214 results on '"Stairs, I. H."'
Search Results
2. A repeating fast radio burst source in a globular cluster
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Kirsten, F., Marcote, B., Nimmo, K., Hessels, J. W. T., Bhardwaj, M., Tendulkar, S. P., Keimpema, A., Yang, J., Snelders, M. P., Scholz, P., Pearlman, A. B., Law, C. J., Peters, W. M., Giroletti, M., Paragi, Z., Bassa, C., Hewitt, D. M., Bach, U., Bezrukovs, V., Burgay, M., Buttaccio, S. T., Conway, J. E., Corongiu, A., Feiler, R., Forssén, O., Gawroński, M. P., Karuppusamy, R., Kharinov, M. A., Lindqvist, M., Maccaferri, G., Melnikov, A., Ould-Boukattine, O. S., Possenti, A., Surcis, G., Wang, N., Yuan, J., Aggarwal, K., Anna-Thomas, R., Bower, G. C., Blaauw, R., Burke-Spolaor, S., Cassanelli, T., Clarke, T. E., Fonseca, E., Gaensler, B. M., Gopinath, A., Kaspi, V. M., Kassim, N., Lazio, T. J. W., Leung, C., Li, D. Z., Lin, H. H., Masui, K. W., Mckinven, R., Michilli, D., Mikhailov, A. G., Ng, C., Orbidans, A., Pen, U. L., Petroff, E., Rahman, M., Ransom, S. M., Shin, K., Smith, K. M., Stairs, I. H., and Vlemmings, W.
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- 2022
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3. Asymmetric mass ratios for bright double neutron-star mergers
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Ferdman, R. D., Freire, P. C. C., Perera, B. B. P., Pol, N., Camilo, F., Chatterjee, S., Cordes, J. M., Crawford, F., Hessels, J. W. T., Kaspi, V. M., McLaughlin, M. A., Parent, E., Stairs, I. H., and van Leeuwen, J.
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- 2020
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4. Relativistic Shapiro delay measurements of an extremely massive millisecond pulsar
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Cromartie, H. T., Fonseca, E., Ransom, S. M., Demorest, P. B., Arzoumanian, Z., Blumer, H., Brook, P. R., DeCesar, M. E., Dolch, T., Ellis, J. A., Ferdman, R. D., Ferrara, E. C., Garver-Daniels, N., Gentile, P. A., Jones, M. L., Lam, M. T., Lorimer, D. R., Lynch, R. S., McLaughlin, M. A., Ng, C., Nice, D. J., Pennucci, T. T., Spiewak, R., Stairs, I. H., Stovall, K., Swiggum, J. K., and Zhu, W. W.
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- 2020
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5. The prospects of pulsar timing with new-generation radio telescopes and the Square Kilometre Array
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Stappers, B. W., Keane, E. F., Kramer, M., Possenti, A., and Stairs, I. H.
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- 2018
6. The black widow pulsar J1641+8049 in the optical, radio, and X-rays.
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Kirichenko, A Yu, Zharikov, S V, Karpova, A V, Fonseca, E, Zyuzin, D A, Shibanov, Yu A, López, E A, Gilfanov, M R, Cabrera-Lavers, A, Geier, S, Dong, F A, Good, D C, McKee, J W, Meyers, B W, Stairs, I H, McLaughlin, M A, and Swiggum, J K
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PULSARS ,X-rays ,PULSE modulation ,NEUTRON stars - Abstract
PSR J1641+8049 is a 2 ms black widow pulsar with the 2.2 h orbital period detected in the radio and γ-rays. We performed new phase-resolved multiband photometry of PSR J1641+8049 using the OSIRIS instrument at the Gran Telescopio Canarias. The obtained data were analysed together with the new radio-timing observations from the Canadian Hydrogen Intensity Mapping Experiment (CHIME), the X-ray data from the Spectrum-RG/ eROSITA all-sky survey, and all available optical photometric observations. An updated timing solution based on CHIME data is presented, which accounts for secular and periodic modulations in pulse dispersion. The system parameters obtained through the light-curve analysis, including the distance to the source 4.6–4.8 kpc and the orbital inclination 56–59 deg, are found to be consistent with previous studies. However, the optical flux of the source at the maximum brightness phase faded by a factor of ∼2 as compared to previous observations. Nevertheless, the face of the J1641+8049 companion remains one of the most heated (8000–9500 K) by a pulsar among the known black widow pulsars. We also report a new estimation on the pulsar proper motion of ≈2 mas yr
−1 , which yields a spin-down luminosity of ≈4.87 × 1034 erg s−1 and a corresponding heating efficiency of the companion by the pulsar of 0.3–0.7. The pulsar was not detected in X-rays implying its X-ray-luminosity was |$\lesssim$| 3 × 1031 erg s−1 at the date of observations. [ABSTRACT FROM AUTHOR]- Published
- 2024
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7. A MeerKAT view of the double pulsar eclipses: Geodetic precession of pulsar B and system geometry.
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Lower, M. E., Kramer, M., Shannon, R. M., Breton, R. P., Wex, N., Johnston, S., Bailes, M., Buchner, S., Hu, H., Venkatraman Krishnan, V., Blackmon, V. A., Camilo, F., Champion, D. J., Freire, P. C. C., Geyer, M., Karastergiou, A., van Leeuwen, J., McLaughlin, M. A., Reardon, D. J., and Stairs, I. H.
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PULSARS ,NEUTRON stars ,MEERKAT ,LIGHT curves ,GENERAL relativity (Physics) - Abstract
The double pulsar system, PSR J0737−3039A/B, consists of two neutron stars bound together in a highly relativistic orbit that is viewed nearly edge-on from the Earth. This alignment results in brief radio eclipses of the fast-rotating pulsar A when it passes behind the toroidal magnetosphere of the slow-rotating pulsar B. The morphology of these eclipses is strongly dependent on the geometric orientation and rotation phase of pulsar B, and their time evolution can be used to constrain the geodetic precession rate of the pulsar. We demonstrate a Bayesian inference framework for modelling high-sensitivity eclipse light curves obtained with MeerKAT between 2019 and 2023. Using a hierarchical inference approach, we obtained a precession rate of Ω
SO B = 5.16°−0.34° +0.32° yr−1 (68% confidence intervals) for pulsar B, consistent with predictions from general relativity to a relative uncertainty of 6.5%. This updated measurement provides a 6.1% test of relativistic spin-orbit coupling in the strong-field regime. We show that a simultaneous fit to all of our observed eclipses can in principle return a ∼1.5% test of spin-orbit coupling. However, systematic effects introduced by the current geometric orientation of pulsar B along with inconsistencies between the observed and predicted eclipse light curves result in difficult to quantify uncertainties when using this approach. Assuming the validity of general relativity, we definitively show that the spin axis of pulsar B is misaligned from the total angular momentum vector by 40.6° ±0.1° and that the orbit of the system is inclined by approximately 90.5° from the direction of our line of sight. Our measured geometry for pulsar B suggests the largely empty emission cone contains an elongated horseshoe-shaped beam centred on the magnetic axis, and that it may not be re-detected as a radio pulsar until early 2035. [ABSTRACT FROM AUTHOR]- Published
- 2024
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8. Searching for continuous Gravitational Waves in the second data release of the International Pulsar Timing Array
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Falxa, M, Babak, S, Baker, P T, Bécsy, B, Chalumeau, A, Chen, S, Chen, Z, Cornish, N J, Guillemot, L, Hazboun, J S, Mingarelli, C M F, Parthasarathy, A, Petiteau, A, Pol, N S, Sesana, A, Spolaor, S B, Taylor, S R, Theureau, G, Vallisneri, M, Vigeland, S J, Witt, C A, Zhu, X, Antoniadis, J, Arzoumanian, Z, Bailes, M, Bhat, N D R, Blecha, L, Brazier, A, Brook, P R, Caballero, N, Cameron, A D, Casey-Clyde, J A, Champion, D, Charisi, M, Chatterjee, S, Cognard, I, Cordes, J M, Crawford, F, Cromartie, H T, Crowter, K, Dai, S, DeCesar, M E, Demorest, P B, Desvignes, G, Dolch, T, Drachler, B, Feng, Y, Ferrara, E C, Fiore, W, Fonseca, E, Garver-Daniels, N, Glaser, J, Goncharov, B, Good, D C, Griessmeier, J, Guo, Y J, Gültekin, K, Hobbs, G, Hu, H, Islo, K, Jang, J, Jennings, R J, Johnson, A D, Jones, M L, Kaczmarek, J, Kaiser, A R, Kaplan, D L, Keith, M, Kelley, L Z, Kerr, M, Key, J S, Laal, N, Lam, M T, Lamb, W G, Lazio, T J W, Liu, K, Liu, T, Luo, J, Lynch, R S, Madison, D R, Main, R, Manchester, R, McEwen, A, McKee, J, McLaughlin, M A, Ng, C, Nice, D J, Ocker, S, Olum, K D, Osłowski, S, Pennucci, T T, Perera, B B P, Perrodin, D, Porayko, N, Possenti, A, Quelquejay-Leclere, H, Ransom, S M, Ray, P S, Reardon, D J, Russell, C J, Samajdar, A, Sarkissian, J, Schult, L, Shaifullah, G, Shannon, R M, Shapiro-Albert, B J, Siemens, X, Simon, J J, Siwek, M, Smith, T L, Speri, L, Spiewak, R, Stairs, I H, Stappers, B, Stinebring, D R, Swiggum, J K, Tiburzi, C, Turner, J, Vecchio, A, Verbiest, Joris, Wahl, H, Wang, S Q, Wang, J, Wang, Jun, Wu, Ziwei, Zhang, L, Zhang, S, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Unité Scientifique de la Station de Nançay (USN), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Univers et Théories (LUTH (UMR_8102)), and IPTA
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noise ,data analysis method ,gravitational radiation ,orbit: circle ,FOS: Physical sciences ,General Relativity and Quantum Cosmology (gr-qc) ,sensitivity ,frequency: high ,General Relativity and Quantum Cosmology ,confidence limit ,frequency: low ,black hole: binary ,[PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc] ,[PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det] ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,pulsar - Abstract
The International Pulsar Timing Array 2nd data release is the combination ofdatasets from worldwide collaborations. In this study, we search for continuouswaves: gravitational wave signals produced by individual supermassive blackhole binaries in the local universe. We consider binaries on circular orbitsand neglect the evolution of orbital frequency over the observational span. Wefind no evidence for such signals and set sky averaged 95% upper limits ontheir amplitude h 95 . The most sensitive frequency is 10nHz with h 95 = 9.110-15 . We achieved the best upper limit to date at low and high frequencies ofthe PTA band thanks to improved effective cadence of observations. In ouranalysis, we have taken into account the recently discovered common red noiseprocess, which has an impact at low frequencies. We also find that the peculiarnoise features present in some pulsars data must be taken into account toreduce the false alarm. We show that using custom noise models is essential insearching for continuous gravitational wave signals and setting the upperlimit.
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- 2023
9. Revealing the Dynamic Magneto-ionic Environments of Repeating Fast Radio Burst Sources through Multi-year Polarimetric Monitoring with CHIME/FRB
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Mckinven, R., Gaensler, B. M., Michilli, D., Masui, K., Kaspi, V. M., Su, J., Bhardwaj, M., Cassanelli, T., Chawla, P., Dong, Fonseca, E., Leung, C., Petroff, E., Pleunis, Z., Rafiei-Ravandi, M., Stairs, I. H., Tendulkar, S., Li, D. Z., Ng, C., Patel, C., Pearlman, A. B., Rahman, M., Sand, K. R., and Shin, K.
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High Energy Astrophysical Phenomena (astro-ph.HE) ,FOS: Physical sciences ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
Fast radio bursts (FRBs) display a confounding variety of burst properties and host galaxy associations. Repeating FRBs offer insight into the FRB population by enabling spectral, temporal and polarimetric properties to be tracked over time. Here, we report on the polarized observations of 12 repeating sources using multi-year monitoring with the Canadian Hydrogen Intensity Mapping Experiment (CHIME) over 400-800 MHz. We observe significant RM variations from many sources in our sample, including RM changes of several hundred $\rm{rad\, m^{-2}}$ over month timescales from FRBs 20181119A, 20190303A and 20190417A, and more modest RM variability ($\rm{\Delta RM \lesssim}$ few tens rad m$^{-2}$) from FRBs 20181030A, 20190208A, 20190213B and 20190117A over equivalent timescales. Several repeaters display a frequency dependent degree of linear polarization that is consistent with depolarization via scattering. Combining our measurements of RM variations with equivalent constraints on DM variability, we estimate the average line-of-sight magnetic field strength in the local environment of each repeater. In general, repeating FRBs display RM variations that are more prevalent/extreme than those seen from radio pulsars in the Milky Way and the Magellanic Clouds, suggesting repeating FRBs and pulsars occupy distinct magneto-ionic environments.
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- 2023
10. The NANOGrav 11 Yr Data Set: Limits on Gravitational Waves from Individual Supermassive Black Hole Binaries
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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, Haasteren, R. van, Vigeland, S. J, Witt, C. A, and Zhu, W. W
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Astrophysics - Abstract
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 f(gw) = 8 nHz, we placed a sky-averaged upper limit of h(0) < 7.3(3) × 10(exp −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 f(gw) = 8 nHz within 120 Mpc for M = 10(exp 9) Solar Mass, and within 5.5 Gpc for M= 10(exp 10) Solar Mass at our most sensitive sky location. We also determined that there are no SMBHBs with M > 1.6 x 10(exp 9) Solar Mass emitting GWs with f(gw) = 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.
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- 2019
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11. The NANOGrav 12.5 yr Data Set: The Frequency Dependence of Pulse Jitter in Precision Millisecond Pulsars
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Lam, M. T, McLaughlin, M. A, Arzoumanian, Z, Blumer, H, Brook, P. R, Cromartie, H. T, Demorest, P. B, DeCesar, M. E, Dolch, T, Ellis, J. A, Ferdman, R. D, Ferrara, E. C, Fonesca, E, Garver-Daniels, N, Gentile, P. A, Jones, M. L, Lorimer, D. R, Lynch, R. S, Ng, C, Nice, D. J, Pennucci, T. T, Ranson, S. M, Spiewak, R, Stairs, I. H, Stovall, K, Swiggum, J. K, Vigeland, S. J, and Zhu, W. W
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Astrophysics - Abstract
Low-frequency gravitational-wave experiments require the highest timing precision from an array of the moststable millisecond pulsars. Several known sources of noise on short timescales in single radio pulsar observationsare well described by a simple model of three components: template fitting from a finite signal-to-noise ratio, pulsephase/amplitude jitter from single-pulse stochasticity, and scintillation errors from short-timescale interstellarscattering variations. Currently template-fitting errors dominate, but as radio telescopes push toward higher signalto-noise ratios, jitter becomes the next dominant term for most millisecond pulsars. Understanding the statistics ofjitter becomes crucial for properly characterizing arrival time uncertainties. We characterize the radio frequencydependence of jitter using data on 48 pulsars in the North American Nanohertz Observatory for GravitationalWaves timing program. We detect significant jitter in 43 of the pulsars and test several functional forms for itsfrequency dependence; we find significant frequency dependence for 30 pulsars. We find moderate correlations ofrms jitter with pulse width (R = 0.62) and number of profile components (R = 0.40); the single-pulse rms jitter istypically 1% of pulse phase. The average frequency dependence for all pulsars using a power-law model hasindex 0.42. We investigate the jitter variations for the interpulse of PSR B1937+21 and find no significantdeviations from the main pulse rms jitter. We also test the time variation of jitter in two pulsars and find thatsystematics likely bias the results for high-precision pulsars. Pulsar timing array analyses must properly modeljitter as a significant component of the noise within the detector.
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- 2019
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12. The NANOGrav 11 yr Data Set: Solar Wind Sounding through Pulsar Timing
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Madison, D.R, Cordes, J.M, Arzoumanian, Z, Chatterjee, S, Crowter, K, DeCesar, M. E, Demorest, P. B, Dolch, T, Ellis, J. A, Ferdman, R. D, Ferrara, E. C, Fonseca, E, Gentile, P. A, Jones, G, Jones, M. L, Lam, M. T, Levin, L, Lorimer, D. R, Lynch, R. S, McLaughlin, M. A, Mingarelli, C. M. F, Ng, C, Nice, D. J, Pennucci, T. T, Ransom, S. M, Ray, P. S, Spiewak, R, Stairs, I. H, Stovall, K, Swiggum, J. K, and Zhu, W. W
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Astronomy ,Astrophysics - Abstract
The North American Nanohertz Observatory for Gravitational Waves (NANOGrav) has observed dozens ofmillisecond pulsars for over a decade. We have accrued a large collection of dispersion measure (DM)measurements sensitive to the total electron content between Earth and the pulsars at each observation. All lines ofsight cross through the solar wind (SW), which produces correlated DM fluctuations in all pulsars. We develop andapply techniques for extracting the imprint of the SW from the full collection of DM measurements in the recentlyreleased NANOGrav 11 yr data set. We filter out long-timescale DM fluctuations attributable to structure in theinterstellar medium and carry out a simultaneous analysis of all pulsars in our sample that can differentiate thecorrelated signature of the wind from signals unique to individual lines of sight. When treating the SW asspherically symmetric and constant in time, we find the electron number density at 1au to be 7.9 ± 0.2 cm(exp -3). Wefind our data to be insensitive to long-term variation in the density of the wind. We argue that our techniques pairedwith a high-cadence, low-radio-frequency observing campaign of near-ecliptic pulsars would be capable ofmapping out large-scale latitudinal structure in the wind.
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- 2019
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13. Narrowband Searches for Continuous and Long-duration Transient Gravitational Waves from Known Pulsars in the LIGO-Virgo Third Observing Run
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Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adhikari, N., Adhikari, R. X., Adya, V. B., Affeldt, C., Agarwal, D., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Akutsu, T., Albanesi, S., Allocca, A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Ando, M., Andrade, T., Andres, N., Angelova, V, Ansoldi, S., Antelis, J. M., Antier, S., Appert, S., Arai, Koji, Arai, Koya, Arai, Y., Araki, S., Araya, A., Araya, M. C., Areeda, J. S., Arene, M., Aritomi, N., Arnaud, N., Aronson, S. M., Arun, K. G., Asada, H., Asali, Y., Ashton, G., Aso, Y., Assiduo, M., Aston, S. M., Astone, P., Aubin, F., Austin, C., Babak, S., Badaracco, F., Bader, M. K. M., Badger, C., Bae, S., Bae, Y., Baer, A. M., Bagnasco, S., Bai, Y., Bailes, M., Baiotti, L., Baird, J., Bajpai, R., Ball, M., Ballardin, G., Ballmer, S. W., Balsamo, A., Baltus, G., Banagiri, S., Bankar, D., Barayoga, J. C., Barbieri, C., Barish, B. C., Barker, D., Barneo, P., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Barton, M. A., Bartos, I, Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Baylor, A. C., Bazzan, M., Becsy, B., Bedakihale, V. M., Bejger, M., Belahcene, I, Benedetto, V, Beniwal, D., Bennett, T. F., Bentley, J. D., Benyaala, M., Bergamin, F., Berger, B. K., Bernuzzi, S., Bersanetti, D., Bertolini, A., Betzwieser, J., Beveridge, D., Are, R., Bhardwaj, U., Bhattacharjee, D., Bhaumik, S., Bilenko, I. A., Billingsley, G., Bini, S., Birney, R., Birnholtz, O., Biscans, S., Bischi, M., Biscoveanu, S., Bisht, A., Biswas, B., Bitossi, M., Bizouard, M-A, Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bobba, F., Bode, N., Boer, M., Bogaert, G., Boldrini, M., Bonavena, L. D., Bondu, F., Bonilla, E., Bonn, Booker, P., Boom, B. A., Bork, R., Boschi, V, Bose, N., Bose, S., Bossilkov, V, Boudart, V, Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branch, A., Branchesi, M., Brau, J. E., Breschi, M., Briant, T., Briggs, J. H., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A. F., Brooks, J., Brown, D. D., Brunett, S., Bruno, G., Bruntz, R., Bryant, J., Bulik, T., Bulten, H. J., Buonanno, A., Buscicchio, R., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Calderon Bustillo, J., Callaghan, J. D., Callister, T. A., Calloni, E., Cameron, J., Camp, J. B., Canepa, M., Canevarolo, S., Cannavacciuolo, M., Cannon, K. C., Cao, H., Cao, Z., Capocasa, E., Capote, E., Carapella, G., Carbognani, F., Carlin, J. B., Carney, M. F., Carpinelli, M., Carrillo, G., Carullo, G., Carver, T. L., Diaz, J. Casanueva, Casentini, C., Castaldi, G., Caudill, S., Cavaglia, M., Cavalier, F., Cavalieri, R., Ceasar, M., Cella, G., Cerda-Duran, P., Cesarini, E., Chaibi, W., Chakravarti, K., Subrahmanya, S. Chalathadka, Champion, E., Chan, C-H, Chan, C., Chan, C. L., Chan, K., Chan, M., Ra, K., Chanial, P., Chao, S., Charlton, P., Chase, E. A., Chass, e-Mottin, E., Chatterjee, C., Chatterjee, Debarati, Chatterjee, Deep, Chaturvedi, M., Chaty, S., Chen, C., Chen, H. Y., Chen, J., Chen, K., Chen, X., Chen, Y-B, Chen, Y-R, Chen, Z., Cheng, H., Cheong, C. K., Cheung, H. Y., Chia, H. Y., Chiadini, F., Chiang, C-Y, Chiarini, G., Chierici, R., Chincarini, A., Chiofalo, M. L., Chiummo, A., Cho, G., Cho, H. S., Choudhary, R. K., Choudhary, S., Christensen, N., Chu, H., Chu, Q., Chu, Y-K, Chua, S., Chung, K. W., Ciani, G., Ciecielag, P., Cifaldi, M., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, E. N., Clark, J. A., Clarke, L., Clearwater, P., Clesse, S., Cleva, F., Coccia, E., Codazzo, E., Cohadon, P-F, Cohen, D. E., Cohen, L., Colleoni, M., Collette, C. G., Colombo, A., Colpi, M., Compton, C. M., Constancio, J, R., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrion, I, Corezzi, S., Corley, K. 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L., Nagano, K., Nagano, S., Nagar, A., Nakamura, K., Nakano, H., Nakano, M., Nakashima, R., Nakayama, Y., Napolano, V., Nardecchia, I., Narikawa, T., Naticchioni, L., Nayak, B., Nayak, R. K., Negishi, R., Neil, B. F., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neubauer, P., Neunzert, A., Ng, K. Y., Ng, S. W. S., Nguyen, C., Nguyen, P., Nguyen, T., Quynh, L. Nguyen, Ni, W. -T., Nichols, S. A., Nishizawa, A., Nissanke, S., Nitoglia, E., Nocera, F., Norman, M., North, C., Nozaki, S., Nuttall, L. K., Oberling, J., O’Brien, B. D., Obuchi, Y., O’Dell, J., Oelker, E., Ogaki, W., Oganesyan, G., Oh, J. J., Oh, K., Oh, S. H., Ohashi, M., Ohishi, N., Ohkawa, M., Ohme, F., Ohta, H., Okada, M. A., Okutani, Y., Okutomi, K., Olivetto, C., Oohara, K., Ooi, C., Oram, R., O’Reilly, B., Ormiston, R. G., Ormsby, N. D., Ortega, L. F., O’Shaughnessy, R., O’Shea, E., Oshino, S., Ossokine, S., Osthelder, C., Otabe, S., Ottaway, D. J., Overmier, H., Pace, A. E., Pagano, G., Page, M. A., Pagliaroli, G., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pan, H., Pan, K., Panda, P. K., Pang, H., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Panther, F. H., Paoletti, F., Paoli, A., Paolone, A., Parisi, A., Park, H., Park, J., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patel, M., Pathak, M., Patricelli, B., Patron, A. S., Patrone, S., Paul, S., Payne, E., Pedraza, M., Pegoraro, M., Pele, A., Arellano, F. E. Peña, Penn, S., Perego, A., Pereira, A., Pereira, T., Perez, C. J., Périgois, C., Perkins, C. C., Perreca, A., Perriès, S., Petermann, J., Petterson, D., Pfeiffer, H. P., Pham, K. A., Phukon, K. S., Piccinni, O. J., Pichot, M., Piendibene, M., Piergiovanni, F., Pierini, L., Pierro, V., Pillant, G., Pillas, M., Pilo, F., Pinard, L., Pinto, I. M., Pinto, M., Piotrzkowski, K., Pirello, M., Pitkin, M. D., Placidi, E., Planas, L., Plastino, W., Pluchar, C., Poggiani, R., Polini, E., Pong, D. Y. T., Ponrathnam, S., Popolizio, P., Porter, E. K., Poulton, R., Powell, J., Pracchia, M., Pradier, T., Prajapati, A. K., Prasai, K., Prasanna, R., Pratten, G., Principe, M., Prodi, G. A., Prokhorov, L., Prosposito, P., Prudenzi, L., Puecher, A., Punturo, M., Puosi, F., Puppo, P., Pürrer, M., Qi, H., Quetschke, V., Quitzow-James, R., Raab, F. J., Raaijmakers, G., Radkins, H., Radulesco, N., Raffai, P., Rail, S. X., Raja, S., Rajan, C., Ramirez, K. E., Ramirez, T. D., Ramos-Buades, A., Rana, J., Rapagnani, P., Rapol, U. D., Ray, A., Raymond, V., Raza, N., Razzano, M., Read, J., Rees, L. A., Regimbau, T., Rei, L., Reid, S., Reid, S. W., Reitze, D. H., Relton, P., Renzini, A., Rettegno, P., Rezac, M., Ricci, F., Richards, D., Richardson, J. W., Richardson, L., Riemenschneider, G., Riles, K., Rinaldi, S., Rink, K., Rizzo, M., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rodriguez, S., Rolland, L., Rollins, J. G., Romanelli, M., Romano, R., Romel, C. L., Romero-Rodríguez, A., Romero-Shaw, I. M., Romie, J. H., Ronchini, S., Rosa, L., Rose, C. A., Rosińska, D., Ross, M. P., Rowan, S., Rowlinson, S. J., Roy, S., Roy, Santosh, Roy, Soumen, Rozza, D., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadiq, J., Sago, N., Saito, S., Saito, Y., Sakai, K., Sakai, Y., Sakellariadou, M., Sakuno, Y., Salafia, O. S., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sanchez, E. J., Sanchez, J. H., Sanchez, L. E., Sanchis-Gual, N., Sanders, J. R., Sanuy, A., Saravanan, T. R., Sarin, N., Sassolas, B., Satari, H., Sato, S., Sato, T., Sauter, O., Savage, R. L., Sawada, T., Sawant, D., Sawant, H. L., Sayah, S., Schaetzl, D., Scheel, M., Scheuer, J., Schiworski, M., Schmidt, P., Schmidt, S., Schnabel, R., Schneewind, M., Schofield, R. M. S., Schönbeck, A., Schulte, B. W., Schutz, B. F., Schwartz, E., Scott, J., Scott, S. M., Seglar-Arroyo, M., Sekiguchi, T., Sekiguchi, Y., Sellers, D., Sengupta, A. S., Sentenac, D., Seo, E. G., Sequino, V., Sergeev, A., Setyawati, Y., Shaffer, T., Shahriar, M. S., Shams, B., Shao, L., Sharma, A., Sharma, P., Shawhan, P., Shcheblanov, N. S., Shibagaki, S., Shikauchi, M., Shimizu, R., Shimoda, T., Shimode, K., Shinkai, H., Shishido, T., Shoda, A., Shoemaker, D. H., Shoemaker, D. M., Shyamsundar, S., Sieniawska, M., Sigg, D., Singer, L. P., Singh, D., Singh, N., Singha, A., Sintes, A. M., Sipala, V., Skliris, V., Slagmolen, B. J. J., Slaven-Blair, T. J., Smetana, J., Smith, J. R., Smith, R. J. E., Soldateschi, J., Somala, S. N., Somiya, K., Son, E. J., Soni, K., Soni, S., Sordini, V., Sorrentino, F., Sorrentino, N., Sotani, H., Soulard, R., Souradeep, T., Sowell, E., Spagnuolo, V., Spencer, A. P., Spera, M., Srinivasan, R., Srivastava, A. K., Srivastava, V., Staats, K., Stachie, C., Steer, D. A., Steinlechner, J., Steinlechner, S., Stops, D. J., Stover, M., Strain, K. A., Strang, L. C., Stratta, G., Strunk, A., Sturani, R., Stuver, A. L., Sudhagar, S., Sudhir, V., Sugimoto, R., Suh, H. G., Summerscales, T. Z., Sun, H., Sun, L., Sunil, S., Sur, A., Suresh, J., Sutton, P. J., Suzuki, Takamasa, Suzuki, Toshikazu, Swinkels, B. L., Szczepańczyk, M. J., Szewczyk, P., Tacca, M., Tagoshi, H., Tait, S. C., Takahashi, H., Takahashi, R., Takamori, A., Takano, S., Takeda, H., Takeda, M., Talbot, C. J., Talbot, C., Tanaka, H., Tanaka, Kazuyuki, Tanaka, Kenta, Tanaka, Taiki, Tanaka, Takahiro, Tanasijczuk, A. J., Tanioka, S., Tanner, D. B., Tao, D., Tao, L., San Martín, E. N. Tapia, Taranto, C., Tasson, J. D., Telada, S., Tenorio, R., Terhune, J. E., Terkowski, L., Thirugnanasambandam, M. P., Thomas, M., Thomas, P., Thompson, J. E., Thondapu, S. R., Thorne, K. A., Thrane, E., Tiwari, Shubhanshu, Tiwari, Srishti, Tiwari, V., Toivonen, A. M., Toland, K., Tolley, A. E., Tomaru, T., Tomigami, Y., Tomura, T., Tonelli, M., Torres-Forné, A., Torrie, C. I., e Melo, I. 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M., Xiao, L., Xu, W-R., Yamada, T., Yamamoto, H., Yamamoto, Kazuhiro, Yamamoto, Kohei, Yamamoto, T., Yamashita, K., Yamazaki, R., Yang, F. W., Yang, L., Yang, Y., Yang, Yang, Yang, Z., Yap, M. J., Yeeles, D. W., Yelikar, A. B., Ying, M., Yokogawa, K., Yokoyama, J., Yokozawa, T., Yoo, J., Yoshioka, T., Yu, Hang, Yu, Haocun, Yuzurihara, H., Zadrożny, A., Zanolin, M., Zeidler, S., Zelenova, T., Zendri, J. -P., Zevin, M., Zhan, M., Zhang, H., Zhang, J., Zhang, L., Zhang, T., Zhang, Y., Zhao, C., Zhao, G., Zhao, Y., Zhao, Yue, Zhou, R., Zhou, Z., Zhu, X. J., Zhu, Z. -H., Zucker, M. E., Zweizig, J., Antonopoulou, D., Arzoumanian, Z., Basu, A., Bogdanov, S., Cognard, I., Crowter, K., Enoto, T., Espinoza, C. M., Flynn, C. M. L., Fonseca, E., Good, D. C., Guillemot, L., Guillot, S., Harding, A. K., Keith, M. J., Kuiper, L., Lower, M. E., Lyne, A. G., Mckee, J. W., Meyers, B. W., Ng, C., Palfreyman, J. L., Shannon, R. M., Shaw, B., Stairs, I. H., Stappers, B. W., Tan, C. M., Theureau, G., Weltevrede, P., Andri??, T., Ar??ne, M., B??csy, B., Bustillo, J. Calder??n., Casanueva Diaz, J., Cavagli??, M., Cerd??-Dur??n, P., Chalathadka Subrahmanya, S., Cie??lar, M., Cordero-Carri??n, I., Cury??o, M., Dal Canton, T., Dall???osso, S., D??lya, G., D???angelo, B., D???antonio, S., Del??glise, S., D???emilio, V., D??az, M. C., Di Fiore, L., Di Fronzo, C., Di Giorgio, C., Di Giovanni, F., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Di Pace, S., Di Palma, I., Di Renzo, F., D???onofrio, L., D???urso, D., Estell??s, H., Fronz??, G. G., Garc??a-N????ez, C., Garc??a-Quir??s, C., Gonz??lez, G., Guix??, G., Hernandez Vivanco, F., H??bner, M. T., K??f??lian, F., Kr??lak, A., La Rosa, I., Lema??tre, A., Lopez Portilla, M., L??ck, H., Hernandez, I. Maga??a., Magazz??, C., M??rka, S., M??rka, Z., Miravet-Ten??s, M., Mu??iz, E. A., Nguyen Quynh, L., O???brien, B. D., O???dell, J., O???reilly, B., O???shaughnessy, R., O???shea, E., Arellano, F. E. 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Phys (API, FNWI), Astroparticle Physics (IHEF, IoP, FNWI), Gravitation and Astroparticle Physics Amsterdam, IoP (FNWI), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut des Hautes Études Scientifiques (IHES), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Abbott, R, Abbott, T, Acernese, F, Ackley, K, Adams, C, Adhikari, N, Adhikari, R, Adya, V, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O, Aiello, L, Ain, A, Ajith, P, Akutsu, T, Albanesi, S, Allocca, A, Altin, P, Amato, A, Anand, C, Anand, S, Ananyeva, A, Anderson, S, Anderson, W, Ando, M, Andrade, T, Andres, N, Andri??, T, Angelova, S, Ansoldi, S, Antelis, J, Antier, S, Appert, S, Arai, K, Arai, Y, Araki, S, Araya, A, Araya, M, Areeda, J, Ar??ne, M, Aritomi, N, Arnaud, N, Aronson, S, Arun, K, Asada, H, Asali, Y, Ashton, G, Aso, Y, Assiduo, M, Aston, S, Astone, P, Aubin, F, Austin, C, Babak, S, Badaracco, F, Bader, M, Badger, C, Bae, S, Bae, Y, Baer, A, Bagnasco, S, Bai, Y, Bailes, M, Baiotti, L, Baird, J, Bajpai, R, Ball, M, Ballardin, G, Ballmer, S, Balsamo, A, Baltus, G, Banagiri, S, Bankar, D, Barayoga, J, Barbieri, C, Barish, B, Barker, D, Barneo, P, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Barton, M, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, J, Baylor, A, Bazzan, M, B??csy, B, Bedakihale, V, Bejger, M, Belahcene, I, Benedetto, V, Beniwal, D, Bennett, T, Bentley, J, Benyaala, M, Bergamin, F, Berger, B, Bernuzzi, S, Bersanetti, D, Bertolini, A, Betzwieser, J, Beveridge, D, Bhandare, R, Bhardwaj, U, Bhattacharjee, D, Bhaumik, S, Bilenko, I, Billingsley, G, Bini, S, Birney, R, Birnholtz, O, Biscans, S, Bischi, M, Biscoveanu, S, Bisht, A, Biswas, B, Bitossi, M, Bizouard, M, Blackburn, J, Blair, C, Blair, D, Blair, R, Bobba, F, Bode, N, Boer, M, Bogaert, G, Boldrini, M, Bonavena, L, Bondu, F, Bonilla, E, Bonnand, R, Booker, P, Boom, B, Bork, R, Boschi, V, Bose, N, Bose, S, Bossilkov, V, Boudart, V, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, P, Bramley, A, Branch, A, Branchesi, M, Brau, J, Breschi, M, Briant, T, Briggs, J, Brillet, A, Brinkmann, M, Brockill, P, Brooks, A, Brooks, J, Brown, D, Brunett, S, Bruno, G, Bruntz, R, Bryant, J, Bulik, T, Bulten, H, Buonanno, A, Buscicchio, R, Buskulic, D, Buy, C, Byer, R, Cadonati, L, Cagnoli, G, Cahillane, C, Bustillo, J, Callaghan, J, Callister, T, Calloni, E, Cameron, J, Camp, J, Canepa, M, Canevarolo, S, Cannavacciuolo, M, Cannon, K, Cao, H, Cao, Z, Capocasa, E, Capote, E, Carapella, G, Carbognani, F, Carlin, J, Carney, M, Carpinelli, M, Carrillo, G, Carullo, G, Carver, T, Casanueva Diaz, J, Casentini, C, Castaldi, G, Caudill, S, Cavagli??, M, Cavalier, F, Cavalieri, R, Ceasar, M, Cella, G, Cerd??-Dur??n, P, Cesarini, E, Chaibi, W, Chakravarti, K, Chalathadka Subrahmanya, S, Champion, E, Chan, C, Chan, K, Chan, M, Chandra, K, Chanial, P, Chao, S, Charlton, P, Chase, E, Chassande-Mottin, E, Chatterjee, C, Chatterjee, D, Chaturvedi, M, Chaty, S, Chen, C, Chen, H, Chen, J, Chen, K, Chen, X, Chen, Y, Chen, Z, Cheng, H, Cheong, C, Cheung, H, Chia, H, Chiadini, F, Chiang, C, Chiarini, G, Chierici, R, Chincarini, A, Chiofalo, M, Chiummo, A, Cho, G, Cho, H, Choudhary, R, Choudhary, S, Christensen, N, Chu, H, Chu, Q, Chu, Y, Chua, S, Chung, K, Ciani, G, Ciecielag, P, Cie??lar, M, Cifaldi, M, Ciobanu, A, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, E, Clark, J, Clarke, L, Clearwater, P, Clesse, S, Cleva, F, Coccia, E, Codazzo, E, Cohadon, P, Cohen, D, Cohen, L, Colleoni, M, Collette, C, Colombo, A, Colpi, M, Compton, C, Constancio, M, Conti, L, Cooper, S, Corban, P, Corbitt, T, Cordero-Carri??n, I, Corezzi, S, Corley, K, Cornish, N, Corre, D, Corsi, A, Cortese, S, Costa, C, Cotesta, R, Coughlin, M, Coulon, J, Countryman, S, Cousins, B, Couvares, P, Coward, D, Cowart, M, Coyne, D, Coyne, R, Creighton, J, Creighton, T, Criswell, A, Croquette, M, Crowder, S, Cudell, J, Cullen, T, Cumming, A, Cummings, R, Cunningham, L, Cuoco, E, Cury??o, M, Dabadie, P, Dal Canton, T, Dall???osso, S, D??lya, G, Dana, A, Daneshgaranbajastani, L, D???angelo, B, Danilishin, S, D???antonio, S, Danzmann, K, Darsow-Fromm, C, Dasgupta, A, Datrier, L, Datta, S, Dattilo, V, Dave, I, Davier, M, Davies, G, Davis, D, Davis, M, Daw, E, Dean, R, Debra, D, Deenadayalan, M, Degallaix, J, De Laurentis, M, Del??glise, S, Del Favero, V, De Lillo, F, De Lillo, N, Del Pozzo, W, Demarchi, L, De Matteis, F, D???emilio, V, Demos, N, Dent, T, Depasse, A, De Pietri, R, De Rosa, R, De Rossi, C, Desalvo, R, De Simone, R, Dhurandhar, S, D??az, M, Diaz-Ortiz, M, Didio, N, Dietrich, T, Di Fiore, L, Di Fronzo, C, Di Giorgio, C, Di Giovanni, F, Di Giovanni, M, Di Girolamo, T, Di Lieto, A, Ding, B, Di Pace, S, Di Palma, I, Di Renzo, F, Divakarla, A, Dmitriev, A, Doctor, Z, D???onofrio, L, Donovan, F, Dooley, K, Doravari, S, Dorrington, I, Drago, M, Driggers, J, Drori, Y, Ducoin, J, Dupej, P, Durante, O, D???urso, D, Duverne, P, Dwyer, S, Eassa, C, Easter, P, Ebersold, M, Eckhardt, T, Eddolls, G, Edelman, B, Edo, T, Edy, O, Effler, A, Eguchi, S, Eichholz, J, Eikenberry, S, Eisenmann, M, Eisenstein, R, Ejlli, A, Engelby, E, Enomoto, Y, Errico, L, Essick, R, Estell??s, H, Estevez, D, Etienne, Z, Etzel, T, Evans, M, Evans, T, Ewing, B, Fafone, V, Fair, H, Fairhurst, S, Farah, A, Farinon, S, Farr, B, Farr, W, Farrow, N, Fauchon-Jones, E, Favaro, G, Favata, M, Fays, M, Fazio, M, Feicht, J, Fejer, M, Fenyvesi, E, Ferguson, D, Fernandez-Galiana, A, Ferrante, I, Ferreira, T, Fidecaro, F, Figura, P, Fiori, I, Fishbach, M, Fisher, R, Fittipaldi, R, Fiumara, V, Flaminio, R, Floden, E, Fong, H, Font, J, Fornal, B, Forsyth, P, Franke, A, Frasca, S, Frasconi, F, Frederick, C, Freed, J, Frei, Z, Freise, A, Frey, R, Fritschel, P, Frolov, V, Fronz??, G, Fujii, Y, Fujikawa, Y, Fukunaga, M, Fukushima, M, Fulda, P, Fyffe, M, Gabbard, H, Gadre, B, Gair, J, Gais, J, Galaudage, S, Gamba, R, Ganapathy, D, Ganguly, A, Gao, D, Gaonkar, S, Garaventa, B, Garc??a-N????ez, C, Garc??a-Quir??s, C, Garufi, F, Gateley, B, Gaudio, S, Gayathri, V, Ge, G, Gemme, G, Gennai, A, George, J, Gerberding, O, Gergely, L, Gewecke, P, Ghonge, S, Ghosh, A, Ghosh, S, Giacomazzo, B, Giacoppo, L, Giaime, J, Giardina, K, Gibson, D, Gier, C, Giesler, M, Giri, P, Gissi, F, Glanzer, J, Gleckl, A, Godwin, P, Goetz, E, Goetz, R, Gohlke, N, Goncharov, B, Gonz??lez, G, Gopakumar, A, Gosselin, M, Gouaty, R, Gould, D, Grace, B, Grado, A, Granata, M, Granata, V, Grant, A, Gras, S, Grassia, P, Gray, C, Gray, R, Greco, G, Green, A, Green, R, Gretarsson, A, Gretarsson, E, Griffith, D, Griffiths, W, Griggs, H, Grignani, G, Grimaldi, A, Grimm, S, Grote, H, Grunewald, S, Gruning, P, Guerra, D, Guidi, G, Guimaraes, A, Guix??, G, Gulati, H, Guo, H, Guo, Y, Gupta, A, Gupta, P, Gustafson, E, Gustafson, R, Guzman, F, Ha, S, Haegel, L, Hagiwara, A, Haino, S, Halim, O, Hall, E, Hamilton, E, Hammond, G, Han, W, Haney, M, Hanks, J, Hanna, C, Hannam, M, Hannuksela, O, Hansen, H, Hansen, T, Hanson, J, Harder, T, Hardwick, T, Haris, K, Harms, J, Harry, G, Harry, I, Hartwig, D, Hasegawa, K, Haskell, B, Hasskew, R, Haster, C, Hattori, K, Haughian, K, Hayakawa, H, Hayama, K, Hayes, F, Healy, J, Heidmann, A, Heidt, A, Heintze, M, Heinze, J, Heinzel, J, Heitmann, H, Hellman, F, Hello, P, Helmling-Cornell, A, Hemming, G, Hendry, M, Heng, I, Hennes, E, Hennig, J, Hennig, M, Hernandez, A, Hernandez Vivanco, F, Heurs, M, Hild, S, Hill, P, Himemoto, Y, Hines, A, Hiranuma, Y, Hirata, N, Hirose, E, Ho, W, Hochheim, S, Hofman, D, Hohmann, J, Holcomb, D, Holland, N, Hollows, I, Holmes, Z, Holt, K, Holz, D, Hong, Z, Hopkins, P, Hough, J, Hourihane, S, Howell, E, Hoy, C, Hoyland, D, Hreibi, A, Hsieh, B, Hsu, Y, Huang, G, Huang, H, Huang, P, Huang, Y, H??bner, M, Huddart, A, Hughey, B, Hui, D, Hui, V, Husa, S, Huttner, S, Huxford, R, Huynh-Dinh, T, Ide, S, Idzkowski, B, Iess, A, Ikenoue, B, Imam, S, Inayoshi, K, Ingram, C, Inoue, Y, Ioka, K, Isi, M, Isleif, K, Ito, K, Itoh, Y, Iyer, B, Izumi, K, Jaberianhamedan, V, Jacqmin, T, Jadhav, S, James, A, Jan, A, Jani, K, Janquart, J, Janssens, K, Janthalur, N, Jaranowski, P, Jariwala, D, Jaume, R, Jenkins, A, Jenner, K, Jeon, C, Jeunon, M, Jia, W, Jin, H, Johns, G, Jones, A, Jones, D, Jones, J, Jones, P, Jones, R, Jonker, R, Ju, L, Jung, P, Jung, K, Junker, J, Juste, V, Kaihotsu, K, Kajita, T, Kakizaki, M, Kalaghatgi, C, Kalogera, V, Kamai, B, Kamiizumi, M, Kanda, N, Kandhasamy, S, Kang, G, Kanner, J, Kao, Y, Kapadia, S, Kapasi, D, Karat, S, Karathanasis, C, Karki, S, Kashyap, R, Kasprzack, M, Kastaun, W, Katsanevas, S, Katsavounidis, E, Katzman, W, Kaur, T, Kawabe, K, Kawaguchi, K, Kawai, N, Kawasaki, T, K??f??lian, F, Keitel, D, Key, J, Khadka, S, Khalili, F, Khan, S, Khazanov, E, Khetan, N, Khursheed, M, Kijbunchoo, N, Kim, C, Kim, J, Kim, K, Kim, W, Kim, Y, Kimball, C, Kimura, N, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J, Kita, N, Kitazawa, H, Kleybolte, L, Klimenko, S, Knee, A, Knowles, T, Knyazev, E, Koch, P, Koekoek, G, Kojima, Y, Kokeyama, K, Koley, S, Kolitsidou, P, Kolstein, M, Komori, K, Kondrashov, V, Kong, A, Kontos, A, Koper, N, Korobko, M, Kotake, K, Kovalam, M, Kozak, D, Kozakai, C, Kozu, R, Kringel, V, Krishnendu, N, Kr??lak, A, Kuehn, G, Kuei, F, Kuijer, P, Kumar, A, Kumar, P, Kumar, R, Kume, J, Kuns, K, Kuo, C, Kuo, H, Kuromiya, Y, Kuroyanagi, S, Kusayanagi, K, Kuwahara, S, Kwak, K, Lagabbe, P, Laghi, D, Lalande, E, Lam, T, Lamberts, A, Landry, M, Lane, B, Lang, R, Lange, J, Lantz, B, La Rosa, I, Lartaux-Vollard, A, Lasky, P, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Y, Lee, H, Lee, J, Lee, K, Lee, R, Lehmann, J, Lema??tre, A, Leonardi, M, Leroy, N, Letendre, N, Levesque, C, Levin, Y, Leviton, J, Leyde, K, Li, A, Li, B, Li, J, Li, K, Li, T, Li, X, Lin, C, Lin, F, Lin, H, Lin, L, Linde, F, Linker, S, Linley, J, Littenberg, T, Liu, G, Liu, J, Liu, K, Liu, X, Llamas, F, Llorens-Monteagudo, M, Lo, R, Lockwood, A, London, L, Longo, A, Lopez, D, Lopez Portilla, M, Lorenzini, M, Loriette, V, Lormand, M, Losurdo, G, Lott, T, Lough, J, Lousto, C, Lovelace, G, Lucaccioni, J, L??ck, H, Lumaca, D, Lundgren, A, Luo, L, Lynam, J, Macas, R, Macinnis, M, Macleod, D, Macmillan, I, Macquet, A, Hernandez, I, Magazz??, C, Magee, R, Maggiore, R, Magnozzi, M, Mahesh, S, Majorana, E, Makarem, C, Maksimovic, I, Maliakal, S, Malik, A, Man, N, Mandic, V, Mangano, V, Mango, J, Mansell, G, Manske, M, Mantovani, M, Mapelli, M, Marchesoni, F, Marchio, M, Marion, F, Mark, Z, M??rka, S, M??rka, Z, Markakis, C, Markosyan, A, Markowitz, A, Maros, E, Marquina, A, Marsat, S, Martelli, F, Martin, I, Martin, R, Martinez, M, Martinez, V, Martinovic, K, Martynov, D, Marx, E, Masalehdan, H, Mason, K, Massera, E, Masserot, A, Massinger, T, Masso-Reid, M, Mastrogiovanni, S, Matas, A, Mateu-Lucena, M, Matichard, F, Matiushechkina, M, Mavalvala, N, Mccann, J, Mccarthy, R, Mcclelland, D, Mcclincy, P, Mccormick, S, Mcculler, L, Mcghee, G, Mcguire, S, Mcisaac, C, Mciver, J, Mcrae, T, Mcwilliams, S, Meacher, D, Mehmet, M, Mehta, A, Meijer, Q, Melatos, A, Melchor, D, Mendell, G, Menendez-Vazquez, A, Menoni, C, Mercer, R, Mereni, L, Merfeld, K, Merilh, E, Merritt, J, Merzougui, M, Meshkov, S, Messenger, C, Messick, C, Meyers, P, Meylahn, F, Mhaske, A, Miani, A, Miao, H, Michaloliakos, I, Michel, C, Michimura, Y, Middleton, H, Milano, L, Miller, A, Miller, B, Millhouse, M, Mills, J, Milotti, E, Minazzoli, O, Minenkov, Y, Mio, N, Mir, L, Miravet-Ten??s, M, Mishra, C, Mishra, T, Mistry, T, Mitra, S, Mitrofanov, V, Mitselmakher, G, Mittleman, R, Miyakawa, O, Miyamoto, A, Miyazaki, Y, Miyo, K, Miyoki, S, Mo, G, Modafferi, L, Moguel, E, Mogushi, K, Mohapatra, S, Mohite, S, Molina, I, Molina-Ruiz, M, Mondin, M, Montani, M, Moore, C, Moragues, J, Moraru, D, Morawski, F, More, A, Moreno, C, Moreno, G, Mori, Y, Morisaki, S, Moriwaki, Y, Mours, B, Mow-Lowry, C, Mozzon, S, Muciaccia, F, Mukherjee, A, Mukherjee, D, Mukherjee, S, Mukund, N, Mullavey, A, Munch, J, Mu??iz, E, Murray, P, Musenich, R, Muusse, S, Nadji, S, Nagano, K, Nagano, S, Nagar, A, Nakamura, K, Nakano, H, Nakano, M, Nakashima, R, Nakayama, Y, Napolano, V, Nardecchia, I, Narikawa, T, Naticchioni, L, Nayak, B, Nayak, R, Negishi, R, Neil, B, Neilson, J, Nelemans, G, Nelson, T, Nery, M, Neubauer, P, Neunzert, A, Ng, K, Ng, S, Nguyen, C, Nguyen, P, Nguyen, T, Nguyen Quynh, L, Ni, W, Nichols, S, Nishizawa, A, Nissanke, S, Nitoglia, E, Nocera, F, Norman, M, North, C, Nozaki, S, Nuttall, L, Oberling, J, O???brien, B, Obuchi, Y, O???dell, J, Oelker, E, Ogaki, W, Oganesyan, G, Oh, J, Oh, K, Oh, S, Ohashi, M, Ohishi, N, Ohkawa, M, Ohme, F, Ohta, H, Okada, M, Okutani, Y, Okutomi, K, Olivetto, C, Oohara, K, Ooi, C, Oram, R, O???reilly, B, Ormiston, R, Ormsby, N, Ortega, L, O???shaughnessy, R, O???shea, E, Oshino, S, Ossokine, S, Osthelder, C, Otabe, S, Ottaway, D, Overmier, H, Pace, A, Pagano, G, Page, M, Pagliaroli, G, Pai, A, Pai, S, Palamos, J, Palashov, O, Palomba, C, Pan, H, Pan, K, Panda, P, Pang, H, Pang, P, Pankow, C, Pannarale, F, Pant, B, Panther, F, Paoletti, F, Paoli, A, Paolone, A, Parisi, A, Park, H, Park, J, Parker, W, Pascucci, D, Pasqualetti, A, Passaquieti, R, Passuello, D, Patel, M, Pathak, M, Patricelli, B, Patron, A, Patrone, S, Paul, S, Payne, E, Pedraza, M, Pegoraro, M, Pele, A, Arellano, F, Penn, S, Perego, A, Pereira, A, Pereira, T, Perez, C, P??rigois, C, Perkins, C, Perreca, A, Perri??s, S, Petermann, J, Petterson, D, Pfeiffer, H, Pham, K, Phukon, K, Piccinni, O, Pichot, M, Piendibene, M, Piergiovanni, F, Pierini, L, Pierro, V, Pillant, G, Pillas, M, Pilo, F, Pinard, L, Pinto, I, Pinto, M, Piotrzkowski, K, Pirello, M, Pitkin, M, Placidi, E, Planas, L, Plastino, W, Pluchar, C, Poggiani, R, Polini, E, Pong, D, Ponrathnam, S, Popolizio, P, Porter, E, Poulton, R, Powell, J, Pracchia, M, Pradier, T, Prajapati, A, Prasai, K, Prasanna, R, Pratten, G, Principe, M, Prodi, G, Prokhorov, L, Prosposito, P, Prudenzi, L, Puecher, A, Punturo, M, Puosi, F, Puppo, P, P??rrer, M, Qi, H, Quetschke, V, Quitzow-James, R, Raab, F, Raaijmakers, G, Radkins, H, Radulesco, N, Raffai, P, Rail, S, Raja, S, Rajan, C, Ramirez, K, Ramirez, T, Ramos-Buades, A, Rana, J, Rapagnani, P, Rapol, U, Ray, A, Raymond, V, Raza, N, Razzano, M, Read, J, Rees, L, Regimbau, T, Rei, L, Reid, S, Reitze, D, Relton, P, Renzini, A, Rettegno, P, Rezac, M, Ricci, F, Richards, D, Richardson, J, Richardson, L, Riemenschneider, G, Riles, K, Rinaldi, S, Rink, K, Rizzo, M, Robertson, N, Robie, R, Robinet, F, Rocchi, A, Rodriguez, S, Rolland, L, Rollins, J, Romanelli, M, Romano, R, Romel, C, Romero-Rodr??guez, A, Romero-Shaw, I, Romie, J, Ronchini, S, Rosa, L, Rose, C, Rosi??ska, D, Ross, M, Rowan, S, Rowlinson, S, Roy, S, Rozza, D, Ruggi, P, Ryan, K, Sachdev, S, Sadecki, T, Sadiq, J, Sago, N, Saito, S, Saito, Y, Sakai, K, Sakai, Y, Sakellariadou, M, Sakuno, Y, Salafia, O, Salconi, L, Saleem, M, Salemi, F, Samajdar, A, Sanchez, E, Sanchez, J, Sanchez, L, Sanchis-Gual, N, Sanders, J, Sanuy, A, Saravanan, T, Sarin, N, Sassolas, B, Satari, H, Sato, S, Sato, T, Sauter, O, Savage, R, Sawada, T, Sawant, D, Sawant, H, Sayah, S, Schaetzl, D, Scheel, M, Scheuer, J, Schiworski, M, Schmidt, P, Schmidt, S, Schnabel, R, Schneewind, M, Schofield, R, Sch??nbeck, A, Schulte, B, Schutz, B, Schwartz, E, Scott, J, Scott, S, Seglar-Arroyo, M, Sekiguchi, T, Sekiguchi, Y, Sellers, D, Sengupta, A, Sentenac, D, Seo, E, Sequino, V, Sergeev, A, Setyawati, Y, Shaffer, T, Shahriar, M, Shams, B, Shao, L, Sharma, A, Sharma, P, Shawhan, P, Shcheblanov, N, Shibagaki, S, Shikauchi, M, Shimizu, R, Shimoda, T, Shimode, K, Shinkai, H, Shishido, T, Shoda, A, Shoemaker, D, Shyamsundar, S, Sieniawska, M, Sigg, D, Singer, L, Singh, D, Singh, N, Singha, A, Sintes, A, Sipala, V, Skliris, V, Slagmolen, B, Slaven-Blair, T, Smetana, J, Smith, J, Smith, R, Soldateschi, J, Somala, S, Somiya, K, Son, E, Soni, K, Soni, S, Sordini, V, Sorrentino, F, Sorrentino, N, Sotani, H, Soulard, R, Souradeep, T, Sowell, E, Spagnuolo, V, Spencer, A, Spera, M, Srinivasan, R, Srivastava, A, Srivastava, V, Staats, K, Stachie, C, Steer, D, Steinlechner, J, Steinlechner, S, Stops, D, Stover, M, Strain, K, Strang, L, Stratta, G, Strunk, A, Sturani, R, Stuver, A, Sudhagar, S, Sudhir, V, Sugimoto, R, Suh, H, Summerscales, T, Sun, H, Sun, L, Sunil, S, Sur, A, Suresh, J, Sutton, P, Suzuki, T, Swinkels, B, Szczepa??czyk, M, Szewczyk, P, Tacca, M, Tagoshi, H, Tait, S, Takahashi, H, Takahashi, R, Takamori, A, Takano, S, Takeda, H, Takeda, M, Talbot, C, Tanaka, H, Tanaka, K, Tanaka, T, Tanasijczuk, A, Tanioka, S, Tanner, D, Tao, D, Tao, L, Tapia San Mart??n, E, Taranto, C, Tasson, J, Telada, S, Tenorio, R, Terhune, J, Terkowski, L, Thirugnanasambandam, M, Thomas, M, Thomas, P, Thompson, J, Thondapu, S, Thorne, K, Thrane, E, Tiwari, S, Tiwari, V, Toivonen, A, Toland, K, Tolley, A, Tomaru, T, Tomigami, Y, Tomura, T, Tonelli, M, Torres-Forn??, A, Torrie, C, Tosta e Melo, I, T??yr??, D, Trapananti, A, Travasso, F, Traylor, G, Trevor, M, Tringali, M, Tripathee, A, Troiano, L, Trovato, A, Trozzo, L, Trudeau, R, Tsai, D, Tsang, K, Tsang, T, Tsao, J, Tse, M, Tso, R, Tsubono, K, Tsuchida, S, Tsukada, L, Tsuna, D, Tsutsui, T, Tsuzuki, T, Turbang, K, Turconi, M, Tuyenbayev, D, Ubhi, A, Uchikata, N, Uchiyama, T, Udall, R, Ueda, A, Uehara, T, Ueno, K, Ueshima, G, Unnikrishnan, C, Uraguchi, F, Urban, A, Ushiba, T, Utina, A, Vahlbruch, H, Vajente, G, Vajpeyi, A, Valdes, G, Valentini, M, Valsan, V, van Bakel, N, van Beuzekom, M, van den Brand, J, Van Den Broeck, C, Vander-Hyde, D, van der Schaaf, L, van Heijningen, J, Vanosky, J, van Putten, M, van Remortel, N, Vardaro, M, Vargas, A, Varma, V, Vas??th, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, P, Venneberg, J, Venugopalan, G, Verkindt, D, Verma, P, Verma, Y, Veske, D, Vetrano, F, Vicer??, A, Vidyant, S, Viets, A, Vijaykumar, A, Villa-Ortega, V, Vinet, J, Virtuoso, A, Vitale, S, Vo, T, Vocca, H, von Reis, E, von Wrangel, J, Vorvick, C, Vyatchanin, S, Wade, L, Wade, M, Wagner, K, Walet, R, Walker, M, Wallace, G, Wallace, L, Walsh, S, Wang, J, Wang, W, Ward, R, Warner, J, Was, M, Washimi, T, Washington, N, Watchi, J, Weaver, B, Webster, S, Weinert, M, Weinstein, A, Weiss, R, Weller, C, Wellmann, F, Wen, L, We??els, P, Wette, K, Whelan, J, White, D, Whiting, B, Whittle, C, Wilken, D, Williams, D, Williams, M, Williamson, A, Willis, J, Willke, B, Wilson, D, Winkler, W, Wipf, C, Wlodarczyk, T, Woan, G, Woehler, J, Wofford, J, Wong, I, Wu, C, Wu, D, Wu, H, Wu, S, Wysocki, D, Xiao, L, Xu, W, Yamada, T, Yamamoto, H, Yamamoto, K, Yamamoto, T, Yamashita, K, Yamazaki, R, Yang, F, Yang, L, Yang, Y, Yang, Z, Yap, M, Yeeles, D, Yelikar, A, Ying, M, Yokogawa, K, Yokoyama, J, Yokozawa, T, Yoo, J, Yoshioka, T, Yu, H, Yuzurihara, H, Zadro??ny, A, Zanolin, M, Zeidler, S, Zelenova, T, Zendri, J, Zevin, M, Zhan, M, Zhang, H, Zhang, J, Zhang, L, Zhang, T, Zhang, Y, Zhao, C, Zhao, G, Zhao, Y, Zhou, R, Zhou, Z, Zhu, X, Zhu, Z, Zucker, M, Zweizig, J, Antonopoulou, D, Arzoumanian, Z, Basu, A, Bogdanov, S, Cognard, I, Crowter, K, Enoto, T, Espinoza, C, Flynn, C, Fonseca, E, Good, D, Guillemot, L, Guillot, S, Harding, A, Keith, M, Kuiper, L, Lower, M, Lyne, A, Mckee, J, Meyers, B, Ng, C, Palfreyman, J, Shannon, R, Shaw, B, Stairs, I, Stappers, B, Tan, C, Theureau, G, Weltevrede, P, National Science Foundation (US), National Aeronautics and Space Administration (US), Science and Technology Facilities Council (UK), Generalitat Valenciana, Generalitat de Catalunya, European Research Council, European Commission, Ministerio de Economía y Competitividad (España), Govern de les Illes Balears, Agencia Nacional de Investigación y Desarrollo (Chile), Fondo Nacional de Desarrollo Científico y Tecnológico (Chile), The LIGO Scientific Collaboration, the Virgo Collaboration, the KAGRA Collaboration, Physics, Theoretical Physics, Elementary Particle Physics, Faculty of Sciences and Bioengineering Sciences, Andric, T., Arai, K., Arene, M., Becsy, B., Bustillo, J. C., Diaz, J. C., Cavaglia, M., Cerda-Duran, P., Subrahmanya, S. C., Chatterjee, D., Chiang, C. -Y., Chu, Y. -K., Cieslar, M., Cordero-Carrion, I., Curylo, M., Canton, T. D., Dall'Osso, S., Dalya, G., D'Angelo, B., D'Antonio, S., Deleglise, S., D'Emilio, V., Diaz, M. C., Fiore, L. D., Fronzo, C. D., Giorgio, C. D., Giovanni, F. D., Giovanni, M. D., Lieto, A. D., Pace, S. D., Palma, I. D., Renzo, F. D., D'Onofrio, L., D'Urso, D., Estelles, H., Fronze, G. G., Garcia-Nunez, C., Garcia-Quiros, C., Ghosh, A., Ghosh, S., Gonzalez, G., Guixe, G., Gupta, A., Vivanco, F. H., Hsieh, B. -H., Huang, G. -Z., Huang, H. -Y., Huang, Y. -C., Hubner, M. T., Kefelian, F., Krolak, A., Kumar, R., Kuo, H. -S., Rosa, I. L., Lemaitre, A., Lin, C. -Y., Lin, F. -K., Lin, F. -L., Portilla, M. B., Luck, H., Hernandez, I. M., Magazzu, C., Marka, S., Marka, Z., Mir, L. M., Miravet-Tenes, M., Mo, G., Mukherjee, A., Mukherjee, S., Muniz, E. A., Quynh, L. N., O'Brien, B. D., O'Dell, J., O'Reilly, B., O'Shaughnessy, R., O'Shea, E., Arellano, F. E. P., Perigois, C., Perries, S., Purrer, M., Romero-Rodriguez, A., Rosinska, D., Schonbeck, A., Suzuki, T., Szczepanczyk, M. J., Tanaka, K., Tanaka, T., San Martin, E. N. T., Tiwari, S., Torres-Forne, A., E Melo, I. T., Toyra, D., Tsao, J. -S., Van Bakel, N., Van Beuzekom, M., Van Den Brand, J. F. J., Van Der Schaaf, L., Van Heijningen, J. V., Van Putten, M. H. P. M., Van Remortel, N., Vasuth, M., Vicere, A., Reis, E. R. G. V., Wrangel, J. S. A. V., Wessels, P., Xu, W. -R., Yamamoto, K., Yu, H., Zadrozny, A., RS: FSE Grav. waves and fundamental physics, Grav. waves and fundamental physics, and RS: FSE MSP
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Gravitational wave astronomy ,Neutron stars ,Pulsars ,long-lived ,Astronomy ,frequency: time dependence ,spin ,General Relativity and Quantum Cosmology ,PRECISE ,QC350 ,LIGO ,neutron star ,QC ,pulsar ,QB ,astro-ph.HE ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,constraint: energy ,gravitational radiation: time dependence ,Physical Sciences ,[PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc] ,Astrophysics - High Energy Astrophysical Phenomena ,asymmetry ,PROPER MOTION ,radiation: electromagnetic ,gr-qc ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Neutron star ,O3 ,General Relativity and Quantum Cosmology (gr-qc) ,Astronomy & Astrophysics ,Transients ,energy loss: rotation ,SPIN-DOWN LIMIT ,Neutron Stars, Transients, Gravitational Waves, LIGO, Virgo, O3 ,SDG 7 - Affordable and Clean Energy ,Gravitational Waves ,Science & Technology ,GLITCHES ,Virgo ,CONSTRAINTS ,Astronomy and Astrophysics ,Neutron Stars ,sensitivity ,Dewey Decimal Classification::500 | Naturwissenschaften::520 | Astronomie, Kartographie ,VIRGO ,Physics and Astronomy ,Space and Planetary Science ,DISCOVERY ,DISTANCE ,ddc:520 ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,EMISSION ,ENERGETIC YOUNG PULSAR - Abstract
Abbott et al., Isolated neutron stars that are asymmetric with respect to their spin axis are possible sources of detectable continuous gravitational waves. This paper presents a fully coherent search for such signals from eighteen pulsars in data from LIGO and Virgo's third observing run (O3). For known pulsars, efficient and sensitive matched-filter searches can be carried out if one assumes the gravitational radiation is phase-locked to the electromagnetic emission. In the search presented here, we relax this assumption and allow both the frequency and the time derivative of the frequency of the gravitational waves to vary in a small range around those inferred from electromagnetic observations. We find no evidence for continuous gravitational waves, and set upper limits on the strain amplitude for each target. These limits are more constraining for seven of the targets than the spin-down limit defined by ascribing all rotational energy loss to gravitational radiation. In an additional search, we look in O3 data for long-duration (hours–months) transient gravitational waves in the aftermath of pulsar glitches for six targets with a total of nine glitches. We report two marginal outliers from this search, but find no clear evidence for such emission either. The resulting duration-dependent strain upper limits do not surpass indirect energy constraints for any of these targets., This material is based upon work supported by NSF's LIGO Laboratory, which is a major facility fully funded by the National Science Foundation. The authors also gratefully acknowledge the support of the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO 600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS), and the Netherlands Organization for Scientific Research (NWO), for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India, the Science & Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigación (AEI), the Spanish Ministerio de Ciencia e Innovación and Ministerio de Universidades, the Conselleria de Fons Europeus, Universitat i Cultura and the Direcció General de Política Universitaria i Recerca del Govern de les Illes Balears, the Conselleria d'Innovació Universitats, Ciència i Societat Digital de la Generalitat Valenciana and the CERCA Programme Generalitat de Catalunya, Spain, the National Science Centre of Poland and the European Union—European Regional Development Fund; Foundation for Polish Science (FNP), the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Social Funds (ESF), the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the French Lyon Institute of Origins (LIO), the Belgian Fonds de la Recherche Scientifique (FRS-FNRS), Actions de Recherche Concertées (ARC) and Fonds Wetenschappelijk Onderzoek—Vlaanderen (FWO), Belgium, the Paris Île-de-France Region, the National Research, Development and Innovation Office Hungary (NKFIH), the National Research Foundation of Korea, the Natural Science and Engineering Research Council Canada, Canadian Foundation for Innovation (CFI), the Brazilian Ministry of Science, Technology, and Innovations, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Leverhulme Trust, the Research Corporation, the Ministry of Science and Technology (MOST), Taiwan, the United States Department of Energy, and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, INFN, and CNRS for provision of computational resources. This work was supported by MEXT, JSPS Leading-edge Research Infrastructure Program, JSPS Grant-in-Aid for Specially Promoted Research 26000005, JSPS Grant-in-Aid for Scientific Research on Innovative Areas 2905: JP17H06358, JP17H06361 and JP17H06364, JSPS Core-to-Core Program A. Advanced Research Networks, JSPS Grant-in-Aid for Scientific Research (S) 17H06133 and 20H05639, JSPS Grant-in-Aid for Transformative Research Areas (A) 20A203: JP20H05854, the joint research program of the Institute for Cosmic Ray Research, University of Tokyo, National Research Foundation (NRF), Computing Infrastructure Project of KISTI-GSDC, Korea Astronomy and Space Science Institute (KASI), and Ministry of Science and ICT (MSIT) in Korea, Academia Sinica (AS), AS Grid Center (ASGC) and the Ministry of Science and Technology (MoST) in Taiwan under grants including AS-CDA-105-M06, Advanced Technology Center (ATC) of NAOJ, and Mechanical Engineering Center of KEK. We acknowledge that CHIME is located on the traditional, ancestral, and unceded territory of the Syilx/Okanagan people. We are grateful to the staff of the Dominion Radio Astrophysical Observatory, which is operated by the National Research Council of Canada. CHIME is funded by a grant from the Canada Foundation for Innovation (CFI) 2012 Leading Edge Fund (Project 31170) and by contributions from the provinces of British Columbia, Québec, and Ontario. The CHIME/FRB Project, which enabled development in common with the CHIME/Pulsar instrument, is funded by a grant from the CFI 2015 Innovation Fund (Project 33213) and by contributions from the provinces of British Columbia and Québec, and by the Dunlap Institute for Astronomy and Astrophysics at the University of Toronto. Additional support was provided by the Canadian Institute for Advanced Research (CIFAR), McGill University, and the McGill Space Institute thanks to the Trottier Family Foundation, and the University of British Columbia. The CHIME/Pulsar instrument hardware was funded by NSERC RTI-1 grant EQPEQ 458893-2014. This research was enabled in part by support provided by WestGrid (www.westgrid.ca) and Compute Canada (www.computecanada.ca). We acknowledge support from the Natural Sciences and Engineering Research Council of Canada (NSERC) funding reference #CITA 490888-16, the Canadian Institute for Advanced Research, and the UBC Four Year Fellowship (6456). We acknowledge support from EPSRC/STFC fellowship (EP/T017325/1), ANID/FONDECYT grants 1171421 and 1211964, and NASA grants 80NSSC19K1444 and 80NSSC21K0091. This work is supported by NASA through the NICER mission and the Astrophysics Explorers Program, and uses data and software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory.
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- 2022
14. The NANOGrav 11 Year Data Set: Pulsar-Timing Constraints on the Stochastic Gravitational-Wave Background
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Arzoumanian, Z, Baker, P. T, Brazier, A, Burke-Spolaor, S, Chamberlin, S. J, Chatterjee, S, Christy, B, Cordes, J. M, Cornish, N. J, Crawford, F, Cromartie, H. Thankful, Crowter, K, DeCesar, M, Demorest, P. B, Dolch, T, Ellis, J. A, Ferdman, R. D, Ferrara, E, Folkner, W. M, Fonseca, E, Garver-Daniels, N, Gentile, P. A, Haas, R, Hazboun, J. S, Huerta, E. A, Islo, K, Jones, G, Jones, M. L, Kaplan, D. L, Kaspi, V. M, Lam, M. T, Lazio, T. J. W, Levin, L, Lommen, A. N, 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, Park, R. S, Pennucci, T. T, Pol, N. S, Ransom, S. M, Ray, P. S, Rasskazov, A, Siemens, X, Simon, J, Spiewak, R, Stairs, I. H, Stinebring, D. R, Stovall, K, Swiggum, J, Taylor, S. R, Vallisneri, M, van Haasteren, R, Vigeland, S, and Zhu, W. W
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Astrophysics - Abstract
We search for an isotropic stochastic gravitational-wave background (GWB) in the newly released 11 year data set from the North American Nanohertz Observatory for Gravitational Waves (NANOGrav). While we find no evidence for a GWB, we place constraints on a population of inspiraling supermassive black hole (SMBH) binaries, a network of decaying cosmic strings, and a primordial GWB. For the first time, we find that the GWB constraints are sensitive to the solar system ephemeris (SSE) model used and that SSE errors can mimic a GWB signal. We developed an approach that bridges systematic SSE differences, producing the first pulsar-timing array (PTA) constraints that are robust against SSE errors. We thus place a 95% upper limit on the GW-strain amplitude of A (sub GWB) < 1.45 × 10 (exp -15) at a frequency of f=1 yr(exp -1) for a fiducial f (exp -2/3) power-law spectrum and with interpulsar correlations modeled. This is a factor of approximately 2 improvement over the NANOGrav nine-year limit calculated using the same procedure. Previous PTA upper limits on the GWB (as well as their astrophysical and cosmological interpretations) will need revision in light of SSE systematic errors. We use our constraints to characterize the combined influence on the GWB of the stellar mass density in galactic cores, the eccentricity of SMBH binaries, and SMBH-galactic-bulge scaling relationships. We constrain the cosmic-string tension using recent simulations, yielding an SSE-marginalized 95% upper limit of G (sub mu) < 5.3 × 10(exp -11) - a factor of approximately 2 better than the published NANOGrav nine-year constraints. Our SSE-marginalized 95% upper limit on the energy density of a primordial GWB (for a radiation-dominated post-inflation universe) is omega (sub GWB)(f) h (exp 2) < 3.4 × 10 (exp -10).
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- 2018
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15. The Nanograv Nine-Year Data Set: Measurement and Analysis of Variations in Dispersion Measures
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Jones, M. L, McLaughlin, M. A, Lam, M. T, Cordes, J. M, Levin, L, Chatterjee, S, Arzoumanian, Z, Crowter, K, Demorest, P. B, Dolch, T, Ellis, J. A, Ferdman, R. D, Fonseca, E, Gonzalez, M. E, Jones, G, Lazio, T. J. W, Nice, D. J, Pennucci, T. T, Ransom, S. M, Stinebring, D. R, Stairs, I. H, Stovall, K, Swiggum, J. K, and Zhu, W. W
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Astrophysics - Abstract
We analyze dispersion measure(DM) variations of 37 millisecond pulsars in the nine-year North American Nanohertz Observatory for Gravitational Waves (NANOGrav) data release and constrain the sources of these variations. DM variations can result from a changing distance between Earth and the pulsar, inhomogeneities in the interstellar medium, and solar effects. Variations are significant for nearly all pulsars, with characteristic timescales comparable to or even shorter than the average spacing between observations. Five pulsars have periodic annual variations, 14 pulsars have monotonically increasing or decreasing trends, and 14 pulsars show both effects. Of the four pulsars with linear trends that have line-of-sight velocity measurements, three are consistent with a changing distance and require an overdensity of free electrons local to the pulsar. Several pulsars show correlations between DM excesses and lines of sight that pass close to the Sun. Mapping of the DM variations as a function of the pulsar trajectory can identify localized interstellar medium features and, in one case, an upper limit to the size of the dispersing region of 4 au. Four pulsars show roughly Kolmogorov structure functions (SFs), and another four show SFs less steep than Kolmogorov. One pulsar has too large an uncertainty to allow comparisons. We discuss explanations for apparent departures from a Kolmogorov-like spectrum, and we show that the presence of other trends and localized features or gradients in the interstellar medium is the most likely cause.
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- 2017
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16. Pulsar Discovery by Global Volunteer Computing
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Knispel, B., Allen, B., Cordes, J. M., Deneva, J. S., Anderson, D., Aulbert, C., Bhat, N. D. R., Bock, O., Bogdanov, S., Brazier, A., Camilo, F., Champion, D. J., Chatterjee, S., Crawford, F., Demorest, P. B., Fehrmann, H., Freire, P. C. C., Gonzalez, M. E., Hammer, D., Hessels, J. W. T., Jenet, F. A., Kasian, L., Kaspi, V. M., Kramer, M., Lazarus, P., van Leeuwen, J., Lorimer, D. R., Lyne, A. G., Machenschalk, B., McLaughlin, M. A., Messenger, C., Nice, D. J., Papa, M. A., Pletsch, H. J., Prix, R., Ransom, S. M., Siemens, X., Stairs, I. H., Stappers, B. W., Stovall, K., and Venkataraman, A.
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- 2010
17. Tests of General Relativity from Timing the Double Pulsar
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Kramer, M., Stairs, I. H., Manchester, R. N., McLaughlin, M. A., Lyne, A. G., Ferdman, R. D., Burgay, M., Lorimer, D. R., Possenti, A., D'Amico, N., Sarkissian, J. M., Hobbs, G. B., Reynolds, J. E., Freire, P. C. C., and Camilo, F.
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- 2006
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18. A repeating fast radio burst
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Spitler, L. G., Scholz, P., Hessels, J. W. T., Bogdanov, S., Brazier, A., Camilo, F., Chatterjee, S., Cordes, J. M., Crawford, F., Deneva, J., Ferdman, R. D., Freire, P. C. C., Kaspi, V. M., Lazarus, P., Lynch, R., Madsen, E. C., McLaughlin, M. A., Patel, C., Ransom, S. M., Seymour, A., Stairs, I. H., Stappers, B. W., van Leeuwen, J., and Zhu, W. W.
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- 2016
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19. The NANOGrav Nine-Year Data Set: Limits on the Isotropic Stochastic Gravitational Wave Background
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Arzoumanian, Z, Brazier, A, Burke-Spolaor, S, Chamberlin, S. J, Chatterjee, S, Christy, B, Cordes, J. M, Cornish, N. J, Crowter, K, Demorest, P. B, Deng, X, Dolch, T, Ellis, J. A, Ferdman, R. D, Fonseca, E, Garver-Daniels, N, Gonzalez, M. E, Jenet, F, Jones, G, Jones, M. L, Kaspi, V. M, Koop, M, Lam, M. T, Lazio, T. J. W, Levin, L, Lommen, A. N, Lorimer, D. R, Luo, J, Lynch, R. S, Madison, D. R, McLaughlin, M. A, McWilliams, S. T, Mingarelli, C. M. F, Nice, D. J, Palliyaguru, N, Pennucci, T. T, Ransom, S. M, Sampson, L, Sanidas, S. A, Sesana, A, Siemens, X, Simon, J, Stairs, I. H, Stinebring, D. R, Stovall, K, Swiggum, J, Taylor, S. R, Vallisneri, M, Haasteren, R. Van, Wang, Y, and Zhu, W. W
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Astrophysics - Abstract
We compute upper limits on the nanohertz-frequency isotropic stochastic gravitational wave background (GWB) using the 9 year data set from the North American Nanohertz Observatory for Gravitational Waves (NANOGrav) collaboration. Well-tested Bayesian techniques are used to set upper limits on the dimensionless strain amplitude (at a frequency of 1 yr(exp -1) for a GWB from supermassive black hole binaries of A(sub gw) less than 1.5 x 10(exp -15). We also parameterize the GWB spectrum with a broken power-law model by placing priors on the strain amplitude derived from simulations of Sesana and McWilliams et al. Using Bayesian model selection we find that the data favor a broken power law to a pure power law with odds ratios of 2.2 and 22 to one for the Sesana and McWilliams prior models, respectively. Using the broken power-law analysis we construct posterior distributions on environmental factors that drive the binary to the GW-driven regime including the stellar mass density for stellar-scattering, mass accretion rate for circumbinary disk interaction, and orbital eccentricity for eccentric binaries, marking the first time that the shape of the GWB spectrum has been used to make astrophysical inferences. Returning to a power-law model, we place stringent limits on the energy density of relic GWs, OMEGA(sub gw) (f) h squared less than 4.2 x 10(exp -10). Our limit on the cosmic string GWB, OMEGA(sub gw) (f) h squared less than 2.2 x 10(exp -10), translates to a conservative limit on the cosmic string tension with G mu less than 3.3 x 10(exp -8), a factor of four better than the joint Planck and high-l‚ cosmic microwave background data from other experiments.
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- 2016
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20. A millisecond pulsar in a stellar triple system
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Ransom, S. M., Stairs, I. H., Archibald, A. M., Hessels, J. W. T., Kaplan, D. L., van Kerkwijk, M. H., Boyles, J., Deller, A. T., Chatterjee, S., Schechtman-Rook, A., Berndsen, A., Lynch, R. S., Lorimer, D. R., Karako-Argaman, C., Kaspi, V. M., Kondratiev, V. I., McLaughlin, M. A., van Leeuwen, J., Rosen, R., Roberts, M. S. E., and Stovall, K.
- Published
- 2014
- Full Text
- View/download PDF
21. Periodic activity from a fast radio burst source
- Author
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Amiri, M., Andersen, B. C., Bandura, K. M., Bhardwaj, M., Boyle, P. J., Brar, C., Chawla, P., Chen, T., Cliche, J. F., Cubranic, D., Deng, M., Denman, N. T., Dobbs, M., Dong, F. Q., Hill, A. S., Höfer, C., Josephy, A., Kania, J. W., Karuppusamy, R., Kaspi, V. M., Keimpema, A., Kirsten, F., Landecker, T. L., Lang, D. A., Leung, C., Li, D. Z., Lin, H.-H., Marcote, B., Masui, K. W., Mckinven, R., Mena-Parra, J., Merryfield, M., Michilli, D., Milutinovic, N., Mirhosseini, A., Naidu, A., Newburgh, L. B., Ng, C., Nimmo, K., Paragi, Z., Patel, C., Pen, U.-L., Pinsonneault-Marotte, T., Pleunis, Z., Rafiei-Ravandi, M, Rahman, M., Ransom, S. M., Renard, A., Sanghavi, P., Scholz, P., Shaw, J. R., Shin, K., Siegel, S. R., Singh, S., Smegal, R. J., Smith, K. M., Stairs, I. H., Tendulkar, S. P., Tretyakov, I., Vanderlinde, K., Wang, H., Wang, X., Wulf, D., Yadav, P., Zwaniga, A. V., The CHIME/FRB Collaboration, High Energy Astrophys. & Astropart. Phys (API, FNWI), Massachusetts Institute of Technology. Department of Mechanical Engineering, Massachusetts Institute of Technology. Department of Physics, and MIT Kavli Institute for Astrophysics and Space Research
- Subjects
Physics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Multidisciplinary ,010308 nuclear & particles physics ,Fast radio burst ,Canadian Hydrogen Intensity Mapping Experiment ,Phase (waves) ,FOS: Physical sciences ,Cosmic ray ,Astrophysics ,01 natural sciences ,Modulation ,0103 physical sciences ,Regular pattern ,Astrophysics - High Energy Astrophysical Phenomena ,010303 astronomy & astrophysics - Abstract
Fast radio bursts (FRBs) are bright, millisecond-duration radio transients originating from sources at extragalactic distances1, the origin of which is unknown. Some FRB sources emit repeat bursts, ruling out cataclysmic origins for those events2,3,4. Despite searches for periodicity in repeat burst arrival times on timescales from milliseconds to many days2,5,6,7, these bursts have hitherto been observed to appear sporadically and—although clustered8—without a regular pattern. Here we report observations of a 16.35 ± 0.15 day periodicity (or possibly a higher-frequency alias of that periodicity) from the repeating FRB 180916.J0158+65 detected by the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst Project4,9. In 38 bursts recorded from 16 September 2018 to 4 February 2020 UTC, we find that all bursts arrive in a five-day phase window, and 50 per cent of the bursts arrive in a 0.6-day phase window. Our results suggest a mechanism for periodic modulation either of the burst emission itself or through external amplification or absorption, and disfavour models invoking purely sporadic processes.
- Published
- 2020
22. Transient radio bursts from rotating neutron stars
- Author
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McLaughlin, M. A., Lyne, A. G., Lorimer, D. R., Kramer, M., Faulkner, A. J., Manchester, R. N., Cordes, J. M., Camilo, F., Possenti, A., Stairs, I. H., Hobbs, G., D'Amico, N., Burgay, M., and O'Brien, J. T.
- Subjects
Environmental issues ,Science and technology ,Zoology and wildlife conservation - Abstract
Author(s): M. A. McLaughlin (corresponding author) [1]; A. G. Lyne [1]; D. R. Lorimer [1]; M. Kramer [1]; A. J. Faulkner [1]; R. N. Manchester [2]; J. M. Cordes [3]; [...]
- Published
- 2006
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23. Swings between rotation and accretion power in a binary millisecond pulsar
- Author
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Papitto, A., Ferrigno, C., Bozzo, E., Rea, N., Pavan, L., Burderi, L., Burgay, M., Campana, S., Di Salvo, T., Falanga, M., Filipović, M. D., Freire, P. C. C., Hessels, J. W. T., Possenti, A., Ransom, S. M., Riggio, A., Romano, P., Sarkissian, J. M., Stairs, I. H., Stella, L., Torres, D. F., Wieringa, M. H., and Wong, G. F.
- Published
- 2013
- Full Text
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24. Fermi LAT Pulsed Detection of PSR J0737-3039A in the Double Pulsar System
- Author
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Guillemot, L, Kramer, M, Johnson, T. J, Craig, H. A, Romani, R. W, Venter, C, Harding, A. K, Ferdman, R. D, Stairs, I. H, and Kerr, M
- Subjects
Astronomy - Abstract
We report the Fermi Large Area Telescope discovery of gamma-ray pulsations from the 22.7 ms pulsar A in the double pulsar system J0737−3039A/B. This is the first mildly recycled millisecond pulsar (MSP) detected in the GeV domain. The 2.7 s companion object PSR J0737−3039B is not detected in gamma rays. PSR J0737−3039A is a faint gamma-ray emitter, so that its spectral properties are only weakly constrained; however, its measured efficiency is typical of other MSPs. The two peaks of the gamma-ray light curve are separated by roughly half a rotation and are well offset from the radio and X-ray emission, suggesting that the GeV radiation originates in a distinct part of the magnetosphere from the other types of emission. From the modeling of the radio and the gamma-ray emission profiles and the analysis of radio polarization data, we constrain the magnetic inclination alpha and the viewing angle zeta to be close to 90 deg., which is consistent with independent studies of the radio emission from PSR J0737−3039A. A small misalignment angle between the pulsar's spin axis and the system's orbital axis is therefore favored, supporting the hypothesis that pulsar B was formed in a nearly symmetric supernova explosion as has been discussed in the literature already.
- Published
- 2013
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25. A Local Universe Host for the Repeating Fast Radio Burst FRB 20181030A.
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Bhardwaj, M., Kirichenko, A. Yu., Michilli, D., Mayya, Y. D., Kaspi, V. M., Gaensler, B. M., Rahman, M., Tendulkar, S. P., Fonseca, E., Josephy, Alexander, Leung, C., Merryfield, Marcus, Petroff, Emily, Pleunis, Z., Sanghavi, Pranav, Scholz, P., Shin, K., Smith, Kendrick M., and Stairs, I. H.
- Published
- 2021
- Full Text
- View/download PDF
26. Evidence for free precession in a pulsar
- Author
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Stairs, I. H., Lyne, A. G., and Shemar, S. L.
- Published
- 2000
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27. Measurement of Gravitational Spin-Orbit Coupling in a Binary Pulsar System
- Author
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Stairs, I. H, Thorsett. S. E, and Arzoumanian, Z
- Subjects
Astronomy - Abstract
In relativistic gravity, a spinning pulsar will precess as it orbits a compact companion star. We have measured the effect of such precession on the average shape and polarization of the radiation from PSR B1534+12. We have also detected, with limited precision, special-relativistic aberration of the revolving pulsar beam due to orbital motion. Our observations fix the system geometry, including the misalignment between the spin and orbital angular momenta, and yield a measurement of the precession timescale consistent with the predictions of General Relativity.
- Published
- 2004
28. Discovery of Radio Pulsations from the X-ray Pulsar JO205+6449 in Supernova Remnant 3C58 with the Green Bank Telescope
- Author
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Camilo, F, Stairs, I. H, Lorimer, D. R, Backer, D. C, Ransom, S. M, Klein, B, Wielebinski, R, Kramer, M, McLaughlin, M. A, Arzoumanian, Z, and White, Nicholas E
- Subjects
Space Radiation - Abstract
We report the discovery with the 100m Green Bank Telescope of 65 ms radio pulsations from the X-ray pulsar J0205+6449 at the center of supernova remnant 3C58, making this possibly the youngest radio pulsar known. From our observations at frequencies of 820 and 1375 MHz, the free electron column density to USSR J0205+6449 is found to be 140.7 +/- 0.3/cc pc. The barycentric pulsar period P and P(dot) determined from a phase-coherent timing solution are consistent with the values previously measured from X-ray observations. The averaged radio profile of USSR J0205+6449 consists of one sharp pulse of width = 3 ms = 0.05 P. The pulsar is an exceedingly weak radio source, with pulse-averaged flux density in the 1400 MHz band of approximately 45 micro-Jy and a spectral index of approximately -2.1. Its radio luminosity of approximately 0.5 may kpc(exp 2) at 1400 MHz is lower than that of approximately 99% of known pulsar and is the lowest among known young pulsars.
- Published
- 2002
29. Refined Mass and Geometric Measurements of the High-mass PSR J0740+6620.
- Author
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Fonseca, E., Cromartie, H. T., Pennucci, T. T., Ray, P. S., Kirichenko, A. Yu., Ransom, S. M., Demorest, P. B., Stairs, I. H., Arzoumanian, Z., Guillemot, L., Parthasarathy, A., Kerr, M., Cognard, I., Baker, P. T., Blumer, H., Brook, P. R., DeCesar, M., Dolch, T., Dong, F. A., and Ferrara, E. C.
- Published
- 2021
- Full Text
- View/download PDF
30. The relativistic binary programme on MeerKAT: science objectives and first results.
- Author
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Kramer, M, Stairs, I H, Venkatraman Krishnan, V, Freire, P C C, Abbate, F, Bailes, M, Burgay, M, Buchner, S, Champion, D J, Cognard, I, Gautam, T, Geyer, M, Guillemot, L, Hu, H, Janssen, G, Lower, M E, Parthasarathy, A, Possenti, A, Ransom, S, and Reardon, D J
- Subjects
- *
RADIO telescopes , *MEERKAT , *STELLAR mass , *NEUTRON stars , *NEUTRON measurement , *FARADAY effect , *BINARY pulsars , *RELATIVISTIC astrophysics - Abstract
We describe the ongoing Relativistic Binary programme (RelBin), a part of the MeerTime large survey project with the MeerKAT radio telescope. RelBin is primarily focused on observations of relativistic effects in binary pulsars to enable measurements of neutron star masses and tests of theories of gravity. We selected 25 pulsars as an initial high priority list of targets based on their characteristics and observational history with other telescopes. In this paper, we provide an outline of the programme, and present polarization calibrated pulse profiles for all selected pulsars as a reference catalogue along with updated dispersion measures. We report Faraday rotation measures for 24 pulsars, twelve of which have been measured for the first time. More than a third of our selected pulsars show a flat position angle swing confirming earlier observations. We demonstrate the ability of the Rotating Vector Model, fitted here to seven binary pulsars, including the Double Pulsar (PSR J0737–3039A), to obtain information about the orbital inclination angle. We present a high time resolution light curve of the eclipse of PSR J0737–3039A by the companion's magnetosphere, a high-phase-resolution position angle swing for PSR J1141–6545, an improved detection of the Shapiro delay of PSR J1811–2405, and pulse scattering measurements for PSRs J1227–6208, J1757–1854, and J1811–1736. Finally, we demonstrate that timing observations with MeerKAT improve on existing data sets by a factor of, typically, 2–3, sometimes by an order of magnitude. [ABSTRACT FROM AUTHOR]
- Published
- 2021
- Full Text
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31. The Green Bank Northern Celestial Cap Pulsar Survey II: The Discovery and Timing of Ten Pulsars
- Author
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Kawash, A. M., McLaughlin, M. A., Kaplan, D. L., DeCesar, M. E., Levin, L., Lorimer, D. R., Lynch, R. S., Stovall, K., Swiggum, J. K., Fonseca, E., Archibald, A. M., Banaszak, S., Biwer, C. M., Boyles, J., Cui, B., Dartez, L. P., Day, D., Ernst, S., Ford, A. J., Flanigan, J., Heatherly, S. A., Hessels, J. W. T., Hinojosa, J., Jenet, F. A., Karako-Argaman, C., Kaspi, V. M., Kondratiev, V. I., Leake, S., Lunsford, G., Martinez, J. G., Mata, A., Matheny, T. D., Mcewen, A. E., Mingyar, M. G., Orsini, A. L., Ransom, S. M., Roberts, M. S. E., Rohr, M. D., Siemens, X., Spiewak, R., Stairs, I. H., van Leeuwen, J., Walker, A. N., and Wells, B. L.
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Instrumentation and Methods for Astrophysics ,FOS: Physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics::Galaxy Astrophysics - Abstract
We present timing solutions for ten pulsars discovered in 350 MHz searches with the Green Bank Telescope. Nine of these were discovered in the Green Bank Northern Celestial Cap survey and one was discovered by students in the Pulsar Search Collaboratory program in analysis of drift-scan data. Following discovery and confirmation with the Green Bank Telescope, timing has yielded phase-connected solutions with high precision measurements of rotational and astrometric parameters. Eight of the pulsars are slow and isolated, including PSR J0930$-$2301, a pulsar with nulling fraction lower limit of $\sim$30\% and nulling timescale of seconds to minutes. This pulsar also shows evidence of mode changing. The remaining two pulsars have undergone recycling, accreting material from binary companions, resulting in higher spin frequencies. PSR J0557$-$2948 is an isolated, 44 \rm{ms} pulsar that has been partially recycled and is likely a former member of a binary system which was disrupted by a second supernova. The paucity of such so-called `disrupted binary pulsars' (DRPs) compared to double neutron star (DNS) binaries can be used to test current evolutionary scenarios, especially the kicks imparted on the neutron stars in the second supernova. There is some evidence that DRPs have larger space velocities, which could explain their small numbers. PSR J1806+2819 is a 15 \rm{ms} pulsar in a 44 day orbit with a low mass white dwarf companion. We did not detect the companion in archival optical data, indicating that it must be older than 1200 Myr., 9 pages, 5 figures
- Published
- 2018
32. An Analysis Pipeline for CHIME/FRB Full-array Baseband Data.
- Author
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Michilli, D., Masui, K. W., Mckinven, R., Cubranic, D., Bruneault, M., Brar, C., Patel, C., Boyle, P. J., Stairs, I. H., Renard, A., Bandura, K., Berger, S., Breitman, D., Cassanelli, T., Dobbs, M., Kaspi, V. M., Leung, C., Mena-Parra, J., Pleunis, Z., and Russell, L.
- Subjects
BASEBAND ,FARADAY effect ,ANTENNA arrays ,DATA recorders & recording ,ELECTRIC fields ,ZODIAC ,PIPELINE inspection - Abstract
The Canadian Hydrogen Intensity Mapping Experiment (CHIME) has become a leading facility for detecting fast radio bursts (FRBs) through the CHIME/FRB backend. CHIME/FRB searches for fast transients in polarization-summed intensity data streams that have 24 kHz spectral and 1 ms temporal resolution. The intensity beams are pointed to predetermined locations in the sky. A triggered baseband system records the coherent electric field measured by each antenna in the CHIME array at the time of FRB detections. Here we describe the analysis techniques and automated pipeline developed to process these full-array baseband data recordings. Whereas the real-time FRB detection pipeline has a localization limit of several arcminutes, offline analysis of baseband data yields source localizations with subarcminute precision, as characterized by using a sample of pulsars and one repeating FRB with known positions. The baseband pipeline also enables resolving temporal substructure on a microsecond scale and the study of polarization including detections of Faraday rotation. [ABSTRACT FROM AUTHOR]
- Published
- 2021
- Full Text
- View/download PDF
33. The Discovery of Nulling and Mode-switching Pulsars with CHIME/Pulsar.
- Author
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Ng, C., Wu, B., Ma, M., Ransom, S. M., Naidu, A., Fonseca, E., Boyle, P. J., Brar, C., Cubranic, D., Demorest, P. B., Good, D. C., Kaspi, V. M., Masui, K. W., Michilli, D., Patel, C., Renard, A., Scholz, P., Stairs, I. H., Tendulkar, S. P., and Tretyakov, I.
- Subjects
PULSARS ,MATCHED filters - Abstract
The Pulsar backend of the Canadian Hydrogen Intensity Mapping Experiment has monitored hundreds of known pulsars in the northern sky since fall 2018, providing a rich data set for the study of temporal variations in pulsar emission. Using a matched filtering technique, we report, for the first time, nulling behavior in five pulsars as well as mode switching in nine pulsars. Only one of the pulsars is observed to show both nulling and moding signals. These new nulling and mode-switching pulsars appear to come from a population with relatively long spin periods, in agreement with previous findings in the literature. [ABSTRACT FROM AUTHOR]
- Published
- 2020
- Full Text
- View/download PDF
34. Understanding and improving the timing of PSR J0737−3039B.
- Author
-
Noutsos, A., Desvignes, G., Kramer, M., Wex, N., Freire, P. C. C., Stairs, I. H., McLaughlin, M. A., Manchester, R. N., Possenti, A., Burgay, M., Lyne, A. G., Breton, R. P., Perera, B. B. P., and Ferdman, R. D.
- Subjects
PULSARS ,DEFLECTION (Mechanics) ,TEST systems ,MASS measurement - Abstract
The double pulsar (PSR J0737−3039A/B) provides some of the most stringent tests of general relativity (GR) and its alternatives. The success of this system in tests of GR is largely due to the high-precision, long-term timing of its recycled-pulsar member, pulsar A. On the other hand, pulsar B is a young pulsar that exhibits significant short-term and long-term timing variations due to the electromagnetic-wind interaction with its companion and geodetic precession. Improving pulsar B's timing precision is a key step towards improving the precision in a number of GR tests with PSR J0737−3039A/B. In this paper, red noise signatures in the timing of pulsar B are investigated using roughly a four-year time span, from 2004 to 2008, beyond which time the pulsar's radio beam precessed out of view. In particular, we discuss the profile variations seen on timescales ranging from minutes – during the so-called "bright" orbital phases – to hours – during its full 2.5 h orbit – to years, as geodetic precession displaces the pulsar's beam with respect to our line of sight. Also, we present our efforts to model the orbit-wide, harmonic modulation that has been previously seen in the timing residuals of pulsar B, using simple geometry and the impact of a radial electromagnetic wind originating from pulsar A. Our model successfully accounts for the long-term precessional changes in the amplitude of the timing residuals but does not attempt to describe the fast profile changes observed during each of the bright phases, nor is it able to reproduce the lack of observable emission between phases. Using a nested sampling analysis, our simple analytical model allowed us to extract information about the general properties of pulsar B's emission beam, such as its approximate shape and intensity, as well as the magnitude of the deflection of that beam, caused by pulsar A's wind. We also determined for the first time that the most likely sense of rotation of pulsar B, consistent with our model, is prograde with respect to its orbital motion. Finally, we discuss the potential of combining our model with future timing of pulsar B, when it becomes visible again, towards improving the precision of tests of GR with the double pulsar. The timing of pulsar B presented in this paper depends on the size of the pulsar's orbit, which was calculated from GR, in order to precisely account for orbital timing delays. Consequently, our timing cannot directly be used to test theories of gravity. However, our modelling of the beam shape and radial wind of pulsar B can indirectly aid future efforts to time this pulsar by constraining part of the additional red noise observed on top of the orbital delays. As such, we conclude that, in the idealised case of zero covariance between our model's parameters and those of the timing model, our model can bring about a factor 2.6 improvement on the measurement precision of the mass ratio, R = m
A /mB , between the two pulsars: a theory-independent parameter, which is pivotal in tests of GR. [ABSTRACT FROM AUTHOR]- Published
- 2020
- Full Text
- View/download PDF
35. Faraday rotation measures of Northern hemisphere pulsars using CHIME/Pulsar.
- Author
-
Ng, C, Pandhi, A, Naidu, A, Fonseca, E, Kaspi, V M, Masui, K W, Mckinven, R, Renard, A, Scholz, P, Stairs, I H, Tendulkar, S P, and Vanderlinde, K
- Subjects
FARADAY effect ,MAGNETIC structure ,PULSARS ,GALACTIC magnetic fields ,IONOSPHERE - Abstract
Using commissioning data from the first year of operation of the Canadian Hydrogen Intensity Mapping Experiment's (CHIME) Pulsar backend system, we conduct a systematic analysis of the Faraday Rotation Measure (RM) of the Northern hemisphere pulsars detected by CHIME. We present 55 new RMs as well as obtain improved RM uncertainties for 25 further pulsars. CHIME's low observing frequency and wide bandwidth between 400 and 800 MHz contribute to the precision of our measurements, whereas the high cadence observation provides extremely high signal-to-noise co-added data. Our results represent a significant increase of the pulsar RM census, particularly regarding the Northern hemisphere. These new RMs are for sources that are located in the Galactic plane out to 10 kpc, as well as off the plane to a scale height of ∼16 kpc. This improved knowledge of the Faraday sky will contribute to future Galactic large-scale magnetic structure and ionosphere modelling. [ABSTRACT FROM AUTHOR]
- Published
- 2020
- Full Text
- View/download PDF
36. Mode switching and oscillations in PSR B1828–11.
- Author
-
Stairs, I H, Lyne, A G, Kramer, M, Stappers, B W, van Leeuwen, J, Tung, A, Manchester, R N, Hobbs, G B, Lorimer, D R, and Melatos, A
- Subjects
- *
OSCILLATIONS , *PULSARS , *TELESCOPES , *GEOMETRIC shapes - Abstract
The young pulsar PSR B1828–11 has long been known to show correlated shape and spindown changes with time-scales of roughly 500 and 250 d, perhaps associated with large-scale magnetospheric switching. Here, we present multihour observations with the Parkes and Green Bank Telescopes at multiple phases across the 500-d cycle and show that the pulsar undergoes mode-changing between two stable, extreme profile states. The fraction of time spent in each profile state naturally accounts for the observed overall 'shape parameter' (defined to be 0 for wide profiles and 1 for narrow ones); this and the variable rate of the mode transitions are directly related to the spindown changes. We observe that the mode transition rate could plausibly function as an additional parameter governing the chaotic behaviour in this object which was proposed earlier by Seymour and Lorimer. Free precession is not needed to account for the variations. [ABSTRACT FROM AUTHOR]
- Published
- 2019
- Full Text
- View/download PDF
37. Tests of gravitational symmetries with pulsar binary J1713+0747.
- Author
-
Zhu, W W, Desvignes, G, Wex, N, Caballero, R N, Champion, D J, Demorest, P B, Ellis, J A, Janssen, G H, Kramer, M, Krieger, A, Lentati, L, Nice, D J, Ransom, S M, Stairs, I H, Stappers, B W, Verbiest, J P W, Arzoumanian, Z, Bassa, C G, Burgay, M, and Cognard, I
- Subjects
PULSARS ,BINARY stars ,CELESTIAL mechanics ,GRAVITATIONAL constant ,BINARY pulsars - Abstract
Symmetries play a fundamental role in modern theories of gravity. The strong equivalence principle (SEP) constitutes a collection of gravitational symmetries which are all implemented by general relativity. Alternative theories, however, are generally expected to violate some aspects of SEP. We test three aspects of SEP using observed change rates in the orbital period and eccentricity of binary pulsar J1713+0747: (1) the gravitational constant's constancy as part of locational invariance of gravitation; (2) the universality of free fall (UFF) for strongly self-gravitating bodies; (3) the post-Newtonian parameter |$\hat{\alpha }_3$| in gravitational Lorentz invariance. Based on the pulsar timing result of the combined data set from the North American Nanohertz Gravitational Observatory and the European Pulsar Timing Array, we find |$\dot{G}/G = (-0.1 \pm 0.9) \times 10^{-12}\, {\rm yr}^{-1}$|, which is weaker than Solar system limits, but applies for strongly self-gravitating objects. Furthermore, we obtain an improved test for a UFF violation by a strongly self-gravitating mass falling in the gravitational field of our Galaxy, with a limit of |Δ| < 0.002 (95 per cent C.L.). Finally, we derive an improved limit on the self-acceleration of a gravitationally bound rotating body, to a preferred reference frame in the Universe, with |$-3\times 10^{-20} \lt \hat{\alpha }_3 \lt 4\times 10^{-20}$| (95 per cent C.L.). These results are based on direct UFF and |$\hat{\alpha }_3$| tests using pulsar binaries, and they overcome various limitations of previous tests of this kind. [ABSTRACT FROM AUTHOR]
- Published
- 2019
- Full Text
- View/download PDF
38. Searching for pulsars using image pattern recognition'
- Author
-
Zhu, W. W., Berndsen, A., Madsen, E. C., Tan, M., Stairs, I. H., Brazier, A., Lazarus, P., Lynch, R., Scholz, P., Stovall, K., Ransom, S. M., Banaszak, S., Biwer, C. M., Cohen, S., Dartez, L. P., Flanigan, J., Lunsford, G., Martinez, J. G., Mata, A., Rohr, M., Walker, A., Allen, B., Bhat, N. D. R., Bogdanov, S., Camilo, F., Chatterjee, S., Cordes, J. M., Crawford, F., Deneva, J. S., Desvignes, G., Ferdman, R. D., Freire, P. C. C., Hessels, J. W. T., Jenet, F. A., Kaplan, D. L., Kaspi, V. M., Knispel, B., Zhu, W. W., Berndsen, Madsen, E. C., Tan, Stairs, I. H., Brazier, Lazarus, Lynch, Scholz, Stovall, Ransom, S. M., Banaszak, Biwer, C. M., Cohen, Dartez, L. P., Flanigan, Lunsford, Martinez, J. G., Mata, Rohr, Walker, Allen, Bhat, N. D. R., Bogdanov, Camilo, Chatterjee, Cordes, J. M., Crawford, Deneva, J. S., Desvignes, Ferdman, R. D., Freire, P. C. C., Hessels, J. W. T., Jenet, F. A., Kaplan, D. L., Kaspi, V. M., and Knispel
- Published
- 2014
39. The PALFA Survey: Going to great depths to find radio pulsars
- Author
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Lazarus, P., Allen, B., Bhat, N. D. R., Bogdanov, S., Bouchard, A., Brazier, A., Camilo, F., Cardoso, F., Chatterjee, S., Cordes, J. M., Crawford, F., Deneva, J. S., Desvignes, G., Freire, P. C. C., Hessels, J. W. T., Jenet, F. A., Kaspi, V. M., Knispel, B., van Leeuwen, J., Lorimer, D. R., Lynch, R., Lyne, A. G., McLaughlin, M. A., Nice, D. J., Ransom, S. M., Scholz, P., Siemens, X., Stairs, I. H., Stappers, B. W., Stovall, K., and Swiggum, J.
- Subjects
Physics ,Spectrometer ,Astronomy ,FOS: Physical sciences ,Astronomy and Astrophysics ,Galactic plane ,Pulsar ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,Millisecond pulsar ,Frequency resolution ,Data analysis ,Arecibo Observatory ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Solar and Stellar Astrophysics (astro-ph.SR) - Abstract
The on-going PALFA survey is searching the Galactic plane (|b| < 5 deg., 32 < l < 77 deg. and 168 < l < 214 deg.) for radio pulsars at 1.4 GHz using ALFA, the 7-beam receiver installed at the Arecibo Observatory. By the end of August 2012, the PALFA survey has discovered 100 pulsars, including 17 millisecond pulsars (P < 30 ms). Many of these discoveries are among the pulsars with the largest DM/P ratios, proving that the PALFA survey is capable of probing the Galactic plane for millisecond pulsars to a much greater depth than any previous survey. This is due to the survey's high sensitivity, relatively high observing frequency, and its high time and frequency resolution. Recently the rate of discoveries has increased, due to a new more sensitive spectrometer, two updated complementary search pipelines, the development of online collaborative tools, and access to new computing resources. Looking forward, focus has shifted to the application of artificial intelligence systems to identify pulsar-like candidates, and the development of an improved full-resolution pipeline incorporating more sophisticated radio interference rejection. The new pipeline will be used in a complete second analysis of data already taken, and will be applied to future survey observations. An overview of recent developments, and highlights of exciting discoveries will be presented., Proceedings of IAUS 291 "Neutron Stars and Pulsars: Challenges and Opportunities after 80 years", J. van Leeuwen (ed.); 6 pages, 4 figures
- Published
- 2012
40. High-Precision Timing of 5 Millisecond Pulsars: Space Velocities, Binary Evolution and Equivalence Principles
- Author
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Gonzalez, M. E., Stairs, I. H., Ferdman, R. D., Freire, P. C. C., Nice, D. J., Demorest, P. B., Ransom, S. M., Kramer, M., Camilo, F., Hobbs, G., Manchester, R. N., and Lyne, A. G.
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
We present high-precision timing of five millisecond pulsars (MSPs) carried out for more than seven years; four pulsars are in binary systems and one is isolated. We are able to measure the pulsars' proper motions and derive an estimate for their space velocities. The measured two-dimensional velocities are in the range 70-210 km/s, consistent with those measured for other MSPs. We also use all the available proper motion information for isolated and binary MSPs to update the known velocity distribution for these populations. As found by earlier works, we find that the velocity distribution of binary and isolated MSPs are indistinguishable with the current data. Four of the pulsars in our observing program are highly recycled with low-mass white dwarf companions and we are able to derive accurate binary parameters for these systems. For three of these binary systems we are able to place initial constraints on the pulsar masses with best-fit values in the range 1.0-1.6 M_sun. The implications of the results presented here to our understanding of binary pulsar evolution are discussed. The updated parameters for the binary systems studied here, together with recently discovered similar systems, allowed us to update previous limits on the the violation of the strong equivalence principle through the parameter |Delta| to 4.6x10^-3 (95% confidence) and the violation of Lorentz-invariance/momentum-conservation through the parameter |hat{alpha}_3| to 5.5x10^-20 (95% confidence)., 24 pages, 8 figures; accepted for publication in The Astrophysical Journal
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- 2011
41. On the nature and evolution of the unique binary pulsar J1903+0327
- Author
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Freire, P. C. C., Bassa, C. G., Wex, N., Stairs, I. H., Champion, D. J., Ransom, S. M., Lazarus, P., Kaspi, V. M., Hessels, J. W. T., Kramer, M., Cordes, J. M., Verbiest, Joris, Podsiadlowski, P., Nice, D. J., Deneva, J. S., Lorimer, D. R., Stappers, B. W., McLaughlin, M. A., Camilo, F., and High Energy Astrophys. & Astropart. Phys (API, FNWI)
- Subjects
Astrophysics of Galaxies (astro-ph.GA) ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Astrophysics::Galaxy Astrophysics - Abstract
(abridged) PSR J1903+0327, a millisecond pulsar in an eccentric (e = 0.44) 95-day orbit with a (~ 1Msun) companion poses a challenge to our understanding of stellar evolution in binary and multiple-star systems. Here we describe optical and radio observations which rule out most of the scenarios proposed to explain formation of this system. Radio timing measurements of three post-Keplerian effects yield the most precise measurement of the mass of a millisecond pulsar to date: 1.667 +/- 0.021 solar masses (99.7% confidence limit) (...). Optical spectroscopy of a proposed main sequence counterpart show that its orbital motion mirrors the pulsar's 95-day orbit; being therefore its binary companion (...) The optical detection also provides a measurement of the systemic radial velocity of the binary; this and the proper motion measured from pulsar timing allow the determination of the systemic 3-D velocity in the Galaxy. We find that the system is always within 270 pc of the plane of the Galaxy, but always more than 3 kpc away from the Galactic centre. Thus an exchange interaction in a dense stellar environment (like a globular cluster or the Galactic centre) is not likely to be the origin of this system. We suggest that after the supernova that formed it, the neutron star was in a tight orbit with a main-sequence star, the present companion was a tertiary farther out. The neutron star then accreted matter from its evolving inner MS companion, forming a millisecond pulsar. The former donor star then disappears, either due to a chaotic 3-body interaction with the outer star (caused by the expansion of the inner orbit that necessarily results from mass transfer), or in the case of a very compact inner system, due to ablation/accretion by the newly formed millisecond pulsar., Comment: 16 pages in emulate MNRAS format, 11 figures, 2 tables, accepted for publication in MNRAS
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- 2011
42. Searches for gravitational waves from known pulsars with science run 5 LIGO data
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Abbott, B. P., Abbott, R., Acernese, F., Adhikari, R., Ajith, P., Allen, B., Allen, G., Alshourbagy, M., Amin, R. S., Anderson, S. B., Anderson, W. G., Antonucci, F., Aoudia, S., Arain, M. A., Araya, M., Armandula, H., Armor, P., Arun, K. G., Aso, Y., Aston, S., Astonea, P., Aufmuth, P., Aulbert, C., Babak, S., Baker, P., Ballardin, G., Ballmer, S., Barker, C., Barker, D., Barone, F., Barr, B., Barriga, P., Barsotti, L., Barsuglia, M., Barton, M. A., Bartos, I., Bassiri, R., Bastarrika, M., Bauer, T. S., Behnke, B., Beker, M., Benacquista, M., Betzwieser, J., Beyersdorf, P. T., Bigotta, S., Bilenko, I. A., Billingsley, G., Birindelli, S., Biswas, R., Bizouard, M. A., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bland, B., Boccara, C., Bodiya, T. P., Bogue, L., Bondub, F., Bonelli, L., Bork, R., Boschi, V., Bose, S., Bosi, L., Braccinia, S., Bradaschia, C., Brady, P. R., Braginsky, V. B., Brau, J. E., Bridges, D. O., Brillet, A., Brinkmann, M., Brisson, V., Den Broeck, C. V., Brooks, A. F., Brown, D. A., Brummit, A., Brunet, G., Budzynski, R., Bulik, T., Bullington, A., Bulten, H. J., Buonanno, A., Burmeister, O., Buskulic, D., Byer, R. L., Cadonati, L., Cagnoli, G., Calloni, E., Camp, J. B., Campagna, E., Cannizzo, J., Cannon, K. C., Canuel, B., Cao, J., Carbognani, F., Cardenas, L., Caride, S., Castaldi, G., Caudill, S., Cavaglia, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C., Cesarini, E., Chalermsongsak, T., Chalkley, E., Charlton, P., Chassande Mottin, E., Chatterji, S., Chelkowski, S., Chen, Y., Chincarini, A., Christensen, N., Chung, C. T. Y., Clark, D., Clark, J., Clayton, J. H., Cleva, F., Coccia, E., Cokelaer, T., Colacino, C. N., Colas, J., Colla, A., Colombini, M., Conte, R., Cook, D., Corbitt, T. R. C., Corda, C., Cornish, N., Corsi, A., Coulon, J. P., Coward, D., Coyne, D. C., Creighton, J. D. E., Creighton, T. D., Cruise, A. M., Culter, R. M., Cumming, A., Cunningham, L., Cuoco, E., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dari, A., Dattilo, V., Daudert, B., Davier, M., Davies, G., Daw, E. J., Day, R., Rosa, R. D., Debra, D., Degallaix, J., Prete, M. d., Dergachev, V., Desai, S., Desalvo, R., Dhurandhar, S., Fiore, L. D., Lieto, A. D., Emilio, M. D. P., Virgilio, A. D., Diaz, M., Dietz, A., Donovan, F., Dooley, K. L., Doomes, E. E., Drago, M., Drever, R. W. P., Dueck, J., Duke, I., Dumas, J. C., Dwyer, J. G., Echols, C., Edgar, M., Effler, A., Ehrens, P., Espinoza, E., Etzel, T., Evans, M., Evans, T., Fafone, V., Fairhurst, S., Faltas, Y., Fan, Y., Fazi, D., Fehrmann, H., Ferrante, I., Fidecaro, F., Finn, L. S., Fiori, I., Flaminio, R., Flasch, K., Foley, S., Forrest, C., Fotopoulos, N., Fournier, J. D., Franc, J., Franzen, A., Frasca, S., Frasconi, F., Frede, M., Frei, M., Frei, Z., Freise, A., Frey, R., Fricke, T., Fritschel, P., Frolov, V. V., Fyffe, M., Galdi, V., Gammaitoni, Luca, Garofoli, J. A., Garufiab, F., Gemme, G., Genin, E., Gennai, A., Gholami, I., Giaime, J. A., Giampanis, S., Giardina, K. D., Giazotto, A., Goda, K., Goetz, E., Goggin, L. M., Gonzalez, G., Gorodetsky, M. L., Gossler, S., Gouaty, R., Granata, M., Granata, V., Grant, A., Gras, S., Gray, C., Gray, M., Greenhalgh, R. J. S., Gretarsson, A. M., Greverie, C., Grimaldi, F., Grosso, R., Grote, H., Grunewald, S., Guenther, M., Guidi, G., Gustafson, E. K., Gustafson, R., Hage, B., Hallam, J. M., Hammer, D., Hammond, G. D., Hanna, C., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Haughian, K., Hayama, K., Heefner, J., Heitmann, H., Hello, P., Heng, I. S., Heptonstall, A., Hewitson, M., Hild, S., Hirose, E., Hoak, D., Hodge, K. A., Holt, K., Hosken, D. J., Hough, J., Hoyland, D., Huet, D., Hughey, B., Huttner, S. H., Ingram, D. R., Isogai, T., Ito, M., Ivanov, A., Jaranowski, P., Johnson, B., Johnson, W. W., Jones, D. I., Jones, G., Jones, R., de la Jordana, L. S., Ju, L., Kalmus, P., Kalogera, V., Kandhasamy, S., Kanner, J., Kasprzyk, D., Katsavounidis, E., Kawabe, K., Kawamura, S., Kawazoe, F., Kells, W., Keppel, D. G., Khalaidovski, A., Khalili, F. Y., Khan, R., Khazanov, E., King, P., Kissel, J. S., Klimenko, S., Kokeyama, K., Kondrashov, V., Kopparapu, R., Koranda, S., Kowalska, I., Kozak, D., Krishnan, B., Krolak, A., Kumar, R., Kwee, P., Penna, P. L., Lam, P. K., Landry, M., Lantz, B., Lazzarini, A., Lei, H., Lei, M., Leindecker, N., Leonor, I., Leroy, N., Letendre, N., Li, C., Lin, H., Lindquist, P. E., Littenberg, T. B., Lockerbie, N. A., Lodhia, D., Longo, M., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lu, P., Lubinski, M., Lucianetti, A., Luck, H., Machenschalk, B., Macinnis, M., Mackowski, J. M., Mageswaran, M., Mailand, K., Majorana, E., Mana, N., Mandel, I., Mandic, V., Mantovani, M., Marchesoni, F., Marion, F., Marka, S., Marka, Z., Markosyan, A., Markowitz, J., Maros, E., Marque, J., Martelli, F., Martin, I. W., Martin, R. M., Marx, J. N., Mason, K., Masserot, A., Matichard, F., Matone, L., Matzner, R. A., Mavalvala, N., Mccarthy, R., Mcclelland, D. E., Mcguire, S. C., Mchugh, M., Mcintyre, G., Mckechan, D. J. A., Mckenzie, K., Mehmet, M., Melatos, A., Melissinos, A. C., Mendell, G., Menendez, D. F., Menzinger, F., Mercer, R. A., Meshkov, S., Messenger, C., Meyer, M. S., Michel, C., Milano, L., Miller, J., Minelli, J., Minenkova, Y., Mino, Y., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Miyakawa, O., Moe, B., Mohan, M., Mohanty, S. D., Mohapatra, S. R. P., Moreau, J., Moreno, G., Morgado, N., Morgia, A., Morioka, T., Mors, K., Mosca, S., Moscatelli, V., Mossavi, K., Mours, B., Mowlowry, C., Mueller, G., Muhammad, D., Muhlen, H. z., Mukherjee, S., Mukhopadhyay, H., Mullavey, A., Muller Ebhardt, H., Munch, J., Murray, P. G., Myers, E., Myers, J., Nash, T., Nelson, J., Neri, I., Newton, G., Nishizawa, A., Nocera, F., Numata, K., Ochsner, E., O'Dell, J., Ogin, G. H., O'Reilly, B., O'Shaughnessy, R., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Pagliaroli, G., Palomba, C., Pan, Y., Pankow, C., Paoletti, F., Papa, M. A., Parameshwaraiah, V., Pardi, S., Pasqualetti, A., Passaquieti, R., Passuello, D., Patel, P., Pedraza, M., Penn, S., Perreca, A., Persichetti, G., Pichot, M., Piergiovanni, F., Pierro, V., Pietka, M., Pinard, L., Pinto, I. M., Pitkin, M., Pletsch, H. J., Plissi, M. V., Poggiani, R., Postiglione, F., Prato, M., Principe, M., Prix, R., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Quetschke, V., Raab, F. J., Rabaste, O., Rabeling, D. S., Radkins, H., Raffai, P., Raics, Z., Rainer, N., Rakhmanov, M., Rapagnani, P., Raymond, V., Re, V., Reed, C. M., Reed, T., Regimbau, T., Rehbein, H., Reid, S., Reitze, D. H., Ricci, F., Riesen, R., Riles, K., Rivera, B., Roberts, P., Robertson, N. A., Robinet, F., Robinson, C., Robinson, E. L., Rocchi, A., Roddy, S., Rolland, L., Rollins, J., Romano, J. D., Romanoac, R., Romie, J. H., Rosinska, D., Rover, C., Rowan, S., Rudiger, A., Ruggi, P., Russell, P., Ryan, K., Sakata, S., Salemi, F., Sandberg, V., Sannibale, V., Santamaria, L., Saraf, S., Sarin, P., Sassolas, B., Sathyaprakash, B. S., Sato, S., Satterthwaite, M., Saulson, P. R., Savage, R., Savov, P., Scanlan, M., Schilling, R., Schnabel, R., Schofield, R., Schulz, B., Schutz, B. F., Schwinberg, P., Scott, J., Scott, S. M., Searle, A. C., Sears, B., Seifert, F., Sellers, D., Sengupta, A. S., Sentenac, D., Sergeev, A., Shapiro, B., Shawhan, P., Shoemaker, D. H., Sibley, A., Siemens, X., Sigg, D., Sinha, S., Sintes, A. M., Slagmolen, B. J. J., Slutsky, J., van der Sluys, M. V., Smith, J. R., Smith, M. R., Smith, N. D., Somiya, K., Sorazu, B., Stein, A., Stein, L. C., Steplewski, S., Stochino, A., Stone, R., Strain, K. A., Strigin, S., Stroeer, A., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, K. X., Sung, M., Sutton, P. J., Swinkels, B., Szokoly, G. P., Talukder, D., Tang, L., Tanner, D. B., Tarabrin, S. P., Taylor, J. R., Taylor, R., Terenzi, R., Thacker, J., Thorne, K. A., Thorne, K. S., Uring, A. T. R., Tokmakov, K. V., Toncelli, A., Tonelli, M., Torres, C., Torrie, C., Tournefier, E., Travasso, F., Traylor, G., Trias, M., Trummer, J., Ugolini, D., Ulmen, J., Urbanek, K., Vahlbruch, H., Vajente, G., Vallisneri, M., van den Brand, J. F. J., der Putten, S. v., Vass, S., Vaulin, R., Vavoulidis, M., Vecchio, A., Vedovato, G., van Veggel, A. A., Veitch, J., Veitch, P., Veltkamp, C., Verkindt, D., Vetrano, F., Vicere, A., Villar, A., Vineta, J. Y., Vocca, Helios, Vorvick, C., Vyachanin, S. P., Waldman, S. J., Wallace, L., Ward, R. L., Was, M., Weidner, A., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Wen, S., Wette, K., Whelan, J. T., Whitcomb, S. E., Whiting, B. F., Wilkinson, C., Willems, P. A., Williams, H. R., Williams, L., Willke, B., Wilmut, I., Winkelmann, L., Winkler, W., Wipf, C. C., Wiseman, A. G., Woan, G., Wooley, R., Worden, J., Wu, W., Yakushin, I., Yamamoto, H., Yan, Z., Yoshida, S., Yvert, M., Zanolin, M., Zhang, J., Zhang, L., Zhao, C., Zotov, N., Zucker, M. E., Zweizig, J., Begin, S., Corongiu, A., D'Amico, N., Freire, P. C. C., Hessels, J. W. T., Hobbs, G. B., Kramer, M., Lyne, A. G., Manchester, R. N., Marshall, F. E., Middleditch, J., Possenti, A., Ransom, S. M., Stairs, I. H., Stappers, B., Collaboration, L. S., Collaboration, V., The LIGO Scientific Collaboration, The Virgo Collaboration, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France ( PCC ), Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire de Paris-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), ESPCI ParisTech, Institut de Physique de Rennes ( IPR ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ) -Université de Rennes ( UNIV-RENNES ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Annecy de Physique des Particules ( LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), APC - Gravitation ( APC-Gravitation ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, Laboratoire des matériaux avancés ( LMA ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Virgo, Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire des matériaux avancés (LMA), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), High Energy Astrophys. & Astropart. Phys (API, FNWI), (Astro)-Particles Physics, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), B. P., Abbott, R., Abbott, F., Acernese, R., Adhikari, P., Ajith, B., Allen, G., Allen, M., Alshourbagy, R. S., Amin, S. B., Anderson, W. G., Anderson, F., Antonucci, S., Aoudia, M. A., Arain, M., Araya, H., Armandula, P., Armor, K. G., Arun, Y., Aso, S., Aston, P., Astone, P., Aufmuth, C., Aulbert, S., Babak, P., Baker, G., Ballardin, S., Ballmer, C., Barker, D., Barker, F., Barone, B., Barr, P., Barriga, L., Barsotti, M., Barsuglia, M. A., Barton, I., Barto, R., Bassiri, M., Bastarrika, Bauer, T. h. S., B., Behnke, M., Beker, M., Benacquista, J., Betzwieser, P. T., Beyersdorf, S., Bigotta, I. A., Bilenko, G., Billingsley, S., Birindelli, R., Biswa, M. A., Bizouard, E., Black, J. K., Blackburn, L., Blackburn, D., Blair, B., Bland, C., Boccara, T. P., Bodiya, L., Bogue, F., Bondu, L., Bonelli, R., Bork, V., Boschi, S., Bose, L., Bosi, S., Braccini, C., Bradaschia, P. R., Brady, V. B., Braginsky, J. E., Brau, D. O., Bridge, A., Brillet, M., Brinkmann, V., Brisson, C., Van Den Broeck, A. 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L., Danilishin, S., D'Antonio, K., Danzmann, A., Dari, V., Dattilo, B., Daudert, M., Davier, G., Davie, E. J., Daw, R., Day, DE ROSA, Rosario, D., Debra, J., Degallaix, M., del Prete, V., Dergachev, S., Desai, R., Desalvo, S., Dhurandhar, L., Di Fiore, A., Di Lieto, M., Di Paolo Emilio, A., Di Virgilio, M., Díaz, A., Dietz, F., Donovan, K. L., Dooley, E. E., Doome, M., Drago, R. W. P., Drever, J., Dueck, I., Duke, J. C., Duma, J. G., Dwyer, C., Echol, M., Edgar, A., Effler, P., Ehren, E., Espinoza, T., Etzel, M., Evan, T., Evan, V., Fafone, S., Fairhurst, Y., Falta, Y., Fan, D., Fazi, H., Fehrmann, I., Ferrante, F., Fidecaro, L. S., Finn, I., Fiori, R., Flaminio, K., Flasch, S., Foley, C., Forrest, N., Fotopoulo, J. D., Fournier, J., Franc, A., Franzen, S., Frasca, F., Frasconi, M., Frede, M., Frei, Z., Frei, A., Freise, R., Frey, T., Fricke, P., Fritschel, V. V., Frolov, M., Fyffe, V., Galdi, L., Gammaitoni, J. A., Garofoli, Garufi, Fabio, G., Gemme, E., Genin, A., Gennai, I., Gholami, J. A., Giaime, S., Giampani, K. D., Giardina, A., Giazotto, K., Goda, E., Goetz, L. M., Goggin, G., González, M. L., Gorodetsky, S., Goßler, R., Gouaty, M., Granata, V., Granata, A., Grant, S., Gra, C., Gray, M., Gray, R. J. S., Greenhalgh, A. M., Gretarsson, C., Greverie, F., Grimaldi, R., Grosso, H., Grote, S., Grunewald, M., Guenther, G., Guidi, E. K., Gustafson, R., Gustafson, B., Hage, J. M., Hallam, D., Hammer, G. D., Hammond, C., Hanna, J., Hanson, J., Harm, G. M., Harry, I. W., Harry, E. D., Harstad, K., Haughian, K., Hayama, J., Heefner, H., Heitmann, P., Hello, I. S., Heng, A., Heptonstall, M., Hewitson, S., Hild, E., Hirose, D., Hoak, K. A., Hodge, K., Holt, D. J., Hosken, J., Hough, D., Hoyland, D., Huet, B., Hughey, S. H., Huttner, D. R., Ingram, T., Isogai, M., Ito, A., Ivanov, P., Jaranowski, B., Johnson, W. W., Johnson, D. I., Jone, G., Jone, R., Jone, L., Sancho de la Jordana, L., Ju, P., Kalmu, V., Kalogera, S., Kandhasamy, J., Kanner, D., Kasprzyk, E., Katsavounidi, K., Kawabe, S., Kawamura, F., Kawazoe, W., Kell, D. G., Keppel, A., Khalaidovski, F. Y., Khalili, R., Khan, E., Khazanov, P., King, J. S., Kissel, S., Klimenko, K., Kokeyama, V., Kondrashov, R., Kopparapu, S., Koranda, I., Kowalska, D., Kozak, B., Krishnan, A., Królak, R., Kumar, P., Kwee, P., La Penna, P. K., Lam, M., Landry, B., Lantz, A., Lazzarini, H., Lei, M., Lei, N., Leindecker, I., Leonor, N., Leroy, N., Letendre, C., Li, H., Lin, P. E., Lindquist, T. B., Littenberg, N. A., Lockerbie, D., Lodhia, M., Longo, M., Lorenzini, V., Loriette, M., Lormand, G., Losurdo, P., Lu, M., Lubinski, A., Lucianetti, H., Lück, B., Machenschalk, M., Macinni, J. M., Mackowski, M., Mageswaran, K., Mailand, E., Majorana, N., Man, I., Mandel, V., Mandic, M., Mantovani, F., Marchesoni, F., Marion, S., Márka, Z., Márka, A., Markosyan, J., Markowitz, E., Maro, J., Marque, F., Martelli, I. W., Martin, R. M., Martin, J. N., Marx, K., Mason, A., Masserot, F., Matichard, L., Matone, R. A., Matzner, N., Mavalvala, R., Mccarthy, D. E., Mcclelland, S. C., Mcguire, M., Mchugh, G., Mcintyre, D. J. A., Mckechan, K., Mckenzie, M., Mehmet, A., Melato, A. C., Melissino, G., Mendell, D. F., Menéndez, F., Menzinger, R. A., Mercer, S., Meshkov, C., Messenger, M. S., Meyer, C., Michel, Milano, Leopoldo, J., Miller, J., Minelli, Y., Minenkov, Y., Mino, V. P., Mitrofanov, G., Mitselmakher, R., Mittleman, O., Miyakawa, B., Moe, M., Mohan, S. D., Mohanty, S. R. P., Mohapatra, J., Moreau, G., Moreno, N., Morgado, A., Morgia, T., Morioka, K., Mor, S., Mosca, V., Moscatelli, K., Mossavi, B., Mour, C., Mowlowry, G., Mueller, D., Muhammad, H., zur Mühlen, S., Mukherjee, H., Mukhopadhyay, A., Mullavey, H., Müller Ebhardt, J., Munch, P. G., Murray, E., Myer, J., Myer, T., Nash, J., Nelson, I., Neri, G., Newton, A., Nishizawa, F., Nocera, K., Numata, E., Ochsner, J., O'Dell, G. H., Ogin, B., O'Reilly, R., O'Shaughnessy, D. J., Ottaway, R. S., Otten, H., Overmier, B. J., Owen, G., Pagliaroli, C., Palomba, Y., Pan, C., Pankow, F., Paoletti, M. A., Papa, V., Parameshwaraiah, S., Pardi, A., Pasqualetti, R., Passaquieti, D., Passuello, P., Patel, M., Pedraza, S., Penn, A., Perreca, G., Persichetti, M., Pichot, F., Piergiovanni, V., Pierro, M., Pietka, L., Pinard, I. M., Pinto, M., Pitkin, H. J., Pletsch, M. V., Plissi, R., Poggiani, F., Postiglione, M., Prato, M., Principe, R., Prix, G. A., Prodi, L., Prokhorov, O., Puncken, M., Punturo, P., Puppo, V., Quetschke, F. J., Raab, O., Rabaste, D. S., Rabeling, H., Radkin, P., Raffai, Z., Raic, N., Rainer, M., Rakhmanov, P., Rapagnani, V., Raymond, V., Re, C. M., Reed, T., Reed, T., Regimbau, H., Rehbein, S., Reid, D. H., Reitze, F., Ricci, R., Riesen, K., Rile, B., Rivera, P., Robert, N. A., Robertson, F., Robinet, C., Robinson, E. L., Robinson, A., Rocchi, S., Roddy, L., Rolland, J., Rollin, J. D., Romano, R., Romano, J. H., Romie, D., Rosińska, C., Röver, S., Rowan, A., Rüdiger, P., Ruggi, P., Russell, K., Ryan, S., Sakata, F., Salemi, V., Sandberg, V., Sannibale, L., Santamaría, S., Saraf, P., Sarin, B., Sassola, B. S., Sathyaprakash, S., Sato, M., Satterthwaite, P. R., Saulson, R., Savage, P., Savov, M., Scanlan, R., Schilling, R., Schnabel, R., Schofield, B., Schulz, B. F., Schutz, P., Schwinberg, J., Scott, S. M., Scott, A. C., Searle, B., Sear, F., Seifert, D., Seller, A. S., Sengupta, D., Sentenac, A., Sergeev, B., Shapiro, P., Shawhan, D. H., Shoemaker, A., Sibley, X., Siemen, D., Sigg, S., Sinha, A. M., Sinte, B. J. J., Slagmolen, J., Slutsky, M. V., van der Sluy, J. R., Smith, M. R., Smith, N. D., Smith, K., Somiya, B., Sorazu, A., Stein, L. C., Stein, S., Steplewski, A., Stochino, R., Stone, K. A., Strain, S., Strigin, A., Stroeer, R., Sturani, A. L., Stuver, T. Z., Summerscale, K. X., Sun, M., Sung, P. J., Sutton, B., Swinkel, G. P., Szokoly, D., Talukder, L., Tang, D. B., Tanner, S. P., Tarabrin, J. R., Taylor, R., Taylor, R., Terenzi, J., Thacker, K. A., Thorne, K. S., Thorne, A., Thüring, K. V., Tokmakov, A., Toncelli, M., Tonelli, C., Torre, C., Torrie, E., Tournefier, F., Travasso, G., Traylor, M., Tria, J., Trummer, D., Ugolini, J., Ulmen, K., Urbanek, H., Vahlbruch, G., Vajente, M., Vallisneri, J. F. J., van den Brand, S., van der Putten, S., Va, R., Vaulin, M., Vavoulidi, A., Vecchio, G., Vedovato, A. A., van Veggel, J., Veitch, P., Veitch, C., Veltkamp, D., Verkindt, F., Vetrano, A., Viceré, A., Villar, J. Y., Vinet, H., Vocca, C., Vorvick, S. P., Vyachanin, S. J., Waldman, L., Wallace, R. L., Ward, M., Wa, A., Weidner, M., Weinert, A. J., Weinstein, R., Wei, L., Wen, S., Wen, K., Wette, J. T., Whelan, S. E., Whitcomb, B. F., Whiting, C., Wilkinson, P. A., Willem, H. R., William, L., William, B., Willke, I., Wilmut, L., Winkelmann, W., Winkler, C. C., Wipf, A. G., Wiseman, G., Woan, R., Wooley, J., Worden, W., Wu, I., Yakushin, H., Yamamoto, Z., Yan, S., Yoshida, M., Yvert, M., Zanolin, J., Zhang, L., Zhang, C., Zhao, N., Zotov, M. E., Zucker, J., Zweizig, S., Bégin, A., Corongiu, N., D'Amico, P. C. C., Freire, J. W. T., Hessel, G. B., Hobb, M., Kramer, A. G., Lyne, R. N., Manchester, F. E., Marshall, J., Middleditch, A., Possenti, S. M., Ransom, I. H., Stair, B., Stapper, and Pinto, Innocenzo
- Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE] ,Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics ,Ephemeris ,01 natural sciences ,LIMIT ,[ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc] ,Pulsar ,Millisecond pulsar ,pulsars: general ,0103 physical sciences ,gravitational waves ,Limit (mathematics) ,010303 astronomy & astrophysics ,QC ,Physics ,010308 nuclear & particles physics ,Crab Pulsar ,Gravitational wave ,[SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE] ,Astrophysics::Instrumentation and Methods for Astrophysics ,[ PHYS.ASTR.HE ] Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE] ,Astronomy and Astrophysics ,LIGO ,Amplitude ,Space and Planetary Science ,DISCOVERY ,DISTANCE ,[PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc] ,SPIN-DOWN ,[ SDU.ASTR.HE ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE] - Abstract
39 pages, 5 figures, Accepted in The Astrophysical Journal; International audience; We present a search for gravitational waves from 116 known millisecond and young pulsars using data from the fifth science run of the LIGO detectors. For this search ephemerides overlapping the run period were obtained for all pulsars using radio and X-ray observations. We demonstrate an updated search method that allows for small uncertainties in the pulsar phase parameters to be included in the search. We report no signal detection from any of the targets and therefore interpret our results as upper limits on the gravitational wave signal strength. The most interesting limits are those for young pulsars. We present updated limits on gravitational radiation from the Crab pulsar, where the measured limit is now a factor of seven below the spin-down limit. This limits the power radiated via gravitational waves to be less than ~2% of the available spin-down power. For the X-ray pulsar J0537-6910 we reach the spin-down limit under the assumption that any gravitational wave signal from it stays phase locked to the X-ray pulses over timing glitches, and for pulsars J1913+1011 and J1952+3252 we are only a factor of a few above the spin-down limit. Of the recycled millisecond pulsars several of the measured upper limits are only about an order of magnitude above their spin-down limits. For these our best (lowest) upper limit on gravitational wave amplitude is 2.3x10^-26 for J1603-7202 and our best (lowest) limit on the inferred pulsar ellipticity is 7.0x10^-8 for J2124-3358.
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- 2010
43. The young, highly relativistic binary pulsar J1906+0746
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Lorimer, D. R., Stairs, I. H., Freire, P. C. C., Cordes, J. M., Camilo, F., Faulkner, A. J., Lyne, A. G., Nice, D. J., Ransom, S. M., Arzoumanian, Z., Manchester, R. N., Champion, D. J., van Leeuwen, J., McLaughlin, M. A., Ramachandran, R., Hessels, J. W. T., Vlemmings, W., Deshpande, A. A., Bhat, N. D. R., Chatterjee, S., Han, J. L., Gaensler, B. M., Kasian, L., Deneva, J. S., Reid, B., Lazio, T. J. W., Kaspi, V. M., Crawford, F., Lommen, A. N., Backer, D. C., Kramer, M., Stappers, B. W., Hobbs, G. B., Possenti, A., D'Amico, N., and Burgay, M.
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Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics (astro-ph) ,FOS: Physical sciences ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
We report the discovery of PSR J1906+0746, a young 144-ms pulsar in a highly relativistic 3.98-hr orbit with an eccentricity of 0.085 and expected gravitational wave coalescence time of 300 Myr. The new pulsar was found during precursor survey observations with the Arecibo 1.4-GHz feed array system and retrospectively detected in the Parkes Multibeam plane pulsar survey data. From radio follow-up observations with Arecibo, Jodrell Bank, Green Bank, and Parkes, we have measured the spin-down and binary parameters of the pulsar and its basic spectral and polarization properties. We also present evidence for pulse profile evolution, which is likely due to geodetic precession, a relativistic effect caused by the misalignment of the pulsar spin and total angular momentum vectors. Our measurements show that PSR J1906+0746 is a young object with a characteristic age of 112 kyr. From the measured rate of orbital periastron advance 7.57+/-0.03 deg/yr, we infer a total system mass of 2.61+/-0.02 Msun. While these parameters suggest that the PSR J1906+0746 binary system might be a younger version of the double pulsar system, intensive searches for radio pulses from the companion have so far been unsuccessful. It is therefore not known whether the companion is another neutron star or a massive white dwarf. Regardless of the nature of the companion, a simple calculation suggests that the Galactic birth rate of binaries similar to PSR J1906+0746 is 60/Myr. This implies that PSR J1906+0746 will make a significant contribution to the computed cosmic inspiral rate of compact binary systems., 19 pages, 3 figures, accepted for publication in ApJ
- Published
- 2005
44. Testing the Universality of Free Fall with the Triple System J0337+1715.
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Archibald, A. M., Gusinskaia, N. V., Hessels, J. W. T., Lorimer, D. R., Lynch, R. S., Ransom, S. M., Stairs, I. H., Weltevrede, P., Perera, B.B.P., Preston, L.L., and Sanidas, S.
- Abstract
The millisecond pulsar PSR J0337+1715 is in a mildly relativistic hierarchical triple system with two white dwarfs. This offers the possibility of testing the universality of free fall: does the neutron star fall with the same acceleration as the inner white dwarf in the gravity of the outer white dwarf? We have carried out an intensive pulsar timing campaign, yielding some 27000 pulse time-of-arrival (TOA) measurements with a median uncertainty of 1.2 μs. Here we describe our analysis procedure and timing model. [ABSTRACT FROM AUTHOR]
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- 2017
- Full Text
- View/download PDF
45. Magnetospheric Switching in PSR B1828–11.
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Stairs, I. H., Lyne, A. G., Kramer, M., Stappers, B. W., van Leeuwen, J., Tung, A., Manchester, R. N., Hobbs, G. B., Lorimer, D. R., Melatos, A., Weltevrede, P., Perera, B.B.P., Preston, L.L., and Sanidas, S.
- Abstract
PSR B1828–11 is a young pulsar once thought to be undergoing free precession and recently found instead to be switching magnetospheric states in tandem with spin-down changes. Here we show the two extreme states of the mode-changing found for this pulsar and comment briefly on its interpretation. [ABSTRACT FROM AUTHOR]
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- 2017
- Full Text
- View/download PDF
46. Two Radio Pulsars with Magnetar Fields
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Mclaughlin, M. A., Lorimer, D. R., Lyne, A. G., Michael Kramer, Faulkner, A. J., Kaspi, V. M., Stairs, I. H., Manchester, R. N., Hobbs, G., Camilo, F., Possenti, A., and D Amico, N.
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Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics (astro-ph) ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
PSRs J1847-0130 and J1718-37184 have inferred surface dipole magnetic fields greater than those of any other known pulsars and well above the ``quantum critical field'' above which some models predict radio emission should not occur.These fields are similar to those of the anomalous X-ray pulsars (AXPs), which growing evidence suggests are ``magnetars''. The lack of AXP-like X-ray emission from these radio pulsars (and the non-detection of radio emission from the AXPs) creates new challenges for understanding pulsar emission physics and the relationship between these classes of apparently young neutron stars., 2 pages. To appear in "Young Neutron Stars and Their Environments" (IAU Symposium 218, ASP Conference Proceedings), eds F. Camilo and B. M. Gaensler
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- 2003
47. Giant pulses in Millisecond Pulsars
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Joshi, B. C., Michael Kramer, Lyne, A. G., Mclaughlin, M. A., and Stairs, I. H.
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Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics (astro-ph) ,FOS: Physical sciences ,Astrophysics - Abstract
Giant pulses (GPs), occasional individual pulses with an intensity 100 times the average intensity, have been detected in four pulsars todate. Their origin is not well understood, but studies suggest a connection between the strength of magnetic field at the light cylinder B_lc and the existence of GPs. Here, we report on detection of significant Large Amplitude Pulses (LAPs) in two more pulsars with high values of B_lc, PSRs J0218+4232 and B1957+20, observed using Giant Meterwave Radio Telescope (GMRT)., 2 pages, 2 figures, To appear in "Young Neutron Stars and Their Environments"(IAU Symposium 218, ASP Conference Proceedings), eds F. Camilo and B. M. Gaensler
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- 2003
48. Yet MORE PM Survey Discoveries....?
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Faulkner, A. J., Kramer, M., Hobbs, G., Lyne, A. G., Manchester, R. N., Camilo, F., Kaspi, V. M., Stairs, I. H., D'Amico, N., Possenti, A., Lorimer, D. R., and McLaughlin, M. A.
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Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics (astro-ph) ,Astrophysics::Instrumentation and Methods for Astrophysics ,FOS: Physical sciences ,Astrophysics - Abstract
The Parkes Multibeam (PM) survey has found nearly 50% of the >1400 known pulsars and detected 20% of the pulsars in binary systems (75% within the survey area), few of these are millisecond pulsars with orbits of less than one day. It is known that the normal search techniques used in the PM Survey have selected against finding binary pulsars, due to the long integration times used. The relative performance of the search techniques used and the improvements made prior to the complete reprocessing of the data currently being undertaken are discussed. The processing is being done on COBRA - the new supercomputer at Jodrell Bank. The results of the reprocessing, as well as adding more solitary pulsars, will give more confidence on the population and types of binaries in the Galactic plane. However, it can be shown that for millisecond pulsars in binary orbits of between 20min and a few hours, the search techniques are still relatively insensitive., 4 pages, 3 figures. Crete conference proceedings
- Published
- 2003
49. The Massive Binary Pulsar J1740-3052
- Author
-
Stairs, I. H., Manchester, R. N., Lyne, A. G., Kramer, M., Kaspi, V. M., Camilo, F., and D'Amico, N.
- Subjects
Astrophysics (astro-ph) ,FOS: Physical sciences ,Astrophysics - Abstract
The young pulsar J1740-3052 is in an 8-month orbit with a companion of at least 11 solar masses. We present multifrequency GBT and Parkes timing observations, and discuss implications for the nature of the companion., 4 pages; to appear in proceedings of "Radio Pulsars," eds. M. Bailes, D. J. Nice, S. E. Thorsett
- Published
- 2002
50. High-Resolution Observations of PSR B1828-11
- Author
-
Stairs, I. H., Athanasiadis, D., Kramer, M., and Lyne, A. G.
- Subjects
Astrophysics (astro-ph) ,Physics::Space Physics ,FOS: Physical sciences ,Astrophysics - Abstract
We present high-time-resolution observations of the young precessing pulsar B1828-11, which yield clues to the true beam shape and the fundamental precession period., 4 pages; to appear in proceedings of "Radio Pulsars," eds. M. Bailes, D. J. Nice, S. E. Thorsett
- Published
- 2002
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