Author: "Cognard I" / Topic: pulsars: general - Searchworks@Jio Institute Digital Library Search Results

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117 results on '"Cognard I"'

1. A pulsar-based time-scale from the International Pulsar Timing Array

Author: Hobbs, G, Guo, L, Caballero, RN, Coles, W, Lee, KJ, Manchester, RN, Reardon, DJ, Matsakis, D, Tong, ML, Arzoumanian, Z, Bailes, M, Bassa, CG, Bhat, NDR, Brazier, A, Burke-Spolaor, S, Champion, DJ, Chatterjee, S, Cognard, I, Dai, S, Desvignes, G, Dolch, T, Ferdman, RD, Graikou, E, Guillemot, L, Janssen, GH, Keith, MJ, Kerr, M, Kramer, M, Lam, MT, Liu, K, Lyne, A, Lazio, TJW, Lynch, R, McKee, JW, McLaughlin, MA, Mingarelli, CMF, Nice, DJ, Osłowski, S, Pennucci, TT, Perera, BBP, Perrodin, D, Possenti, A, Russell, CJ, Sanidas, S, Sesana, A, Shaifullah, G, Shannon, RM, Simon, J, Spiewak, R, Stairs, IH, Stappers, BW, Swiggum, JK, Taylor, SR, Theureau, G, Toomey, L, van Haasteren, R, Wang, JB, Wang, Y, and Zhu, XJ
Subjects: time, pulsars: general, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract: We have constructed a new time-scale, TT(IPTA16), based on observations of radio pulsars presented in the first data release from the International Pulsar Timing Array (IPTA). We used two analysis techniques with independent estimates of the noise models for the pulsar observations and different algorithms for obtaining the pulsar time-scale. The two analyses agree within the estimated uncertainties and both agree with TT(BIPM17), a post-corrected time-scale produced by the Bureau International des Poids et Mesures (BIPM). We show that both methods could detect significant errors in TT(BIPM17) if they were present. We estimate the stability of the atomic clocks from which TT(BIPM17) is derived using observations of four rubidium fountain clocks at the US Naval Observatory. Comparing the power spectrum of TT(IPTA16) with that of these fountain clocks suggests that pulsar-based time-scales are unlikely to contribute to the stability of the best time-scales over the next decade, but they will remain a valuable independent check on atomic time-scales. We also find that the stability of the pulsar-based time-scale is likely to be limited by our knowledge of solar-system dynamics, and that errors in TT(BIPM17) will not be a limiting factor for the primary goal of the IPTA, which is to search for the signatures of nano-Hertz gravitational waves.
Published: 2020

2. The second data release from the European Pulsar Timing Array: V. Search for continuous gravitational wave signals.

Author: Antoniadis, J., Arumugam, P., Arumugam, S., Babak, S., Bagchi, M., Bak Nielsen, A.-S., Bassa, C. G., Bathula, A., Berthereau, A., Bonetti, M., Bortolas, E., Brook, P. R., Burgay, M., Caballero, R. N., Chalumeau, A., Champion, D. J., Chanlaridis, S., Chen, S., Cognard, I., and Dandapat, S.
Subjects: BINARY black holes, SUPERMASSIVE black holes, BAYESIAN analysis, DATA release, PULSARS
Abstract: We present the results of a search for continuous gravitational wave signals (CGWs) in the second data release (DR2) of the European Pulsar Timing Array (EPTA) Collaboration. The most significant candidate event from this search has a gravitational wave frequency of 4–5 nHz. Such a signal could be generated by a supermassive black hole binary (SMBHB) in the local Universe. We present the results of a follow-up analysis of this candidate using both Bayesian and frequentist methods. The Bayesian analysis gives a Bayes factor of 4 in favour of the presence of the CGW over a common uncorrelated noise process. In contrast, the frequentist analysis estimates the p-value of the candidate to be < 1%, also assuming the presence of common uncorrelated red noise. However, comparing a model that includes both a CGW and a gravitational wave background (GWB) to a GWB only, the Bayes factor in favour of the CGW model is only 0.7. Therefore, we cannot conclusively determine the origin of the observed feature, nor can we rule it out as a CGW source. We present results of simulations that demonstrate that data containing a weak gravitational wave background can be misinterpreted as data including a CGW and vice versa, providing two plausible explanations for the EPTA DR2 data. Further investigations combining data from all PTA collaborations will be needed to reveal the true origin of this feature. [ABSTRACT FROM AUTHOR]
Published: 2024
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3. Improving pulsar timing precision through superior time-of-arrival creation.

Author: Wang, J., Verbiest, J. P. W., Shaifullah, G. M., Cognard, I., Guillemot, L., Janssen, G. H., Mickaliger, M. B., Possenti, A., and Theureau, G.
Subjects: ROOT-mean-squares, PHASE noise, PULSARS, DATA analysis, TELESCOPES
Abstract: Context. The measurement of pulsar pulse times-of-arrival (ToAs) is a crucial step in detecting low-frequency gravitational waves. To determine ToAs, we can use template-matching to compare each observed pulse profile with a standard template. However, using different combinations of templates and template-matching methods (TMMs) without careful consideration can lead to inconsistent results. Aims. In pulsar timing array (PTA) experiments, distinct ToAs from the same observations can be obtained due to the use of diverse templates and TMMs. In other words, employing diverse approaches can yield different timing results and would thus have a significant impact on subsequent gravitational wave searches. In this paper we examine several commonly used combinations to analyze their effect on pulse ToAs. Methods. We evaluated the potential impact of template and TMM selection on 13 typical millisecond pulsars within the European PTA. We employed pulsar timing methods, specifically the root mean square and reduced chi-square (χ2r) of the residuals of the best timing solution, to assess the outcomes. Additionally, we evaluated the system-limited noise floor (SLNF) for each pulsar at various telescopes operating around 1.4 GHz using frequency-resolved templates. Results. Our findings suggest that utilizing data-derived and smoothed templates in conjunction with the Fourier-domain with Markov chain Monte Carlo TMM is generally the most effective approach, though there may be exceptions that require further attention. Furthermore, we determine that pulse phase jitter noise does not significantly limit the current precision of the European PTA's timing, as jitter levels derived from other studies are much lower than the SLNF. [ABSTRACT FROM AUTHOR]
Published: 2024
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4. A targeted radio pulsar survey of redback candidates with MeerKAT.

Author: Thongmeearkom, T, Clark, C J, Breton, R P, Burgay, M, Nieder, L, Freire, P C C, Barr, E D, Stappers, B W, Ransom, S M, Buchner, S, Calore, F, Champion, D J, Cognard, I, Grießmeier, J -M, Kramer, M, Levin, L, Padmanabh, P V, Possenti, A, Ridolfi, A, and Krishnan, V Venkatraman
Subjects: PULSAR detection, STELLAR mass, MEERKAT, NEUTRON stars, BINARY pulsars, RADIO technology, SPIDERS
Abstract: Redbacks are millisecond pulsar binaries with low-mass, irradiated companions. These systems have a rich phenomenology that can be used to probe binary evolution models, pulsar wind physics, and the neutron star mass distribution. A number of high-confidence redback candidates have been identified through searches for variable optical and X-ray sources within the localization regions of unidentified but pulsar-like Fermi -LAT gamma-ray sources. However, these candidates remain unconfirmed until pulsations are detected. As part of the TRAPUM project, we searched for radio pulsations from six of these redback candidates with MeerKAT. We discovered three new radio millisecond pulsars, PSRs J0838−2827, J0955−3947, and J2333−5526, confirming their redback nature. PSR J0838−2827 remained undetected for 2 yr after our discovery despite repeated observations, likely due to evaporated material absorbing the radio emission for long periods of time. While, to our knowledge, this system has not undergone a transition to an accreting state, the disappearance, likely caused by extreme eclipses, illustrates the transient nature of spider pulsars and the heavy selection bias in uncovering their radio population. Radio timing enabled the detection of gamma-ray pulsations from all three pulsars, from which we obtained 15-yr timing solutions. All of these sources exhibit complex orbital period variations consistent with gravitational quadrupole moment variations in the companion stars. These timing solutions also constrain the binary mass ratios, allowing us to narrow down the pulsar masses. We find that PSR J2333−5526 may have a neutron star mass in excess of 2 M⊙. [ABSTRACT FROM AUTHOR]
Published: 2024
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5. From spin noise to systematics: stochastic processes in the first International Pulsar Timing Array data release

Author: Lentati, L, Shannon, RM, Coles, WA, Verbiest, JPW, van Haasteren, R, Ellis, JA, Caballero, RN, Manchester, RN, Arzoumanian, Z, Babak, S, Bassa, CG, Bhat, NDR, Brem, P, Burgay, M, Burke-Spolaor, S, Champion, D, Chatterjee, S, Cognard, I, Cordes, JM, Dai, S, Demorest, P, Desvignes, G, Dolch, T, Ferdman, RD, Fonseca, E, Gair, JR, Gonzalez, ME, Graikou, E, Guillemot, L, Hessels, JWT, Hobbs, G, Janssen, GH, Jones, G, Karuppusamy, R, Keith, M, Kerr, M, Kramer, M, Lam, MT, Lasky, PD, Lassus, A, Lazarus, P, Lazio, TJW, Lee, KJ, Levin, L, Liu, K, Lynch, RS, Madison, DR, McKee, J, McLaughlin, M, McWilliams, ST, Mingarelli, CMF, Nice, DJ, Osłowski, S, Pennucci, TT, Perera, BBP, Perrodin, D, Petiteau, A, Possenti, A, Ransom, SM, Reardon, D, Rosado, PA, Sanidas, SA, Sesana, A, Shaifullah, G, Siemens, X, Smits, R, Stairs, I, Stappers, B, Stinebring, DR, Stovall, K, Swiggum, J, Taylor, SR, Theureau, G, Tiburzi, C, Toomey, L, Vallisneri, M, van Straten, W, Vecchio, A, Wang, J-B, Wang, Y, You, XP, Zhu, WW, and Zhu, X-J
Subjects: methods: data analysis, pulsars: general, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract: We analyse the stochastic properties of the 49 pulsars that comprise the first International Pulsar Timing Array (IPTA) data release. We use Bayesian methodology, performing model selection to determine the optimal description of the stochastic signals present in each pulsar. In addition to spin-noise and dispersion-measure (DM) variations, these models can include timing noise unique to a single observing system, or frequency band. We show the improved radio-frequency coverage and presence of overlapping data from different observing systems in the IPTA data set enables us to separate both system and band-dependent effects with much greater efficacy than in the individual pulsar timing array (PTA) data sets. For example, we show that PSR J1643-1224 has, in addition to DM variations, significant band-dependent noise that is coherent between PTAs which we interpret as coming from time-variable scattering or refraction in the ionized interstellar medium. Failing to model these different contributions appropriately can dramatically alter the astrophysical interpretation of the stochastic signals observed in the residuals. In some cases, the spectral exponent of the spin-noise signal can vary from 1.6 to 4 depending upon the model, which has direct implications for the long-term sensitivity of the pulsar to a stochastic gravitational-wave (GW) background. By using a more appropriate model, however, we can greatly improve a pulsar's sensitivity to GWs. For example, including system and band-dependent signals in the PSR J0437-4715 data set improves the upper limit on a fiducial GW background by ~60 per cent compared to a model that includes DM variations and spin-noise only.
Published: 2016

6. The second data release from the European Pulsar Timing Array: IV. Implications for massive black holes, dark matter, and the early Universe.

Author: EPTA Collaboration and InPTA Collaboration, Antoniadis, J., Arumugam, P., Arumugam, S., Babak, S., Bagchi, M., Bak Nielsen, A.-S., Bassa, C. G., Bathula, A., Berthereau, A., Bonetti, M., Bortolas, E., Brook, P. R., Burgay, M., Caballero, R. N., Chalumeau, A., Champion, D. J., Chanlaridis, S., Chen, S., and Cognard, I.
Subjects: BLACK holes, DARK matter, INFLATIONARY universe, DATA release, BINARY black holes, UNIVERSE
Abstract: The European Pulsar Timing Array (EPTA) and Indian Pulsar Timing Array (InPTA) collaborations have measured a low-frequency common signal in the combination of their second and first data releases, respectively, with the correlation properties of a gravitational wave background (GWB). Such a signal may have its origin in a number of physical processes including a cosmic population of inspiralling supermassive black hole binaries (SMBHBs); inflation, phase transitions, cosmic strings, and tensor mode generation by the non-linear evolution of scalar perturbations in the early Universe; and oscillations of the Galactic potential in the presence of ultra-light dark matter (ULDM). At the current stage of emerging evidence, it is impossible to discriminate among the different origins. Therefore, for this paper, we consider each process separately, and investigated the implications of the signal under the hypothesis that it is generated by that specific process. We find that the signal is consistent with a cosmic population of inspiralling SMBHBs, and its relatively high amplitude can be used to place constraints on binary merger timescales and the SMBH-host galaxy scaling relations. If this origin is confirmed, this would be the first direct evidence that SMBHBs merge in nature, adding an important observational piece to the puzzle of structure formation and galaxy evolution. As for early Universe processes, the measurement would place tight constraints on the cosmic string tension and on the level of turbulence developed by first-order phase transitions. Other processes would require non-standard scenarios, such as a blue-tilted inflationary spectrum or an excess in the primordial spectrum of scalar perturbations at large wavenumbers. Finally, a ULDM origin of the detected signal is disfavoured, which leads to direct constraints on the abundance of ULDM in our Galaxy. [ABSTRACT FROM AUTHOR]
Published: 2024
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7. THE SECOND FERMI LARGE AREA TELESCOPE CATALOG OF GAMMA-RAY PULSARS

Author: Abdo, AA, Ajello, M, Allafort, A, Baldini, L, Ballet, J, Barbiellini, G, Baring, MG, Bastieri, D, Belfiore, A, Bellazzini, R, Bhattacharyya, B, Bissaldi, E, Bloom, ED, Bonamente, E, Bottacini, E, Brandt, TJ, Bregeon, J, Brigida, M, Bruel, P, Buehler, R, Burgay, M, Burnett, TH, Busetto, G, Buson, S, Caliandro, GA, Cameron, RA, Camilo, F, Caraveo, PA, Casandjian, JM, Cecchi, C, Çelik, Ö, Charles, E, Chaty, S, Chaves, RCG, Chekhtman, A, Chen, AW, Chiang, J, Chiaro, G, Ciprini, S, Claus, R, Cognard, I, Cohen-Tanugi, J, Cominsky, LR, Conrad, J, Cutini, S, D'Ammando, F, de Angelis, A, DeCesar, ME, De Luca, A, Hartog, PR den, de Palma, F, Dermer, CD, Desvignes, G, Digel, SW, Di Venere, L, Drell, PS, Drlica-Wagner, A, Dubois, R, Dumora, D, Espinoza, CM, Falletti, L, Favuzzi, C, Ferrara, EC, Focke, WB, Franckowiak, A, Freire, PCC, Funk, S, Fusco, P, Gargano, F, Gasparrini, D, Germani, S, Giglietto, N, Giommi, P, Giordano, F, Giroletti, M, Glanzman, T, Godfrey, G, Gotthelf, EV, Grenier, IA, Grondin, M-H, Grove, JE, Guillemot, L, Guiriec, S, Hadasch, D, Hanabata, Y, Harding, AK, Hayashida, M, Hays, E, Hessels, J, Hewitt, J, Hill, AB, Horan, D, Hou, X, Hughes, RE, Jackson, MS, Janssen, GH, Jogler, T, Jóhannesson, G, Johnson, RP, and Johnson, AS
Subjects: catalogs, pulsars: general, stars: neutron, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract: This catalog summarizes 117 high-confidence ≥0.1 GeV gamma-ray pulsar detections using three years of data acquired by the Large Area Telescope (LAT) on the Fermi satellite. Half are neutron stars discovered using LAT data through periodicity searches in gamma-ray and radio data around LAT unassociated source positions. The 117 pulsars are evenly divided into three groups: millisecond pulsars, young radio-loud pulsars, and young radio-quiet pulsars. We characterize the pulse profiles and energy spectra and derive luminosities when distance information exists. Spectral analysis of the off-peak phase intervals indicates probable pulsar wind nebula emission for four pulsars, and off-peak magnetospheric emission for several young and millisecond pulsars. We compare the gamma-ray properties with those in the radio, optical, and X-ray bands. We provide flux limits for pulsars with no observed gamma-ray emission, highlighting a small number of gamma-faint, radio-loud pulsars. The large, varied gamma-ray pulsar sample constrains emission models. Fermi's selection biases complement those of radio surveys, enhancing comparisons with predicted population distributions. © 2013. The American Astronomical Society. All rights reserved..
Published: 2013

8. Variable scintillation arcs of millisecond pulsars observed with the Large European Array for Pulsars.

Author: Main, R A, Antoniadis, J, Chen, S, Cognard, I, Hu, H, Jang, J, Karuppusamy, R, Kramer, M, Liu, K, Liu, Y, Mall, G, McKee, J W, Mickaliger, M B, Perrodin, D, Sanidas, S A, Stappers, B W, Sprenger, T, Wucknitz, O, Bassa, C G, and Burgay, M
Subjects: SCINTILLATION counters, VERY long baseline interferometry
Abstract: We present the first large sample of scintillation arcs in millisecond pulsars (MSPs), analysing 12 sources observed with the Large European Array for Pulsars (LEAP), and the Effelsberg 100-m telescope. We estimate the delays from multipath propagation, measuring significant correlated changes in scattering time-scales over a 10 yr time span. Many sources show compact concentrations of power in the secondary spectrum, which in PSRs J0613−0200 and J1600−3053 can be tracked between observations, and are consistent with compact scattering at fixed angular positions. Other sources such as PSRs J1643−1224 and J0621+1002 show diffuse, asymmetric arcs which are likely related to phase-gradients across the scattering screen. PSR B1937+21 shows at least three distinct screens which dominate at different times and evidence of varying screen axes or multiscreen interactions. We model annual and orbital arc curvature variations in PSR J0613−0200, providing a measurement of the longitude of ascending node, resolving the sense of the orbital inclination, where our best-fit model is of a screen with variable axis of anisotropy over time, corresponding to changes in the scattering of the source. Unmodelled variations of the screen's axis of anisotropy are likely to be a limiting factor in determining orbital parameters with scintillation, requiring careful consideration of variable screen properties, or independent very long baseline interferometry (VLBI) measurements. Long-term scintillation studies such as this serve as a complementary tool to pulsar timing, to measure a source of correlated noise for pulsar timing arrays, solve pulsar orbits, and to understand the astrophysical origin of scattering screens. [ABSTRACT FROM AUTHOR]
Published: 2023
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9. The TRAPUM L-band survey for pulsars in Fermi-LAT gamma-ray sources.

Author: Clark, C J, Breton, R P, Barr, E D, Burgay, M, Thongmeearkom, T, Nieder, L, Buchner, S, Stappers, B, Kramer, M, Becker, W, Mayer, M, Phosrisom, A, Ashok, A, Bezuidenhout, M C, Calore, F, Cognard, I, Freire, P C C, Geyer, M, Grießmeier, J-M, and Karuppusamy, R
Subjects: PULSAR detection, NEUTRON stars, GRAVITATIONAL waves, GAMMA ray astronomy, ACTINIC flux, RANDOM forest algorithms, WHITE dwarf stars
Abstract: More than 100 millisecond pulsars (MSPs) have been discovered in radio observations of gamma-ray sources detected by the Fermi Large Area Telescope (LAT), but hundreds of pulsar-like sources remain unidentified. Here, we present the first results from the targeted survey of Fermi -LAT sources being performed by the Transients and Pulsars with MeerKAT (TRAPUM) Large Survey Project. We observed 79 sources identified as possible gamma-ray pulsar candidates by a Random Forest classification of unassociated sources from the 4FGL catalogue. Each source was observed for 10 min on two separate epochs using MeerKAT's L -band receiver (856–1712 MHz), with typical pulsed flux density sensitivities of |$\sim 100\, \mu$| Jy. Nine new MSPs were discovered, eight of which are in binary systems, including two eclipsing redbacks and one system, PSR J1526−2744, that appears to have a white dwarf companion in an unusually compact 5 h orbit. We obtained phase-connected timing solutions for two of these MSPs, enabling the detection of gamma-ray pulsations in the Fermi -LAT data. A follow-up search for continuous gravitational waves from PSR J1526−2744 in Advanced LIGO data using the resulting Fermi -LAT timing ephemeris yielded no detection, but sets an upper limit on the neutron star ellipticity of 2.45 × 10−8. We also detected X-ray emission from the redback PSR J1803−6707 in data from the first eROSITA all-sky survey, likely due to emission from an intrabinary shock. [ABSTRACT FROM AUTHOR]
Published: 2023
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10. Robust parameter estimation from pulsar timing data.

Author: Samajdar, A, Shaifullah, G M, Sesana, A, Antoniadis, J, Burgay, M, Chen, S, Cognard, I, Guillemot, L, Kramer, M, McKee, J W, Mickaliger, M B, Theureau, G, and Van der Wateren, E
Subjects: MARKOV chain Monte Carlo, PARAMETER estimation, PULSARS
Abstract: Recently, global pulsar timing arrays have released results from searching for a nano-Hertz gravitational wave background signal. Although there has not been any definite evidence of the presence of such a signal in residuals of pulsar timing data yet, with more and improved data in future, a statistically significant detection is expected to be made. Stochastic algorithms are used to sample a very large parameter space to infer results from data. In this paper, we attempt to rule out effects arising from the stochasticity of the sampler in the inference process. We compare different configurations of nested samplers and the more commonly used markov chain monte carlo method to sample the pulsar timing array parameter space and account for times taken by the different samplers on same data. Although we obtain consistent results on parameters from different sampling algorithms, we propose two different samplers for robustness checks on data in the future to account for cross-checks between sampling methods as well as realistic run-times. [ABSTRACT FROM AUTHOR]
Published: 2022
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11. Modelling annual scintillation arc variations in PSR J1643−1224 using the Large European Array for Pulsars.

Author: Mall, G, Main, R A, Antoniadis, J, Bassa, C G, Burgay, M, Chen, S, Cognard, I, Concu, R, Corongiu, A, Gaikwad, M, Hu, H, Janssen, G H, Karuppusamy, R, Kramer, M, Lee, K J, Liu, K, McKee, J W, Melis, A, Mickaliger, M B, and Perrodin, D
Subjects: PULSARS, BINARY pulsars, INTERSTELLAR medium, RELATIVE velocity, POWER spectra
Abstract: In this work, we study variations in the parabolic scintillation arcs of the binary millisecond pulsar PSR J1643−1224 over five years using the Large European Array for Pulsars (LEAP). The two-dimensional (2D) power spectrum of scintillation, called the secondary spectrum, often shows a parabolic distribution of power, where the arc curvature encodes the relative velocities and distances of the pulsar, ionized interstellar medium, and Earth. We observe a clear parabolic scintillation arc, which varies in curvature throughout the year. The distribution of power in the secondary spectra is inconsistent with a single scattering screen, which is fully 1D or entirely isotropic. We fit the observed arc curvature variations with two models: an isotropic scattering screen and a model with two independent 1D screens. We measure the distance to the scattering screen to be in the range 114–223 pc, depending on the model, consistent with the known distance of the foreground large-diameter H ii region Sh 2-27 (112 ± 17 pc), suggesting that it is the dominant source of scattering. We obtain only weak constraints on the pulsar's orbital inclination and longitude of ascending node, since the scintillation pattern is not very sensitive to the pulsar's motion and the screen is much closer to the Earth than the pulsar. More measurements of this kind – where scattering screens can be associated with foreground objects – will help to inform the origins and distribution of scattering screens within our galaxy. [ABSTRACT FROM AUTHOR]
Published: 2022
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12. Removal and replacement of interference in tied-array radio pulsar observations using the spectral kurtosis estimator.

Author: Purver, M, Bassa, C G, Cognard, I, Janssen, G H, Karuppusamy, R, Kramer, M, Lee, K J, Liu, K, McKee, J W, Perrodin, D, Sanidas, S, Smits, R, and Stappers, B W
Subjects: KURTOSIS, RADIO interference, PULSARS, SIGNAL-to-noise ratio, NULL hypothesis, DATA reduction, SURVEILLANCE radar
Abstract: We describe how to implement the spectral kurtosis method of interference removal (zapping) on a digitized signal of averaged power values. Spectral kurtosis is a hypothesis test, analogous to the t-test, with a null hypothesis that the amplitudes from which power is formed belong to a 'good' distribution – typically Gaussian with zero mean – where power values are zapped if the hypothesis is rejected at a specified confidence level. We derive signal-to-noise ratios (SNRs) as a function of amount of zapping for folded radio pulsar observations consisting of a sum of signals from multiple telescopes in independent radio-frequency interference environments, comparing four methods to compensate for lost data with coherent (tied-array) and incoherent summation. For coherently summed amplitudes, scaling amplitudes from non-zapped telescopes achieves a higher SNR than replacing zapped amplitudes with artificial noise. For incoherently summed power values, the highest SNR is given by scaling power from non-zapped telescopes to maintain a constant mean. We use spectral kurtosis to clean a tied-array radio pulsar observation by the Large European Array for Pulsars: the signal from one telescope is zapped with time and frequency resolutions of |$6.25\, \mathrm{ms}$| and |$0.16\, \mathrm{MHz}$|⁠ , removing interference, along with 0.27 per cent of 'good' data, giving an uncertainty of |$0.25\, \mathrm{\mu \mathrm{ s}}$| in pulse time of arrival (TOA) for PSR J1022+1001. We use a single-telescope observation to demonstrate recovery of the pulse profile shape, with 0.6 per cent of data zapped and a reduction from 1.22 to |$0.70\, \mathrm{\mu \mathrm{ s}}$| in TOA uncertainty. [ABSTRACT FROM AUTHOR]
Published: 2022
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13. The relativistic binary programme on MeerKAT: science objectives and first results.

Author: 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
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14. Measuring interstellar delays of PSR J0613−0200 over 7 yr, using the Large European Array for Pulsars.

Author: Main, R A, Sanidas, S A, Antoniadis, J, Bassa, C, Chen, S, Cognard, I, Gaikwad, M, Hu, H, Janssen, G H, Karuppusamy, R, Kramer, M, Lee, K J, Liu, K, Mall, G, McKee, J W, Mickaliger, M B, Perrodin, D, Stappers, B W, Tiburzi, C, and Wucknitz, O
Subjects: RELATIVE velocity, WAVE analysis, GRAVITATIONAL waves, POWER spectra, BINARY pulsars, PULSARS
Abstract: Using data from the Large European Array for Pulsars, and the Effelsberg telescope, we study the scintillation parameters of the millisecond pulsar PSR J0613−0200 over a 7 yr timespan. The 'secondary spectrum' – the 2D power spectrum of scintillation – presents the scattered power as a function of time delay, and contains the relative velocities of the pulsar, observer, and scattering material. We detect a persistent parabolic scintillation arc, suggesting scattering is dominated by a thin, anisotropic region. The scattering is poorly described by a simple exponential tail, with excess power at high delays; we measure significant, detectable scattered power at times out to |${\sim}5 \, \mu {\rm s}$|⁠ , and measure the bulk scattering delay to be between 50 to 200 ns with particularly strong scattering throughout 2013. These delays are too small to detect a change of the pulse profile shape, yet they would change the times of arrival as measured through pulsar timing. The arc curvature varies annually, and is well fitted by a one-dimensional scattering screen |${\sim}40{{\ \rm per\ cent}}$| of the way towards the pulsar, with a changing orientation during the increased scattering in 2013. Effects of uncorrected scattering will introduce time delays correlated over time in individual pulsars, and may need to be considered in gravitational wave analyses. Pulsar timing programmes would benefit from simultaneously recording in a way that scintillation can be resolved, in order to monitor the variable time delays caused by multipath propagation. [ABSTRACT FROM AUTHOR]
Published: 2020
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15. The LOFAR tied-array all-sky survey (LOTAAS): Characterization of 20 pulsar discoveries and their single-pulse behaviour.

Author: Michilli, D, Bassa, C, Cooper, S, Hessels, J W T, Kondratiev, V I, Sanidas, S, Stappers, B W, Tan, C M, van Leeuwen, J, Cognard, I, Grießmeier, J-M, Lyne, A G, Verbiest, J P W, and Weltevrede, P
Subjects: PULSARS, RADIO telescopes, PULSAR detection
Abstract: We are using the LOw-Frequency ARray (LOFAR) to perform the LOFAR Tied-Array All-Sky (LOTAAS) survey for pulsars and fast transients. Here, we present the astrometric and rotational parameters of 20 pulsars discovered as part of LOTAAS. These pulsars have regularly been observed with LOFAR at 149 MHz and the Lovell telescope at 1532 MHz, supplemented by some observations with the Lovell telescope at 334 MHz and the Nançay Radio Telescope at 1484 MHz. Timing models are calculated for the 20 pulsars, some of which are among the slowest spinning pulsars known. PSR J1236 − 0159 rotates with a period P ∼ 3.6 s, while five additional pulsars show P > 2 s. Also, the spin-down rates |$\dot{P}$| are, on average, low, with PSR J0815 + 4611 showing |$\dot{P} \sim 4\times 10^{-18}$|⁠. Some of the pulse profiles, generically single-peaked, present complex shapes evolving with frequency. Multifrequency flux measurements show that these pulsars have generically relatively steep spectra but exceptions are present, with values ranging between ∼−4 and −1. Among the pulsar sample, a large fraction shows large single-pulse variability, with four pulsars being undetectable more than |$15{{\ \rm per\ cent}}$| of the time and one tentatively classified as a Rotating Radio Transient. Two single-peaked pulsars show drifting sub-pulses. [ABSTRACT FROM AUTHOR]
Published: 2020
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16. Timing of PSR J2055+3829, an eclipsing black widow pulsar discovered with the Nançay Radio Telescope.

Author: Guillemot, L., Octau, F., Cognard, I., Desvignes, G., Freire, P. C. C., Smith, D. A., Theureau, G., and Burnett, T. H.
Subjects: RADIO telescopes, PULSARS, GAMMA ray astronomy, GLOBULAR clusters, WIDOWS, BINARY pulsars, DISTRIBUTION (Probability theory)
Abstract: We report on the timing observations of the millisecond pulsar PSR J2055+3829 originally discovered as part of the SPAN512 survey conducted with the Nançay Radio Telescope. The pulsar has a rotational period of 2.089 ms and is in a tight 3.1 h orbit around a very low mass (0.023 ≤ mc ≲ 0.053 M⊙, 90% c.l.) companion. Our 1.4 GHz observations reveal the presence of eclipses of the radio signal of the pulsar, caused by the outflow of material from the companion, for a few minutes around superior conjunction of the pulsar. The very low companion mass, the observation of radio eclipses, and the detection of time variations of the orbital period establish PSR J2055+3829 as a "black widow" (BW) pulsar. Inspection of the radio signal from the pulsar during ingress and egress phases shows that the eclipses in PSR J2055+3829 are asymmetric and variable, as is commonly observed in other similar systems. More generally, the orbital properties of the new pulsar are found to be very similar to those of other known eclipsing BW pulsars. No gamma-ray source has been detected at the location of the pulsar in recent Fermi-LAT source catalogs. We used the timing ephemeris to search ten years of Fermi Large Area Telescope (LAT) data for gamma-ray pulsations, but were unable to detect any. This non-detection could be a consequence of the large distance of the pulsar compared to those of known gamma-ray millisecond pulsars outside of globular clusters. We finally compared the mass functions of eclipsing and non-eclipsing BW pulsars and confirmed previous findings that eclipsing BWs have higher mass functions than their non-eclipsing counterparts. Larger inclinations could explain the higher mass functions of eclipsing BWs. On the other hand, the mass function distributions of Galactic disk and globular cluster BWs appear to be consistent, suggesting, despite the very different environments, the existence of common mechanisms taking place in the last stages of evolution of BWs. [ABSTRACT FROM AUTHOR]
Published: 2019
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17. detailed study of giant pulses from PSR B1937+21 using the Large European Array for Pulsars.

Author: McKee, J W, Stappers, B W, Bassa, C G, Chen, S, Cognard, I, Gaikwad, M, Janssen, G H, Karuppusamy, R, Kramer, M, Lee, K J, Liu, K, Perrodin, D, Sanidas, S A, Smits, R, Wang, L, and Zhu, W W
Subjects: NEUTRON stars, RADIO telescopes, PULSATING stars, MAGNETOSPHERE, STELLAR atmospheres
Abstract: We have studied 4265 giant pulses (GPs) from the millisecond pulsar B1937+21; the largest-ever sample gathered for this pulsar, in observations made with the Large European Array for Pulsars. The pulse energy distribution of GPs associated with the interpulse are well-described by a power law, with index α = −3.99 ± 0.04, while those associated with the main pulse are best-described by a broken power law, with the break occurring at ∼7 Jy |$\mu$| s, with power-law indices αlow = −3.48 ± 0.04 and αhigh = −2.10 ± 0.09. The modulation indices of the GP emission are measured, which are found to vary by ∼0.5 at pulse phases close to the centre of the GP phase distributions. We find the frequency-resolved structure of GPs to vary significantly, and in a manner that cannot be attributed to the interstellar medium influence on the observed pulses. We examine the distribution of polarization fractions of the GPs and find no correlation between GP emission phase and fractional polarization. We use the GPs to time PSR B1937+21 and although the achievable time of arrival precision of the GPs is approximately a factor of two greater than that of the average pulse profile, there is a negligible difference in the precision of the overall timing solution when using the GPs. [ABSTRACT FROM AUTHOR]
Published: 2019
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18. Discovery of Pulsed γ-Rays from PSR J0034-0534 with the Fermi Large Area Telescope: A Case for Co-Located Radio and γ-Ray Emission Regions

Author: Abdo, A.A., Ackermann, M., Ajello, M., Allafort, A., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Blandford, R. D., Bloom, E.D., Bonamente, E., Borgland, A.W., Bouvier, A., Bregeon, J., Brez, A., Brigida, M., Bruel, P., Burnett, T.H., Buson, S., Caliandro, G. A., Cameron, R. A., Camilo, F., Caraveo, P. A., Carrigan, S., Casandjian, J. M., Cecchi, C., Celik, O., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cognard, I., Cohen-Tanugi, J., Conrad, J., Corbet, R., DeCesar, M. E., Dermer, C. D., Desvignes, G., de, Angelis A., de, Palma F., Digel, S. W., Dormody, M., do, Couto e Silva E., Drell, P. S., Dubois, R., Dumora, D., Espinoza, C., Farnier, C., Favuzzi, C., Fegan, S. J., Focke, W. B., Frailis, M., Freire, P. C. C., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giavitto, G., Giglietto, N., Giordano, F., Glanzman, T., Godfrey, G., Grenier, I. A., Grondin, M.-H., Grove, J. E., Guillemot, L., Guiriec, S., Hadasch, D., Harding, A. K., Hays, E., Hobbs, G., Horan, D., Hughes, R. E., Johannesson, G., Johnson, A. S., Johnson, T. J., Johnson, W. N., Johnston, S., Kerr, M., Knodlseder, J., Kramer, M., Kuss, M., Lande, J., Latronico, L., Lemoine-Goumard, M., Llena, Garde M., Longo, F., Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Lyne, A. G., Makeev, A., Manchester, R. N., Marelli, M., Mazziotta, M. N., McConville, W., McEnery, J. E., McGlynn, S., Meurer, C., Michelson, P. F., Mitthumsiri, W., Moiseev, A. A., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nolan, P. L., Norris, J. P., Noutsos, A., Nuss, E., Omodei, N., Orlando, E., Ormes, J. F., Fukazawa, Y., Kamae, T., Katagiri, H., Kataoka, J., Kawai, N., Mizuno, T., Ohsugi, T., Ozaki, Masanobu, 12006653 - Venter, Christo, Abdo, A. A., Ackermann, M., Ajello, M., Allafort, A., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Blandford, R. D., Bloom, E. D., Bonamente, E., Borgland, A. W., Bouvier, A., Bregeon, J., Brez, A., Brigida, M., Bruel, P., Burnett, T. H., Buson, S., Caliandro, G. A., Cameron, R. A., Camilo, F., Caraveo, P. A., Carrigan, S., Casandjian, J. M., Cecchi, C., Celik, O., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cognard, I., Cohen Tanugi, J., Conrad, J., Corbet, R., Decesar, M. E., Dermer, C. D., Desvignes, G., Angelis, A. d., Palma, F. d., Digel, S. W., Dormody, M., Silva, E. D. E., Drell, P. S., Dubois, R., Dumora, D., Espinoza, C., Farnier, C., Favuzzi, C., Fegan, S. J., Focke, W. B., Frailis, M., Freire, P. C. C., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giavitto, G., Giglietto, N., Giordano, F., Glanzman, T., Godfrey, G., Grenier, I. A., Grondin, M. H., Grove, J. E., Guillemot, L., Guiriec, S., Hadasch, D., Harding, A. K., Hays, E., Hobbs, G., Horan, D., Hughes, R. E., Johannesson, G., Johnson, A. S., Johnson, T. J., Johnson, W. N., Johnston, S., Kamae, T., Katagiri, H., Kataoka, J., Kawai, N., Kerr, M., Knodlseder, J., Kramer, M., Kuss, M., Lande, J., Latronico, L., Lemoine Goumard, M., Garde, M. L., Longo, Francesco, Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Lyne, A. G., Makeev, A., Manchester, R. N., Marelli, M., Mazziotta, M. N., Mcconville, W., Mcenery, J. E., Mcglynn, S., Meurer, C., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Moiseev, A. A., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nolan, P. L., Norris, J. P., Noutsos, A., Nuss, E., Ohsugi, T., Omodei, N., Orlando, E., Ormes, J. F., Ozaki, M., Paneque, D., Panetta, J. H., Parent, D., Pelassa, V., Pepe, M., Pesce Rollins, M., Pierbattista, M., Piron, F., Porter, T. A., Raino, S., Rando, R., Ransom, S. M., Razzano, M., Reimer, A., Reimer, O., Reposeur, T., Ripken, J., Ritz, S., Rochester, L. S., Rodriguez, A. Y., Romani, R. W., Roth, M., Ryde, F., Sadrozinski, H. F. W., Sander, A., Parkinson, P. M. S., Scargle, J. D., Sgro, C., Siskind, E. J., Smith, D. A., Smith, P. D., Spandre, G., Spinelli, P., Stappers, B. W., Starck, J. L., Strickman, M. S., Suson, D. J., Takahashi, H., Tanaka, T., Thayer, J. B., Thayer, J. G., Theureau, G., Thompson, D. J., Thorsett, S. E., Tibaldo, L., Torres, D. F., Tosti, G., Tramacere, A., Usher, T. L., Etten, A. V., Vasileiou, V., Venter, C., Vilchez, N., Vitale, V., Waite, A. P., Wallace, E., Wang, P., Weltevrede, P., Winer, B. L., Wood, K. S., Ylinen, T., and Ziegler, M.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Pulsar planet, general [Gamma rays], general [Pulsars], Fermi satellite, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, High Energy Gamma-ray Astronomy, law.invention, Telescope, Pulsar, Millisecond pulsar, law, pulsars: general, 0103 physical sciences, gamma rays: general, pulsars: individual (PSR J0034–0534), 010306 general physics, 010303 astronomy & astrophysics, Pulsars, Physics, Crab Pulsar, Gamma rays: general, pulsars: individual (PSR J0034-0534), Gamma ray, Astronomy, Astronomy and Astrophysics, pulsars: individual: PSR J0034–0534, Light curve, individual (PSR J0034−0534) [Pulsars], Space and Planetary Science, Fermi Gamma-ray Space Telescope
Abstract: 著者人数：191名, Accepted: 2010-02-08, 資料番号: SA1002610000
Published: 2010

19. Erratum: Placing limits on the stochastic gravitational-wave background using European Pulsar Timing Array data

Author: van Haasteren, R., Levin, Y., Janssen, G. H., Lazaridis, K., Kramer, M., Stappers, B. W., Desvignes, G., Purver, M. B., Lyne, A. G., Ferdman, R. D., Jessner, A., Cognard, I., Theureau, G., D'Amico, N., Possenti, A., Burgay, M., Corongiu, A., Hessels, J. W. T., Smits, R., Verbiest, Joris, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], Max-Planck-Institut für Radioastronomie (MPIFR), Netherlands Institute for Radio Astronomy (ASTRON), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), 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 Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Laboratoire Univers et Théories (LUTH (UMR_8102)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), INAF - Osservatorio Astronomico di Cagliari (OAC), Istituto Nazionale di Astrofisica (INAF), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: gravitational waves, 010308 nuclear & particles physics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, 010303 astronomy & astrophysics, 01 natural sciences, addenda, methods: data analysis, pulsars: general, errata
Abstract: International audience; The paper ‘Placing limits on the stochastic gravitational-wave background using European Pulsar Timing Array data’ was published in Mon. Not. R. Astron. Soc. 414, 3117–3128 (2011).
Published: 2012

20. Suzaku X-ray Follow-up Observations of Seven Unassociated Fermi-LAT Gamma-ray Sources at High Galactic Latitudes

Author: Cheung, C. C., Stawarz, Lukasz, Guillemot, L., Freire, P. C. C., Cognard, I., Takahashi, Yosuke, Kataoka, Jun, Nakamori, T., Maeda, K., Makiya, R., Totani, T., Research Institute for Science and Engineering, Waseda University, Kyoto University [Kyoto], Naval Research Laboratory (NRL), Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Uniwersytet Jagielloński w Krakowie = Jagiellonian University (UJ), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Departamento de Física [Fortaleza], Universidade Federal do Ceará = Federal University of Ceará (UFC), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-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)-Université d'Orléans (UO), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), and 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)
Subjects: 010504 meteorology & atmospheric sciences, Point source, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, pulsars: individual (PSR J2302+4442), 01 natural sciences, general [pulsars], Pulsar, Millisecond pulsar, Observatory, general [X-rays], pulsars: general, 0103 physical sciences, X-rays, Blazar, 010303 astronomy & astrophysics, galaxies: activ, 0105 earth and related environmental sciences, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), [PHYS]Physics [physics], Gamma ray, Astronomy and Astrophysics, gamma rays: general, Neutron star, individual (PSR J2302+4442) [pulsars], Space and Planetary Science, [SDU]Sciences of the Universe [physics], active [galaxies], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [gamma rays], Fermi Gamma-ray Space Telescope
Abstract: 著者人数: 11名, Accepted: 2011-12-20, 資料番号: SA1003026000
Published: 2012

21. Discovery of the millisecond pulsar PSR J2043+1711 in a Fermi source with the Nanc¸ay Radio Telescope

Author: Guillemot, L., Freire, P. C. C., Cognard, I., Johnson, T. J., Takahashi, Y., Kataoka, J., Desvignes, G., Camilo, F., Ferrara, E. C., Harding, A. K., Janssen, G. H., Keith, M., Kerr, M., Kramer, M., Parent, D., Ransom, S. M., Ray, P. S., Parkinson, P. M. Saz, Smith, D. A., Stappers, B. W., Theureau, G., Max-Planck-Institut für Radioastronomie (MPIFR), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-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)-Université d'Orléans (UO), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), 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), National Research Council Associate, Research Institute for Science and Engineering, Waseda University, Columbia Astrophysics Laboratory (CAL), Columbia University [New York], NASA Goddard Space Flight Center (GSFC), Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], CSIRO Astronomy and Space Science, Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), W. W. Hansen Experimental Physics Laboratory (HEPL), Stanford University, Center for Earth Observing and Space Research [Fairfax] (CEOSR), George Mason University [Fairfax], National Radio Astronomy Observatory (NRAO), Santa Cruz Institute for Particle Physics, GLAST, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), and Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS]Physics [physics], High Energy Astrophysical Phenomena (astro-ph.HE), [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], gamma-rays: general, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, pulsars: individual: PSR J2043+1711, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, [SDU]Sciences of the Universe [physics], pulsars: general, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract: We report the discovery of the millisecond pulsar PSR J2043+1711 in a search of a Fermi Large Area Telescope (LAT) source with no known associations, with the Nancay Radio Telescope. The new pulsar, confirmed with the Green Bank Telescope, has a spin period of 2.38 ms, is relatively nearby (d, Comment: 14 pages, 6 figures, 3 tables, accepted for publication in MNRAS
Published: 2012

22. Fermi-LAT Search for Pulsar Wind Nebulae around gamma-ray Pulsars

Author: Ackermann, M., Ajello, M., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Bloom, E. D., Bonamente, E., Borgland, A. W., Bouvier, A., Bregeon, J., Brez, A., Brigida, M., Bruel, P., Buehler, R., Buson, S., Caliandro, G. A., Cameron, R. A., Camilo, F., Caraveo, P. A., Casandjian, J. M., Cecchi, C., Celik, O., Charles, E., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cognard, I., Cohen-Tanugi, J., Conrad, J., Dermer, C. D., de, Angelis A., de, Luca A., de, Palma F., Digel, S. W., do, Couto e Silva E., Drell, P. S., Dubois, R., Dumora, D., Favuzzi, C., Focke, W. B., Frailis, M., Funk, S., Fusco, P., Gargano, F., Germani, S., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Grenier, I. A., Grondin, M.-H., Grove, J. E., Guillemot, L., Guiriec, S., Hadasch, D., Harding, A. K., Hayashi, K., Hays, E., Hobbs, G., Hughes, R. E., Johannesson, G., Johnson, A. S., Johnson, W. N., Johnston, S., Keith, M., Kerr, M., Knodlseder, J., Kramer, M., Kuss, M., Lande, J., Latronico, L., Lee, S.-H., Lemoine-Goumard, M., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Lyne, A. G., Makeev, A., Marelli, M., Mazziotta, M. N., McEnery, J. E., Mehault, J., Michelson, P. F., Moiseev, A. A., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nakamori, T., Naumann-Godo, M., Nolan, P. L., Noutsos, A., Nuss, E., Ormes, J. F., Paneque, D., Panetta, J. H., Parent, D., Pelassa, V., Pepe, M., Pesce-Rollins, M., Piron, F., Porter, T. A., Raino, S., Rando, R., Ransom, S. M., Ray, P. S., Razzano, M., Rea, N., Reimer, A., Reimer, O., Reposeur, T., Ripken, J., Ritz, S., Romani, R. W., Sadrozinski, H. F.-W., Sander, A., Saz, Parkinson P. M., Sgro, C., Siskind, E. J., Smith, D. A., Smith, P. D., Spandre, G., Spinelli, P., Strickman, M. S., Suson, D. J., Fukazawa, Y., Hanabata, Y., Kamae, T., Katagiri, H., Kataoka, J., Mizuno, T., Ohsugi, T., Okumura, Akira, Takahashi, H., Takahashi, Tadayuki, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique et chimie de l'environnement (LPCE), Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), 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 Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), 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), Fermi-LAT, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université d'Orléans (UO)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, M., Ackermann, M., Ajello, L., Baldini, J., Ballet, G., Barbiellini, D., Bastieri, K., Bechtol, R., Bellazzini, B., Berenji, E. D., Bloom, E., Bonamente, A. W., Borgland, A., Bouvier, J., Bregeon, A., Brez, M., Brigida, P., Bruel, R., Buehler, S., Buson, G. A., Caliandro, R. A., Cameron, F., Camilo, P. A., Caraveo, J. M., Casandjian, C., Cecchi, Celik, ., E., Charle, A., Chekhtman, C. C., Cheung, J., Chiang, S., Ciprini, R., Clau, I., Cognard, J., Cohen Tanugi, J., Conrad, C. D., Dermer, Angelis, A., Luca, A., Palma, F., S. W., Digel, E. d., C., P. S., Drell, R., Duboi, D., Dumora, C., Favuzzi, W. B., Focke, M., Fraili, Y., Fukazawa, S., Funk, P., Fusco, F., Gargano, S., Germani, N., Giglietto, P., Giommi, F., Giordano, M., Giroletti, T., Glanzman, G., Godfrey, I. A., Grenier, M., Grondin, J. E., Grove, L., Guillemot, S., Guiriec, D., Hadasch, Y., Hanabata, A. K., Harding, K., Hayashi, E., Hay, G., Hobb, R. E., Hughe, G., Johannesson, A. S., Johnson, W. N., Johnson, S., Johnston, T., Kamae, H., Katagiri, J., Kataoka, M., Keith, M., Kerr, J., Kn\odlseder, M., Kramer, M., Ku, J., Lande, L., Latronico, S., Lee, M., Lemoine Goumard, Longo, Francesco, F., Loparco, M. N., Lovellette, P., Lubrano, A. G., Lyne, A., Makeev, M., Marelli, M. N., Mazziotta, J. E., Mcenery, J., Mehault, P. F., Michelson, T., Mizuno, A. A., Moiseev, C., Monte, M. E., Monzani, A., Morselli, I. V., Moskalenko, S., Murgia, T., Nakamori, M., Naumann Godo, P. L., Nolan, A., Noutso, E., Nu, T., Ohsugi, A., Okumura, J. F., Orme, D., Paneque, J. H., Panetta, D., Parent, V., Pelassa, M., Pepe, M., Pesce Rollin, F., Piron, T. A., Porter, S., Rain\`o, R., Rando, S. M., Ransom, P. S., Ray, M., Razzano, N., Rea, A., Reimer, O., Reimer, T., Reposeur, J., Ripken, S., Ritz, R. W., Romani, H. F., Sadrozinski, A., Sander, P. M., Saz, C., Sgr\`o, E. J., Siskind, D. A., Smith, P. D., Smith, G., Spandre, P., Spinelli, M. S., Strickman, D. J., Suson, H., Takahashi, T., Takahashi, T., Tanaka, J. B., Thayer, J. G., Thayer, G., Theureau, D. J., Thompson, S. E., Thorsett, L., Tibaldo, D. F., Torre, G., Tosti, A., Tramacere, Y., Uchiyama, T., Uehara, T. L., Usher, J., Vandenbroucke, Etten, A., V., Vasileiou, N., Vilchez, V., Vitale, A. P., Waite, P., Wang, P., Weltevrede, B. L., Winer, K. S., Wood, Z., Yang, T., Ylinen, and M., Ziegler
Subjects: catalog, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, general [pulsars], 01 natural sciences, Pulsar wind nebula, Binary pulsar, Astronomi, astrofysik och kosmologi, Pulsar, Millisecond pulsar, pulsars: general, catalogs, gamma rays: general, 0103 physical sciences, Astronomy, Astrophysics and Cosmology, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, 97.60.Gb, 98.58.Mj, 98.58,.Hf, 95.55.Ka, 98.70.Rz, 97.10.Ex, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astronomy, Astronomy and Astrophysics, Crab Nebula, Space and Planetary Science, Spectral energy distribution, Astrophysics - High Energy Astrophysical Phenomena, general [gamma rays], X-ray pulsar, Fermi Gamma-ray Space Telescope
Abstract: 著者人数：171名, Accepted: 2010-10-28, 資料番号: SA1002649000
Published: 2011

23. The discovery of two mildly recycled binary pulsars in the Northern High Time Resolution Universe pulsar survey.

Author: Berezina, M., Champion, D. J., Freire, P. C. C., Tauris, T. M., Kramer, M., Lyne, A. G., Stappers, B. W., Guillemot, L., Cognard, I., Barr, E. D., Eatough, R. P., Karuppusamy, R., Spitler, L. G., and Desvignes, G.
Subjects: WHITE dwarf stars, PULSAR detection, AMPLITUDE estimation, GENERAL relativity (Physics), BLACK holes
Abstract: We report the discovery and the results of follow-up timing observations of PSR J2045+3633 and PSR J2053+4650, two binary pulsars found in the Northern High Time Resolution Universe pulsar survey being carried out with the Effelsberg radio telescope. Having spin periods of 31.7 and 12.6 ms, respectively, and both with massive white dwarf companions,Mc >0.8M☉, the pulsars can be classified as mildly recycled. PSR J2045+3633 is remarkable due to its orbital period (32.3 d) and eccentricity e=0.017 212 44(5), which is amongst the largest ever measured for this class. After almost two years of timing, the large eccentricity has allowed the measurement of the rate of advance of periastron at the 5σ level, 0.0010(2)°yr-1. Combining this with a detection of the orthometric amplitude of the Shapiro delay, we obtained the following constraints on the component masses (within general relativity):Mp = 1.33-0.28+0.30M☉; andMc = 0.94-0.13+0.14M☉. PSR J2053+4650 has a 2.45 d circular orbit inclined to the plane of the sky at an angle i = 85.0-0.9+0.8 deg. In this nearly edge-on case the masses can be obtained from the Shapiro delay alone. Our timing observations resulted in a significant detection of this effect giving: Mp = 1.40-0.18+0.21M☉; and Mc = 0.86-0.6+0.07M☉. [ABSTRACT FROM AUTHOR]
Published: 2017
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24. Detection of the magnetar SGR J1745-2900 up to 291GHz with evidence of polarized millimetre emission.

Author: Torne, P., Desvignes, G., Eatough, R. P., Karuppusamy, R., Paubert, G., Kramer, M., Cognard, I., Champion, D. J., and Spitler, L. G.
Subjects: MAGNETARS, MILLIMETER astronomy, PULSAR detection, POLARIZATION (Nuclear physics), GALACTIC center
Abstract: In 2015, Torne et al. reported detections of the magnetar SGR J1745-2900 up to 225 GHz (1.33 mm), which was the highest radio frequency detection of pulsar emission at that time. In this work, we present the results of new observations of the same magnetar with detections up to 291GHz (1.03mm), together with evidence of linear polarization in its millimetre emission. SGR J1745-2900 continues to show variability and is, on average, a factor ~4 brighter in the millimetre band than in our observations of 2014 July. The new measured spectrum is slightly inverted, with (α) = +0.4 ± 0.2 (for Sv ∝ vα). However, the spectrum does not seem to be well described by a single power law, which might be due to the intrinsic variability of the source, or perhaps a turn-up somewhere between 8.35 and 87GHz. These results may help us to improve our still incomplete model of pulsar emission and, in addition, they further support the search for and study of pulsars located at the Galactic Centre using millimetre wavelengths. [ABSTRACT FROM AUTHOR]
Published: 2017
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25. GRAVITATIONAL WAVES FROM KNOWN PULSARS: RESULTS FROM THE INITIAL DETECTOR ERA

Author: Aasi, J., Abadie, J., Abbott, B. P., Abbott, R., Abbott, T., Abernathy, M. R., Accadia, T., Acernese, F., Adams, C., Adams, T., Adhikari, R. X., Affeldt, C., Agathos, M., Aggarwal, N., Aguiar, O. D., Ajith, P., Allen, B., Allocca, A., Amador Ceron, E., Amariutei, D., Anderson, R. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C., Areeda, J., Ast, S., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Austin, L., Aylott, B. E., Babak, S., Baker, P. T., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barker, D., Barnum, S. H., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barton, M. A., Bartos, I., Bassiri, R., Basti, A., Batch, J., Bauchrowitz, J., Bauer, Th S., Bebronne, M., Behnke, B., Bejger, M., Beker, M. G., Bell, A. S., Bell, C., Belopolski, I., Bergmann, G., Berliner, J. M., Bersanetti, D., Bertolini, A., Bessis, D., Betzwieser, J., Beyersdorf, P. T., Bhadbhade, T., Bilenko, I. A., Billingsley, G., Birch, J., Bitossi, M., Bizouard, M. A., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Blom, M., Bock, O., Bodiya, T. P., Boer, M., Bogan, C., Bond, C., Bondu, F., Bonelli, L., Bonnand, R., Bork, R., Born, M., Boschi, V., Bose, S., Bosi, L., Bowers, J., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brannen, C. A., Brau, J. E., Breyer, J., Briant, T., Bridges, D. O., Brillet, A., Brinkmann, M., Brisson, V., Britzger, M., Brooks, A. F., Brown, D. A., Brown, D. D., Brueckner, F., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Calderon Bustillo, J., Calloni, E., Camp, J. B., Campsie, P., Cannon, K. C., Canuel, B., Cao, J., Capano, C. D., Carbognani, F., Carbone, L., Caride, S., Castiglia, A., Caudill, S., Cavaglia, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chao, S., Charlton, P., Chassande Mottin, E., Chen, X., Chen, Y., Chincarini, A., Chiummo, A., Cho, H. S., Chow, J., Christensen, N., Chu, Q., Chua, S. S. Y., Chung, S., Ciani, G., Clara, F., Clark, D. E., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. F., Colla, A., Colombini, M., Constancio Jr, M., Conte, Andrea, Conte, R., Cook, D., Corbitt, T. R., Cordier, M., Cornish, N., Corsi, A., Costa, C. A., Coughlin, M. W., Coulon, J. P., Countryman, S., Couvares, P., Coward, D. M., Cowart, M., Coyne, D. C., Craig, K., Creighton, J. D. E., Creighton, T. D., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Dahl, K., Dal Canton, T., Damjanic, M., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dattilo, V., Daudert, B., Daveloza, H., Davier, M., Davies, G. S., Daw, E. J., Day, R., Dayanga, T., De Rosa, R., Debreczeni, G., Degallaix, J., Del Pozzo, W., Deleeuw, E., Deleglise, S., Denker, T., Dent, T., Dereli, H., Dergachev, V., Derosa, R., Desalvo, R., Dhurandhar, S., Di Fiore, L., Di Lieto, A., Di Palma, I., Di Virgilio, A., Diaz, M., Dietz, A., Dmitry, K., Donovan, F., Dooley, K. L., Doravari, S., Drago, M., Drever, R. W. P., Driggers, J. C., Du, Z., Dumas, J. C., Dwyer, S., Eberle, T., Edwards, M., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S. S., Endroczi, G., Essick, R., Etzel, T., Evans, K., Evans, M., Evans, T., Factourovich, M., Fafone, V., Fairhurst, S., Fang, Q., Farinon, S., Farr, B., Farr, W., Favata, M., Fazi, D., Fehrmann, H., Feldbaum, D., Ferrante, I., Ferrini, F., Fidecaro, F., Finn, L. S., Fiori, I., Fisher, R., Flaminio, R., Foley, E., Foley, S., Forsi, E., Fotopoulos, N., Fournier, J. D., Franco, S., Frasca, Sergio, Frasconi, F., Frede, M., Frei, M., Frei, Z., Freise, A., Frey, R., Fricke, T. T., Fritschel, P., Frolov, V. V., Fujimoto, M. K., Fulda, P., Fyffe, M., Gair, J., Gammaitoni, L., Garcia, J., Garufi, F., Gehrels, N., Gemme, G., Genin, E., Gennai, A., Gergely, L., Ghosh, S., Giaime, J. A., Giampanis, S., Giardina, K. D., Giazotto, A., Gil Casanova, S., Gill, C., Gleason, J., Goetz, E., Goetz, R., Gondan, L., Gonzalez, G., Gordon, N., Gorodetsky, M. L., Gossan, S., Gossler, S., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greenhalgh, R. J. S., Gretarsson, A. M., Griffo, C., Groot, P., Grote, H., Grover, K., Grunewald, S., Guidi, G. M., Guido, C., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Hall, B., Hall, E., Hammer, D., Hammond, G., Hanke, M., Hanks, J., Hanna, C., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Hartman, M. T., Haughian, K., Hayama, K., Heefner, J., Heidmann, A., Heintze, M., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Heptonstall, A. W., Heurs, M., Hild, S., Hoak, D., Hodge, K. A., Holt, K., Holtrop, M., Hong, T., Hooper, S., Horrom, T., Hosken, D. J., Hough, J., Howell, E. J., Hu, Y., Hua, Z., Huang, V., Huerta, E. A., Hughey, B., Husa, S., Huttner, S. H., Huynh, M., Huynh Dinh, T., Iafrate, J., Ingram, D. R., Inta, R., Isogai, T., Ivanov, A., Iyer, B. R., Izumi, K., Jacobson, M., James, E., Jang, H., Jang, Y. J., Jaranowski, P., Jimenez Forteza, F., Johnson, W. W., Jones, D., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Haris, K., Kalmus, P., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Kasprzack, M., Kasturi, R., Katsavounidis, E., Katzman, W., Kaufer, H., Kaufman, K., Kawabe, K., Kawamura, S., Kawazoe, F., Kefelian, F., Keitel, D., Kelley, D. B., Kells, W., Keppel, D. G., Khalaidovski, A., Khalili, F. Y., Khazanov, E. A., Kim, B. K., Kim, C., Kim, K., Kim, N., Kim, W., Kim, Y. M., King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Klimenko, S., Kline, J., Koehlenbeck, S., Kokeyama, K., Kondrashov, V., Koranda, S., Korth, W. Z., Kowalska, I., Kozak, D., Kremin, A., Kringel, V., Krishnan, B., Krolak, A., Kucharczyk, C., Kudla, S., Kuehn, G., Kumar, A., Kumar, P., Kumar, R., Kurdyumov, R., Kwee, P., Landry, M., Lantz, B., Larson, S., Lasky, P. D., Lawrie, C., Lazzarini, A., Le Roux, A., Leaci, P., Lebigot, E. O., Lee, C. H., Lee, H. K., Lee, H. M., Lee, J., Leonardi, M., Leong, J. R., Leroy, N., Letendre, N., Levine, B., Lewis, J. B., Lhuillier, V., T. G. F., Li, Lin, A. C., Littenberg, T. B., Litvine, V., Liu, F., Liu, H., Liu, Y., Liu, Z., Lloyd, D., Lockerbie, N. A., Lockett, V., Lodhia, D., Loew, K., Logue, J., Lombardi, A. L., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J., Luan, J., Lubinski, M. J., Lueck, H., Lundgren, A. P., Macarthur, J., Macdonald, E., Machenschalk, B., Macinnis, M., Macleod, D. M., Magana Sandoval, F., Mageswaran, M., Mailand, K., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Manca, G. M., Mandel, I., Mandic, V., Mangano, V., Mantovani, M., Marchesoni, F., Marion, F., Marka, S., Marka, Z., Markosyan, A., Maros, E., Marque, J., Martelli, F., Martin, I. W., Martin, R. M., Martinelli, L., Martynov, D., Marx, J. N., Mason, K., Masserot, A., Massinger, T. J., Matichard, F., Matone, L., Matzner, R. A., Mavalvala, N., May, G., Mazumder, N., Mazzolo, G., Mccarthy, R., Mcclelland, D. E., Mcguire, S. C., Mcintyre, G., Mciver, J., Meacher, D., Meadors, G. D., Mehmet, M., Meidam, J., Meier, T., Melatos, A., Mendell, G., Mercer, R. A., Meshkov, S., Messenger, C., Meyer, M. S., Miao, H., Michel, C., Mikhailov, E. E., Milano, L., Miller, J., Minenkov, Y., Mingarelli, C. M. F., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moe, B., Mohan, M., Mohapatra, S. R. P., Mokler, F., Moraru, D., Moreno, G., Morgado, N., Mori, T., Morriss, S. R., Mossavi, K., Mours, B., Mow Lowry, C. M., Mueller, C. L., Mueller, G., Mukherjee, S., Mullavey, A., Munch, J., Murphy, D., Murray, P. G., Mytidis, A., Nagy, M. F., Nanda Kumar, D., Nardecchia, I., Nash, T., Naticchioni, Luca, Nayak, R., Necula, V., Nelemans, G., Neri, I., Neri, M., Newton, G., Nguyen, T., Nishida, E., Nishizawa, A., Nitz, A., Nocera, F., Nolting, D., Normandin, M. E., Nuttall, L. K., Ochsner, E., O'Dell, J., Oelker, E., Ogin, G. H., J. J., Oh, S. H., Oh, Ohme, F., Oppermann, P., O'Reilly, B., Ortega Larcher, W., O'Shaughnessy, R., Osthelder, C., Ottaway, D. J., Ottens, R. S., Ou, J., Overmier, H., Owen, B. J., Padilla, C., Pai, A., Palomba, C., Pan, Y., Pankow, C., Paoletti, F., Paoletti, R., Papa, M. A., Paris, H., Pasqualetti, A., Passaquieti, R., Passuello, D., Pedraza, M., Peiris, P., Penn, S., Perreca, A., Phelps, M., Pichot, M., Pickenpack, M., Piergiovanni, F., Pierro, V., Pinard, L., Pindor, B., Pinto, I. M., Pitkin, M., Poeld, J., Poggiani, R., Poole, V., Poux, C., Predoi, V., Prestegard, T., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prix, R., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Quetschke, V., Quintero, E., Quitzow James, R., Raab, F. J., Rabeling, D. S., Acz, I. R., Radkins, H., Raffai, P., Raja, S., Rajalakshmi, G., Rakhmanov, M., Ramet, C., Rapagnani, Piero, Raymond, V., Re, V., Reed, C. M., Reed, T., Regimbau, T., Reid, S., Reitze, D. H., Ricci, Fulvio, Riesen, R., Riles, K., Robertson, N. A., Robinet, F., Rocchi, A., Roddy, S., Rodriguez, C., Rodruck, M., Roever, C., Rolland, L., Rollins, J. G., Romano, J. D., Romano, R., Romanov, G., Romie, J. H., Rosinska, D., Rowan, S., Ruediger, A., Ruggi, P., Ryan, K., Salemi, F., Sammut, L., Sandberg, V., Sanders, J., Sannibale, V., Santiago Prieto, I., Saracco, E., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Savage, R., Schilling, R., Schnabel, R., Schofield, R. M. S., Schreiber, E., Schuette, D., Schulz, B., Schutz, B. F., Schwinberg, P., Scott, J., Scott, S. M., Seifert, F., Sellers, D., Sengupta, A. S., Sentenac, D., Sergeev, A., Shaddock, D., Shah, S., Shahriar, M. S., Shaltev, M., Shapiro, B., Shawhan, P., Shoemaker, D. H., Sidery, T. L., Siellez, K., Siemens, X., Sigg, D., Simakov, D., Singer, A., Singer, L., Sintes, A. M., Skelton, G. R., Slagmolen, B. J. J., Slutsky, J., Smith, J. R., Smith, M. R., Smith, R. J. E., Smith Lefebvre, N. D., Soden, K., Son, E. J., Sorazu, B., Souradeep, T., Sperandio, L., Staley, A., Steinert, E., Steinlechner, J., Steinlechner, S., Steplewski, S., Stevens, D., Stochino, A., Stone, R., Strain, K. A., Straniero, N., Strigin, S., Stroeer, A. S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Susmithan, S., Sutton, P. J., Swinkels, B., Szeifert, G., Tacca, M., Talukder, D., Tang, L., Tanner, D. B., Tarabrin, S. P., Taylor, R., Ter Braack, A. P. M., Thirugnanasambandam, M. P., Thomas, M., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Tiwari, V., Tokmakov, K. V., Tomlinson, C., Toncelli, A., Tonelli, M., Torre, O., Torres, C. V., Torrie, C. I., Travasso, F., Traylor, G., Tse, M., Ugolini, D., Unnikrishnan, C. S., Vahlbruch, H., Vajente, G., Vallisneri, M., Van den Brand, J. F. J., Van den Broeck, C., Van der Putten, S., Van der Sluys, M. V., Van Heijningen, J., Van Veggel, A. A., Vass, S., Vasuth, M., Vaulin, R., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Verkindt, D., Verma, S., Vetrano, F., Vicere, A., Vincent Finley, R., Vinet, J. Y., Vitale, S., Vlcek, B., Vo, T., Vocca, H., Vorvick, C., Vousden, W. D., Vrinceanu, D., Vyachanin, S. P., Wade, A., Wade, L., Wade, M., Waldman, S. J., Walker, M., Wallace, L., Wan, Y., Wang, J., Wang, M., Wang, X., Wanner, A., Ward, R. L., Was, M., Weaver, B., Wei, L. W., Weinert, M., Weinstein, A. J., Weiss, R., Welborn, T., Wen, L., Wessels, P., West, M., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., White, D. J., Whiting, B. F., Wibowo, S., Wiesner, K., Wilkinson, C., Williams, L., Williams, R., Williams, T., Willis, J. L., Willke, B., Wimmer, M., Winkelmann, L., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Worden, J., Yablon, J., Yakushin, I., Yamamoto, H., Yancey, C. C., Yang, H., Yeaton Massey, D., Yoshida, S., Yum, H., Yvert, M., Zadrozny, A., Zanolin, M., Zendri, J. P., Zhang, F., Zhang, L., Zhao, C., Zhu, H., Zhu, X. J., Zotov, N., Zucker, M. E., Zweizig, J., Ligo Sci Collaboration, Virgo, Collaboration, Buchner, S., Cognard, I., Corongiu, A., D'Amico, N., Espinoza, C. M., Freire, P. C. C., Gotthelf, E. V., Guillemot, L., Hessels, J. W. T., Hobbs, G. B., Kramer, M., Lyne, A. G., Marshall, F. E., Possenti, A., Ransom, S. M., Ray, P. S., Roy, J., Stappers, B. W., 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 - 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 ), 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 ), 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 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 ), 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 ), APC - Gravitation ( APC-Gravitation ), 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, Observatoire de la Côte d'Azur ( OCA ), Centre National de la Recherche Scientifique ( CNRS ), ESPCI ParisTech, Unité Scientifique de la Station de Nançay ( USN ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace ( LPC2E ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), High Energy Astrophys. & Astropart. Phys (API, FNWI), 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), 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)-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), 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), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), 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), APC - Gravitation (APC-Gravitation), 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), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL), 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), (Astro)-Particles Physics, 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), 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 de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-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)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, 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), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), LVC Collaboration, The, Pierro, V., Pinto, I. M., Principe, M., The LIGO Scientific Collaboration, The Virgo Collaboration, Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), 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), 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), 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), Centre National de la Recherche Scientifique (CNRS), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), and PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES)
Subjects: PROPER MOTION, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], NEUTRON-STARS, Astronomy, CRAB PULSAR, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), DEFORMATIONS, Vela, General Relativity and Quantum Cosmology, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Settore FIS/05 - Astronomia e Astrofisica, SPIN-DOWN LIMIT, X-RAY PULSAR, Pulsar, Observatory, Millisecond pulsar, pulsars: general, GLOBULAR-CLUSTERS, SEARCH, QC, Pulsars, QB, High Energy Astrophysical Phenomena (astro-ph.HE), Gravitation, Gravitational waves, Physics, Gravitational wave, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Settore FIS/01 - Fisica Sperimentale, Astrophysics::Instrumentation and Methods for Astrophysics, [ PHYS.ASTR.HE ] Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astronomy and Astrophysics, gravitational waves, Space and Planetary Science, BINARY, GEO600, LIGO, Amplitude, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [ SDU.ASTR.HE ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics - High Energy Astrophysical Phenomena, EMISSION
Abstract: We present the results of searches for gravitational waves from a large selection of pulsars using data from the most recent science runs (S6, VSR2 and VSR4) of the initial generation of interferometric gravitational wave detectors LIGO (Laser Interferometric Gravitational-wave Observatory) and Virgo. We do not see evidence for gravitational wave emission from any of the targeted sources but produce upper limits on the emission amplitude. We highlight the results from seven young pulsars with large spin-down luminosities. We reach within a factor of five of the canonical spin-down limit for all seven of these, whilst for the Crab and Vela pulsars we further surpass their spin-down limits. We present new or updated limits for 172 other pulsars (including both young and millisecond pulsars). Now that the detectors are undergoing major upgrades, and, for completeness, we bring together all of the most up-to-date results from all pulsars searched for during the operations of the first-generation LIGO, Virgo and GEO600 detectors. This gives a total of 195 pulsars including the most recent results described in this paper., Comment: Version accepted by The Astrophysical Journal. Science summary of results available at http://www.ligo.org/science/Publication-S6VSR24KnownPulsar/
Published: 2014

26. 21 year timing of the black-widow pulsar J2051-0827.

Author: Shaifullah, G., Verbiest, J. P. W., Freire, P. C. C., Tauris, T. M., Wex, N., Osłowski, S., Stappers, B. W., Bassa, C. G., Caballero, R. N., Champion, D. J., Cognard, I., Desvignes, G., Graikou, E., Guillemot, L., Janssen, G. H., Jessner, A., Jordan, C., Karuppusamy, R., Kramer, M., and Lazaridis, K.
Subjects: GEOMAGNETIC secular variation, PULSARS, RADIO telescopes, BINARY stars, ECLIPSING binaries
Abstract: Timing results for the black-widow pulsar J2051-0827 are presented, using a 21 year data set from four European Pulsar Timing Array telescopes and the Parkes radio telescope. This data set, which is the longest published to date for a black-widow system, allows for an improved analysis that addresses previously unknown biases. While secular variations, as identified in previous analyses, are recovered, short-term variations are detected for the first time. Concurrently, a significant decrease of ~2.5 × 10-3 cm-3 pc in the dispersion measure associated with PSR J2051-0827 is measured for the first time and improvements are also made to estimates of the proper motion. Finally, PSR J2051-0827 is shown to have entered a relatively stable state suggesting the possibility of its eventual inclusion in pulsar timing arrays. [ABSTRACT FROM AUTHOR]
Published: 2016
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27. A glitch in the millisecond pulsar J0613-0200.

Author: McKee, J. W., Janssen, G. H., Stappers, B. W., Lyne, A. G., Caballero, R. N., Lentati, L., Desvignes, G., Jessner, A., Jordan, C. A., Karuppusamy, R., Kramer, M., Cognard, I., Champion, D. J., Graikou, E., Lazarus, P., Osłowski, S., Perrodin, D., Shaifullah, G., Tiburzi, C., and Verbiest, J. P. W.
Subjects: PULSAR detection, VERY large array telescopes, ANTENNA arrays, RADIO telescopes
Abstract: We present evidence for a small glitch in the spin evolution of the millisecond pulsar J0613-0200, using the EPTA Data Release 1.0, combined with Jodrell Bank analogue filterbank times of arrival (TOAs) recorded with the Lovell telescope and Effelsberg Pulsar Observing System TOAs. A spin frequency step of 0.82(3) nHz and frequency derivative step of -1.6(39) × 10-19 Hz s-1 are measured at the epoch of MJD 50888(30). After PSR B1821-24A, this is only the second glitch ever observed in a millisecond pulsar, with a fractional size in frequency of Δv/v = 2.5(1) × 10-12, which is several times smaller than the previous smallest glitch. PSR J0613-0200 is used in gravitational wave searches with pulsar timing arrays, and is to date only the second such pulsar to have experienced a glitch in a combined 886 pulsar-years of observations. We find that accurately modelling the glitch does not impact the timing precision for pulsar timing array applications. We estimate that for the current set of millisecond pulsars included in the International Pulsar Timing Array, there is a probability of ~50 per cent that another glitch will be observed in a timing array pulsar within 10 years. [ABSTRACT FROM AUTHOR]
Published: 2016
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28. The noise properties of 42 millisecond pulsars from the European Pulsar Timing Array and their impact on gravitational-wave searches.

Author: Caballero, R. N., Lee, K. J., Lentati, L., Desvignes, G., Champion, D. J., Verbiest, J. P. W., Janssen, G. H., Stappers, B. W., Kramer, M., Lazarus, P., Possenti, A., Tiburzi, C., Perrodin, D., Osłowski, S., Babak, S., Bassa, C. G., Brem, P., Burgay, M., Cognard, I., and Gair, J. R.
Subjects: PULSARS, GRAVITATIONAL wave astronomy, SCATTERING (Physics), NOISE, TELESCOPES
Abstract: The sensitivity of Pulsar Timing Arrays to gravitational waves (GWs) depends on the noise present in the individual pulsar timing data. Noise may be either intrinsic or extrinsic to the pulsar. Intrinsic sources of noise will include rotational instabilities, for example. Extrinsic sources of noise include contributions from physical processes which are not sufficiently well modelled, for example, dispersion and scattering effects, analysis errors and instrumental instabilities. We present the results from a noise analysis for 42 millisecond pulsars (MSPs) observed with the European Pulsar Timing Array. For characterizing the low-frequency, stochastic and achromatic noise component, or 'timing noise', we employ two methods, based on Bayesian and frequentist statistics. For 25 MSPs, we achieve statistically significant measurements of their timing noise parameters and find that the two methods give consistent results. For the remaining 17 MSPs, we place upper limits on the timing noise amplitude at the 95 per cent confidence level. We additionally place an upper limit on the contribution to the pulsar noise budget from errors in the reference terrestrial time standards (below 1 per cent), and we find evidence for a noise component which is present only in the data of one of the four used telescopes. Finally, we estimate that the timing noise of individual pulsars reduces the sensitivity of this data set to an isotropic, stochastic GW background by a factor of >9.1 and by a factor of >2.3 for continuous GWs from resolvable, inspiralling supermassive black hole binaries with circular orbits. [ABSTRACT FROM AUTHOR]
Published: 2016
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29. Cool white dwarf companions to four millisecond pulsars.

Author: Bassa, C. G., Antoniadis, J., Camilo, F., Cognard, I., Koester, D., Kramer, M., Ransom, S. R., and Stappers, B. W.
Subjects: SUPERNOVA remnants, NEUTRON stars, DWARF galaxies, RADIATION sources, LUMINESCENCE
Abstract: We report on photometric and spectroscopic observations of white dwarf companions to four binary radio millisecond pulsars, leading to the discovery of companions to PSRs J0614--3329, J1231--1411 and J2017+0603. We place limits on the brightness of the companion to PSR J0613--0200. Optical spectroscopy of the companion to PSR J0614--3329 identifies it as a DA-type white dwarf with a temperature of Teff = 6460 ± 80 K, a surface gravity log g = 7.0 ± 0.2 cgs and a mass of MWD = 0.24 ± 0.04 M☉. We find that the distance to PSR J0614--3329 is smaller than previously estimated, removing the need for the pulsar to have an unrealistically high γ -ray efficiency. Comparing the photometry with predictions from white dwarf cooling models allows us to estimate temperatures and cooling ages of the companions to PSRs J0613--0200, J1231--1411 and J2017+0603. We find that the white dwarfs in these systems are cool Teff < 4000 K and old ≳5 Gyr. Thin hydrogen envelopes are required for these white dwarfs to cool to the observed temperatures, and we suggest that besides hydrogen shell flashes, irradiation driven mass loss by the pulsar may have been important. [ABSTRACT FROM AUTHOR]
Published: 2016
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30. European Pulsar Timing Array limits on continuous gravitational waves from individual supermassive black hole binaries.

Author: Babak, S., Petiteau, A., Sesana, A., Brem, P., Rosado, P. A., Taylor, S. R., Lassus, A., Hessels, J. W. T., Bassa, C. G., Burgay, M., Caballero, R. N., Champion, D. J., Cognard, I., Desvignes, G., Gair, J. R., Guillemot, L., Janssen, G. H., Karuppusamy, R., Kramer, M., and Lazarus, P.
Subjects: GRAVITATIONAL waves, SUPERMASSIVE black holes, BINARY stars, SIGNAL processing, ALGORITHMS, PULSARS
Abstract: We have searched for continuous gravitational wave (CGW) signals produced by individually resolvable, circular supermassive black hole binaries (SMBHBs) in the latest European Pulsar Timing Array (EPTA) data set, which consists of ultraprecise timing data on 41-ms pulsars. We develop frequentist and Bayesian detection algorithms to search both for monochromatic and frequency-evolving systems. None of the adopted algorithms show evidence for the presence of such a CGW signal, indicating that the data are best described by pulsar and radiometer noise only. Depending on the adopted detection algorithm, the 95 per cent upper limit on the sky-averaged strain amplitude lies in the range 6 × 10-15 < A < 1.5 × 10-14 at 5 nHz < f < 7 nHz. This limit varies by a factor of five, depending on the assumed source position and the most constraining limit is achieved towards the positions of the most sensitive pulsars in the timing array. The most robust upper limit - obtained via a full Bayesian analysis searching simultaneously over the signal and pulsar noise on the subset of ours six best pulsars - is A 10-14. These limits, the most stringent to date at f < 10 nHz, exclude the presence of sub-centiparsec binaries with chirp mass Mc > 109M⊙ out to a distance of about 25 Mpc, and with Mc > 1010M⊙ out to a distance of about 1Gpc (z 0.2). We show that state-ofthe- art SMBHB population models predict <1 per cent probability of detecting a CGW with the current EPTA data set, consistent with the reported non-detection. We stress, however, that PTA limits on individual CGW have improved by almost an order of magnitude in the last five years. The continuing advances in pulsar timing data acquisition and analysis techniques will allow for strong astrophysical constraints on the population of nearby SMBHBs in the coming years. [ABSTRACT FROM AUTHOR]
Published: 2016
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31. European Pulsar Timing Array limits on an isotropic stochastic gravitational-wave background.

Author: Lentati, L., Taylor, S. R., Mingarelli, C. M. F., Sesana, A., Sanidas, S. A., Vecchio, A., Caballero, R. N., Lee, K. J., van Haasteren, R., Babak, S., Bassa, C. G., Brem, P., Burgay, M., Champion, D. J., Cognard, I., Desvignes, G., Gair, J. R., Guillemot, L., Hessels, J. W. T., and Janssen, G. H.
Subjects: PULSARS, ISOTROPIC properties, GRAVITATIONAL waves, STOCHASTIC processes, BAYESIAN analysis, DATA analysis
Abstract: We present new limits on an isotropic stochastic gravitational-wave background (GWB) using a six pulsar data set spanning 18 yr of observations from the 2015 European Pulsar Timing Array data release. Performing a Bayesian analysis, we fit simultaneously for the intrinsic noise parameters for each pulsar, along with common correlated signals including clock, and Solar system ephemeris errors, obtaining a robust 95 percent upper limit on the dimensionless strain amplitude A of the background of A < 3.0 × 10-15 at a reference frequency of 1yr-1 and a spectral index of 13/3, corresponding to a background from inspiralling supermassive black hole binaries, constraining the GW energy density to Ogw(f)h² < 1.1 × 10-9 at 2.8 nHz. We also present limits on the correlated power spectrum at a series of discrete frequencies, and show that our sensitivity to a fiducial isotropic GWB is highest at a frequency of ~5 × 10-9 Hz. Finally, we discuss the implications of our analysis for the astrophysics of supermassive black hole binaries, and present 95 percent upper limits on the string tension, Gµ/c2, characterizing a background produced by a cosmic string network for a set of possible scenarios, and for a stochastic relic GWB. For a Nambu-Goto field theory cosmic string network, we set a limit Gµ/c² < 1.3 × 10-7, identical to that set by the Planck Collaboration, when combining Planck and high-l cosmic microwave background data from other experiments. For a stochastic relic background, we set a limit of $\Omega \mathrm{relic}_\mathrm{gw}(f)h²<1.2 \times 10{-9}$, a factor of 9 improvement over the most stringent limits previously set by a pulsar timing array. [ABSTRACT FROM AUTHOR]
Published: 2015
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32. Measuring pulse times of arrival from broad-band pulsar observations.

Author: Liu, K., Desvignes, G., Cognard, I., Stappers, B. W., Verbiest, J. P. W., Lee, K. J., Champion, D. J., Kramer, M., Freire, P. C. C., and Karuppusamy, R.
Subjects: PULSARS, ASTRONOMICAL observations, BANDWIDTHS, INTERSTELLAR medium, SCINTILLATION of stars, DISCRETE Fourier transforms
Abstract: In recent years, instrumentation enabling pulsar observations with unprecedentedly high fractional bandwidth has been under development which can be used to substantially improve the precision of pulsar timing experiments. The traditional template-matching method used to calculate pulse times of arrival (ToAs) may not function effectively on these broad-band data due to a variety of effects such as diffractive scintillation in the interstellar medium, profile variation as a function of frequency, dispersion measure (DM) evolution, and so forth. In this paper, we describe the channelized discrete Fourier transform method that can greatly mitigate the influence of the aforementioned effects when measuring ToAs from broad-band timing data. The method is tested on simulated data, and its potential in improving timing precision is shown. We further apply the method to PSR J1909−3744 data collected at the Nançay Radio Telescope with the Nançay Ultimate Pulsar Processing Instrument. We demonstrate removal of systematics due to the scintillation effect as well as improvement on ToA measurement uncertainties. Our method also determines temporal variations in DM, which are consistent with multichannel timing approaches used earlier. [ABSTRACT FROM PUBLISHER]
Published: 2014
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33. PSR J1756−2251: a pulsar with a low-mass neutron star companion.

Author: Ferdman, R. D., Stairs, I. H., Kramer, M., Janssen, G. H., Bassa, C. G., Stappers, B. W., Demorest, P. B., Cognard, I., Desvignes, G., Theureau, G., Burgay, M., Lyne, A. G., Manchester, R. N., and Possenti, A.
Subjects: NEUTRON stars, BINARY systems (Astronomy), GENERAL relativity (Physics), ASTRONOMICAL observations, PULSARS, DENSITY of stars, STAR observations
Abstract: The pulsar PSR J1756−2251 resides in a relativistic double neutron star binary system with a 7.67-h orbit. We have conducted long-term precision timing on more than 9 yr of data acquired from five telescopes, measuring five post-Keplerian parameters. This has led to several independent tests of general relativity (GR), the most constraining of which shows agreement with the prediction of GR at the 4 per cent level. Our measurement of the orbital decay rate disagrees with that predicted by GR, likely due to systematic observational biases. We have derived the pulsar distance from parallax and orbital decay measurements to be $0.73_{-0.24}^{+0.60}\,$kpc (68 per cent) and <1.2 kpc (95 per cent upper limit), respectively; these are significantly discrepant from the distance estimated using Galactic electron density models. We have found the pulsar mass to be 1.341 ± 0.007 M⊙, and a low neutron star (NS) companion mass of 1.230 ± 0.007 M⊙. We also determined an upper limit to the spin–orbit misalignment angle of 34° (95 per cent) based on a system geometry fit to long-term profile width measurements. These and other observed properties have led us to hypothesize an evolution involving a low mass–loss, symmetric supernova progenitor to the second-formed NS companion, as is thought to be the case for the double pulsar system PSR J0737−3039A/B. This would make PSR J1756−2251 the second compact binary system providing concrete evidence for this type of NS formation channel. [ABSTRACT FROM PUBLISHER]
Published: 2014
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34. Detection of decametre-wavelength pulsed radio emission of 40 known pulsars.

Author: Zakharenko, V. V., Vasylieva, I. Y., Konovalenko, A. A., Ulyanov, O. M., Serylak, M., Zarka, P., Grießmeier, J.-M., Cognard, I., and Nikolaenko, V. S.
Subjects: PULSAR detection, WAVELENGTHS, RADIO frequency, ASTRONOMICAL observations, COSMIC background radiation, IONOSPHERIC radio wave propagation
Abstract: The study of pulsars at the lowest radio frequencies observable from the ground (10–30 MHz) is complicated by strong interstellar (dispersion, scattering) and ionospheric (scintillation, refraction) propagation effects, as well as intense Galactic background noise and interference. However, it permits us to measure interstellar plasma parameters (the effects of which increase by a power of two to >4 times the wavelength), the spectrum and the pulse profile at low frequencies more accurately. Up to now, only ∼10 pulsars have been successfully detected at these frequencies. The recent upgrade of the receivers at the Ukrainian T-shaped Radio telescope, second modification (UTR-2) has increased its sensitivity and motivated a new search for pulsed radio emissions. In this work we carried out a survey of known pulsars with declination above −10°, period >0.1 s and dispersion measure (DM) < 30 pc cm−3, i.e. a sample of 74 sources. Our goal was either to detect pulsars not recorded before in the decametre range or to identify factors that prevent their detection. As a result, we have detected the radio emission of 40 pulsars, i.e. 55 per cent of the observed sample. For 30 of them, this was a first detection at these frequencies. Parameters of their average profiles have been calculated, including the intrinsic widening of the pulse (not due to interstellar scattering) with decreasing frequency. Furthermore, two pulsars beyond the selected DM (B0138+59 with DM ≈ 35 pc cm−3 and B0525+21 with DM ≈51 pc cm−3) were also detected. Our results indicate that there is still room to detect new transient and pulsed sources with low-frequency observations. [ABSTRACT FROM AUTHOR]
Published: 2013
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35. Six millisecond pulsars detected by the Fermi Large Area Telescope and the radio/gamma-ray connection of millisecond pulsars.

Author: Espinoza, C. M., Guillemot, L., Çelik, Ö., Weltevrede, P., Stappers, B. W., Smith, D. A., Kerr, M., Zavlin, V. E., Cognard, I., Eatough, R. P., Freire, P. C. C., Janssen, G. H., Camilo, F., Desvignes, G., Hewitt, J. W., Hou, X., Johnston, S., Keith, M., Kramer, M., and Lyne, A.
Subjects: PULSAR detection, GAMMA rays, RADIO (Medium), LARGE astronomical telescopes, X-rays, ASTRONOMICAL observations, COSMIC magnetic fields
Abstract: We report on the discovery of gamma-ray pulsations from five millisecond pulsars (MSPs) using the Fermi Large Area Telescope (LAT) and timing ephemerides provided by various radio observatories. We also present confirmation of the gamma-ray pulsations from a sixth source, PSR J2051−0827. Five of these six MSPs are in binary systems: PSRs J1713+0747, J1741+1351, J1600−3053 and the two black widow binary pulsars PSRs J0610−2100 and J2051−0827. The only isolated MSP is the nearby PSR J1024−0719, which is also known to emit X-rays. We present X-ray observations in the direction of PSRs J1600−3053 and J2051−0827. While PSR J2051−0827 is firmly detected, we can only give upper limits for the X-ray flux of PSR J1600−3053. There are no dedicated X-ray observations available for the other three objects.The MSPs mentioned above, together with most of the MSPs detected by Fermi, are used to put together a sample of 30 gamma-ray MSPs. This sample is used to study the morphology and phase connection of radio and gamma-ray pulse profiles. We show that MSPs with pulsed gamma-ray emission which is phase-aligned with the radio emission present the steepest radio spectra and the largest magnetic fields at the light cylinder among all MSPs. Also, we observe a trend towards very low, or undetectable, radio linear polarization levels. These properties could be attributed to caustic radio emission produced at a range of different altitudes in the magnetosphere. We note that most of these characteristics are also observed in the Crab pulsar, the only other radio pulsar known to exhibit phase-aligned radio and gamma-ray emission. [ABSTRACT FROM AUTHOR]
Published: 2013
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36. AN ASTEROID BELT INTERPRETATION FOR THE TIMING VARIATIONS OF THE MILLISECOND PULSAR B1937+21.

Author: SHANNON, R. M., CORDES, J. M., METCALFE, T. S., LAZIO, T. J. W., COGNARD, I., DESVIGNES, G., JANSSEN, G. H., JESSNER, A., KRAMER, M., LAZARIDIS, K., PURVER, M. B., STAPPERS, B. W., and THEU, G.
Subjects: ASTEROID belt, PULSARS, NEUTRON stars, WHITE dwarf stars, ASTRONOMICAL observations, ASTROPHYSICS research
Abstract: Pulsar timing observations have revealed companions to neutron stars that include other neutron stars, white dwarfs, main-sequence stars, and planets. We demonstrate that the correlated and apparently stochastic residual times of arrival from the millisecond pulsar B1937+21 are consistent with the signature of an asteroid belt having a total mass ≲0.05M⊕. Unlike the solar system's asteroid belt, the best fit pulsar asteroid belt extends over a wide range of radii, consistent with the absence of any shepherding companions. We suggest that any pulsar that has undergone accretion-driven spin-up and subsequently evaporated its companion may harbor orbiting asteroid mass objects. The resulting timing variations may fundamentally limit the timing precision of some of the other millisecond pulsars. Observational tests of the asteroid belt model include identifying periodicities from individual asteroids, which are difficult; testing for statistical stationarity, which becomes possible when observations are conducted over a longer observing span; and searching for reflected radio emission. [ABSTRACT FROM AUTHOR]
Published: 2013
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37. Long-term radio observations of the intermittent pulsar B1931+24.

Author: Young, N. J., Stappers, B. W., Lyne, A. G., Weltevrede, P., Kramer, M., and Cognard, I.
Subjects: ASTRONOMICAL observations, RADIO astronomy, SOLAR radio emission, MAGNETOSPHERE, PULSARS, PLASMA gases, MAGNETOSPHERIC physics
Abstract: We present an analysis of approximately 13 yr of observations of the intermittent pulsar B1931+24 to further elucidate its behaviour. We find that while the source exhibits a wide range of nulling (∼4–39 d) and radio-emitting (∼1–19 d) time-scales, it cycles between its different emission phases over an average time-scale of approximately 38 d, which is remarkably stable over many years. On average, the neutron star is found to be radio-emitting for 26 ± 6 per cent of the time. No evidence is obtained to suggest that the pulsar undergoes any systematic, intrinsic variations in pulse intensity during the radio-emitting phases. In addition, we find no evidence for any correlation between the length of consecutive emission phases. An analysis of the rotational behaviour of the source shows that it consistently assumes the same spin-down rates, i.e. $\dot{\nu }=-16 \pm 1\times 10^{-15}$ s−2 when emitting and $\dot{\nu }=-10.8 \pm 0.4\times 10^{-15}$ s−2 when not emitting, over the entire observation span. Coupled with the stable switching time-scale, this implies that the pulsar retains a high degree of magnetospheric memory, and stability, in spite of comparatively rapid (∼ ms) dynamical plasma time-scales. While this provides further evidence to suggest that the behaviour of the neutron star is governed by magnetospheric-state switching, the underlying trigger mechanism remains illusive. This should be elucidated by future surveys with next generation telescopes such as LOFAR, MeerKAT and the SKA, which should detect similar sources and provide more clues to how their radio emission is regulated. [ABSTRACT FROM PUBLISHER]
Published: 2013
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38. Pulsar searches of Fermi unassociated sources with the Effelsberg telescope.

Author: Barr, E. D., Guillemot, L., Champion, D. J., Kramer, M., Eatough, R. P., Lee, K. J., Verbiest, J. P. W., Bassa, C. G., Camilo, F., Çelik, Ö., Cognard, I., Ferrara, E. C., Freire, P. C. C., Janssen, G. H., Johnston, S., Keith, M., Lyne, A. G., Michelson, P. F., Parkinson, P. M. Saz, and Ransom, S. M.
Subjects: PULSAR detection, RADIO telescopes, BINARY stars, GAMMA rays, PHOTONS, NUMERICAL calculations
Abstract: Using the 100-m Effelsberg radio telescope operating at 1.36 GHz, we have performed a targeted radio pulsar survey of 289 unassociated γ-ray sources discovered by the Large Area Telescope (LAT) aboard the Fermi satellite and published in the 1FGL catalogue (Abdo et al. 2010a). This survey resulted in the discovery of millisecond pulsar J1745+1017, which resides in a short-period binary system with a low-mass companion, $M_{c,\text{min}} \sim 0.0137\,\mathrm{M}_{\odot }$, indicative of ‘black widow’ type systems. A 2-yr timing campaign has produced a refined radio ephemeris, accurate enough to allow for phase-folding of the LAT photons, resulting in the detection of a dual-peaked γ-ray light curve, proving that PSR J1745+1017 is the source responsible for the γ-ray emission seen in 1FGL J1745.5+1018 (2FGL J1745.6+1015; Nolan et al. 2012). We find the γ-ray spectrum of PSR J1745+1017 to be well modelled by an exponentially cut-off power law with cut-off energy 3.2 GeV and photon index 1.6. The observed sources are known to contain a further 10 newly discovered pulsars which were undetected in this survey. Our radio observations of these sources are discussed and in all cases limiting flux densities are calculated. The reasons behind the seemingly low yield of discoveries are also discussed. [ABSTRACT FROM AUTHOR]
Published: 2013
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39. SUZAKU X-RAY FOLLOW-UP OBSERVATIONS OF SEVEN UNASSOCIATED FERMI-LAT GAMMA-RAY SOURCES AT HIGH GALACTIC LATITUDES.

Author: Y. TAKAHASHI, J. KATAOKA, T. NAKAMORI, K. MAEDA, R. MAKIYA, T. TOTANI, C. C. CHEUNG, STAWARZ, Ł., GUILLEMOT, L., FREIRE, P. C. C., and COGNARD, I.
Subjects: GALAXIES, GAMMA rays, PULSARS, TELESCOPES, PHOTONS
Abstract: We report on our second-year campaign of X-ray follow-up observations of unidentified Fermi Large Area Telescope (LAT) γ-ray sources at high Galactic latitudes (|b| > 10°) using the X-ray Imaging Spectrometer on board the Suzaku X-ray Observatory. In this second year of the project, seven new targets were selected from the First Fermi-LAT Catalog, and studied with 20-40 ks effective Suzaku exposures. We detected an X-ray point source coincident with the position of the recently discovered millisecond pulsar (MSP) PSR J2302+4442 within the 95% confidence error circle of 1FGL J2302.8+4443. The X-ray spectrum of the detected counterpart was well fit by a blackbody model with temperature of kT ⋍ 0.3 keV, consistent with an origin of the observed X-ray photons from the surface of a rotating magnetized neutron star. For four other targets that were also recently identified with a normal pulsar (1FGL J0106.7+4853) and MSPs (1FGL J1312.6+0048, J1902.0-5110, and J2043.2+1709), only upper limits in the 0.5-10 keV band were obtained at the flux levels of ⋍10-14 erg cm-2 s-1. A weak X-ray source was found in the field of 1FGL J1739.4+8717, but its association with the variable γ -ray emitter could not be confirmed with the available Suzaku data alone. For the remaining Fermi-LAT object 1FGL J1743.8-7620 no X-ray source was detected within the LAT 95% error ellipse. We briefly discuss the general properties of the observed high Galactic-latitude Fermi-LAT objects by comparing their multiwavelength properties with those of known blazars and MSPs. [ABSTRACT FROM AUTHOR]
Published: 2012
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40. PULSED GAMMA RAYS FROM THE ORIGINAL MILLISECOND AND BLACK WIDOW PULSARS: A CASE FOR CAUSTIC RADIO EMISSION?

Author: Guillemot, L., Johnson, T. J., Venter, C., Kerr, M., Pancrazi, B., Livingstone, M., Janssen, G. H., Jaroenjittichai, P., Kramer, M., Cognard, I., Stappers, B. W., Harding, A. K., Camilo, F., Espinoza, C. M., Freire, P. C. C., Gargano, F., Grove, J. E., Johnston, S., Michelson, P. F., and Noutsos, A.
Subjects: PULSARS, RADAR telescopes, MAGNETOSPHERE, GAMMA ray astronomy, COSMIC dust
Abstract: We report the detection of pulsed gamma-ray emission from the fast millisecond pulsars (MSPs) B1937+21 (also known as J1939+2134) and B1957+20 (J 1959+2048) using 18 months of survey data recorded by the Fermi Large Area Telescope and timing solutions based on radio observations conducted at the Westerbork and Nançay radio telescopes. In addition, we analyzed archival Rossi X-ray Timing Explorer and XMM-Newton X-ray data for the two MSPs, confirming the X-ray emission properties of PSR B1937+21 and finding evidence (~4σ) for pulsed emission from PSR B 1957+20 for the first time. In both cases the gamma-ray emission profile is characterized by two peaks separated by half a rotation and are in close alignment with components observed in radio and X-rays. These two pulsars join PSRs J0034-0534 and J2214+3000 to form an emerging class of gamma-ray MSPs with phase-aligned peaks in different energy bands. The modeling of the radio and gamma-ray emission profiles suggests co-located emission regions in the outer magnetosphere. [ABSTRACT FROM AUTHOR]
Published: 2012
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41. SUB-LUMINOUS γ-RAY PULSARS.

Author: ROMANI, R. W., KERR, M., CRAIG, H. A., JOHNSTON, S., COGNARD, I., and SMITH, D. A.
Subjects: PULSARS, RADIATION sources, TELESCOPES, NEUTRON stars, GAMMA rays, STELLAR oscillations
Abstract: Most pulsars observed by the Fermi Large Area Telescope have γ-ray luminosities scaling with spin-down power Ė as Lγ ≈ (Ė x 1033 erg s-1)1/2. However, there exist one detection and several upper limits an order of magnitude or more fainter than this trend. We describe these "sub-luminous" γ-ray pulsars and discuss the case for this being an orientation effect. Of the 12 known young radio pulsars with Ė > 1034erg s-1 and d ⩽ 2 kpc several are substantially sub-luminous. The limited available geometrical constraints favor aligned geometries for these pulsars, although no one case for alignment is compelling. In this scenario GeV emission detected from such sub-luminous pulsars can be due to a lower altitude, lower-power accelerator gap. [ABSTRACT FROM AUTHOR]
Published: 2011
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42. DETECTION OF THE PULSAR WIND NEBULA HESS J1825-137 WITH THE FERMI LARGE AREA TELESCOPE.

Author: GRONDIN, M.-H., FUNK, S., LEMOINE-GOUMARD, M., VAN ETTEN, A., HINTON, J. A., CAMILO, F., COGNARD, I., ESPINOZA, C. M., FREIRE, P. C. C., GROVE, J. E., GUILLEMOT, L., JOHNSTON, S., KRAMER, M., LANDE, J., MICHELSON, P., POSSENTI, A., ROMANI, R. W., SKILTON, J. L., THEUREAU, G., and WELTEVREDE, P.
Subjects: MAGNETIC fields, PULSARS, RADIATION sources, GAMMA rays, NEBULAE
Abstract: We announce the discovery of 1-100 GeV gamma-ray emission from the archetypal TeV pulsar wind nebula (PWN) HESS J1825-137 using 20 months of survey data from the Fermi-Large Area Telescope (LAT). The gamma-ray emission detected by the LAT is significantly spatially extended, with a best-fit rms extension of σ = 0°.56 ± 0°.07 for an assumed Gaussian model. The 1-100 GeV LAT spectrum of this source is well described by a power law with a spectral index of 1.38 ± 0.12 ± 0.16 and an integral flux above 1 GeV of (6.50 ± 0.21 ± 3.90) x 10-9 cm-2s-1. The first errors represent the statistical errors on the fit parameters, while the second ones are the systematic uncertainties. Detailed morphological and spectral analyses bring new constraints on the energetics and magnetic field of the PWN system. The spatial extent and hard spectrum of the GeV emission are consistent with the picture of an inverse Compton origin of the GeV-TeV emission in a cooling-limited nebula powered by the pulsar PSRJ1826-1334. [ABSTRACT FROM AUTHOR]
Published: 2011
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43. Generic tests of the existence of the gravitational dipole radiation and the variation of the gravitational constant.

Author: Lazaridis, K., Wex, N., Jessner, A., Kramer, M., Stappers, B. W., Janssen, G. H., Desvignes, G., Purver, M. B., Cognard, I., Theureau, G., Lyne, A. G., Jordan, C. A., and Zensus, J. A.
Subjects: CELESTIAL mechanics, NEUTRON stars, RADIATION sources, WHITE dwarf stars, GRAVITY waves
Abstract: We present results from the high-precision timing analysis of the pulsar-white dwarf (WD) binary PSR using 15 years of multitelescope data. Observations were performed regularly by the European Pulsar Timing Array (EPTA) network, consisting of Effelsberg, Jodrell Bank, Westerbork and Nançay. All the timing parameters have been improved from the previously published values, most by an order of magnitude. In addition, a parallax measurement of is obtained for the first time for PSR , being consistent with the optical estimation from the WD companion. Combining improved 3D velocity information and models for the Galactic potential, the complete evolutionary Galactic path of the system is obtained. A new intrinsic eccentricity upper limit of is acquired, one of the smallest calculated for a binary system and a measurement of the variation of the projected semimajor axis also constrains the system's orbital orientation for the first time. It is shown that PSR is an ideal laboratory for testing alternative theories of gravity. The measurement of the change of the orbital period of the system of is used to set an upper limit on the dipole gravitational wave emission that is valid for a wide class of alternative theories of gravity. Moreover, it is shown that in combination with other binary pulsars PSR is an ideal system to provide self-consistent, generic limits, based only on millisecond pulsar data, for the dipole radiation and the variation of the gravitational constant . [ABSTRACT FROM AUTHOR]
Published: 2009
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44. Searches for Gravitational Waves from Known Pulsars at Two Harmonics in 2015-2017 LIGO Data

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Anand, S., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arene, M., Arnaud, N., Aronson, S. M., Ascenzi, S., Ashton, G., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., Aultoneal, K., Austin, C., Avendano, V., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baird, J., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Bals, A., Banagiri, S., Barayoga, J. C., Barbieri, C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., Becsy, B., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Benjamin, M. G., Berger, B. K., Bergmann, G., Bernuzzi, S., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bidler, J., Biggs, E., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Birney, R., Birnholtz, O., Biscans, S., Bischi, M., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bobba, F., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bondu, F., Bonnand, R., Booker, P., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Breschi, M., Briant, T., Briggs, J. H., Brighenti, F., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A. F., Brooks, J., Brown, D. D., Brunett, S., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Calderon Bustillo, J., Callister, T. A., Calloni, E., Camp, J. B., Campbell, W. A., Cannon, K. C., Cao, H., Cao, J., Carapella, G., Carbognani, F., Caride, S., Carney, M. F., Carullo, G., Casanueva Diaz, J., Casentini, C., Caudill, S., Cavaglia, M., Cavalier, F., Cavalieri, R., Cella, G., Cerda-Duran, P., Cesarini, E., Chaibi, O., Chakravarti, K., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, D., Chaturvedi, M., Cheeseboro, B. D., Chen, H. Y., Chen, X., Chen, Y., Cheng, H. -P., Cheong, C. K., Chia, H. Y., Chiadini, F., Chincarini, A., Chiummo, A., Cho, G., Cho, H. S., Cho, M., Christensen, N., Chu, Q., Chua, S., Chung, K. W., Chung, S., Ciani, G., Cieslar, M., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Coccia, E., Cohadon, P. -F., Cohen, D., Colleoni, M., Collette, C. G., Collins, C., Colpi, M., Cominsky, L. R., Constancio, M., J, R., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrion, I., Corezzi, S., Corley, K. R., Cornish, N., Corre, D., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Croquette, M., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Dal Canton, T., Dalya, G., D'Angelo, B., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Da Silva Costa, C. F., Datrier, L. E. H., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. J., Debra, D., Deenadayalan, M., Degallaix, J., De laurentis, M., Deleglise, S., Del Pozzo, W., Demarchi, L. M., Demos, N., Dent, T., De Pietri, R., De Rosa, R., De Rossi, C., Desalvo, R., de Varona, O., Dhurandhar, S., Diaz, M. C., Dietrich, T., Di Fiore, L., Difronzo, 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. K., Dmitriev, A., Doctor, Z., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Downes, T. P., Drago, M., Driggers, J. C., Du, Z., Ducoin, J. -G., Dupej, P., Durante, O., Dwyer, S. E., Easter, P. J., Eddolls, G., Edo, T. B., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Errico, L., Essick, R. C., Estelles, H., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Fafone, V., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fazio, M., Fee, C., Feicht, J., Fejer, M. M., Feng, F., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferreira, T. A., Fidecaro, F., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fishner, J. M., Fittipaldi, R., Fitz-Axen, M., Fiumara, V., Flaminio, R., Fletcher, M., Floden, E., Flynn, E., Fong, H., Font, J. A., Forsyth, P. W. F., Fournier, J. -D., Vivanco, Francisco Hernandez, Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fritschel, P., Frolov, V. V., Fronze, G., Fulda, P., Fyffe, M., Gabbard, H. A., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garcia-Quiros, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giacomazzo, B., Giaime, J. A., Giardina, K. D., Gibson, D. R., Gill, K., Glover, L., Gniesmer, J., Godwin, P., Goetz, E., Goetz, R., Goncharov, B., Gonzalez, G., Gonzalez Castro, J. M., Gopakumar, A., Gossan, S. E., Gosselin, M., Gouaty, R., Grace, B., Grado, A., Granata, M., Grant, A., Gras, S., Grassia, P., Gray, C., Gray, R., Greco, G., Green, A. C., Green, R., Gretarsson, E. M., Grimaldi, A., Grimm, S. J., Groot, P., Grote, H., Grunewald, S., Gruning, P., Guidi, G. M., Gulati, H. K., Guo, Y., Gupta, A., Gupta, Anchal, Gupta, P., Gustafson, E. K., Gustafson, R., Haegel, L., Halim, O., Hall, B. R., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannuksela, O. A., Hansen, T. J., Hanson, J., Harder, T., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hasskew, R. K., Haster, C. J., Haughian, K., Hayes, F. J., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hellman, F., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heurs, M., Hild, S., Hinderer, T., Hochheim, S., Hofman, D., Holgado, A. M., Holland, N. A., Holt, K., Holz, D. E., Hopkins, P., Horst, C., Hough, J., Howell, E. J., Hoy, C. G., Huang, Y., Huebner, M. T., Huerta, E. A., Huet, D., Hughey, B., Hui, V., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idzkowski, B., Iess, A., Inchauspe, H., Ingram, C., Inta, R., Intini, G., Irwin, B., Isa, H. N., Isac, J. -M., Isi, M., Iyer, B. R., Jacqmin, T., Jadhav, S. J., Jani, K., Janthalur, N. N., Jaranowski, P., Jariwala, D., Jenkins, A. C., Jiang, J., Johnson, D. S., Jones, A. W., Jones, D. I., Jones, J. D., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Kashyap, R., Kasprzack, M., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Keerthana, N. V., Kefelian, F., Keitel, D., Kennedy, R., Key, J. S., Khalili, F. Y., Khan, I., Khan, S., Khazanov, E. A., Khetan, N., Khursheed, M., Kijbunchoo, N., Kim, Chunglee, Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y. -M., Kimball, C., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klika, J. H., Klimenko, S., Knowles, T. D., Koch, P., Koehlenbeck, S. M., Koekoek, G., Koley, S., Kondrashov, V., Kontos, A., Koper, N., Korobko, M., Korth, W. Z., Kovalam, M., Kozak, D. B., Kraemer, C., Kringel, V., Krishnendu, N., Krolak, A., Krupinski, N., Kuehn, G., Kumar, A., Kumar, P., Kumar, Rahul, Kumar, Rakesh, Kuo, L., Kutynia, A., Kwang, S., Lackey, B. D., Laghi, D., Lai, K. H., Lam, T. L., Landry, M., Lane, B. B., Lang, R. N., Lange, J., Lantz, B., Lanza, R. K., Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lecoeuche, K., Lee, C. H., Lee, H. K., Lee, H. M., Lee, H. W., Lee, J., Lee, K., Lehmann, J., Lenon, A. K., Leroy, N., Letendre, N., Levin, Y., Li, A., Li, J., K. J. L., Li, T. G. F., Li, Li, X., Lin, F., Linde, F., Linker, S. D., Littenberg, T. B., Liu, J., Liu, X., Llorens-Monteagudo, M., R. K. L., Lo, London, L. T., Longo, A., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Lower, M. E., Lueck, H., Lumaca, D., Lundgren, A. P., Lynch, R., Ma, Y., Macas, R., Macfoy, S., Macinnis, M., Macleod, D. M., Macquet, A., Magana Hernandez, I., Magana-Sandoval, F., Magee, R. M., Majorana, E., Maksimovic, I., Malik, A., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Mapelli, M., Marchesoni, F., Marion, F., Marka, S., Marka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsat, S., Martelli, F., Martin, I. W., Martin, R. M., Martinez, V., Martynov, D. V., Masalehdan, H., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Matone, L., Mavalvala, N., Mccann, J. J., Mccarthy, R., Mcclelland, D. E., Mccormick, S., Mcculler, L., Mcguire, S. C., Mcisaac, C., Mciver, J., Mcmanus, D. J., Mcrae, T., Mcwilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Mehta, A. K., Meidam, J., Villa, E. Mejuto, Melatos, A., Mendell, G., Mercer, R. A., Mereni, L., Merfeld, K., Merilh, E. 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P., Rowan, S., Ruediger, A., Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sakellariadou, M., Salafia, O. S., Salconi, L., Saleem, M., Samajdar, A., Sammut, L., Sanchez, E. J., Sanchez, L. E., Sanchis-Gual, N., Sanders, J. R., Santiago, K. A., Santos, E., Sarin, N., Sassolas, B., Saulson, P. R., Sauter, O., Savage, R. L., Schale, P., Scheel, M., Scheuer, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schoenbeck, A., Schreiber, E., Schulte, B. W., Schutz, B. F., Scott, J., Scott, S. M., Seidel, E., Sellers, D., Sengupta, A. S., Sennett, N., Sentenac, D., Sequino, V., Sergeev, A., Setyawati, Y., Shaddock, D. A., Shaffer, T., Shahriar, M. S., Shaner, M. B., Sharma, A., Sharma, P., Shawhan, P., Shen, H., Shink, R., Shoemaker, D. H., Shoemaker, D. M., Shukla, K., Shyamsundar, S., Siellez, K., Sieniawska, M., Sigg, D., Singer, L. P., Singh, D., Singh, N., Singhal, A., Sintes, A. M., Sitmukhambetov, S., Skliris, V., Slagmolen, B. J. J., Slaven-Blair, T. J., Smith, J. 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W., Tse, M., Tso, R., Tsukada, L., Tsuna, D., Tsutsui, T., Tuyenbayev, D., Ueno, K., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., Valentini, M., van Bakel, N., van Beuzekom, M., van den Brand, J. F. J., Van Den Broeck, C., Vander-Hyde, D. C., van der Schaaf, L., Vanheijningen, J. V., van Veggel, A. A., Vardaro, M., Varma, V., Vass, S., Vasuth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venugopalan, G., Verkindt, D., Vetrano, F., Vicere, A., Viets, A. D., Vinciguerra, S., Vine, D. J., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walet, R., Walker, M., Wallace, L., Walsh, S., Wang, H., Wang, J. Z., Wang, S., Wang, W. H., Wang, Y. F., Ward, R. L., Warden, Z. A., Warner, J., Was, M., Watchi, J., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Wellmann, F., Wen, L., Wessel, K., Wessels, P., Westhouse, J. 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E., Zweizig, J., 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, 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)), 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 de Paris (UP), 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), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Centre National de la Recherche Scientifique (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)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Institut des Fonctions Optiques pour les Technologies de l'informatiON (Institut FOTON), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Laboratoire Kastler Brossel (LKB [Collège de France]), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Collège de France (CdF (institution)), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon, Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL), Institut des Hautes Etudes Scientifiques (IHES), IHES, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), 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 - 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CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), The LIGO Scientific Collaboration, The Virgo Collaboration, 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 sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Nice Sophia Antipolis (1965 - 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, 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 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), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF (institution))-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut des Hautes Études Scientifiques (IHES), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-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), IoP (FNWI), Astroparticle Physics (IHEF, IoP, FNWI), RS: FSE Grav. waves and fundamental physics, Grav. waves and fundamental physics, RS: FSE MSP, Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arene, M., Arnaud, N., Ascenzi, S., Ashton, G., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., Aultoneal, K., Austin, C., Avendano, V., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Bailes, M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., Becsy, B., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Berger, B. K., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bidler, J., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Booth, C. D., Bork, R., Boschi, V., Bose, S., Bossie, K., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Briant, T., Briggs, J. H., Brighenti, F., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. D., Brunett, S., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T. A., Calloni, E., Camp, J. B., Campbell, W. A., Canepa, M., Cannon, K. C., Cao, H., Cao, J., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Carullo, G., Diaz, J. C., Casentini, C., Caudill, S., Cavaglia, M., Cavalier, F., Cavalieri, R., Cella, G., Cerda-Duran, P., Cerretani, G., Cesarini, E., Chaibi, O., Chakravarti, K., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, D., Chaturvedi, M., Cheeseboro, B. D., Chen, H. Y., Chen, X., Chen, Y., Cheng, H. -P., Cheong, C. K., Chia, H. Y., Chincarini, A., Chiummo, A., Cho, G., Cho, H. S., Cho, M., Christensen, N., Chu, Q., Chua, S., Chung, K. W., Chung, S., Ciani, G., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P. -F., Cohen, D., Colgan, R., Colleoni, M., Collette, C. G., Collins, C., Cominsky, L. R., Constancio, M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrion, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Croquette, M., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. D., Dalya, G., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Costa, C. F. D. S., Datrier, L. E. H., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. J., Debra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Deleglise, S., Pozzo, W. D., Demarchi, L. M., Demos, N., Dent, T., Pietri, R. D., Derby, J., De Rosa, R., Rossi, C. D., Desalvo, R., Varona, O. D., Dhurandhar, S., D'Az, M. C., Dietrich, T., Di Fiore, L., Giovanni, M. D., Di Girolamo, T., Lieto, A. D., Ding, B., Pace, S. D., Palma, I. D., Renzo, F. D., Dmitriev, A., Doctor, Z., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Downes, T. P., Drago, M., Driggers, J. C., Du, Z., Ducoin, J. -G., Dupej, P., Dwyer, S. E., Easter, P. J., Edo, T. B., Edwards, M. C., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Essick, R. C., Estelles, H., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fazio, M., Fee, C., Feicht, J., Fejer, M. M., Feng, F., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferreira, T. A., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fishner, J. M., Fitz-Axen, M., Flaminio, R., Fletcher, M., Flynn, E., Fong, H., Font, J. A., Forsyth, P. W. F., Fournier, J. -D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fritschel, P., Frolov, V. 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V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Karvinen, K. S., Kashyap, R., Kasprzack, M., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Keerthana, N. V., Kefelian, F., Keitel, D., Kennedy, R., Key, J. S., Khalili, F. Y., Khan, H., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Khursheed, M., Kijbunchoo, N., Kim, C., Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y. -M., Kimball, C., King, E. J., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klika, J. H., Klimenko, S., Knowles, T. D., Koch, P., Koehlenbeck, S. M., Koekoek, G., Koley, S., Kondrashov, V., Kontos, A., Koper, N., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Krishnendu, N., Krolak, A., Kuehn, G., Kumar, A., Kumar, P., Kumar, R., Kumar, S., Kuo, L., Kutynia, A., Kwang, S., Lackey, B. D., Lai, K. H., Lam, T. L., Landry, M., Lane, B. B., Lang, R. N., Lange, J., Lantz, B., Lanza, R. 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W., Martin, R. M., Martynov, D. V., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mccann, J. J., Mccarthy, R., Mcclelland, D. E., Mccormick, S., Mcculler, L., Mcguire, S. C., Mciver, J., Mcmanus, D. J., Mcrae, T., Mcwilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Mehta, A. K., Meidam, J., Melatos, A., Mendell, G., Mercer, R. A., Mereni, L., Merilh, E. L., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, A. L., Miller, A., Millhouse, M., Mills, J. C., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Mishkin, A., Mishra, C., Mistry, T., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Mo, G., Moffa, D., Mogushi, K., Mohapatra, S. R. P., Montani, M., Moore, C. J., Moraru, D., Moreno, G., Morisaki, S., Mours, B., Mow-Lowry, C. M., Mukherjee, A., Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Mu'Iz, E. A., Muratore, M., Murray, P. G., Nagar, A., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Ng, K. Y., Ng, S., Nguyen, P., Nichols, D., Nissanke, S., Nocera, F., North, C., Nuttall, L. K., Obergaulinger, M., Oberling, J., O'Brien, B. D., O'Dea, G. D., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Ohta, H., Okada, M. A., Oliver, M., Oppermann, P., Oram, R. J., O'Reilly, B., Ormiston, R. G., Ortega, L. F., O'Shaughnessy, R., Ossokine, S., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Pagano, G., Page, M. A., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal-Singh, A., Pan, H. -W., Pang, B., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patil, M., Patricelli, B., Pearlstone, B. 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Nguyen, P, Nichols, D, Nissanke, S, Nocera, F, North, C, Nuttall, L, Obergaulinger, M, Oberling, J, O'Brien, B, O'Dea, G, Ogin, G, Oh, J, Oh, S, Ohme, F, Ohta, H, Okada, M, Oliver, M, Oppermann, P, Oram, R, O'Reilly, B, Ormiston, R, Ortega, L, O'Shaughnessy, R, Ossokine, S, Ottaway, D, Overmier, H, Owen, B, Pace, A, Pagano, G, Page, M, Pai, A, Pai, S, Palamos, J, Palashov, O, Palomba, C, Pal-Singh, A, Pan, H, Pang, B, Pang, P, Pankow, C, Pannarale, F, Pant, B, Paoletti, F, Paoli, A, Parida, A, Parker, W, Pascucci, D, Pasqualetti, A, Passaquieti, R, Passuello, D, Patil, M, Patricelli, B, Pearlstone, B, Pedersen, C, Pedraza, M, Pedurand, R, Pele, A, Penn, S, Perez, C, Perreca, A, Pfeiffer, H, Phelps, M, Phukon, K, Piccinni, O, Pichot, M, Piergiovanni, F, Pillant, G, Pinard, L, Pirello, M, Pitkin, M, Poggiani, R, Pong, D, Ponrathnam, S, Popolizio, P, Porter, E, Powell, J, Prajapati, A, Prasad, J, Prasai, K, Prasanna, R, Pratten, G, Prestegard, T, Privitera, S, Prodi, G, Prokhorov, L, Puncken, O, Punturo, M, Puppo, P, Purrer, M, Qi, H, Quetschke, V, Quinonez, P, Quintero, E, Quitzow-James, R, Raab, F, Radkins, H, Radulescu, N, Raffai, P, Raja, S, Rajan, C, Rajbhandari, B, Rakhmanov, M, Ramirez, K, Ramos-Buades, A, Rana, J, Rao, K, Rapagnani, P, Raymond, V, Razzano, M, Read, J, Regimbau, T, Rei, L, Reid, S, Reitze, D, Ren, W, Ricci, F, Richardson, C, Richardson, J, Ricker, P, Riles, K, Rizzo, M, Robertson, N, Robie, R, Robinet, F, Rocchi, A, Rolland, L, Rollins, J, Roma, V, Romanelli, M, Romano, R, Romel, C, Romie, J, Rose, K, Rosinska, D, Rosofsky, S, Ross, M, Rowan, S, Rudiger, A, Ruggi, P, Rutins, G, Ryan, K, Sachdev, S, Sadecki, T, Sakellariadou, M, Salconi, L, Saleem, M, Samajdar, A, Sammut, L, Sanchez, E, Sanchez, L, Sanchis-Gual, N, Sandberg, V, Sanders, J, Santiago, K, Sarin, N, Sassolas, B, Saulson, P, Sauter, O, Savage, R, Schale, P, Scheel, M, Scheuer, J, Schmidt, P, Schnabel, R, Schofield, R, Schonbeck, A, Schreiber, E, Schulte, B, Schutz, B, Schwalbe, S, Scott, J, Scott, S, Seidel, E, Sellers, D, Sengupta, A, Sennett, N, Sentenac, D, Sequino, V, Sergeev, A, Setyawati, Y, Shaddock, D, Shaffer, T, Shahriar, M, Shaner, M, Shao, L, Sharma, P, Shawhan, P, Shen, H, Shink, R, Shoemaker, D, Shyamsundar, S, Siellez, K, Sieniawska, M, Sigg, D, Silva, A, Singer, L, Singh, N, Singhal, A, Sintes, A, Sitmukhambetov, S, Skliris, V, Slagmolen, B, Slaven-Blair, T, Smith, J, Smith, R, Somala, S, Son, E, Sorazu, B, Sorrentino, F, Souradeep, T, Sowell, E, Spencer, A, Srivastava, A, Srivastava, V, Staats, K, Stachie, C, Standke, M, Steer, D, Steinke, M, Steinlechner, J, Steinlechner, S, Steinmeyer, D, Stevenson, S, Stocks, D, Stone, R, Stops, D, Strain, K, Stratta, G, Strigin, S, Strunk, A, Sturani, R, Stuver, A, Sudhir, V, Summerscales, T, Sun, L, Sunil, S, Suresh, J, Sutton, P, Swinkels, B, Szczepanczyk, M, Tacca, M, Tait, S, Talbot, C, Talukder, D, Tanner, D, Tapai, M, Taracchini, A, Tasson, J, Taylor, R, Thies, F, Thomas, M, Thomas, P, Thondapu, S, Thorne, K, Thrane, E, Tiwari, S, Tiwari, V, Toland, K, Tonelli, M, Tornasi, Z, Torres-Forne, A, Torrie, C, Toyr, D, Travasso, F, Traylor, G, Tringali, M, Trovato, A, Trozzo, L, Trudeau, R, Tsang, K, Tse, M, Tso, R, Tsukada, L, Tsuna, D, Tuyenbayev, D, Ueno, K, Ugolini, D, Unnikrishnan, C, Urban, A, Usman, S, Vahlbruch, H, Vajente, G, Valdes, G, Bakel, N, Beuzekom, M, Van Den Brand, J, Broeck, C, Vander-Hyde, D, Heijningen, J, Schaaf, L, Veggel, A, Vardaro, M, Varma, V, Vass, S, Vas'Th, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, P, Venkateswara, K, Venugopalan, G, Verkindt, D, Vetrano, F, Vicere, A, Viets, A, Vine, D, Vinet, J, Vitale, S, Vo, T, Vocca, H, Vorvick, C, Vyatchanin, S, Wade, A, Wade, L, Wade, M, Walet, R, Walker, M, Wallace, L, Walsh, S, Wang, G, Wang, H, Wang, J, Wang, W, Wang, Y, Ward, R, Warden, Z, Warner, J, Was, M, Watchi, J, Weaver, B, Wei, L, Weinert, M, Weinstein, A, Weiss, R, Wellmann, F, Wen, L, Wessel, E, Wessels, P, Westhouse, J, Wette, K, Whelan, J, Whiting, B, Whittle, C, Wilken, D, Williams, D, Williamson, A, Willis, J, Willke, B, Wimmer, M, Winkler, W, Wipf, C, Wittel, H, Woan, G, Woehler, J, Wofford, J, Worden, J, Wright, J, Wu, D, Wysocki, D, Xiao, L, Yamamoto, H, Yancey, C, Yang, L, Yap, M, Yazback, M, Yeeles, D, Yu, H, Yuen, S, Yvert, M, Zadrozny, A, Zanolin, M, Zelenova, T, Zendri, J, Zevin, M, Zhang, J, Zhang, L, Zhang, T, Zhao, C, Zhou, M, Zhou, Z, Zhu, X, Zucker, M, Zweizig, J, Arzoumanian, Z, Bogdanov, S, Cognard, I, Corongiu, A, Enoto, T, Freire, P, Gendreau, K, Guillemot, L, Harding, A, Jankowski, F, Keith, M, Kerr, M, Lyne, A, Palfreyman, J, Possenti, A, Ridolfi, A, Stappers, B, Theureau, G, Weltervrede, P, Abbott, Bp, Abbott, Td, Adhikari, Rx, Adya, Vb, Aguiar, Od, Aloy, Ma, Altin, Pa, Anderson, Sb, Anderson, Wg, Angelova, Sv, Araya, Mc, Aston, Sm, Bader, Mkm, Baker, Pt, Ballmer, Sw, Barayoga, Jc, Barclay, Se, Barish, Bc, Bayley, Jc, Berger, Bk, Bero, Jj, Berry, Cpl, Bilenko, Ia, Bilgili, Sa, Bizouard, Ma, Blackburn, Jk, Blair, Cd, Blair, Dg, Blair, Rm, Boom, Ba, Booth, Cd, Brady, Pr, Brau, Je, Briggs, Jh, Brooks, Af, Brown, Dd, Bulten, Hj, Byer, Rl, Bustillo, Jc, Callister, Ta, Camp, Jb, Campbell, Wa, Cannon, Kc, Carney, Mf, Diaz, Jc, Chamberlin, Sj, Chase, Ea, Cheeseboro, Bd, Chen, Hy, Cheng, Hp, Cheong, Ck, Chia, Hy, Chung, Kw, Ciobanu, Aa, Clark, Ja, Cohadon, Pf, Collette, Cg, Cominsky, Lr, Cooper, Sj, Corbitt, Tr, Corley, Kr, Costa, Ca, Coughlin, Mw, Coughlin, Sb, Coulon, Jp, Countryman, St, Covas, Pb, Cowan, Ee, Coward, Dm, Cowart, Mj, Coyne, Dc, Creighton, Jde, Creighton, Td, Crowder, Sg, Cullen, Tj, Danilishin, Sl, Costa, Cfd, Datrier, Leh, Daw, Ej, Demarchi, Lm, Diaz, Mc, Di Renzo, F, Dooley, Kl, Downes, Tp, Driggers, Jc, Ducoin, Jg, Dwyer, Se, Easter, Pj, Edo, Tb, Edwards, Mc, Eisenstein, Ra, Essick, Rc, Etienne, Zb, Evans, Tm, Farr, Wm, Fauchon-Jones, Ej, Fejer, Mm, Ferreira, Ec, Ferreira, Ta, Fisher, Rp, Fishner, Jm, Font, Ja, Forsyth, Pwf, Fournier, Jd, Frolov, Vv, Gabbard, Ha, Gadre, Bu, Gaebel, Sm, Gair, Jr, Ganija, Mr, Gaonkar, Sg, Garcia-Quiros, C, Giaime, Ja, Giardina, Kd, Castro, Jmg, Gorodetsky, Ml, Gossan, Se, Green, Ac, Gretarsson, Em, Guidi, Gm, Gulati, Hk, Gupta, Mk, Gustafson, Ek, Hall, Br, Hall, Ed, Hamilton, Ez, Hanke, Mm, Hannam, Md, Hannuksela, Oa, Harry, Gm, Harry, Iw, Haster, Cj, Hayes, Fj, Heintze, Mc, Heptonstall, Aw, Vivanco, Fh, Ho, Wcg, Holgado, Am, Holland, Na, Holz, De, Howell, Ej, Hoy, Cg, Huerta, Ea, Huttner, Sh, Isa, Hn, Isac, Jm, Iyer, Br, Jadhav, Sj, Janthalur, Nn, Jenkins, Ac, Jones, Aw, Jones, Di, Jonker, Rjg, Kalaghatgi, Cv, Kanner, Jb, Kapadia, Sj, Keerthana, Nv, Khalili, Fy, Khazanov, Ea, Kim, Jc, Kim, Ym, King, Ej, King, Pj, Klika, Jh, Knowles, Td, Koehlenbeck, Sm, Korth, Wz, Kozak, Db, Lackey, Bd, Lai, Kh, Lam, Tl, Lane, Bb, Lang, Rn, Lanza, Rk, Lasky, Pd, Lecoeuche, Yk, Lee, Ch, Lee, Hk, Lee, Hm, Lee, Hw, Li, Kjl, Li, Tgf, Linker, Sd, Littenberg, Tb, Lo, Rkl, Lockerbie, Na, London, Lt, Long, A, Lough, Jd, Lousto, Co, Lower, Me, Lundgren, Ap, Macleod, Dm, Magana-Sandoval, F, Zertuche, Lm, Magee, Rm, Mansell, Gl, Martin, Iw, Martin, Rm, Martynov, Dv, Massinger, Tj, Mccann, Jj, Mcclelland, De, Mcguire, Sc, Mcmanus, Dj, Mcwilliams, St, Meadors, Gd, Mehta, Ak, Mercer, Ra, Merilh, El, Meyers, Pm, Mikhailov, Ee, Miller, Al, Mills, Jc, Milovich-Goff, Mc, Mitrofanov, Vp, Mohapatra, Srp, Moore, Cj, Mow-Lowry, Cm, Muniz, Ea, Murray, Pg, Nayak, Rk, Nelson, Tjn, Ng, Ky, Nuttall, Lk, O'Brien, Bd, O'Dea, Gd, Ogin, Gh, Oh, Jj, Oh, Sh, Okada, Ma, Oram, Rj, Ormiston, Rg, Ortega, Lf, Ottaway, Dj, Owen, Bj, Pace, Ae, Page, Ma, Pai, Sa, Palamos, Jr, Pan, Hw, Pang, Pth, Pant, Bc, Pearlstone, Bl, Perez, Cj, Pfeiffer, Hp, Piccinni, Oj, Pong, Dyt, Porter, Ek, Prajapati, Ak, Prodi, Ga, Prokhorov, Lg, Quinonez, Pj, Quintero, Ea, Raab, Fj, Ramirez, Ke, Reitze, Dh, Richardson, Cj, Richardson, Jw, Ricker, Pm, Robertson, Na, Rollins, Jg, Roma, Vj, Romel, Cl, Romie, Jh, Rosofsky, Sg, Ross, Mp, Sanchez, Ej, Sanchez, Le, Sanders, Jr, Santiago, Ka, Saulson, Pr, Savage, Rl, Schofield, Rm, Schulte, Bw, Schutz, Bf, Schwalbe, Sg, Scott, Sm, Shaddock, Da, Shaner, Mb, Shoemaker, Dh, Shoemaker, Dm, Silva, Ad, Singer, Lp, Sintes, Am, Slagmolen, Bjj, Slaven-Blair, Tj, Smith, Jr, Smith, Rje, Son, Ej, Spencer, Ap, Srivastava, Ak, Steer, Da, Stevenson, Sp, Stops, Dj, Strain, Ka, Strigin, Se, Stuver, Al, Summerscales, Tz, Sutton, Pj, Swinkels, Bl, Szczepanczyk, Mj, Tait, Sc, Tanner, Db, Tasson, Jd, Thondapu, Sr, Thorne, Ka, Torrie, Ci, Toyra, D, Tringali, Mc, Tsang, Kw, Urban, Al, Usman, Sa, den Brand, Jfj, den Broeck, C, Vander-Hyde, Dc, Heijningen, Jv, Schaaf, Ld, Veggel, Aa, Vasuth, M, Veitch, Pj, Viets, Ad, Vine, Dj, Vinet, Jy, Vyatchanin, Sp, Wade, Ar, Wade, Le, Wang, Jz, Wang, Wh, Wang, Yf, Ward, Rl, Warden, Za, Wei, Lw, Weinstein, Aj, Wessel, Ek, Westhouse, Jw, Whelan, Jt, Whiting, Bf, Wilken, Dm, Williamson, Ar, Willis, Jl, Wimmer, Mh, Wipf, Cc, Wofford, Jk, Wright, Jl, Wysocki, Dm, Yancey, Cc, Yap, Mj, Yeeles, Dw, Yuen, Shr, Zadrozny, Ak, Zendri, Jp, Zhu, Xj, Zucker, Me, Ligo, S, Gendreau, Kc, Harding, Ak, and Keith, Mj
Subjects: TIMING NOISE, 010504 meteorology & atmospheric sciences, Astronomy, Gravitational Wave, Astrophysics, 01 natural sciences, PRECESSING RIGID BODIES, General Relativity and Quantum Cosmology, Luminosity, NEAR-INFRARED PROPERTIES, star, Millisecond pulsar, Stars: Neutron Supporting Material: Machine-Readable Table, LIGO, 010303 astronomy & astrophysics, QC, Settore FIS/01, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], MAGNETIC-FIELD, Astrophysics::Instrumentation and Methods for Astrophysics, Pulsars: General, general | stars, Moment of inertia, gravitational wave ligo millisecond pulsar neutron star, Amplitude, pulsars: general, stars: neutron, gravitational waves, Gravitational Waves, Pulsars, General, Stars, Neutron Supporting Material, Machine-Readable Table, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - High Energy Astrophysical Phenomena, pulsar: frequency, ACCRETING NEUTRON-STAR, gr-qc, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Neutron Supporting Material: Machine-Readable Table [Stars], neutron [stars], Pulsar, GLOBULAR-CLUSTERS, 0103 physical sciences, MILLISECOND PULSARS, General, Neutron Supporting Material, STFC, Pulsars, 0105 earth and related environmental sciences, Gravitational Waves, Gravitational wave, Stars: Neutron Supporting Material: Machine-Readable Table [Gravitational Waves, Pulsars], pulsar: rotation, RCUK, Astronomy and Astrophysics, neutron | gravitational waves, Machine-Readable Table, General [Pulsars], sensitivity, Stars, moment, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], gravitational radiation: emission, Quadrupole, DISTANCE, X-RAY, pulsars, EMISSION, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We present a search for gravitational waves from 221 pulsars with rotation frequencies $\gtrsim 10$ Hz. We use advanced LIGO data from its first and second observing runs spanning 2015-2017, which provides the highest-sensitivity gravitational-wave data so far obtained. In this search we target emission from both the $l = m = 2$ mass quadrupole mode, with a frequency at twice that of the pulsar's rotation, and from the $l = 2$, $m = 1$ mode, with a frequency at the pulsar rotation frequency. The search finds no evidence for gravitational-wave emission from any pulsar at either frequency. For the $l = m = 2$ mode search, we provide updated upper limits on the gravitational-wave amplitude, mass quadrupole moment, and fiducial ellipticity for 167 pulsars, and the first such limits for a further 55. For 20 young pulsars these results give limits that are below those inferred from the pulsars' spin-down. For the Crab and Vela pulsars our results constrain gravitational-wave emission to account for less than 0.017% and 0.18% of the spin-down luminosity, respectively. For the recycled millisecond pulsar J0711-6830 our limits are only a factor of 1.3 above the spin-down limit, assuming the canonical value of $10^{38}$ kg m$^2$ for the star's moment of inertia, and imply a gravitational-wave-derived upper limit on the star's ellipticity of $1.2\!\times\!10^{-8}$. We also place new limits on the emission amplitude at the rotation frequency of the pulsars., Comment: Main paper: 39 pages, 9 figures, 2 tables. Accepted for publication in The Astrophysical Journal. Results from the tables are contained in the ancillary file Erratum: 11 pages, 4 figures, 1 table
Published: 2019

45. Long-term scintillation studies of EPTA pulsars I. Observations and basic results

Author: Yulan Liu, Joris P. W. Verbiest, Robert A. Main, Ziwei Wu, Krishnakumar Moochickal Ambalappat, David J. Champion, Ismaël Cognard, Lucas Guillemot, Madhuri Gaikwad, Gemma H. Janssen, Michael Kramer, Michael J. Keith, Ramesh Karuppusamy, Lars Künkel, Kuo Liu, James W. McKee, Mitchell B. Mickaliger, Ben W. Stappers, Golam. M. Shaifullah, Gilles Theureau, Liu, Y, Verbiest, J, Main, R, Wu, Z, Ambalappat, K, Champion, D, Cognard, I, Guillemot, L, Gaikwad, M, Janssen, G, Kramer, M, Keith, M, Karuppusamy, R, Künkel, L, Liu, K, Mckee, J, Mickaliger, M, Stappers, B, Shaifullah, G, and Theureau, G
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Astronomy, pulsars: general, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, ISM: general
Abstract: Interstellar scintillation analysis of pulsars allows us to probe the small-scale distribution and inhomogeneities of the ionized interstellar medium. Our priority is to present the data set and the basic measurements of scintillation parameters of pulsars employing long-term scintillation observations carried out from 2011 January to 2020 August by the European Pulsar Timing Array radio telescopes in the 21-cm and 11-cm bands. Additionally, we aim to identify future possible lines of study using this long-term scintillation dataset. We present the long-term time series of $\nu_{\rm d}$ and $\tau_{\rm d}$ for 13 pulsars. Sanity-checks and comparisons indicate that the scintillation parameters of our work and previously published works are mostly consistent. For two pulsars, PSRs~J1857+0943 and J1939+2134, we were able to obtain measurements of the $\nu_{\rm d}$ at both bands, which allows us to derive the time series of frequency scaling indices with a mean and a standard deviation of 2.82$\pm$1.95 and 3.18$\pm$0.60, respectively. We found some interesting features which will be studied in more detail in subsequent papers in this series: (i) in the time series of PSR~J1939+2134, where the scintillation bandwidth sharply increases or decreases associated with a sharp change of dispersion measure; (ii) PSR~J0613$-$0200 and PSR~J0636+5126 show a strong annual variation in the time series of the $\tau_{\rm d}$; (iii) PSR~J1939+2134 shows a weak anti-correlation between scintillation timescale and dispersion in WSRT data., Comment: 18 pages, 6 figures, 4 tables, accepted for publication in A&A
Published: 2022

46. The Second Fermi Large Area Telescope Catalog of Gamma-ray Pulsars

Author: G. Busetto, Brian L Winer, John J. Ruan, A. A. Moiseev, Eric Charles, Steven Ritz, D. J. Suson, Luca Baldini, Simon Johnston, F. Loparco, N. Renault, W. Mitthumsiri, Na Wang, Sylvain Guiriec, I. A. Grenier, James Chiang, Jeffrey D. Scargle, Roger W. Romani, Jürgen Knödlseder, S. Germani, K. S. Wood, P. Lubrano, M. Marelli, Jayashree Roy, R. Buehler, Jun Kataoka, Gloria Spandre, Ronaldo Bellazzini, A. S. Johnson, S. Cutini, Michael Kramer, T. Ohsugi, Eleonora Troja, Miranda Jackson, Maura McLaughlin, T. Reposeur, Peter F. Michelson, Marcello Giroletti, Francesco Longo, R. C. G. Chaves, Yasunobu Uchiyama, Johann Cohen-Tanugi, M. Orienti, Alex Drlica-Wagner, Dario Gasparrini, M. Hayashida, Sylvain Chaty, Nanda Rea, E. D. Bloom, Jean Ballet, A. Morselli, Xian Hou, V. Vitale, T. Jogler, Charles D. Dermer, R. N. Manchester, D. Parent, M. E. Monzani, Andrea Belfiore, Stefano Ciprini, Bhaswati Bhattacharyya, Gemma H. Janssen, R. Rousseau, J. Lande, Scott M. Ransom, Michael Keith, Luca Latronico, P. R. den Hartog, Gino Tosti, M. Mayer, Francesco Massaro, R. E. Hughes, A. W. Chen, A. B. Hill, L. R. Cominsky, Igor V. Moskalenko, Melissa Pesce-Rollins, J. G. Thayer, M. Burgay, Elisabetta Bissaldi, Olaf Reimer, Paul S. Ray, Holger J. Pletsch, M. Tinivella, T. L. Usher, M. E. DeCesar, Jason W. T. Hessels, Paulo C. C. Freire, G. A. Caliandro, Jan Conrad, Elizabeth C. Ferrara, Takeshi Nakamori, J. M. Casandjian, Terri Brandt, Hiromitsu Takahashi, André Schulz, Patrick Weltevrede, Andrew W. Strong, M. N. Mazziotta, D. Dumora, C. Favuzzi, J. Mehault, Christo Venter, A. De Angelis, P. Fusco, L. Guillemot, D. J. Thompson, T. H. Burnett, Diego F. Torres, A. A. Abdo, E. Orlando, Gregory Desvignes, W. N. Johnson, Gilles Theureau, L. Tibaldo, S. Murgia, M. T. Wolff, C. Cecchi, Alberto Sartori, T. Glanzman, F. Piron, Rodrigo Nemmen, Matthew Kerr, Matthew G. Baring, D. Horan, Giacomo Vianello, Fernando Camilo, L. Di Venere, Gudlaugur Johannesson, O. Tibolla, Masanori Ohno, D. L. Wood, E. Hays, Y. Hanabata, G. Pivato, M. Roth, F. Gargano, Alice K. Harding, Ismaël Cognard, Benjamin Stappers, Justin Vandenbroucke, Emanuele Bonamente, J. F. Ormes, Eugenio Bottacini, T. A. Porter, Guido Barbiellini, E. J. Siskind, David A. Smith, L. Falletti, Denis Bastieri, R. Claus, Marianne Lemoine-Goumard, Johan Bregeon, D. Hadasch, Ryan Shannon, A. Possenti, A. Reimer, J. H. Panetta, M. Razzano, S. Rainò, Eric V. Gotthelf, Tsunefumi Mizuno, Filippo D'Ammando, Julie McEnery, T. Kamae, M. Brigida, Stephen E. Thorsett, R. P. Johnson, G. Chiaro, J. E. Grove, P. M. Saz Parkinson, J. S. Perkins, Paolo Giommi, Marco Ajello, J. B. Thayer, S. Larsson, S. Buson, Nicola Giglietto, A. De Luca, M. N. Lovellette, P. A. Caraveo, Persis S. Drell, Alice Allafort, Roberto Mignani, Tyrel J. Johnson, R. A. Cameron, A. Chekhtman, R. Dubois, W. B. Focke, P. Spinelli, Seth Digel, Francesco Giordano, John W. Hewitt, P. Bruel, V. Vasileiou, Matthew Wood, G. Godfrey, F. de Palma, Andrew Lyne, M.-H. Grondin, Robert R. Rando, M. Pierbattista, Cristobal M. Espinoza, Omer Celik, A. Franckowiak, Stefan Funk, Zhenwei Yang, Carmelo Sgrò, E. Nuss, David Paneque, M. Kuss, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Unité Scientifique de la Station de Nançay (USN), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), FERMI, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Istituto Nazionale di Fisica Nucleare, sezione di Bari (INFN, sezione di Bari), National Institute for Nuclear Physics (INFN), IEEC-CSIC, Universitat Autònoma de Barcelona [Barcelona] (UAB), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Fermi-LAT, High Energy Astrophys. & Astropart. Phys (API, FNWI), Abdo AA, Ajello M, Allafort A, Baldini L, Ballet J, Barbiellini G, Baring MG, Bastieri D, Belfiore A, Bellazzini R, Bhattacharyya B, Bissaldi E, Bloom ED, Bonamente E, Bottacini E, Brandt TJ, Bregeon J, Brigida M, Bruel P, Buehler R, Burgay M, Burnett TH, Busetto G, Buson S, Caliandro GA, Cameron RA, Camilo F, Caraveo PA, Casandjian JM, Cecchi C, Celik O, Charles E, Chaty S, Chaves RCG, Chekhtman A, Chen AW, Chiang J, Chiaro G, Ciprini S, Claus R, Cognard I, Cohen-Tanugi J, Cominsky LR, Conrad J, Cutini S, DAmmando F, De Angelis A, DeCesar ME, De Luca A, Den Hartog PR, De Palma F, Dermer CD, Desvignes G, Digel SW, Di Venere L, Drell PS, Drlica-Wagner A, Dubois R, Dumora D, Espinoza CM, Falletti L, Favuzzi C, Ferrara EC, Focke WB, Franckowiak A, Freire PCC, Funk S, Fusco P, Gargano F, Gasparrini D, Germani S, Giglietto N, Giommi P, Giordano F, Giroletti M, Glanzman T, Godfrey G, Gotthelf EV, Grenier IA, Grondin MH, Grove JE, Guillemot L, Guiriec S, Hadasch D, Hanabata Y, Harding AK, Hayashida M, Hays E, Hessels J, Hewitt J, Hill AB, Horan D, Hou X, Hughes RE, Jackson MS, Janssen GH, Jogler T, Johannesson G, Johnson RP, Johnson AS, Johnson TJ, Johnson WN, Johnston S, Kamae T, Kataoka J, Keith M, Kerr M, Knodlseder J, Kramer M, Kuss M, Lande J, Larsson S, Latronico L, Lemoine-Goumard M, Longo F, Loparco F, Lovellette MN, Lubrano P, Lyne AG, Manchester RN, Marelli M, Massaro F, Mayer M, Mazziotta MN, McEnery JE, McLaughlin MA, Mehault J, Michelson PF, Mignani RP, Mitthumsiri W, Mizuno T, Moiseev AA, Monzani ME, Morselli A, Moskalenko IV, Murgia S, Nakamori T, Nemmen R, Nuss E, Ohno M, Ohsugi T, Orienti M, Orlando E, Ormes JF, Paneque D, Panetta JH, Parent D, Perkins JS, Pesce-Rollins M, Pierbattista M, Piron F, Pivato G, Pletsch HJ, Porter TA, Possenti A, Raino S, Rando R, Ransom SM, Ray PS, Razzano M, Rea N, Reimer A, Reimer O, Renault N, Reposeur T, Ritz S, Romani RW, Roth M, Rousseau R, Roy J, Ruan J, Sartori A, Parkinson PMS, Scargle JD, Schulz A, Sgro C, Shannon R, Siskind EJ, Smith DA, Spandre G, Spinelli P, Stappers BW, Strong AW, Suson DJ, Takahashi H, Thayer JG, Thayer JB, Theureau G, Thompson DJ, Thorsett SE, Tibaldo L, Tibolla O, Tinivella M, Torres DF, Tosti G, Troja E, Uchiyama Y, Usher TL, Vandenbroucke J, Vasileiou V, Venter C, Vianello G, Vitale V, Wang N, Weltevrede P, Winer BL, Wolff MT, Wood DL, Wood KS, Wood M, Yang Z, Abdo, A. A., Ajello, M., Allafort, A., Baldini, L., Ballet, J., BARBIELLINI AMIDEI, Guido, Baring, M. G., Bastieri, D., Belfiore, A., Bellazzini, R., Bhattacharyya, B., Bissaldi, Elisabetta, Bloom, E. D., Bonamente, E., Bottacini, E., Brandt, T. J., Bregeon, J., Brigida, M., Bruel, P., Buehle, R., Burgay, M., Burnett, T. H., Busetto, G., Buson, S., Caliandro, G. A., Cameron, R. A., Camilo, F., Caraveo, P. A., Casandjian, J. M., Cecchi, C., Çelik, Ö., Charles, E., Chaty, S., Chaves, R. C. G., Chekhtman, A., Chen, A. W., Chiang, J., Chiaro, G., Ciprini, S., Claus, R., Cognard, I., Cohen Tanugi, J., Cominsky, L. R., Conrad, J., Cutini, S., D'Ammando, F., de Angelis, A., Decesar, M. E., De Luca, A., den Hartog, P. R., de Palma, F., Dermer, C. D., Desvignes, G., Digel, S. W., Di Venere, L., Drell, P. S., Drlica Wagner, A., Dubois, R., Dumora, D., Espinoza, C. M., Falletti, L., Favuzzi, C., Ferrara, E. C., Focke, W. B., Franckowiak, A., Freire, P. C. C., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Germani, S., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Gotthelf, E. V., Grenier, I. A., Grondin, M. H., Grove, J. E., Guillemot, L., Guiriec, S., Hadasch, D., Hanabata, Y., Harding, A. K., Hayashida, M., Hays, E., Hessels, J., Hewitt, J., Hill, A. B., Horan, D., Hou, X., Hughes, R. E., Jackson, M. S., Janssen, G. H., Jogler, T., Jóhannesson, G., Johnson, R. P., Johnson, A. S., Johnson, T. J., Johnson, W. N., Johnston, S., Kamae, T., Kataoka, J., Keith, M., Kerr, M., Knödlseder, J., Kramer, M., Kuss, M., Lande, J., Larsson, S., Latronico, L., Lemoine Goumard, M., Longo, Francesco, Loparco, F., Lovellette, M. N., Lubrano, P., Lyne, A. G., Manchester, R. N., Marelli, M., Massaro, F., Mayer, M., Mazziotta, M. N., Mcenery, J. E., Mclaughlin, M. A., Mehault, J., Michelson, P. F., Mignani, R. P., Mitthumsiri, W., Mizuno, T., Moiseev, A. A., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nakamori, T., Nemmen, R., Nuss, E., Ohno, M., Ohsugi, T., Orienti, M., Orlando, E., Ormes, J. F., Paneque, D., Panetta, J. H., Parent, D., Perkins, J. S., Pesce Rollins, M., Pierbattista, M., Piron, F., Pivato, G., Pletsch, H. J., Porter, T. A., Possenti, A., Rainò, S., Rando, R., Ransom, S. M., Ray, P. S., Razzano, M., Rea, N., Reimer, A., Reimer, O., Renault, N., Reposeur, T., Ritz, S., Romani, R. W., Roth, M., Rousseau, R., Roy, J., Ruan, J., Sartori, A., Saz Parkinson, P. M., Scargle, J. D., Schulz, A., Sgrò, C., Shannon, R., Siskind, E. J., Smith, D. A., Spandre, G., Spinelli, P., Stappers, B. W., Strong, A. W., Suson, D. J., Takahashi, H., Thayer, J. G., Thayer, J. B., Theureau, G., Thompson, D. J., Thorsett, S. E., Tibaldo, L., Tibolla, O., Tinivella, M., Torres, D. F., Tosti, G., Troja, E., Uchiyama, Y., Usher, T. L., Vandenbroucke, J., Vasileiou, V., Venter, C., Vianello, G., Vitale, V., Wang, N., Weltevrede, P., Winer, B. L., Wolff, M. T., Wood, D. L., Wood, K. S., Wood, M., and Yang, Z.
Subjects: Catalogs pulsars, general stars, neutron, catalog, CRAB PULSAR, Astrophysics, 01 natural sciences, Pulsar wind nebula, general [pulsars], law.invention, neutron, Millisecond pulsar, law, catalogs, pulsars: general, stars: neutron, 010303 astronomy & astrophysics, general stars, Physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::Instrumentation and Methods for Astrophysics, WIND NEBULA, SUPERNOVA REMNANT G21.5-0.9, Astrophysics - High Energy Astrophysical Phenomena, PHOTON IMAGING CAMERA, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], WHITE-DWARF COMPANION, MIDDLE-AGED PULSAR, DEEP OPTICAL OBSERVATIONS, NANCAY RADIO TELESCOPE, MILLISECOND PULSARS, LIGHT CURVES, Astrophysics::High Energy Astrophysical Phenomena, Catalogs pulsars, Astrophysics::Cosmology and Extragalactic Astrophysics, catalogs , pulsars: general , stars: neutron, Telescope, neutron [stars], Pulsar, 0103 physical sciences, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Crab Pulsar, catalogs – pulsars: general – stars: neutron, Astronomy, Astronomy and Astrophysics, Neutron star, Space and Planetary Science, ddc:520, X-ray pulsar, Fermi Gamma-ray Space Telescope
Abstract: This catalog summarizes 117 high-confidence > 0.1 GeV gamma-ray pulsar detections using three years of data acquired by the Large Area Telescope (LAT) on the Fermi satellite. Half are neutron stars discovered using LAT data, through periodicity searches in gamma-ray and radio data around LAT unassociated source positions. The 117 pulsars are evenly divided into three groups: millisecond pulsars, young radio-loud pulsars, and young radio-quiet pulsars. We characterize the pulse profiles and energy spectra and derive luminosities when distance information exists. Spectral analysis of the off-peak phase intervals indicates probable pulsar wind nebula emission for four pulsars, and off-peak magnetospheric emission for several young and millisecond pulsars. We compare the gamma-ray properties with those in the radio, optical, and X-ray bands. We provide flux limits for pulsars with no observed gamma-ray emission, highlighting a small number of gamma-faint, radio-loud pulsars. The large, varied gamma-ray pulsar sample constrains emission models. Fermi's selection biases complement those of radio surveys, enhancing comparisons with predicted population distributions., Comment: 145 pages. Online files at http://fermi.gsfc.nasa.gov/ssc/data/access/lat/2nd_PSR_catalog/ A typo in the value of the photon flux for CTA 1 (PSR J0007+7303) has been corrected in Table 9. NASA ADS at http://cdsads.u-strasbg.fr/abs/2013ApJS..208...17A
Published: 2013

47. The International Pulsar Timing Array second data release: Search for an isotropic gravitational wave background

Author: J Antoniadis, Z Arzoumanian, S Babak, M Bailes, A-S Bak Nielsen, P T Baker, C G Bassa, B Bécsy, A Berthereau, M Bonetti, A Brazier, P R Brook, M Burgay, S Burke-Spolaor, R N Caballero, J A Casey-Clyde, A Chalumeau, D J Champion, M Charisi, S Chatterjee, S Chen, I Cognard, J M Cordes, N J Cornish, F Crawford, H T Cromartie, K Crowter, S Dai, M E DeCesar, P B Demorest, G Desvignes, T Dolch, B Drachler, M Falxa, E C Ferrara, W Fiore, E Fonseca, J R Gair, N Garver-Daniels, B Goncharov, D C Good, E Graikou, L Guillemot, Y J Guo, J S Hazboun, G Hobbs, H Hu, K Islo, G H Janssen, R J Jennings, A D Johnson, M L Jones, A R Kaiser, D L Kaplan, R Karuppusamy, M J Keith, L Z Kelley, M Kerr, J S Key, M Kramer, M T Lam, W G Lamb, T J W Lazio, K J Lee, L Lentati, K Liu, J Luo, R S Lynch, A G Lyne, D R Madison, R A Main, R N Manchester, A McEwen, J W McKee, M A McLaughlin, M B Mickaliger, C M F Mingarelli, C Ng, D J Nice, S Osłowski, A Parthasarathy, T T Pennucci, B B P Perera, D Perrodin, A Petiteau, N S Pol, N K Porayko, A Possenti, S M Ransom, P S Ray, D J Reardon, C J Russell, A Samajdar, L M Sampson, S Sanidas, J M Sarkissian, K Schmitz, L Schult, A Sesana, G Shaifullah, R M Shannon, B J Shapiro-Albert, X Siemens, J Simon, T L Smith, L Speri, R Spiewak, I H Stairs, B W Stappers, D R Stinebring, J K Swiggum, S R Taylor, G Theureau, C Tiburzi, M Vallisneri, E van der Wateren, A Vecchio, J P W Verbiest, S J Vigeland, H Wahl, J B Wang, J Wang, L Wang, C A Witt, S Zhang, X J Zhu, Antoniadis, J, Arzoumanian, Z, Babak, S, Bailes, M, Bak Nielsen, A, Baker, P, Bassa, C, Becsy, B, Berthereau, A, Bonetti, M, Brazier, A, Brook, P, Burgay, M, Burke-Spolaor, S, Caballero, R, Casey-Clyde, J, Chalumeau, A, Champion, D, Charisi, M, Chatterjee, S, Chen, S, Cognard, I, Cordes, J, Cornish, N, Crawford, F, Cromartie, H, Crowter, K, Dai, S, Decesar, M, Demorest, P, Desvignes, G, Dolch, T, Drachler, B, Falxa, M, Ferrara, E, Fiore, W, Fonseca, E, Gair, J, Garver-Daniels, N, Goncharov, B, Good, D, Graikou, E, Guillemot, L, Guo, Y, Hazboun, J, Hobbs, G, Hu, H, Islo, K, Janssen, G, Jennings, R, Johnson, A, Jones, M, Kaiser, A, Kaplan, D, Karuppusamy, R, Keith, M, Kelley, L, Kerr, M, Key, J, Kramer, M, Lam, M, Lamb, W, Lazio, T, Lee, K, Lentati, L, Liu, K, Luo, J, Lynch, R, Lyne, A, Madison, D, Main, R, Manchester, R, Mcewen, A, Mckee, J, Mclaughlin, M, Mickaliger, M, Mingarelli, C, Ng, C, Nice, D, Oslowski, S, Parthasarathy, A, Pennucci, T, Perera, B, Perrodin, D, Petiteau, A, Pol, N, Porayko, N, Possenti, A, Ransom, S, Ray, P, Reardon, D, Russell, C, Samajdar, A, Sampson, L, Sanidas, S, Sarkissian, J, Schmitz, K, Schult, L, Sesana, A, Shaifullah, G, Shannon, R, Shapiro-Albert, B, Siemens, X, Simon, J, Smith, T, Speri, L, Spiewak, R, Stairs, I, Stappers, B, Stinebring, D, Swiggum, J, Taylor, S, Theureau, G, Tiburzi, C, Vallisneri, M, Van Der Wateren, E, Vecchio, A, Verbiest, J, Vigeland, S, Wahl, H, Wang, J, Wang, L, Witt, C, Zhang, S, Zhu, X, 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), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), 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 Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire Univers et Théories (LUTH (UMR_8102)), ANR-18-CE31-0015,PTA-France,Recherche d'ondes gravitationnelles avec un réseau de pulsars en France(2018), ITA, USA, GBR, FRA, DEU, AUS, CAN, GRC, NLD, CHN, RUS, CHE, and HUN
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, [PHYS]Physics [physics], Astrophysics and Astronomy, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, methods: Data analysi, pulsars: General, methods: data analysis, gravitational waves, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), gravitational wave, astro-ph.IM
Abstract: We searched for an isotropic stochastic gravitational wave background in the second data release of the International Pulsar Timing Array, a global collaboration synthesizing decadal-length pulsar-timing campaigns in North America, Europe, and Australia. In our reference search for a power law strain spectrum of the form $h_c = A(f/1\,\mathrm{yr}^{-1})^{\alpha}$, we found strong evidence for a spectrally-similar low-frequency stochastic process of amplitude $A = 3.8^{+6.3}_{-2.5}\times10^{-15}$ and spectral index $\alpha = -0.5 \pm 0.5$, where the uncertainties represent 95\% credible regions, using information from the auto- and cross-correlation terms between the pulsars in the array. For a spectral index of $\alpha = -2/3$, as expected from a population of inspiralling supermassive black hole binaries, the recovered amplitude is $A = 2.8^{+1.2}_{-0.8}\times10^{-15}$. Nonetheless, no significant evidence of the Hellings-Downs correlations that would indicate a gravitational-wave origin was found. We also analyzed the constituent data from the individual pulsar timing arrays in a consistent way, and clearly demonstrate that the combined international data set is more sensitive. Furthermore, we demonstrate that this combined data set produces comparable constraints to recent single-array data sets which have more data than the constituent parts of the combination. Future international data releases will deliver increased sensitivity to gravitational wave radiation, and significantly increase the detection probability., 17 pages, 12 figures, accepted in MNRAS
Published: 2022

48. Robust parameter estimation from pulsar timing data

Author: A Samajdar, G Shaifullah, A Sesana, J Antoniadis, M Burgay, S Chen, I Cognard, L Guillemot, M Kramer, J W McKee, M B Mickaliger, G Theureau, E Van&nbsp, derundefined Wateren, Samajdar, A, Shaifullah, G, Sesana, A, Antoniadis, J, Burgay, M, Chen, S, Cognard, I, Guillemot, L, Kramer, M, W McKee, J, B Mickaliger, M, Theureau, G, Van&nbsp, E, and Wateren, D
Subjects: Space and Planetary Science, pulsars: general, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, General Relativity and Quantum Cosmology (gr-qc), gravitational wave, methods: data analysi, General Relativity and Quantum Cosmology
Abstract: Recently, global pulsar timing arrays have released results from searching for a nano-Hertz gravitational wave background signal. Although there has not been any definite evidence of the presence of such a signal in residuals of pulsar timing data yet, with more and improved data in future, a statistically significant detection is expected to be made. Stochastic algorithms are used to sample a very large parameter space to infer results from data. In this paper, we attempt to rule out effects arising from the stochasticity of the sampler in the inference process. We compare different configurations of nested samplers and the more commonly used markov chain monte carlo method to sample the pulsar timing array parameter space and account for times taken by the different samplers on same data. Although we obtain consistent results on parameters from different sampling algorithms, we propose two different samplers for robustness checks on data in the future to account for cross-checks between sampling methods as well as realistic run-times., Comment: 8 pages, 5 figures, 4 tables
Published: 2022

49. A comparative analysis of pulse time-of-arrival creation methods

Author: J. Wang, G. M. Shaifullah, J. P. W. Verbiest, C. Tiburzi, D. J. Champion, I. Cognard, M. Gaikwad, E. Graikou, L. Guillemot, H. Hu, R. Karuppusamy, M. J. Keith, M. Kramer, Y. Liu, A. G. Lyne, M. B. Mickaliger, B. W. Stappers, G. Theureau, Wang, J, Shaifullah, G, Verbiest, J, Tiburzi, C, Champion, D, Cognard, I, Gaikwad, M, Graikou, E, Guillemot, L, Hu, H, Karuppusamy, R, Keith, M, Kramer, M, Liu, Y, Lyne, A, Mickaliger, M, Stappers, B, Theureau, G, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), 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 Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Laboratoire Univers et Théories (LUTH (UMR_8102)), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, Pulsars: general, Computer Science::Systems and Control, Space and Planetary Science, Physics::Space Physics, 0103 physical sciences, [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), 010303 astronomy & astrophysics, Methods: data analysi
Abstract: Context.Extracting precise pulse times of arrival (TOAs) and their uncertainties is the first and most fundamental step in high-precision pulsar timing. In the classical method, TOAs are derived from total intensity pulse profiles of pulsars via cross-correlation with an idealised 1D template of that profile. While a number of results have been presented in the literature that rely on the ever increasing sensitivity of these pulsar timing experiments, there is no consensus on the most reliable methods for creating TOAs, and, more importantly, on the associated TOA uncertainties for each scheme.Aims.We present a comprehensive comparison of TOA determination practices. We focus on creating timing templates, TOA determination methods, and the most useful TOA bandwidth. The aim is to present a possible approach towards TOA optimisation, the (partial) identification of an optimal TOA-creation scheme, and the demonstration of optimisation differences between pulsars and data sets.Methods.We compared the values of data-derived template profiles with analytic profiles and evaluated the three most commonly used template-matching methods. Finally, we studied the relation between timing precision and TOA bandwidth to identify any potential breaks in this relation. As a practical demonstration, we applied our selected methods to European Pulsar Timing Array data on three test pulsars, PSRs J0218+4232, J1713+0747, and J2145−0750.Results.Our demonstration shows that data-derived and smoothed templates are typically preferred to some more commonly applied alternatives. The template-matching method called Fourier domain with Markov chain Monte Carlo is generally superior to or competitive with other methods. While the optimal TOA bandwidth is strongly dependent on pulsar brightness, telescope sensitivity, and scintillation properties, some significant frequency averaging seems required for the data we investigated.
Published: 2022

50. Common-red-signal analysis with 24-yr high-precision timing of the European Pulsar Timing Array: inferences in the stochastic gravitational-wave background search

Author: Cees Bassa, J. W. McKee, A.-S. Bak Nielsen, E. van der Wateren, J. Wang, Antoine Petiteau, Andrea Possenti, Mitchell B. Mickaliger, Alberto Sesana, Kejia Lee, Delphine Perrodin, E. Graikou, Lan Wang, A. Chalumeau, R. N. Caballero, Kang Liu, Caterina Tiburzi, N. K. Porayko, Siyuan Chen, H. Xu, Alberto Vecchio, H. Hu, M. Falxa, Gemma H. Janssen, X. J. Liu, Ramesh Karuppusamy, John Antoniadis, David Champion, Ismaël Cognard, Michael Kramer, Benetge Perera, Gregory Desvignes, Stanislav Babak, Aditya Parthasarathy, Gilles Theureau, Y J Guo, L. Speri, Lucas Guillemot, Robert D. Ferdman, S. A. Sanidas, Paulo C. C. Freire, Michael Keith, Ben Stappers, J. Jang, Jonathan R. Gair, A. Berthereau, Andrew Lyne, G. Shaifullah, A. Samajdar, R. A. Main, M. Burgay, Joris P. W. Verbiest, RUS, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), 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 Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), 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 de Paris (UP), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), ANR-18-CE31-0015,PTA-France,Recherche d'ondes gravitationnelles avec un réseau de pulsars en France(2018), Chen, S, Caballero, R, Guo, Y, Chalumeau, A, Liu, K, Shaifullah, G, Lee, K, Babak, S, Desvignes, G, Parthasarathy, A, Hu, H, Van Der Wateren, E, Antoniadis, J, Bak Nielsen, A, Bassa, C, Berthereau, A, Burgay, M, Champion, D, Cognard, I, Falxa, M, Ferdman, R, Freire, P, Gair, J, Graikou, E, Guillemot, L, Jang, J, Janssen, G, Karuppusamy, R, Keith, M, Kramer, M, Liu, X, Lyne, A, Main, R, Mckee, J, Mickaliger, M, Perera, B, Perrodin, D, Petiteau, A, Porayko, N, Possenti, A, Samajdar, A, Sanidas, S, Sesana, A, Speri, L, Stappers, B, Theureau, G, Tiburzi, C, Vecchio, A, Verbiest, J, Wang, J, Wang, L, and Xu, H
Subjects: Spatial correlation, General relativity, Astronomy, Astrophysics, 01 natural sciences, Gravitational wave background, Pulsar, Millisecond pulsar, pulsars: general, 0103 physical sciences, gravitational wave, 010303 astronomy & astrophysics, Physics, Spectral index, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, methods: data analysis, European Pulsar Timing Array, Amplitude, gravitational waves, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics - High Energy Astrophysical Phenomena, methods: data analysi, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present results from the search for a stochastic gravitational-wave background (GWB) as predicted by the theory of General Relativity using six radio millisecond pulsars from the Data Release 2 (DR2) of the European Pulsar Timing Array (EPTA) covering a timespan up to 24 years. A GWB manifests itself as a long-term low-frequency stochastic signal common to all pulsars, a common red signal (CRS), with the characteristic Hellings-Downs (HD) spatial correlation. Our analysis is performed with two independent pipelines, \eprise{} and \tn{}+\ftwo{}, which produce consistent results. A search for a CRS with simultaneous estimation of its spatial correlations yields spectral properties compatible with theoretical GWB predictions, but does not result in the required measurement of the HD correlation, as required for GWB detection. Further Bayesian model comparison between different types of CRSs, including a GWB, finds the most favoured model to be the common uncorrelated red noise described by a power-law with $A = 5.13_{-2.73}^{+4.20} \times 10^{-15}$ and $\gamma = 3.78_{-0.59}^{+0.69}$ (95\% credible regions). Fixing the spectral index to $\gamma=13/3$ as expected from the GWB by circular, inspiralling supermassive black-hole binaries results in an amplitude of $A =2.95_{-0.72}^{+0.89} \times 10^{-15}$. We implement three different models, BAYESEPHEM, LINIMOSS and EPHEMGP, to address possible Solar-system ephemeris (SSE) systematics and conclude that our results may only marginally depend on these effects. This work builds on the methods and models from the studies on the EPTA DR1. We show that under the same analysis framework the results remain consistent after the data set extension., Comment: 25 pages, 10 figures, 7 tables, 2 appendix tables and 1 appendix figure
Published: 2021

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