,J.-F.,et al. 1993,Nature,366, 320
Cordes, J. M.,&Jenet, F. A. 2012, ApJ, 752, 54
Cordes,J. M.,Freire,P. C. C.,Lorimer,D. R., et al. 2006, ApJ,637, 446
Cordes,J. M.,&Shannon, R. M. 2010,-ArXiV 1010, 3785:http://adsabs.harvard.edu/abs/2010 arXiv1010.3785C
Demorest,P. B.,2011.MNRAS,416, 2821
Demorest, P. B., Ferdman, R. D., Gonzalez, M. E., et al. 2013,ApJ, 762, 94
Deng, X. P., Hobbs, G., You, X. P., et al. 2013, Advances in Space Research, 52, 1602
Edwards, R. T., Hobbs, G. B.,&Manchester, R. N. 2006,MNRAS,372, 1549
Ellis, J. A. 2013, Classical and Quantum Gravity, 30, 224004
Ellis, J. A., Siemens, X.,&Creighton, J. D. E. 2012, ApJ, 756,175
Faulkner, A. J., Stairs, I. H., Kramer, M., et al. 2004, MNRAS,355, 147
Fienga, A., Manche, H., Laskar, J.,&Gastineau, M. 2008, A&A,477,315
Foster, R. S.,&Backer, D. C. 1990, ApJ, 361, 300
Freire, P. C. C., Wex, N., Esposito-Farese, G., et al. 2012,MNRAS,423, 3328
Hellings, R. W.,&Downs, G. S. 1983, ApJ, 265, L39
Hobbs, G. 2013, Classical and Quantum Gravity, 30, 224007
Hobbs, G. B., Edwards, R. T.,&Manchester, R. N. 2006,MNRAS, 369, 655
Hobbs.G.,Hollow,R.,Champion,D.,et al. 2009, PASA,26, 468
Hobbs,G.,Lyne,A. G.,&Kramer, M. 2010a,MNRAS,402,1027
Hobbs,G.,Archibald, A., Arzoumanian, Z., et al. 2010b,Classical and Quantum Gravity, 27, 084013
Hobbs, G.,Miller,D.,Manchester,R. N.,et al. 2011,PASA,28,202
Hobbs, G., Coles, W., Manchester, R. N., et al. 2012, MNRAS,427, 2780
Hotan, A.W., van Straten,W.,&Manchester, R. N. 2004, PAS A,21,302
Hulse,R. A.,&Taylor,J. H. 1975, ApJ,195, L51
Jenet,F. A., Armstrong,J. W.,&Tinto, M. 2011,Phys. Rev. D,83,081301
Jenet,F. A.,Lommen,A.,Larson,S. L.,&Wen,L. 2004, ApJ,606, 799
Jenet,F. A., Hobbs,G. B., van Straten,W., et al. 2006, ApJ,653,1571
Keith,M. J., Johnston,S.,Bailes,M.,et al. 2012, MNRAS,419,1752
Keith,M. J.,Coles,W., Shannon,R. M.,et al. 2013, MNRAS,429,2161
Kesteven,M.,Hobbs,G.,Clement,R.,et al. 2005,Radio Science, 40, 5
Knispel,B., Allen,B.,Cordes,J. M.,et al. 2010, Science, 329,1305
Kramer, M.,&Champion, D. J. 2013, Classical and Quantum Gravity,30, 224009
Lee, K. J. 2013, Classical and Quantum Gravity, 30, 224016
Lee,K. J., Jenet,F. A.,&Price,R. H. 2008, ApJ,685,1304
Lee,K.,Jenet,F. A.,Price,R. H.,Wex, N.,&Kramer,M. 2010,ApJ,722, 1589
Lee,K. J., Wex,N.,Kramer,M.,et al. 2011,MNRAS,414, 3251
Lee, K. J., Bassa, C. G., Janssen, G. H., et al. 2012, MNRAS,423,2642
Li, D., Nan, R.,&Pan, Z. 2013, in IAU Symposium, 291,Neutron Stars and Pulsars:Challenges and Opportunities After80 Years, ed. J. van Leeuwen, 325
Lyne,A.,Hobbs,G.,Kramer,M.,Stairs, I.,&Stappers, B. 2010,Science,329, 408
Madison, D. R.,Chatterjee,S.,&Cordes,J. M. 2013, ApJ, 777,104
Maitia, V., Lestrade,J.-F.,&Cognard,I. 2003, ApJ,582, 972
Manchester,R. N. 2013, arXiv:1309.7392
Manchester,R. N.,Hobbs, G. B.,Teoh, A.,&Hobbs,M. 2005,AJ,129, 1993
Manchester,R. N.,Hobbs,G.,Bailes,M.,et al. 2013, PASA,30,e017
McLaughlin, M. A. 2013, Classical and Quantum Gravity, 30,224008
Melatos,A.,&Link, B. 2014, MNRAS,437, 21
Mingarelli, C. M. F., Sidery,T., Mandel,I.,&Vecchio, A. 2013,Phys. Rev. D,88, 062005
Nan,R.,Li,D.,Jin,C.,et al. 2011,International Journal of Modern Physics D,20, 989
Newhall,X. X., Standish,E. M.,&Williams,J. G. 1983, A&A,125, 150
Ng,C.,&HTRU Collaboration. 2013, in IAU Symposium,291,Neutron Stars and Pulsars:Challenges and Opportunities After80 Years, ed. J. van Leeuwen, 53
Nita,G. M.,&Gary, D. E. 2010, MNRAS,406, L60
Olmez,S.,Mandic, V.,&Siemens, X. 2010, Phys. Rev. D, 81,104028
Oslowski,S.,van Straten,W., Demorest,P.,&Bailes,M. 2013,MNRAS,430,416
Oslowski, S., van Straten, W., Hobbs, G. B., Bailes, M.,&Demorest,P. 2011, MNRAS,418, 1258
Petiteau, A., Babak, S., Sesana, A.,&de Araujo, M. 2013,Phys. Rev. D, 87, 064036
Pitjeva, E. V. 2005, Solar System Research, 39, 176
Ravi, V.,Wyithe,J. S. B.,Hobbs, G.,et al. 2012, ApJ,761,84
Ravi, V., Wyithe, J. S. B., Shannon, R. M., Hobbs, G.,&Manchester,R. N. 2014, MNRAS,442, 56
Sanidas, S. A., Battye, R. A.,&Stappers, B. W. 2012,Phys. Rev. D, 85, 122003
Sanidas,S. A., Battye,R. A.,&Stappers,B. W. 2013, ApJ,764,108
Sesana, A. 2013, Classical and Quantum Gravity, 30, 244009
Sesana,A., Vecchio, A.,&Colacino, C. N. 2008, MNRAS,390,192
Shannon, R. M.,&Cordes, J. M. 2010, ApJ, 725, 1607
Shannon,R. M.,&Cordes,J. M. 2012, ApJ,761,64
Shannon, R. M., Cordes, J. M., Metcalfe, T. S., et al. 2013a, ApJ,766, 5
Shannon, R. M., Ravi, V., Coles, W. A., et al. 2013b, Science,342, 334
Shannon, R. M., Ostowski, S., Dai, S., et al. 2014,arXiv:1406.4716
Siemens, X., Ellis, J., Jenet, F.,&Romano, J. D. 2013, Classical and Quantum Gravity, 30, 224015
Stinebring, D. 2013, Classical and Quantum Gravity, 30, 224006
Tong, M. L., Zhang, Y., Zhao, W., et al. 2014, Classical and Quantum Gravity, 31, 035001
van Haasteren, R.,&Levin, Y. 2010, MNRAS, 401, 2372
van Haasteren, R.,Levin, Y., Janssen,G. H., et al. 2011,MNRAS,414, 3117
van Straten,W. 2013, ApJS,204, 13
Verbiest,J. P. W., Bailes.,M.,van Straten,W., et al. 2008, ApJ,679, 675
Wang,J. B.,Hobbs,G.,Coles,W., et al. 2015, MNRAS, 446,1657
Wolszczan,A.,&Frail,D. A. 1992, Nature,355, 145
Yan, W. M., Manchester, R. N., van Straten, W., et al. 2011a,MNRAS,414, 2087
Yan, W. M., Manchester, R. N., Hobbs, G., et al. 2011b, Ap&SS,335, 485
Yardley, D. R. B., Hobbs, G. B., Jenet, F. A., et al. 2010,MNRAS,407, 669
Yardley, D. R. B., Coles, W. A., Hobbs, G. B., et al. 2011,MNRAS,414, 1777
You,X. P.,Hobbs,G.,Coles,W. A.,et al. 2007, MNRAS,378,493
You, X. P., Coles, W. A., Hobbs, G. B.,&Manchester, R. N.2012, MNRAS, 422, 1160
Zhu, X.-J.,Wen, L.,Hobbs, G.,et al. 2015, MNRAS,449, 1650
1 http://syrte.obspm.fr/jsr/journees2010/pdf/Hilton.pdf
2 Os?owski et al.(2011)suggest that this phenomenon should be termed Stochastic Wideband Impulse Modulated Self-noise(SWIMS).
3 The Xinjiang Qitai 110 m Radio Telescope(QTT)has been funded and will be a fully-steerable single-dish telescope that will operate over a large frequency range. It is not clear which telescopes in the Northern Hemisphere will still be operating in the FAST-era, but it is likely that a large number of 100-m class telescopes(in Europe, China and North America)will continue to observe pulsars.
4 We note that multi-path scattering effects may limit the availability of the lower part of the band for determining DM variations that can be applied to arrival times determined from the high-frequency end of the band.
5 In this latter case a large telescope such as FAST is not needed and identical results could be obtained from a smaller telescope.
6 The mean duty cycle for the pulsars currently observed for the IPTA is 0.09. However the standard deviation is 0.07.
7 For completeness we note that the pulsar with the smallest flux density in the figure is PSR J1911+1347. This was discovered in the Parkes multibeam survey(Faulkner et al. 2004)and has a flux density significantly lower than the nominal sensitivity of that survey.
8 The PPTA team is finding it useful to have multiple backends recording the same data. This enables determination of instrumental effects that are otherwise hard to identify.
9 http://www.atnf.csiro.au/research/pulsar/index.html?n=Main.Psrfits
10 In contrast pulsar surveys are suited to citizen science projects. See,for example, the Einstein@Home project; Knispel et al.(2010).
Backer, D. C., Kulkarni, S. R., Heiles, C., Davis, M. M.,&Goss,W. M. 1982, Nature, 300, 615
Boyles,J.,Lynch, R. S.,Ransom,S. M.,et al. 2013, ApJ,763,80
Chamberlin, S. J.,&Siemens, X. 2012, Phys. Rev. D, 85, 082001
Champion, D. J., Ransom, S. M., Lazarus, P., et al. 2008, Science,320,1309
Champion,D. J.,Hobbs,G. B.,Manchester,R. N.,et al. 2010,ApJ,720, L201
Cognard,I.,&Backer,D. C. 2004, ApJ,612, L125
Cognard,I.,Bourgois,G.,Lestrade,J.-F.,et al. 1993,Nature,366, 320
Cordes, J. M.,&Jenet, F. A. 2012, ApJ, 752, 54
Cordes,J. M.,Freire,P. C. C.,Lorimer,D. R., et al. 2006, ApJ,637, 446
Cordes,J. M.,&Shannon, R. M. 2010,-ArXiV 1010, 3785:http://adsabs.harvard.edu/abs/2010 arXiv1010.3785C
Demorest,P. B.,2011.MNRAS,416, 2821
Demorest, P. B., Ferdman, R. D., Gonzalez, M. E., et al. 2013,ApJ, 762, 94
Deng, X. P., Hobbs, G., You, X. P., et al. 2013, Advances in Space Research, 52, 1602
Edwards, R. T., Hobbs, G. B.,&Manchester, R. N. 2006,MNRAS,372, 1549
Ellis, J. A. 2013, Classical and Quantum Gravity, 30, 224004
Ellis, J. A., Siemens, X.,&Creighton, J. D. E. 2012, ApJ, 756,175
Faulkner, A. J., Stairs, I. H., Kramer, M., et al. 2004, MNRAS,355, 147
Fienga, A., Manche, H., Laskar, J.,&Gastineau, M. 2008, A&A,477,315
Foster, R. S.,&Backer, D. C. 1990, ApJ, 361, 300
Freire, P. C. C., Wex, N., Esposito-Farese, G., et al. 2012,MNRAS,423, 3328
Hellings, R. W.,&Downs, G. S. 1983, ApJ, 265, L39
Hobbs, G. 2013, Classical and Quantum Gravity, 30, 224007
Hobbs, G. B., Edwards, R. T.,&Manchester, R. N. 2006,MNRAS, 369, 655
Hobbs.G.,Hollow,R.,Champion,D.,et al. 2009, PASA,26, 468
Hobbs,G.,Lyne,A. G.,&Kramer, M. 2010a,MNRAS,402,1027
Hobbs,G.,Archibald, A., Arzoumanian, Z., et al. 2010b,Classical and Quantum Gravity, 27, 084013
Hobbs, G.,Miller,D.,Manchester,R. N.,et al. 2011,PASA,28,202
Hobbs, G., Coles, W., Manchester, R. N., et al. 2012, MNRAS,427, 2780
Hotan, A.W., van Straten,W.,&Manchester, R. N. 2004, PAS A,21,302
Hulse,R. A.,&Taylor,J. H. 1975, ApJ,195, L51
Jenet,F. A., Armstrong,J. W.,&Tinto, M. 2011,Phys. Rev. D,83,081301
Jenet,F. A.,Lommen,A.,Larson,S. L.,&Wen,L. 2004, ApJ,606, 799
Jenet,F. A., Hobbs,G. B., van Straten,W., et al. 2006, ApJ,653,1571
Keith,M. J., Johnston,S.,Bailes,M.,et al. 2012, MNRAS,419,1752
Keith,M. J.,Coles,W., Shannon,R. M.,et al. 2013, MNRAS,429,2161
Kesteven,M.,Hobbs,G.,Clement,R.,et al. 2005,Radio Science, 40, 5
Knispel,B., Allen,B.,Cordes,J. M.,et al. 2010, Science, 329,1305
Kramer, M.,&Champion, D. J. 2013, Classical and Quantum Gravity,30, 224009
Lee, K. J. 2013, Classical and Quantum Gravity, 30, 224016
Lee,K. J., Jenet,F. A.,&Price,R. H. 2008, ApJ,685,1304
Lee,K.,Jenet,F. A.,Price,R. H.,Wex, N.,&Kramer,M. 2010,ApJ,722, 1589
Lee,K. J., Wex,N.,Kramer,M.,et al. 2011,MNRAS,414, 3251
Lee, K. J., Bassa, C. G., Janssen, G. H., et al. 2012, MNRAS,423,2642
Li, D., Nan, R.,&Pan, Z. 2013, in IAU Symposium, 291,Neutron Stars and Pulsars:Challenges and Opportunities After80 Years, ed. J. van Leeuwen, 325
Lyne,A.,Hobbs,G.,Kramer,M.,Stairs, I.,&Stappers, B. 2010,Science,329, 408
Madison, D. R.,Chatterjee,S.,&Cordes,J. M. 2013, ApJ, 777,104
Maitia, V., Lestrade,J.-F.,&Cognard,I. 2003, ApJ,582, 972
Manchester,R. N. 2013, arXiv:1309.7392
Manchester,R. N.,Hobbs, G. B.,Teoh, A.,&Hobbs,M. 2005,AJ,129, 1993
Manchester,R. N.,Hobbs,G.,Bailes,M.,et al. 2013, PASA,30,e017
McLaughlin, M. A. 2013, Classical and Quantum Gravity, 30,224008
Melatos,A.,&Link, B. 2014, MNRAS,437, 21
Mingarelli, C. M. F., Sidery,T., Mandel,I.,&Vecchio, A. 2013,Phys. Rev. D,88, 062005
Nan,R.,Li,D.,Jin,C.,et al. 2011,International Journal of Modern Physics D,20, 989
Newhall,X. X., Standish,E. M.,&Williams,J. G. 1983, A&A,125, 150
Ng,C.,&HTRU Collaboration. 2013, in IAU Symposium,291,Neutron Stars and Pulsars:Challenges and Opportunities After80 Years, ed. J. van Leeuwen, 53
Nita,G. M.,&Gary, D. E. 2010, MNRAS,406, L60
Olmez,S.,Mandic, V.,&Siemens, X. 2010, Phys. Rev. D, 81,104028
Oslowski,S.,van Straten,W., Demorest,P.,&Bailes,M. 2013,MNRAS,430,416
Oslowski, S., van Straten, W., Hobbs, G. B., Bailes, M.,&Demorest,P. 2011, MNRAS,418, 1258
Petiteau, A., Babak, S., Sesana, A.,&de Araujo, M. 2013,Phys. Rev. D, 87, 064036
Pitjeva, E. V. 2005, Solar System Research, 39, 176
Ravi, V.,Wyithe,J. S. B.,Hobbs, G.,et al. 2012, ApJ,761,84
Ravi, V., Wyithe, J. S. B., Shannon, R. M., Hobbs, G.,&Manchester,R. N. 2014, MNRAS,442, 56
Sanidas, S. A., Battye, R. A.,&Stappers, B. W. 2012,Phys. Rev. D, 85, 122003
Sanidas,S. A., Battye,R. A.,&Stappers,B. W. 2013, ApJ,764,108
Sesana, A. 2013, Classical and Quantum Gravity, 30, 244009
Sesana,A., Vecchio, A.,&Colacino, C. N. 2008, MNRAS,390,192
Shannon, R. M.,&Cordes, J. M. 2010, ApJ, 725, 1607
Shannon,R. M.,&Cordes,J. M. 2012, ApJ,761,64
Shannon, R. M., Cordes, J. M., Metcalfe, T. S., et al. 2013a, ApJ,766, 5
Shannon, R. M., Ravi, V., Coles, W. A., et al. 2013b, Science,342, 334
Shannon, R. M., Ostowski, S., Dai, S., et al. 2014,arXiv:1406.4716
Siemens, X., Ellis, J., Jenet, F.,&Romano, J. D. 2013, Classical and Quantum Gravity, 30, 224015
Stinebring, D. 2013, Classical and Quantum Gravity, 30, 224006
Tong, M. L., Zhang, Y., Zhao, W., et al. 2014, Classical and Quantum Gravity, 31, 035001
van Haasteren, R.,&Levin, Y. 2010, MNRAS, 401, 2372
van Haasteren, R.,Levin, Y., Janssen,G. H., et al. 2011,MNRAS,414, 3117
van Straten,W. 2013, ApJS,204, 13
Verbiest,J. P. W., Bailes.,M.,van Straten,W., et al. 2008, ApJ,679, 675
Wang,J. B.,Hobbs,G.,Coles,W., et al. 2015, MNRAS, 446,1657
Wolszczan,A.,&Frail,D. A. 1992, Nature,355, 145
Yan, W. M., Manchester, R. N., van Straten, W., et al. 2011a,MNRAS,414, 2087
Yan, W. M., Manchester, R. N., Hobbs, G., et al. 2011b, Ap&SS,335, 485
Yardley, D. R. B., Hobbs, G. B., Jenet, F. A., et al. 2010,MNRAS,407, 669
Yardley, D. R. B., Coles, W. A., Hobbs, G. B., et al. 2011,MNRAS,414, 1777
You,X. P.,Hobbs,G.,Coles,W. A.,et al. 2007, MNRAS,378,493
You, X. P., Coles, W. A., Hobbs, G. B.,&Manchester, R. N.2012, MNRAS, 422, 1160
Zhu, X.-J.,Wen, L.,Hobbs, G.,et al. 2015, MNRAS,449, 1650
1 http://syrte.obspm.fr/jsr/journees2010/pdf/Hilton.pdf
2 Os?owski et al.(2011)suggest that this phenomenon should be termed Stochastic Wideband Impulse Modulated Self-noise(SWIMS).
3 The Xinjiang Qitai 110 m Radio Telescope(QTT)has been funded and will be a fully-steerable single-dish telescope that will operate over a large frequency range. It is not clear which telescopes in the Northern Hemisphere will still be operating in the FAST-era, but it is likely that a large number of 100-m class telescopes(in Europe, China and North America)will continue to observe pulsars.
4 We note that multi-path scattering effects may limit the availability of the lower part of the band for determining DM variations that can be applied to arrival times determined from the high-frequency end of the band.
5 In this latter case a large telescope such as FAST is not needed and identical results could be obtained from a smaller telescope.
6 The mean duty cycle for the pulsars currently observed for the IPTA is 0.09. However the standard deviation is 0.07.
7 For completeness we note that the pulsar with the smallest flux density in the figure is PSR J1911+1347. This was discovered in the Parkes multibeam survey(Faulkner et al. 2004)and has a flux density significantly lower than the nominal sensitivity of that survey.
8 The PPTA team is finding it useful to have multiple backends recording the same data. This enables determination of instrumental effects that are otherwise hard to identify.
9 http://www.atnf.csiro.au/research/pulsar/index.html?n=Main.Psrfits
10 In contrast pulsar surveys are suited to citizen science projects. See,for example, the Einstein@Home project; Knispel et al.(2010).