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1. Propagation effects at low frequencies seen in the LOFAR long-term monitoring of the periodically active FRB 20180916B

Author

Gopinath, A., Bassa, C. G., Pleunis, Z., Hessels, J. W. T., Chawla, P., Keane, E. F., Kondratiev, V., Michilli5, D., and Nimmo, K.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract

LOFAR (LOw Frequency ARray) has previously detected bursts from the periodically active, repeating fast radio burst (FRB) source FRB 20180916B down to unprecedentedly low radio frequencies of 110 MHz. Here we present 11 new bursts in 223 more hours of continued monitoring of FRB 20180916B in the 110-188 MHz LOFAR band. We place new constraints on the LOFAR activity width $w = 4.3^{+0.7}_{-0.2}$ day, and phase centre $\phi_{\mathrm{c}}^{\mathrm{LOFAR}} = 0.67^{+0.03}_{-0.02}$ in its 16.33-day activity cycle, strengthening the evidence for its frequency-dependent activity cycle. Propagation effects like Faraday rotation and scattering are especially pronounced at low frequencies and constrain properties of FRB 20180916B's local environment. We track variations in scattering and time-frequency drift rates, and find no evidence for trends in time or activity phase. Faraday rotation measure (RM) variations seen between June 2021 and August 2022 show a fractional change $>$50% with hints of flattening of the gradient of the previously reported secular trend seen at 600 MHz. The frequency-dependent window of activity at LOFAR appears stable despite the significant changes in RM, leading us to deduce that these two effects have different causes. Depolarization of and within individual bursts towards lower radio frequencies is quantified using LOFAR's large fractional bandwidth, with some bursts showing no detectable polarization. However, the degree of depolarization seems uncorrelated to the scattering timescales, allowing us to evaluate different depolarization models. We discuss these results in the context of models that invoke rotation, precession, or binary orbital motion to explain the periodic activity of FRB 20180916B., Comment: 17 pages, 10 figures, Submitted to MNRAS

Published
2023
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2. Searching for FRB persistent radio source counterparts in dwarf galaxies using LOFAR

Author

Vohl, D., Vedantham, H . K., Hessels, J. W. T., and Bassa, C. G.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The repeating FRB 20121102A was localized to a star-forming region in a dwarf galaxy and found to be co-located with a persistent radio source (PRS). FRB 20190520B is only the second known source sharing phenomenology akin to FRB 20121102A's, with similar burst activity, host galaxy properties, as well as being associated with a PRS. PRS emission is potentially a calorimeter, allowing us to estimate the energy output of the central FRB engine. Independently of FRB studies, PRSs have been found in dwarf galaxies and interpreted as intermediate mass black holes. To improve our understanding of such sources associated with dwarf galaxies, it is imperative to increase the known sample size. Here, we present a search for compact radio sources coincident with dwarf galaxies, discuss source candidates and planned strategies to differentiate them between candidate FRB hosts and intermediate mass black holes., Comment: To appear in the proceedings of "IAUS 369: The dawn of cosmology & multi-messenger studies with fast radio bursts" eds: E.F. Keane, A. Fialkov, K.M. Rajwade & C.R.H. Walker

Published
2023
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3. PRECISE localizations of repeating Fast Radio Bursts

Author

Marcote, B., Kirsten, F., Hessels, J. W. T., Nimmo, K., and Paragi, Z.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Fast Radio Bursts (FRBs) are extremely luminous and brief signals (with duration of milliseconds or even shorter) of extragalactic origin. Despite the fact that hundreds of FRBs have been discovered to date, their nature still remains unclear. Precise localizations of FRBs can unveil their host galaxies and local environments -- and thus shed light on the physical processes that led to the burst production. However, this has only been achieved for a few FRBs to date. The European VLBI Network (EVN) is currently the only instrument capable of localizing FRBs down to the milliarcsecond level. This level of precision was critical to associate the first localized FRB, 20121102A, to a star-forming region in a low-metallicity dwarf galaxy and physically related it to a compact persistent radio source. Analogously, a second repeating FRB, 20180916B, was found to just outside the edge of a prominent star-forming region of a nearby spiral galaxy. The PRECISE project (Pinpointing REpeating ChIme Sources with EVN dishes), starting from 2019, has observed hundreds of hours per year with a subset of EVN telescopes with the goal of localizing repeating FRBs discovered by the CHIME/FRB Collaboration. The ultimate goal of PRECISE is to disentangling the environments where FRBs can be produced. Here we present the state of the art of the FRB field, the PRECISE project, and the localizations achieved until now, which have unveiled a variety of environments where FRBs can be found that challenges the current models., Comment: 8 pages, 1 figure, to appear in the proceedings of the European VLBI Network Mini-Symposium and Users' Meeting 2021, Proceedings of Science, PoS(EVN2021)035

Published
2022
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4. Burst timescales and luminosities link young pulsars and fast radio bursts

Author

Nimmo, K., Hessels, J. W. T., Kirsten, F., Keimpema, A., Cordes, J. M., Snelders, M. P., Hewitt, D. M., Karuppusamy, R., Archibald, A. M., Bezukovs, V., Bhardwaj, M., Blaauw, R., Buttaccio, S. T., Cassanelli, T., Conway, J. E., Corongiu, A., Feiler, R., Fonseca, E., Forssen, O., Gawronski, M., Giroletti, M., Kharinov, M. A., Leung, C., Lindqvist, M., Maccaferri, G., Marcote, B., Masui, K. W., Mckinven, R., Melnikov, A., Michilli, D., Mikhailov, A., Ng, C., Orbidans, A., Ould-Boukattine, O. S., Paragi, Z., Pearlman, A. B., Petroff, E., Rahman, M., Scholz, P., Shin, K., Smith, K. M., Stairs, I. H., Surcis, G., Tendulkar, S. P., Vlemmings, W., Wang, N., Yang, J., and Yuan, J.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

Fast radio bursts (FRBs) are extragalactic radio flashes of unknown physical origin. Their high luminosities and short durations require extreme energy densities, like those found in the vicinity of neutron stars and black holes. Studying the burst intensities and polarimetric properties on a wide range of timescales, from milliseconds down to nanoseconds, is key to understanding the emission mechanism. However, high-time-resolution studies of FRBs are limited by their unpredictable activity levels, available instrumentation and temporal broadening in the intervening ionised medium. Here we show that the repeating FRB 20200120E can produce isolated shots of emission as short as about 60 nanoseconds in duration, with brightness temperatures as high as $3\times 10^{41}$ K (excluding relativistic effects), comparable to `nano-shots' from the Crab pulsar. Comparing both the range of timescales and luminosities, we find that FRB 20200120E observationally bridges the gap between known Galactic young pulsars and magnetars, and the much more distant extragalactic FRBs. This suggests a common magnetically powered emission mechanism spanning many orders of magnitude in timescale and luminosity. In this work, we probe a relatively unexplored region of the short-duration transient phase space; we highlight that there likely exists a population of ultra-fast radio transients at nanosecond to microsecond timescales, which current FRB searches are insensitive to., Comment: Submitted. Comments welcome

Published
2021
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5. Highly polarised microstructure from the repeating FRB 20180916B

Author

Nimmo, K., Hessels, J. W. T., Keimpema, A., Archibald, A. M., Cordes, J. M., Karuppusamy, R., Kirsten, F., Li, D. Z., Marcote, B., and Paragi, Z.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

Fast radio bursts (FRBs) are bright, coherent, short-duration radio transients of as-yet unknown extragalactic origin. FRBs exhibit a wide variety of spectral, temporal and polarimetric properties, which can unveil clues into their emission physics and propagation effects in the local medium. Here we present the high-time-resolution (down to 1 $\mu$s) polarimetric properties of four 1.7-GHz bursts from the repeating FRB 20180916B, which were detected in voltage data during observations with the European VLBI Network (EVN). We observe a range of emission timescales spanning three orders of magnitude, with the shortest component width reaching 3-4 $\mu$s (below which we are limited by scattering). This is the shortest timescale measured in any FRB, to date. We demonstrate that all four bursts are highly linearly polarised ($\gtrsim 80\%$), show no evidence for significant circular polarisation ($\lesssim 15\%$), and exhibit a constant polarisation position angle (PPA) during and between bursts. On short timescales ($\lesssim 100$ $\mu$s), however, there appear to be subtle (few degree) PPA variations across the burst profiles. These observational results are most naturally explained in an FRB model where the emission is magnetospheric in origin, as opposed to models where the emission originates at larger distances in a relativistic shock., Comment: Submitted; comments welcome

Published
2020
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6. LOFAR discovery of a 23.5-second radio pulsar

Author

Tan, C. M., Bassa, C. G., Cooper, S., Dijkema, T. J., Esposito, P., Hessels, J. W. T., Kondratiev, V. I., Kramer, M., Michilli, D., Sanidas, S., Shimwell, T. W., Stappers, B. W., van Leeuwen, J., Cognard, I., Grießmeier, J. -M., Karastergiou, A., Keane, E. F., Sobey, C., and Weltevrede, P.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

We present the discovery of PSR J0250+5854, a radio pulsar with a spin period of 23.5 s. This is the slowest-spinning radio pulsar known. PSR J0250+5854 was discovered by the LOFAR Tied-Array All-Sky Survey (LOTAAS), an all-Northern-sky survey for pulsars and fast transients at a central observing frequency of 135 MHz. We subsequently detected pulsations from the pulsar in the interferometric images of the LOFAR Two-metre Sky Survey, allowing for sub-arcsecond localization. This, along with a pre-discovery detection 2 years prior, allowed us to measure the spin-period derivative to be $\dot{P}=2.7 \times 10^{-14}$ s s$^{-1}$. The observed spin period derivative of PSR J0250+5854 indicates a surface magnetic field strength, characteristic age and spin-down luminosity of $2.6 \times 10^{13}$G, $13.7$ Myr and $8.2 \times 10^{28}$ erg s$^{-1}$ respectively, for a dipolar magnetic field configuration. This also places the pulsar beyond the conventional pulsar death line, where radio emission is expected to cease. The spin period of PSR J0250+5854 is similar to those of the high-energy-emitting magnetars and X-ray dim isolated neutron stars (XDINSs). However, the pulsar was not detected by the Swift/XRT in the energy band of 0.3-10 keV, placing a bolometric luminosity limit of $1.5 \times 10^{32}$ erg s$^{-1}$ for an assumed $N_{\rm H}=1.35\times10^{21}$ cm$^{-2}$ and a temperature of 85 eV (typical of XDINSs). We discuss the implications of the discovery for models of the pulsar death line as well as the prospect of finding more similarly long-period pulsars, including the advantages provided by LOTAAS for this., Comment: 16 pages, 9 figures, Accepted for publication in the Astrophysical Journal

Published
2018
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7. A millisecond pulsar discovery in a survey of unidentified Fermi $��$-ray sources with LOFAR

Author

Pleunis, Z., Bassa, C. G., Hessels, J. W. T., Kondratiev, V. I., Camilo, F., Cognard, I., Griessmeier, J. -M., Stappers, B. W., van Amesfoort, A. S., and Sanidas, S.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract

Using LOFAR, we have performed a very-low-frequency (115-155 MHz) radio survey for millisecond pulsars (MSPs). The survey targeted 52 unidentified Fermi $��$-ray sources. Employing a combination of coherent and incoherent dedispersion, we have mitigated the dispersive effects of the interstellar medium while maintaining sensitivity to fast-spinning pulsars. Toward 3FGL J1553.1+5437 we have found PSR J1552+5437, the first MSP to be discovered (through its pulsations) at a radio frequency $, 10 pages, 4 figures, published in ApJL

Published
2017
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8. A Cosmic Census of Radio Pulsars with the SKA

Author

Keane, E., Bhattacharyya, B., Kramer, M., Stappers, B., Keane, E. F., Stappers, B. W., Bates, S. D., BURGAY, MARTA, Chatterjee, S., Champion, D. J., Eatough, R. P., Hessels, J. W. T., Janssen, G., Lee, K. J., van Leeuwen, J., Margueron, J., Oertel, M., POSSENTI, ANDREA, Ransom, S., Theureau, G., and Torne, P.

Subjects
Physics, Supermassive black hole, 010308 nuclear & particles physics, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Binary pulsar, Pulsar timing array, Pulsar, Tests of general relativity, 0103 physical sciences, 010303 astronomy & astrophysics, X-ray pulsar
Abstract

The Square Kilometre Array (SKA) will make ground breaking discoveries in pulsar science. In this chapter we outline the SKA surveys for new pulsars, as well as how we will perform the necessary follow-up timing observations. The SKA's wide field-of-view, high sensitivity, multi-beaming and sub-arraying capabilities, coupled with advanced pulsar search backends, will result in the discovery of a large population of pulsars. These will enable the SKA's pulsar science goals (tests of General Relativity with pulsar binary systems, investigating black hole theorems with pulsar-black hole binaries, and direct detection of gravitational waves in a pulsar timing array). Using SKA1-MID and SKA1-LOW we will survey the Milky Way to unprecedented depth, increasing the number of known pulsars by more than an order of magnitude. SKA2 will potentially find all the Galactic radio-emitting pulsars in the SKA sky which are beamed in our direction. This will give a clear picture of the birth properties of pulsars and of the gravitational potential, magnetic field structure and interstellar matter content of the Galaxy. Targeted searches will enable detection of exotic systems, such as the ~1000 pulsars we infer to be closely orbiting Sgr A*, the supermassive black hole in the Galactic Centre. In addition, the SKA's sensitivity will be sufficient to detect pulsars in local group galaxies. To derive the spin characteristics of the discoveries we will perform live searches, and use sub-arraying and dynamic scheduling to time pulsars as soon as they are discovered, while simultaneously continuing survey observations. The large projected number of discoveries suggests that we will uncover currently unknown rare systems that can be exploited to push the boundaries of our understanding of astrophysics and provide tools for testing physics, as has been done by the pulsar community in the past.

Published
2015
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9. Arecibo Pulsar Survey Using ALFA. IV. Mock Spectrometer Data Analysis, Survey Sensitivity, and the Discovery of 41 Pulsars

Author

Lazarus, P., Brazier, A., Hessels, J. W. T., Karako-Argaman, C., Kaspi, V. M., Lynch, R., Madsen, E., Patel, C., Ransom, S. M., Scholz, P., Swiggum, J., Zhu, W. W., Allen, B., Bogdanov, S., Camilo, F., Cardoso, F., Chatterjee, S., Cordes, J. M., Crawford, F., Deneva, J. S., Ferdman, R., Freire, P. C. C., Jenet, F. A., Knispel, B., Lee, K. J., van Leeuwen, J., Lorimer, D. R., Lyne, A. G., McLaughlin, M. A., Siemens, X., Spitler, L. G., Stairs, I. H., Stovall, K., and Venkataraman, A.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The on-going PALFA survey at the Arecibo Observatory began in 2004 and is searching for radio pulsars in the Galactic plane at 1.4 GHz. Observations since 2009 have been made with new wider-bandwidth spectrometers than were previously employed in this survey. A new data reduction pipeline has been in place since mid-2011 which consists of standard methods using dedispersion, searches for accelerated periodic sources, and search for single pulses, as well as new interference-excision strategies and candidate selection heuristics. This pipeline has been used to discover 41 pulsars, including 8 millisecond pulsars (MSPs; P < 10 ms), bringing the PALFA survey's discovery totals to 145 pulsars, including 17 MSPs, and one Fast Radio Burst (FRB). The pipeline presented here has also re-detected 188 previously known pulsars including 60 found in PALFA data by re-analyzing observations previously searched by other pipelines. A comprehensive description of the survey sensitivity, including the effect of interference and red noise, has been determined using synthetic pulsar signals with various parameters and amplitudes injected into real survey observations and subsequently recovered with the data reduction pipeline. We have confirmed that the PALFA survey achieves the sensitivity to MSPs predicted by theoretical models. However, we also find that compared to theoretical survey sensitivity models commonly used there is a degradation in sensitivity to pulsars with periods P >= 100 ms that gradually becomes up to a factor of ~10 worse for P > 4 s at DM < 150 pc/cc. This degradation of sensitivity at long periods is largely due to red noise. We find that 35 +- 3% of pulsars are missed despite being bright enough to be detected in the absence of red noise. This reduced sensitivity could have implications on estimates of the number of long-period pulsars in the Galaxy., 24 pages, 13 figures, submitted to ApJ

Published
2015
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10. Timing and Interstellar Scattering of Thirty-five Distant Pulsars Discovered in the PALFA Survey

Author

Nice, D. J., Altiere, E., Bogdanov, S., Cordes, J. M., Farrington, D., Hessels, J. W. T., Kaspi, V. M., Lyne, A. G., Popa, L., Ransom, S. M., Sanpa-arsa, S., Stappers, B. W., Wang, Y., Allen, B., Bhat, N. D. R., Brazier, A., Camilo, F., Champion, D. J., Chatterjee, S., Crawford, F., Deneva, J. S., Desvignes, G., Freire, P. C. C., Jenet, F. A., Knispel, B., Lazarus, P., Lee, K. J., van Leeuwen, J., Lorimer, D. R., Lynch, R., McLaughlin, M. A., Scholz, P., Siemens, X., Stairs, I. H., Stovall, K., Venkataraman, A., and Zhu, W.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics - Solar and Stellar Astrophysics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract

We have made extensive observations of 35 distant slow (non-recycled) pulsars discovered in the ongoing Arecibo PALFA pulsar survey. Timing observations of these pulsars over several years at Arecibo Observatory and Jodrell Bank Observatory have yielded high-precision positions and measurements of rotation properties. Despite being a relatively distant population, these pulsars have properties that mirror those of the previously known pulsar population. Many of the sources exhibit timing noise, and one underwent a small glitch. We have used multifrequency data to measure the interstellar scattering properties of these pulsars. We find scattering to be higher than predicted along some lines of sight, particularly in the Cygnus region. Lastly, we present XMM-Newton and Chandra observations of the youngest and most energetic of the pulsars, J1856+0245, which has previously been associated with the GeV-TeV pulsar wind nebula HESS J1857+026., Published in the Astrophysical Journal

Published
2013

11. The missing GeV ��-ray binary: Searching for HESS J0632+057 with Fermi-LAT

Author

Caliandro, G. A., Hill, A. B., Torres, D. F., Hadasch, D., Ray, P., Abdo, A., Hessels, J. W. T., Ridolfi, A., Possenti, A., Burgay, M., Rea, N., Tam, P. H. T., Dubois, R., Dubus, G., Glanzman, T., and Jogler, T.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences
Abstract

The very high energy (VHE; >100 GeV) source HESS J0632+057 has been recently confirmed as a ��-ray binary, a subclass of the high mass X-ray binary (HMXB) population, through the detection of an orbital period of 321 days. We performed a deep search for the emission of HESS J0632+057 in the GeV energy range using data from the Fermi Large Area Telescope (LAT). The analysis was challenging due to the source being located in close proximity to the bright ��-ray pulsar PSR J0633+0632 and lying in a crowded region of the Galactic plane where there is prominent diffuse emission. We formulated a Bayesian block algorithm adapted to work with weighted photon counts, in order to define the off-pulse phases of PSR J0633+0632. A detailed spectral-spatial model of a 5 deg circular region centred on the known location of HESS J0632+057 was generated to accurately model the LAT data. No significant emission from the location of HESS J0632+057 was detected in the 0.1-100 GeV energy range integrating over ~3.5 years of data; with a 95% flux upper limit of F_{0.1-100 GeV} < 3 x 10-8 ph cm-2 s-1. A search for emission over different phases of the orbit also yielded no significant detection. A search for source emission on shorter timescales (days--months) did not yield any significant detections. We also report the results of a search for radio pulsations using the 100-m Green Bank Telescope (GBT). No periodic signals or individual dispersed bursts of a likely astronomical origin were detected. We estimated the flux density limit of < 90/40 ��Jy at 2/9 GHz. The LAT flux upper limits combined with the detection of HESS J0632+057 in the 136-400 TeV energy band by the MAGIC collaboration imply that the VHE spectrum must turn over at energies, 11 pages, 4 figures, accepted for publication in Monthly Notices of the Royal Astronomical Society (MNRAS) Main Journal

Published
2013
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12. Swings between rotation and accretion power in a millisecond binary pulsar

Author

Papitto, A., Ferrigno, C., Bozzo, E., Rea, N., Pavan, L., Burderi, L., Burgay, M., Campana, S., Di Salvo, T., Falanga, M., Filipović, M. D., Freire, P. C. C., Hessels, J. W. T., Possenti, A., Ransom, S. M., Riggio, A., Romano, P., Sarkissian, J. M., Stairs, I. H., Stella, L., Torres, D. F., Wieringa, M. H., and Wong, G. F.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

It is thought that neutron stars in low-mass binary systems can accrete matter and angular momentum from the companion star and be spun-up to millisecond rotational periods. During the accretion stage, the system is called a low-mass X-ray binary, and bright X-ray emission is observed. When the rate of mass transfer decreases in the later evolutionary stages, these binaries host a radio millisecond pulsar whose emission is powered by the neutron star's rotating magnetic field. This evolutionary model is supported by the detection of millisecond X-ray pulsations from several accreting neutron stars and also by the evidence for a past accretion disc in a rotation-powered millisecond pulsar. It has been proposed that a rotation-powered pulsar may temporarily switch on during periods of low mass inflow in some such systems. Only indirect evidence for this transition has hitherto been observed. Here we report observations of accretion-powered, millisecond X-ray pulsations from a neutron star previously seen as a rotation-powered radio pulsar. Within a few days after a month-long X-ray outburst, radio pulses were again detected. This not only shows the evolutionary link between accretion and rotation-powered millisecond pulsars, but also that some systems can swing between the two states on very short timescales., Comment: 43 pages, 9 figures, 4 table. Published by Nature on 26 Sep 2013. Includes Supplementary information. Minor differences with published version may exist

Published
2013
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13. Searches for gravitational waves from known pulsars with S5 LIGO data

Author

The LIGO Scientific Collaboration, The Virgo Collaboration, Abbott, B. P., Abbott, R., Acernese, F., Adhikari, R., Ajith, P., Allen, B., Allen, G., Alshourbagy, M., Amin, R. S., Anderson, S. B., Anderson, W. G., Antonucci, F., Aoudia, S., Arain, M. A., Araya, M., Armandula, H., Armor, P., Arun, K. G., Aso, Y., Aston, S., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Baker, P., Ballardin, G., Ballmer, S., Barker, C., Barker, D., Barone, F., Barr, B., Barriga, P., Barsotti, L., Barsuglia, M., Barton, M. A., Bartos, I., Bassiri, R., Bastarrika, M., Bauer, Th. S., Behnke, B., Beker, M., Benacquista, M., Betzwieser, J., Beyersdorf, P. T., Bigotta, S., Bilenko, I. A., Billingsley, G., Birindelli, S., Biswas, R., Bizouard, M. A., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bland, B., Boccara, C., Bodiya, T. P., Bogue, L., Bondu, F., Bonelli, L., Bork, R., Boschi, V., Bose, S., Bosi, L., Braccini, S., Bradaschia, C., Brady, P. R., Braginsky, V. B., Brau, J. E., Bridges, D. O., Brillet, A., Brinkmann, M., Brisson, V., Broeck, C. Van Den, Brooks, A. F., Brown, D. A., Brummit, A., Brunet, G., Budzynski, R., Bulik, T., Bullington, A., Bulten, H. J., Buonanno, A., Burmeister, O., Buskulic, D., Byer, R. L., Cadonati, L., Cagnoli, G., Calloni, E., Camp, J. B., Campagna, E., Cannizzo, J., Cannon, K. C., Canuel, B., Cao, J., Carbognani, F., Cardenas, L., Caride, S., Castaldi, G., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C., Cesarini, E., Chalermsongsak, T., Chalkley, E., Charlton, P., Chassande-Mottin, E., Chatterji, S., Chelkowski, S., Chen, Y., Chincarini, A., Christensen, N., Chung, C. T. Y., Clark, D., Clark, J., Clayton, J. H., Cleva, F., Coccia, E., Cokelaer, T., Colacino, C. N., Colas, J., Colla, A., Colombini, M., Conte, R., Cook, D., Corbitt, T. R. C., Corda, C., Cornish, N., Corsi, A., Coulon, J. -P., Coward, D., Coyne, D. C., Creighton, J. D. E., Creighton, T. D., Cruise, A. M., Culter, R. M., Cumming, A., Cunningham, L., Cuoco, E., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dari, A., Dattilo, V., Daudert, B., Davier, M., Davies, G., Daw, E. J., Day, R., De Rosa, R., DeBra, D., Degallaix, J., del Prete, M., Dergachev, V., Desai, S., DeSalvo, R., Dhurandhar, S., Di Fiore, L., Di Lieto, A., Emilio, M. Di Paolo, Di Virgilio, A., Díaz, M., Dietz, A., Donovan, F., Dooley, K. L., Doomes, E. E., Drago, M., Drever, R. W. P., Dueck, J., Duke, I., Dumas, J. -C., Dwyer, J. G., Echols, C., Edgar, M., Effler, A., Ehrens, P., Espinoza, E., Etzel, T., Evans, M., Evans, T., Fafone, V., Fairhurst, S., Faltas, Y., Fan, Y., Fazi, D., Fehrmann, H., Ferrante, I., Fidecaro, F., Finn, L. S., Fiori, I., Flaminio, R., Flasch, K., Foley, S., Forrest, C., Fotopoulos, N., Fournier, J. -D., Franc, J., Franzen, A., Frasca, S., Frasconi, F., Frede, M., Frei, M., Frei, Z., Freise, A., Frey, R., Fricke, T., Fritschel, P., Frolov, V. V., Fyffe, M., Galdi, V., Gammaitoni, L., Garofoli, J. A., Garufi, F., Gemme, G., Genin, E., Gennai, A., Gholami, I., Giaime, J. A., Giampanis, S., Giardina, K. D., Giazotto, A., Goda, K., Goetz, E., Goggin, L. M., González, G., Gorodetsky, M. L., Goßler, S., Gouaty, R., Granata, M., Granata, V., Grant, A., Gras, S., Gray, C., Gray, M., Greenhalgh, R. J. S., Gretarsson, A. M., Greverie, C., Grimaldi, F., Grosso, R., Grote, H., Grunewald, S., Guenther, M., Guidi, G., Gustafson, E. K., Gustafson, R., Hage, B., Hallam, J. M., Hammer, D., Hammond, G. D., Hanna, C., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Haughian, K., Hayama, K., Heefner, J., Heitmann, H., Hello, P., Heng, I. S., Heptonstall, A., Hewitson, M., Hild, S., Hirose, E., Hoak, D., Hodge, K. A., Holt, K., Hosken, D. J., Hough, J., Hoyland, D., Huet, D., Hughey, B., Huttner, S. H., Ingram, D. R., Isogai, T., Ito, M., Ivanov, A., Jaranowski, P., Johnson, B., Johnson, W. W., Jones, D. I., Jones, G., Jones, R., de la Jordana, L. Sancho, Ju, L., Kalmus, P., Kalogera, V., Kandhasamy, S., Kanner, J., Kasprzyk, D., Katsavounidis, E., Kawabe, K., Kawamura, S., Kawazoe, F., Kells, W., Keppel, D. G., Khalaidovski, A., Khalili, F. Y., Khan, R., Khazanov, E., King, P., Kissel, J. S., Klimenko, S., Kokeyama, K., Kondrashov, V., Kopparapu, R., Koranda, S., Kowalska, I., Kozak, D., Krishnan, B., Królak, A., Kumar, R., Kwee, P., La Penna, P., Lam, P. K., Landry, M., Lantz, B., Lazzarini, A., Lei, H., Lei, M., Leindecker, N., Leonor, I., Leroy, N., Letendre, N., Li, C., Lin, H., Lindquist, P. E., Littenberg, T. B., Lockerbie, N. A., Lodhia, D., Longo, M., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lu, P., Lubinski, M., Lucianetti, A., Lück, H., Machenschalk, B., MacInnis, M., Mackowski, J. -M., Mageswaran, M., Mailand, K., Majorana, E., Man, N., Mandel, I., Mandic, V., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A., Markowitz, J., Maros, E., Marque, J., Martelli, F., Martin, I. W., Martin, R. M., Marx, J. N., Mason, K., Masserot, A., Matichard, F., Matone, L., Matzner, R. A., Mavalvala, N., McCarthy, R., McClelland, D. E., McGuire, S. C., McHugh, M., McIntyre, G., McKechan, D. J. A., McKenzie, K., Mehmet, M., Melatos, A., Melissinos, A. C., Mendell, G., Menéndez, D. F., Menzinger, F., Mercer, R. A., Meshkov, S., Messenger, C., Meyer, M. S., Michel, C., Milano, L., Miller, J., Minelli, J., Minenkov, Y., Mino, Y., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Miyakawa, O., Moe, B., Mohan, M., Mohanty, S. D., Mohapatra, S. R. P., Moreau, J., Moreno, G., Morgado, N., Morgia, A., Morioka, T., Mors, K., Mosca, S., Moscatelli, V., Mossavi, K., Mours, B., MowLowry, C., Mueller, G., Muhammad, D., Mühlen, H. zur, Mukherjee, S., Mukhopadhyay, H., Mullavey, A., Müller-Ebhardt, H., Munch, J., Murray, P. G., Myers, E., Myers, J., Nash, T., Nelson, J., Neri, I., Newton, G., Nishizawa, A., Nocera, F., Numata, K., Ochsner, E., O'Dell, J., Ogin, G. H., O'Reilly, B., O'Shaughnessy, R., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Pagliaroli, G., Palomba, C., Pan, Y., Pankow, C., Paoletti, F., Papa, M. A., Parameshwaraiah, V., Pardi, S., Pasqualetti, A., Passaquieti, R., Passuello, D., Patel, P., Pedraza, M., Penn, S., Perreca, A., Persichetti, G., Pichot, M., Piergiovanni, F., Pierro, V., Pietka, M., Pinard, L., Pinto, I. M., Pitkin, M., Pletsch, H. J., Plissi, M. V., Poggiani, R., Postiglione, F., Prato, M., Principe, M., Prix, R., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Quetschke, V., Raab, F. J., Rabaste, O., Rabeling, D. S., Radkins, H., Raffai, P., Raics, Z., Rainer, N., Rakhmanov, M., Rapagnani, P., Raymond, V., Re, V., Reed, C. M., Reed, T., Regimbau, T., Rehbein, H., Reid, S., Reitze, D. H., Ricci, F., Riesen, R., Riles, K., Rivera, B., Roberts, P., Robertson, N. A., Robinet, F., Robinson, C., Robinson, E. L., Rocchi, A., Roddy, S., Rolland, L., Rollins, J., Romano, J. 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G., Woan, G., Wooley, R., Worden, J., Wu, W., Yakushin, I., Yamamoto, H., Yan, Z., Yoshida, S., Yvert, M., Zanolin, M., Zhang, J., Zhang, L., Zhao, C., Zotov, N., Zucker, M. E., Zweizig, J., Bégin, S., Corongiu, A., D'Amico, N., Freire, P. C. C., Hessels, J. W. T., Hobbs, G. B., Kramer, M., Lyne, A. G., Manchester, R. N., Marshall, F. E., Middleditch, J., Possenti, A., Ransom, S. M., Stairs, I. H., and Stappers, B.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, General Relativity and Quantum Cosmology
Abstract

We present a search for gravitational waves from 116 known millisecond and young pulsars using data from the fifth science run of the LIGO detectors. For this search ephemerides overlapping the run period were obtained for all pulsars using radio and X-ray observations. We demonstrate an updated search method that allows for small uncertainties in the pulsar phase parameters to be included in the search. We report no signal detection from any of the targets and therefore interpret our results as upper limits on the gravitational wave signal strength. The most interesting limits are those for young pulsars. We present updated limits on gravitational radiation from the Crab pulsar, where the measured limit is now a factor of seven below the spin-down limit. This limits the power radiated via gravitational waves to be less than ~2% of the available spin-down power. For the X-ray pulsar J0537-6910 we reach the spin-down limit under the assumption that any gravitational wave signal from it stays phase locked to the X-ray pulses over timing glitches, and for pulsars J1913+1011 and J1952+3252 we are only a factor of a few above the spin-down limit. Of the recycled millisecond pulsars several of the measured upper limits are only about an order of magnitude above their spin-down limits. For these our best (lowest) upper limit on gravitational wave amplitude is 2.3x10^-26 for J1603-7202 and our best (lowest) limit on the inferred pulsar ellipticity is 7.0x10^-8 for J2124-3358., Comment: 39 pages, 5 figures, Accepted in The Astrophysical Journal

Published
2009
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14. Recent Globular Cluster Searches with Arecibo and the Green Bank Telescope

Author

Ransom, S. M., Hessels, J. W. T., Stairs, I. H., Kaspi, V. M., Backer, D. C., Greenhill, L. J., and Lorimer, D. R.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We report the discovery of seven new millisecond pulsars during 20 cm searches of 19 globular clusters using the recently upgraded Arecibo Telescope and the new Green Bank Telescope (GBT). Five of the pulsars are in compact binaries, three of which are eclipsing. One of the systems is in an eccentric orbit which is almost certainly highly relativistic. Additional searches and timing observations are underway., Comment: 4 pages. To appear in "Radio Pulsars" (ASP Conf. Ser.), eds M. Bailes, D. Nice, & S. Thorsett

Published
2002
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15. 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
Full Text
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16. ionFR: Ionospheric Faraday rotation

Author

Sotomayor-Beltran, C., Sobey, C., Hessels, J. W. T., Bruyn, G., Noutsos, A., Alexov, A., Anderson, J., Asgekar, A., Avruch, I. M., Beck, R., Bell, M. E., Bell, M. R., Bentum, M. J., Bernardi, G., Best, P., Birzan, L., Bonafede, A., Breitling, F., Broderick, J., Brouw, W. N., Brueggen, M., Ciardi, B., Gasperin, F., Dettmar, R. -J, Duin, A., Duscha, S., Eisloeffel, J., Falcke, H., Fallows, R. A., Fender, R., Ferrari, C., Frieswijk, W., Garrett, M. A., Griessmeier, J., Grit, T., Gunst, A. W., Hassall, T. E., Heald, G., Hoeft, M., Horneffer, A., Iacobelli, M., Juette, E., Karastergiou, A., Keane, E., Kohler, J., Kramer, M., Kondratiev, V. I., Koopmans, L. V. E., Kuniyoshi, M., Kuper, G., Leeuwen, J., Maat, P., Macario, G., Markoff, S., Mckean, J. P., Mulcahy, D. D., Munk, H., Orru, E., Paas, H., Pandey-Pommier, M., Pilia, M., Pizzo, R., Polatidis, A. G., Reich, W., Roettgering, H., Serylak, M., Sluman, J., Stappers, B. W., Tagger, M., Tang, Y., Tasse, C., Ter Veen, S., Vermeulen, R., Reinout van Weeren, Wijers, R. A. M. J., Wijnholds, S. J., Wise, M. W., Wucknitz, O., Yatawatta, S., and Zarka, P.

17. Finding Pulsars with Einstein@Home

Author

Knispel, Benjamin, Allen, B., Cordes, J., Deneva, J., Anderson, D., Aulbert, C., Bhat, N. D. R., Bock, O., Bogdanov, S., Brazier, A., Camilo, F., Champion, D. J., Chatterjee, S., Crawford, F., Demorest, P. B., Fehrmann, H., Freire, P. C. C., Gonzalez, M. E., Hammer, D., Hessels, J. W. T., Jenet, F. A., Kasian, L., Kaspi, V. M., Kramer, M., Lazarus, P., Leeuwen, J., Lorimer, D. R., Lyne, A. G., Machenschalk, B., Mclaughlin, M. A., Messenger, C., David Nice, Papa, M. A., Pletsch, H. J., Prix, R., Ransom, S. M., Siemens, X., Stairs, I. H., Stappers, B. W., Stovall, K., Venkataraman, A., and Desvignes, G.

18. Radio Searches of Fermi LAT Sources and Blind Search Pulsars: The Fermi Pulsar Search Consortium

Author

Ray, P. S., Abdo, A. A., Parent, D., Bhattacharya, D., Bhattacharyya, B., Camilo, F., Cognard, I., Theureau, G., Ferrara, E. C., Harding, A. K., Thompson, D. J., Freire, P. C. C., Guillemot, L., Gupta, Y., Roy, J., Hessels, J. W. T., Johnston, S., Keith, M., Shannon, R., Kerr, M., Michelson, P. F., Romani, R. W., Michael Kramer, Mclaughlin, M. A., Ransom, S. M., Roberts, M. S. E., Saz Parkinson, P. M., Ziegler, M., Smith, D. A., Stappers, B. W., Weltevrede, P., and Wood, K. S.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present a summary of the Fermi Pulsar Search Consortium (PSC), an international collaboration of radio astronomers and members of the Large Area Telescope (LAT) collaboration, whose goal is to organize radio follow-up observations of Fermi pulsars and pulsar candidates among the LAT gamma-ray source population. The PSC includes pulsar observers with expertise using the world's largest radio telescopes that together cover the full sky. We have performed very deep observations of all 35 pulsars discovered in blind frequency searches of the LAT data, resulting in the discovery of radio pulsations from four of them. We have also searched over 300 LAT gamma-ray sources that do not have strong associations with known gamma-ray emitting source classes and have pulsar-like spectra and variability characteristics. These searches have led to the discovery of a total of 43 new radio millisecond pulsars (MSPs) and four normal pulsars. These discoveries greatly increase the known population of MSPs in the Galactic disk, more than double the known population of so-called `black widow' pulsars, and contain many promising candidates for inclusion in pulsar timing arrays., Comment: 2011 Fermi Symposium proceedings - eConf C110509

19. The Radio Sky on Short Timescales with LOFAR: Pulsars and Fast Transients

Author

Hessels, J. W. T., Stappers, B. W., Joeri van Leeuwen, and LOFAR

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

LOFAR, the "low-frequency array", will be one of the first in a new generation of radio telescopes and Square Kilometer Array (SKA) pathfinders that are highly flexible in capability because they are largely software driven. LOFAR will not only open up a mostly unexplored spectral window, the lowest frequency radio light observable from the Earth's surface, but it will also be an unprecented tool with which to monitor the transient radio sky over a large field of view and down to timescales of milliseconds or less. Here we discuss LOFAR's current and upcoming capabilities for observing fast transients and pulsars, and briefly present recent commissioning observations of known pulsars., Comment: 6 pages, 1 figure, to appear in the proceedings of "The Low-Frequency Radio Universe", eds. D.J. Saikia, D. Green, Y. Gupta, and T. Venturi

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