Details
| Original language | English |
|---|---|
| Journal | Astrophysical Journal |
| Volume | 879 |
| Issue number | 1 |
| Early online date | 26 Jun 2019 |
| Publication status | Published - 1 Jul 2019 |
Abstract
Two analysis errors have been identified that affect the results for a handful of the high-value pulsars given in Table 1 of Abbott et al. (2019). One affects the Bayesian analysis for the five pulsars that glitched during the analysis period, and the other affects the 5n-vector analysis for J0711-6830. Updated results after correcting the errors are shown in Table 1, which now supersedes the results given for those pulsars in Table 1 of Abbott et al. (2019). Updated versions of figures can be seen in Figures 1-4. Bayesian analysis.-For the glitching pulsars, the signal phase evolution caused by the glitch was wrongly applied twice and was therefore not consistent with our expected model of the pulsar phase. This error did not affect the F/G-statistic or 5n-vector analysis. Analyses of the five pulsars PSR J0205+6449, PSR J0534+2200, PSR J0835-4510, PSR J1028-5819, and PSR J1718-3825 have been repeated after correcting for the error. There are small quantitative differences in the results, but the changes do not affect the main conclusions of the paper. The largest differences are for PSR J0835-4510 (the Vela pulsar), for which the updated upper limits from the Bayesian method are found to be between 1.1 and 2 times larger than those obtained when the error was present. This appears primarily to be due to the error leading to the decohering of a strong spectral line in the LIGO Livingston detector and thus lowering the amplitude limit. 5n-vector analysis.-An error was also identified in the settings of the 5n-vector analysis, which affected the upper limit computation at the rotation frequency for C21 95% of J0711-6830. Specifically, we found an incorrect choice for the range of amplitudes used to inject simulated signals in the O2 data. The updated upper limit is about 2.5 times worse than that obtained when the error was present. This error did not affect the Bayesian or F/G-statistic results. (Table Presented) (Figure Presented).
ASJC Scopus subject areas
- Physics and Astronomy(all)
- Astronomy and Astrophysics
- Earth and Planetary Sciences(all)
- Space and Planetary Science
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In: Astrophysical Journal, Vol. 879, No. 1, 01.07.2019.
Research output: Contribution to journal › Article › Research › peer review
}
TY - JOUR
T1 - Searches for Gravitational Waves from Known Pulsars at Two Harmonics in 2015–2017 LIGO Data
AU - The LIGO Scientific Collaboration
AU - The Virgo Collaboration
AU - Abbott, B. P.
AU - Abbott, R.
AU - Abbott, T. D.
AU - Abraham, S.
AU - Acernese, F.
AU - Ackley, K.
AU - Adams, C.
AU - Adhikari, R. X.
AU - Adya, V. B.
AU - Affeldt, C.
AU - Agathos, M.
AU - Agatsuma, K.
AU - Aggarwal, N.
AU - Aguiar, O. D.
AU - Aiello, L.
AU - Ain, A.
AU - Ajith, P.
AU - Allen, G.
AU - Allocca, A.
AU - Bose, S.
AU - Brown, D. D.
AU - Cheng, H. P.
AU - Danilishin, S. L.
AU - Danzmann, K.
AU - Hanke, M. M.
AU - Hennig, J.
AU - Heurs, M.
AU - Hreibi, A.
AU - Kumar, S.
AU - Lang, R. N.
AU - Lee, H. K.
AU - Lee, H. M.
AU - Lee, H. W.
AU - Li, X.
AU - Lück, H.
AU - Sanders, J. R.
AU - Schmidt, P.
AU - Steinmeyer, D.
AU - Sun, L.
AU - Vahlbruch, H.
AU - Wei, L. W.
AU - Wilken, D. M.
AU - Willke, B.
AU - Wittel, H.
AU - Wu, D. S.
AU - Zhang, L.
AU - Zhou, M.
AU - Zhu, X. J.
AU - Bergmann, Gerald
AU - Lee, J.
AU - Bode, Nina
AU - Booker, Phillip
AU - Brinkmann, Marc
AU - Cabero, M.
AU - Dent, T.
AU - de Varona, Omar
AU - Doravari, S.
AU - Hochheim, S.
AU - Junker, Jonas
AU - Karvinen, Kai S.
AU - Khan, S.
AU - Kirchhoff, R.
AU - Koch, Patrick
AU - Koehlenbeck, S.
AU - Kringel, Volker
AU - Koper, N.
AU - Kuehn, G.
AU - Leavey, S.
AU - Lehmann, J.
AU - Lough, J. D.
AU - Mehmet, M.
AU - Mukherjee, Arunava
AU - Trad Nery, Marina
AU - Ohme, F.
AU - Oppermann, P.
AU - Phelps, M.
AU - Puncken, O.
AU - Rüdiger, A.
AU - Schreiber, E.
AU - Schulte, B. W.
AU - Setyawati, Y.
AU - Standke, M.
AU - Steinke, M.
AU - Thies, F.
AU - Weinert, M.
AU - Wellmann, F.
AU - Weßels, Peter
AU - Wimmer, M. H.
AU - Winkler, W.
AU - Woehler, J.
N1 - Funding Information: The authors are grateful for the research grant received from Ministry of Higher Education through Fundamental Research Grant Scheme (FRGS) FRGS/1/2017/TK10/UNIKL/02/6.
PY - 2019/7/1
Y1 - 2019/7/1
N2 - Two analysis errors have been identified that affect the results for a handful of the high-value pulsars given in Table 1 of Abbott et al. (2019). One affects the Bayesian analysis for the five pulsars that glitched during the analysis period, and the other affects the 5n-vector analysis for J0711-6830. Updated results after correcting the errors are shown in Table 1, which now supersedes the results given for those pulsars in Table 1 of Abbott et al. (2019). Updated versions of figures can be seen in Figures 1-4. Bayesian analysis.-For the glitching pulsars, the signal phase evolution caused by the glitch was wrongly applied twice and was therefore not consistent with our expected model of the pulsar phase. This error did not affect the F/G-statistic or 5n-vector analysis. Analyses of the five pulsars PSR J0205+6449, PSR J0534+2200, PSR J0835-4510, PSR J1028-5819, and PSR J1718-3825 have been repeated after correcting for the error. There are small quantitative differences in the results, but the changes do not affect the main conclusions of the paper. The largest differences are for PSR J0835-4510 (the Vela pulsar), for which the updated upper limits from the Bayesian method are found to be between 1.1 and 2 times larger than those obtained when the error was present. This appears primarily to be due to the error leading to the decohering of a strong spectral line in the LIGO Livingston detector and thus lowering the amplitude limit. 5n-vector analysis.-An error was also identified in the settings of the 5n-vector analysis, which affected the upper limit computation at the rotation frequency for C21 95% of J0711-6830. Specifically, we found an incorrect choice for the range of amplitudes used to inject simulated signals in the O2 data. The updated upper limit is about 2.5 times worse than that obtained when the error was present. This error did not affect the Bayesian or F/G-statistic results. (Table Presented) (Figure Presented).
AB - Two analysis errors have been identified that affect the results for a handful of the high-value pulsars given in Table 1 of Abbott et al. (2019). One affects the Bayesian analysis for the five pulsars that glitched during the analysis period, and the other affects the 5n-vector analysis for J0711-6830. Updated results after correcting the errors are shown in Table 1, which now supersedes the results given for those pulsars in Table 1 of Abbott et al. (2019). Updated versions of figures can be seen in Figures 1-4. Bayesian analysis.-For the glitching pulsars, the signal phase evolution caused by the glitch was wrongly applied twice and was therefore not consistent with our expected model of the pulsar phase. This error did not affect the F/G-statistic or 5n-vector analysis. Analyses of the five pulsars PSR J0205+6449, PSR J0534+2200, PSR J0835-4510, PSR J1028-5819, and PSR J1718-3825 have been repeated after correcting for the error. There are small quantitative differences in the results, but the changes do not affect the main conclusions of the paper. The largest differences are for PSR J0835-4510 (the Vela pulsar), for which the updated upper limits from the Bayesian method are found to be between 1.1 and 2 times larger than those obtained when the error was present. This appears primarily to be due to the error leading to the decohering of a strong spectral line in the LIGO Livingston detector and thus lowering the amplitude limit. 5n-vector analysis.-An error was also identified in the settings of the 5n-vector analysis, which affected the upper limit computation at the rotation frequency for C21 95% of J0711-6830. Specifically, we found an incorrect choice for the range of amplitudes used to inject simulated signals in the O2 data. The updated upper limit is about 2.5 times worse than that obtained when the error was present. This error did not affect the Bayesian or F/G-statistic results. (Table Presented) (Figure Presented).
UR - http://www.scopus.com/inward/record.url?scp=85094194593&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ab20cb
DO - 10.3847/1538-4357/ab20cb
M3 - Article
AN - SCOPUS:85094194593
VL - 879
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1
ER -